sec1 - european space agency · 2004-08-19 · chief scientist sci-a sci-sr astrophysics missions...

SP-1268

Report on the activities of the

2001 — 2002

Research and

Scientific Support

Department

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SP-1268March 2003

Report on the activities of the

Research andScientific SupportDepartment2001 – 2002

Scientific EditorK.-P. Wenzel

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ESA SP-1268 Report on the Activities of the Research and Scientific Support Department from 2001 to 2002

ISBN 92-9092-992-8ISSN 0379-6566

Scientific Editor K.-P. Wenzel

Editor A. Wilson

Published and distributed by ESA Publications Division

Copyright © 2003 by the European Space Agency

Price €30


CONTENTS

1. Introduction 5

1.1 Report Overview 5

1.2 The Role, Structure and Staffing of RSSD 5

1.3 Department Outlook 9

2. Research Activities 11

2.1 Research Support Division 13

2.2 High-energy Astrophysics Research 14

2.3 Optical/UV Astrophysics 19

2.4 Infrared/Submillimetre Astrophysics 24

2.5 Exoplanets and Stellar Environments 27

2.6 Solar Physics and Seismology 28

2.7 Heliospheric Physics 33

2.8 Plasma and Gas Environment of 36Solar System Bodies

2.9 Comparative Planetology and Astrobiology 44

2.10 Cosmic Dust and Comets 49

2.11 Development and Exploitation of Super- 54conducting Cameras for Astronomy

2.12 Advanced Sensor, Optics and Instrument 60Development Research

3. Scientific Support Activities 65

3.1 Astrophysics Missions Division 68

3.2 Solar and Solar-Terrestrial 74Missions Division

3.3 Planetary Missions Division 80

3.4 Fundamental Physics Missions Division 85

3.5 Space Telescope Operations Division 89

3.6 Science Operations and Data Systems 90Division

3.7 Science Payloads Technologies Division/ 98Science Payload and Advanced ConceptsOffice

4. Other Activities 105

4.1 Symposia and Workshops organised 105by RSSD

4.2 Science Communications 109

4.3 Other Coordination and Support Activities 110

Annex 1: Manpower Deployment 113

Annex 2: Publications (separated into 121refereed and non-refereed literature)

Annex 3: Seminars and Colloquia 153

Annex 4: Acronyms 157

3


introduction 5

1. INTRODUCTION

1.1 Report Overview

This report on the activities of the Research andScientific Support Department (RSSD, previously theSpace Science Department) covers the 2-year period of2001-2002. It is input to the Department’s AdvisoryCommittee, a group of independent external scientistsinvited by the Director of ESA’s Scientific Programme toreview the Department’s activities. It forms the basis ofthe oral reports made every second year to ESA’s SpaceScience Advisory Committee and Science ProgrammeCommittee. Through the publication of the report as an‘SP’ (Special Publication) by the ESA PublicationsDivision, the activities of the Department are brought tothe attention of the scientific community and to a broaderaudience.

These Biennial Reports have been produced since 1980.In this edition, a number of changes have beenintroduced to reflect the modified scope of activities andthe reorganisation of the Department that occurredduring the reporting period. The report is divided intofour Chapters plus four Annexes.

Chapter 1 deals with the Department’s role andorganisation. Its mandate and structure both evolvedconsiderably during the reporting period. Based on arevision of the responsibilities of the Department, thestructural changes that began at the end of 2000 werefinalised during the initial year of the present reportingperiod. A reorganisation of the whole ScientificProgramme Directorate, also affecting the Department,took place in the second year. This led to a furtherevolution to its current structure, described below. Thenames of staff, their locations, duties and scientificresearch interests are given in Annex 1.

Chapter 2 addresses the scientific research of theDepartment’s staff, broken down according to‘discipline’ rather than the divisional structure ofprevious reports. A complete listing of the scientificpapers published in the literature is given in Annex 2.Some 380 refereed papers were published during 2001and 2002, and more than 400 conference papers andother publications appeared.

Chapter 3 provides a top-level summary of the mission-related activities at Divisional level. For the fourMissions Divisions, the prime contributions to thescientific support of the various elements of the ScienceProgramme are summarised. For the two OperationsSupport Divisions, special mention is also made of thepost-operational and archiving phases. The activities ofthe Science Payloads Technology Division, whichevolved and very recently expanded into the Director-

ate’s Science Payload and Advanced Concepts Office,are included. Although formally outside the Departmentsince late 2002, the close links of this Office with theDepartment for both research and scientific supportactivities will be maintained.

Finally, Chapter 4 addresses a variety of activities carriedout by RSSD in its support role to the community. TheChapter summarises important scientific Symposia andWorkshops organised by the Department, support to theDirectorate’s science communication activities andvarious other activities.

While this Biennial Report provides perspective on thebreadth and quality of the activities of the staff, both intheir research and functional work, it is not intended to becomprehensive. Up-to-date information on the Depart-ment’s activities can be obtained at http://www.rssd.esa.int

The production and content of the report reflects theefforts of the whole Department. Special acknowledge-ment for its preparation is due to K.-P. Wenzel, whoedited the different contributions.

1.2 The Role, Structure and Staffing of RSSD

RSSD, one of the two Departments of ESA’s ScientificDirectorate, provides the direct interface to the scientificcommunity throughout all mission phases. Following in-orbit checkout and commissioning, it is also responsiblefor the management of the missions. In addition, theDepartment plays its part in the dissemination ofscientific knowledge to the public and for educationalpurposes.

The role and responsibilities of RSSD have evolvedconsiderably during the reporting period. This is clearlyexpressed through the change of its name. The primemotivation for the reorganisation was to achieve greaterefficiency and effectiveness in the provision of support tothe scientific community, particularly in the areas ofpayload technology, science operations and communica-tions. Specifically, the departmental organisation hasbeen adapted to respond to the overall strategicobjectives of the Agency, and be responsive to the needsof the science community. It was also motivated by thedesire to give more responsibility and authority to theDepartment’s scientific staff, and to provide opportuni-ties for increased mobility, while maintaining a healthyscientific environment where staff can pursue their ownresearch within a balanced programme. The role of theDepartment’s staff in support of the revised Directorate’sand Agency’s communications activities was also

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6 introduction

reconsidered. More details about the Department’s tasksare given below.

Changes to the structure of the Department wereimplemented in a three-stage process. The first phasebegan in late 2000/early 2001 with the introduction of theScience Payloads Technology Division, the ScienceOperations and Data Systems Division and a ResearchDivision. This phase was essentially completed with thearrival of the new Head of Department on 1 July 2001. Ina subsequent stage initiated in September 2001, thePlanetary Missions Division, the Solar and Solar-Terrestrial Missions Division, the Space TelescopeOperations Division and the Fundamental PhysicsMissions Division were created. Further, a reorganisationin July 2002 of the Science Directorate was started thatalso affected the structure of RSSD. In this third stageleading to the current structure, the Department’s SciencePayloads Technology Division expanded into theDirectorate’s Science Payload and Advanced ConceptsOffice. Based on the experience gained in theDepartment, the organisation of internal research wasrecently adjusted.

In essence, the role of RSSD is to ensure the best possiblescientific performance of ESA’s Science Programmemissions. To this end, the Department Head, under thedirect authority of the Director of the ScientificProgramme, is responsible for the implementation of allscience management aspects of the missions in theScience Directorate. This responsibility is carried out infull coordination with the Directorate’s Scientific

Projects Department, the Science Programme Coordina-tion and Planning Office and the Science ProjectManagement Coordination Office.

In particular, the Department is responsible for providingscientific expertise to studies and projects in all phases,and for ensuring that maximum scientific return withinpractical technical and budgetary constraints ismaintained as a target through all phases of a scientificmission. The Department also manages, through itsStudy or Project Scientists, the activities of each missionscience team.

RSSD is responsible for all aspects of science operations(definition, development, implementation and execution)through all mission phases and manages the operationsphase of missions following in-orbit commissioning,supported, as necessary, by system engineering expertisefrom the Scientific Projects Department.

In very close coordination with the Science Payload andAdvanced Concepts Office, RSSD provides scientificand payload expertise within the Agency in all phases ofscientific missions, including to other directorates of theAgency, such as the Directorate of Human Spaceflight onISS payloads. RSSD works with external science teamsto define the science requirements for studies on futurepayloads and the associated technologies, and passesthese to the Science Payload and Advanced ConceptsOffice for follow-up.

The Department provides input to the Directorate’sScience Communications Service regarding the scientificaspects of the missions, and ensures that the scientificoutput of each mission is fully exploited in a timelymanner for the benefit of public awareness and publiccommunication.

It is, of course, very important that members of the RSSDscientific staff maintain their scientific proficiency byundertaking personal research.

In order to discharge its responsibilities and tasks in anefficient manner, the Department is structured into fourMissions Divisions:

— the Astrophysics Missions Division;— the Planetary Missions Division;— the Solar and Solar-Terrestrial Missions Division;— the Fundamental Physics Missions Division;

and two Operations Support Divisions:

— the Science Operations and Data Systems Division;— the Space Telescope Operations Division.

The role and functions of the Chief Scientist, replacingthose of the previous Research (Support) Division Head,are described briefly in Section 2.1.

Figure 1.2/1: Structure of RSSD staff at the end of2002. The Science Payload and Advanced ConceptsOffice evolved from the Department’s SciencePayloads Technology Division in late 2002.

Head of Research andScientific Support

DepartmentSCI-S

Science Payload and AdvancedConcepts Office

SCI-AChief ScientistSCI-SR

Astrophysics MissionsDivisionSCI-SA

Planetary MissionsDivisionSCI-SB

Solar & Solar-TerrestrialMissions Division

SCI-SH

Fundamental PhysicsMissions Division

SCI-SP

Scientific Operations andData Systems Division

SCI-SD

Space TelescopeOperations Division

SCI-SN

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introduction 7

Table 1: RSSD Staff in Post at end of 2002.

Head of Department: A. Gimenez Admin. Assistant: C. Bingham Project Controller: R. FontaineDivisional Assistants: S. Ihaddadene, B. Schroeder, C. Villien

Chief Scientist: B.H. Foing

Astrophysics Missions DivisionJ. Clavel (Head) M. Fridlund R. Laureijs M.A.C. Perryman T. PrustiJ. de Bruin A. Heras A. Parmar G.L. Pilbratt J. TauberF. Favata P. Jakobsen

Solar and Solar-Terrestrial Missions DivisionK.P. Wenzel (Head) C.P. Escoubet B.G. Fleck* R.G. Marsden T.R. SandersonP. Brekke* M. Fehringer S. Haugan* L. Sanchez Duarte*

* located at SOHO/EOF, NASA Goddard Space Flight Center

Planetary Missions DivisionG. Schwehm (Head) R.J.L. Grard H. Laakso P. Martin R.M. SchulzA. Chicarro D.V. Koschny J.-P. Lebreton A. Ocampo L.H. Svedhem

Fundamental Physics Missions DivisionR. Reinhard (Head) Y. Jafry O. Jennrich

Space Telescope Operations DivisionD. Machetto (Head) R.A.E. Fosbury T. Boeker G. Meylan M. Robberto

A. Micol A. Clampin-Nota M. Miebach L. StanghelliniST-ECF (Garching) M.R. Rosa G. De Marchi B. Mobasher T. WiklindP. Benvenuti (Head) J. Maiz-Apellaniz P. PadovaniR. Albrecht STScI (Baltimore) H. Jenkner N. PanagiaM. Dolensky S. Arribas

Science Operations and Data Systems DivisionM.F. Kessler (Head) F. Jansen M.J. Szumlas G. Thoerner W. Wamsteker**C. Arviset** S. Ott D. Texier* A. Toni J.J. ZenderK. Bennett J. Riedinger

* located at Integral Science Data Centre Geneva; ** located at Vilspa

Integral Science OperationsL. Hansson (Head) P. Barr R. Much A. Orr J. Sternberg

ISO Data Centre (Vilspa)A. Salama (Head) C. Gry R. Lorente S. Peschke E. VerdugoP. Garcia Lario

XMM-Newton Science Operations (Vilspa)B. Altieri J.C. Gabriel M. Kirsch J. Munoz Peiro M. Santos-LleoM. Arpizou M. Guainazzi L. Metcalfe A. Pollock N. SchartelM. Ehle

Science Payload and Advanced Concepts Office (Science Payloads Technology Division)A. Peacock (Head) T. Beaufort P. Falkner D. Klinge J. RomstedtS. Andersson J.F. van der Biezen Ph. Gondoin D. Lumb L.C. SmitT. Appourchaux B.A.C. Butler J. Heida D. Martin U. TelljohannH.J. Arends A. van Dordrecht B. Johlander N. Rando J. VerveerM. Bavdaz C. Erd

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8 introduction

The new Office for Science Payload and AdvancedConcepts (having its origin in the previous SciencePayloads Technology Division) is under the directauthority of the Director of the Scientific Programme.This Office is responsible for the assessment phase andthe strategic approach for future missions, as well fornew payload technologies in support of the CosmicVision long-term Science Programme. The Office works,in close liaison with the RSSD study scientists and thescience community, to determine the science andtechnology needs of this programme. The Office is alsoresponsible for laboratory support throughout theDirectorate, including those RSSD research activitiesrequiring such support.

The current organigram of RSSD is shown in Fig. 1.2/1.The office of the Department Head is supported by abudget controller. The role and functions of the sixDivisions and of the Science Payload and AdvancedConcepts Office are further described in the sevensections of Chapter 3.

The staff of the Department (55 at the end of 2002,including the Science Payload and Advanced ConceptsOffice) hold posts within the overall ESA staff comple-ment and are funded from the RSSD budget. Staffassociated with the Science Operations Teams holdsupernumerary positions and are funded from thebudgets allocated to the Projects. By the end of 2002there was a complement of 69 supernumeraries. It shouldbe noted that, in these Teams, many contractors and oftenstaff from Principal Investigator institutes work togetherin an integrated structure. An overview of the staff in postat the end of 2002 is given in Table 1. Fig. 1.2/2 gives thedistribution of staff according to functions, integratingpersonnel from RSSD proper and the Science Payloadand Advanced Concepts Office.

Staff of the Department are located not only at ESTEC,

close to the Science Directorate’s project teams and theTechnical Directorate, but also in Villafranca (ISO andXXM-Newton science operations teams), in Garchingand Baltimore (Space Telescope Operations Division)and Greenbelt (SOHO Project Scientist Team at NASAGoddard Space Flight Center). Fig. 1.2/3 shows the distri-bution of RSSD staff according to location.

While not formally on the ESA staff complement,Internal Research Fellows, on contracts of maximum2 years and funded by the Agency’s education budget,play a major role in the Department’s research activities.Typically, some 15 Research Fellows were in post at anyone time during the reporting period. The Departmentalso hosted several Young Graduate Trainees on 1-yearcontracts, and offered numerous opportunities forTrainees and Stagiaires.

Highlights for the Department in the reporting periodinclude:

— the successful launch of Integral and the verypromising first-light images from all its instruments;

— RSSD’s contributions to the replanning of ESA’slong-term Science Programme ‘Horizons 2000’ to‘Cosmic Vision’, required after the Council atMinisterial Level in late 2001;

— the completion, testing and delivery of Co-Investigator contributions to Rosetta and SMART-1instruments;

— the approval of the Eddington and Venus Expressmissions;

— the continued excellent science return from HST,Ulysses, SOHO, Cluster and XMM-Newton in orbit;

— RSSD’s contribution to the implementation of thenew Huygens mission scenario;

— maintaining a high level of research with a signifi-cant number of publications in spite of the increasingpressure of the scientific support activities;

Figure 1.2/2: Distribution of RSSD staff according toprime function. Staff from the Science Payload andAdvanced Concepts Office are included.

Figure 1.2/3: Distribution of RSSD staff according tolocation.

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introduction 9

— the active organisation of a number of Symposia andWorkshops for the space science community.

1.3 Department Outlook

During the past 2 years, time was devoted to thereorganisation of the Department, in line with its newrole and goals. This also affected its interfaces within theoverall organisation of the Directorate to improveefficiency further. Changes were mandated by the need tofind new ways to implement the Programme, followingthe Ministerial Council in 2001. The next 2 years areexpected to see a consolidation of the present structuretogether with a further refinement of the internalworkings of the Directorate.

The Cosmic Vision 2012 Programme was approved aftera replanning exercise involving the scientific community.The challenge was to deliver as much science as possiblewhile keeping a realistic plan within the approved budgetboundaries. This implies difficult decisions for institu-tions providing payloads and a more focused role forindustry. The way to define and implement missions ischanging considerably. For example, the introduction ofproduction groups relies not only on the reuse of spaceplatforms, but also on an optimised use of teams and thetailoring of budgets and schedules to the availableresources. Examples are Eddington, incorporated into theexisting Herschel/Planck package, and Venus Express,based on Mars Express and Rosetta.

Concerning the research activities in the Department, thecoming years are an important challenge. The pressure ofthe scientific support activities continues to increaserapidly to the detriment of the time available for research– a dangerous situation that should be avoided.Following the streamlining of the internal organisation ofthe research programme at the end of 2002, it isimportant to see how these activities develop andwhether further adjustments will be necessary in the lightof experience.

Our opportunities for the analysis of data from missionsin orbit will be improved with the new opportunitiesoffered by Integral and, soon, by SMART-1 and MarsExpress. In astronomy, the data exploitation of success-ful missions such as XMM-Newton and HST or ground-based observatories continues, as well as that of dataarchives from previous missions like ISO. Solar Systemresearch flourishes, in close collaboration with partnersin the scientific community, thanks to Ulysses, SOHOand Cluster data. New flight instrumentation is underdevelopment for the COROT and STEREO missions.The arrival of Cassini at Saturn in mid-2004 and theentry of the Huygens probe into the atmosphere of Titanin early 2005 will be milestones for our researchactivities. Finally, we foresee the start of an increasedeffort in Fundamental Physics research very soon.

Scientific support activities to missions underdevelopment or study will require close attention.Continued efforts will be devoted to the preparation ofHerschel, Planck and Eddington, as well as to theEuropean contribution to JWST and to Gaia. The LISAgravitational wave observatory and its SMART-2technology mission will require special efforts in thisemerging area of space science. In the Solar Systemdomain, our activities will focus on Double Star, acooperative mission with China, and Venus Express, bothto be launched in the next 3 years. Equally, the prepara-tions for BepiColombo, travelling to Mercury, and forSolar Orbiter will need to be intensified.

One of the most important responsibilities of RSSD – thescience operations of the various scientific missions –continues to require our full attention as well as thefurther development of skills and tools to cope with anincreasingly demanding activity. The availability ofproperly processed scientific data, to the full satisfactionof the scientific community at large and valid for bothobservatory-type missions, with its high pressure fromthe scientific community, and for PI-type missions, is aclear objective and goal for the future.

The need to maintain and improve the links with researchinstitutions in Member States through active cooperativeprogrammes remains a prime goal of the Department.Another aim for the future is the support to thedevelopment of science communications and scienceeducation activities in ESA.

AcknowledgementsThe Scientific Editor acknowledges the invaluablesupport of C. Bingham, who coordinated multifariousactivities and prepared some of the Annexes. Input toChapter 2 was coordinated and compiled by T. Appour-chaux, M. Bavdaz, K. Bennett, F. Favata, B.H. Foing,M. Fridlund, J.-P. Lebreton, N. Panagia, A. Parmar,A. Peacock, A. Salama, T. Sanderson and G. Schwehm.Chapter 3 was compiled by the Heads of Division basedon the contributions from the Project Scientists.S. Ihaddadene and M. Riemens compiled the publicationlist and A. Toni provided technical support.

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11

2. RESEARCH ACTIVITIES

2.1 Research Support Division

2.2 High-Energy Astrophysics Research2.2.1 X-ray binaries2.2.2 X-ray emission from star-forming regions and

young stellar objects2.2.3 X-ray background and large-scale structure2.2.4 Deep XXM-Newton survey of the galaxy M332.2.5 The starburst-AGN connection2.2.6 The revival of fossil AGN2.2.7 X-ray spectroscopy of general relativistic effects

in AGN2.2.8 Discovery of an ionised Fe K edge in the z = 3.91

quasar APM 08279+52552.2.9 The signature of SN ejecta in the X-ray afterglow

of GRB011211

2.3 Optical/UV Astrophysics2.3.1 Stars and stellar systems2.3.2 Galaxies2.3.3 High-energy activity of radio galaxies and blazars2.3.4 Cosmological Studies

2.4 Infrared/Submillimetre Astrophysics2,4.1 ISO data exploitation2.4.2 Preparations for Planck2.4.3 Sub-mm emission of extra-galactic objects

2.5 Exoplanets and Stellar Environments2.5.1 Study of outflows in star-forming regions2.5.2 Pulsations of Beta-Pictoris stars2.5.3 Exploitation of MUSICOS2.5.4 Preparations for Eddington

2.6 Solar Physics and Seismology2.6.1 The Phoebus Group: the search for g modes

continues2.6.2 Solar activity and p modes2.6.3 The SUMER spectral atlas of solar disc features2.6.4 Oscillations above sunspots2.6.5 Self-organised criticality and solar flares2.6.6 Magnetic interaction of waves in the chromo-

sphere2.6.7 Asteroseismology

2.7 Heliospheric Physics2.7.1 Composition measurements of energetic particles

above the southern solar pole by the UlyssesCOSPIN/LET instrument

2.7.2 Propagation of solar energetic particles: analysisof the events’ decay phase

2.7.3 3He-rich events2.7.4 Observations of the Sun’s magnetic field during

recent solar maximum2.7.5 The SEPT/IMPACT instrument on the STEREO

mission

2.8 Plasma and Gas Environment of SolarSystem Bodies

2.8.1 Cluster-related research2.8.2 Electron density distribution in the Earth’s

magnetosphere2.8.3 Plasma and wave phenomena induced by neutral

gas releases in the solar wind2.8.4 Instrument developments

2.9 Comparative Planetology and Astrobiology2.9.1 Comparative planetology of Earth-like planets

and moons 2.9.2 Lunar research and SMART-1 exploitation2.9.3 Mars research 2.9.4 Impact cratering processes2.9.5 Contributions to astrobiology

2.10 Cosmic Dust and Comets2.10.1 In situ measurements of cosmic dust2.10.2 Infrared investigations of interplanetary dust

particles2.10.3 Ground-based observations of comets2.10.4 Leonid observations2.10.5 The Rosetta imaging system (OSIRIS)

2.11 Development and Exploitation of Super-conducting Cameras for Astronomy

2.11.1 Overview of activities2.11.2 The SCAM-1 programme2.11.3 The SCAM-2 programme2.11.4 The SCAM-3 programme2.11.5 The SCAM-4 programme2.11.6 The SCAM-5 programme2.11.7 The SCAM-6 programme2.11.8 SCAM programme conclusions

2.12 Advanced Sensor, Optics and InstrumentDevelopment Research

2.12.1 Compound semiconductor photon detectors2.12.2 Low-mass X-ray optics

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research activities 13

2.1 Research Support Division

Research at RSSD is an integral part of the activities ofthe scientific staff, needed to maintain and develop theirscientific skills, peer recognition and hands-onexperience in space science. Active involvement inresearch is necessary for Project Scientists to remain partof the community when performing their mission-relatedduties.

In the new RSSD structure, put in place in early 2001, theResearch Division (later renamed the Research SupportDivision) was formed to facilitate and assist incoordinating the research activities performed by staffacross the various Mission Divisions, in parallel to theirmain functional activities of scientific support toprojects. The Departmental research programme wassub-structured into thematic Research Groups. TheResearch Groups also provided a basis for the integrationand regular interaction of Research Fellows and Traineeswith staff scientists and support staff. The Head of theResearch Support Division was responsible for theoverall supervision of the Research Fellows andTrainees. He also supported the annual assessment of thescientific activities and organised annual reviews of theresults and new proposals for these activities.

The research in RSSD reflects the breadth of the CosmicVision programme in the different fields related to ESAscience missions. The activities have been influenced byopportunities given by the ESA Science Programme, butalso constrained by the limited time available to thescientists owing to an increased workload on projects,studies and other functional activities. RSSD staffconduct research collaborations with institutes from allMember States and with the international community,mostly in the areas of data exploitation from ESA andother space science missions and of instrumentdevelopment. In one or two cases, external researchersalso contribute to the scientific output of the Departmentthrough extended visits to RSSD.

Internal Research Fellows on post-doctoral contracts ofup to 2 years play a major role in the Department’sresearch activities. On average, some 15 ResearchFellows are in post at any one time, covering the largerange of topics in RSSD. They are recruited through thestandard ESA process of interviews, chaired by the Headof the Research Support Division. The excellence andpublication record of candidates, their researchprogramme matching RSSD research priorities, and thetraining opportunity at RSSD for their career prospectswere prime selection criteria. RSSD also hosted a coupleof post-doctoral researchers funded through EUEuropean Network collaborations. The Department alsohosted some Young Graduate Trainees on 1-yearcontracts, as well as Portuguese and Spanish Trainees on2-year grants funded by their respective nations. TheDepartment also offered opportunities to a number of

Stagiaires for up to 6 months, as part of their research orgraduate engineering studies, as well as to a fewexternally-supported research students. The scheme ofInternal Research Fellows, Trainees and Stagiaires,besides offering training and experience at RSSD,permits a continuous exchange and collaboration withtheir institutes of origin or of their future destinations. Anumber of Master or PhD theses were co-supervised byRSSD staff scientists and colleagues from academicinstitutions.

RSSD scientists managed to maintain a leading role inmore than a third of their research papers, despite theirfunctional workload in scientific support to projects,thanks to their commitment, collaborations withinResearch Groups and with the outside community, andthe contribution of Research Fellows. The publications in2001 and 2002 involving RSSD staff are listed inAnnex 2.

RSSD staff organised Symposia and Workshops insupport of ESA science missions or in relation toscientific themes or collaborative research topics (seeSection 4.1). They also contributed to sciencecommunications and education activities (see Section4.2), as well as to several coordination and supportingtasks (see Section 4.3). The programme of RSSDseminars, arranged by the Research Support Division(and open to other interested scientists), continued with amixture of external and internal speakers, presentingresults or reviews over a wide range of space sciencetopics (see Annex 3). The colloquia programmepresenting prestigious speakers to all ESTEC staffcontinued during the reporting period (see Annex 3). In aprogramme of informal internal seminars, RSSDscientists reported on their research activities or gavetutorials across disciplines.

Based on the experience gained during the reportingperiod and with the goal of reinforcing and maintainingthe high standard of the Departmental research prog-ramme, the research organisation was recently adjusted.At the same time, internal procedures were streamlined.The Head of the Research Support Division now fulfillsthe role of Chief Scientist, advising the Head ofDepartment on the research activities and their evalua-tion, as well as supporting science communications andrelated activities. Some adjustments to the ResearchGroups, including Lead Scientists coordinating present-ations and the availability of funds, have also beenimplemented.

The Sections following are arranged according todiscipline. They follow in general, but not systematically,the Research Group structure that existed during most ofthe reporting period.

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14 research activities

2.2 High-Energy Astrophysics Research

2.2.1 X-ray binaries

In the field of X-ray binary research, the Group has usedthe outstanding sensitivity and spectral resolution of theXMM-Newton instruments to investigate narrowabsorption features in a number of low-mass X-raybinaries (LMXRBs). These features allow the ionisationstate, location, abundance and dynamics of the accretingmaterial to be studied. Three systems have been studiedin detail: the dipping sources MXB 1659-298 andX 1624-490 and the non-dipping source GX 13+1 (Sidoliet al., 2002). It is likely that the dipping systems areviewed closer to the orbital plane than the non-dippingsystems because obscuration by material in anazimuthally-structured accretion disc is thought to beresponsible for the dipping activity.

Sidoli et al. (2001) report the discovery of narrow X-rayabsorption lines from the low-mass X-ray binaryMXB 1659-298 during an XMM-Newton observation inFebruary 2001. MXB 1659-298 is a transient, burstingX-ray source that exhibits 15-min X-ray eclipses every7.11 h. The eclipses are preceded by intense dippingactivity that lasts for about 2 h. During dips, the amountof low-energy absorption increases strongly. EPIC andRGS spectra reveal the presence of narrow resonantabsorption features identified with O VIII 1s-2p, 1s-3pand 1s-4p, Ne X 1s-2p, Fe XXV 1s-2p, and Fe XXVI 1s-

2p transitions, together with a broad Fe emission featureat 6.47 keV (Fig. 2.2.1/1). The large range of ionsimplies either that the absorbing material is present overa wide range of distances from the central source, or thatit has a large range of densities. Strangely, the equivalentwidths of the Fe absorption features show no obviousdependence on orbital phase, even during dippingintervals (Fig. 2.2.1/2). The equivalent widths of theother features are consistent with having the same valuesduring persistent and dipping intervals. This implies thatthe material responsible for the narrow absorptionfeatures is not the same as that responsible for the dips.Previously, the only X-ray binaries known to exhibitnarrow X-ray absorption lines were two superluminal jetsources and it had been suggested that these features arerelated to the jet formation mechanism. This now appearsunlikely, and instead their presence may be related to theviewing angle of the system.

An idea of the spectral complexity that XMM-Newton isbeginning to see around the iron line from low-massX-ray binaries can perhaps best be seen in an observationof the dipping source X 1624-490 reported in Parmar etal. (2002). In this source the dips repeat every 21 h andno X-ray eclipses are present. Features identified withthe K alpha absorption lines of Fe XXV and Fe XXVIare again present and their properties show no obviousdependence on orbital phase, except during a dip. Inaddition, faint absorption features tentatively identifiedwith Ni XXVII K alpha and Fe XXVI K beta might bepresent (Fig. 2.2.1/3). A broad emission feature is alsoevident. A deep absorption line is present during the dipwith an energy consistent with Fe XXV K alpha. This isthe second dipping LMXRB source from which narrowFe absorption features have been observed.

Figure 2.2.1/2: The equivalent widths of the two ironabsorption features seen in the EPIC PN spectra ofMXB 1659-298 as a function of orbital phase. There isno obvious orbital dependence, even during thedipping activity at around phase 0.8.

Figure 2.2.1/1: XMM-Newton RGS spectra in theregions around some of the narrow absorptionfeatures seen from the low-mass X-ray binaryMXB 1659-298. The arrows indicate theoreticalwavelengths.

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ReferencesParmar, A.N., Oosterbroek, T., Boirin, L., Lumb, D.,

2002, A&A 386, 910.Sidoli, L., Oosterbroek, T., Parmar, A.N. et al., 2001,

A&A 379, 540.Sidoli, L., Parmar, A.N., Oosterbroek, T., Lumb, D.,

2002, A&A 385, 940.

2.2.2 X-ray emission from star-forming regions andyoung stellar objects

X-rays are produced copiously in all stages of starformation and, thanks to their ability to penetrate theshrouds of gas and dust that obscure very young stars,they are an ideal tool to study all the stages of starformation. F. Favata and collaborators from PalermoObservatory have studied a number of young nearby star-forming regions using deep XMM-Newton observations.The high sensitivity of XMM-Newton has produced anumber of new discoveries, including the detection ofX-ray emission from protostellar jets (Herbig-Haroobjects) and the presence of significant differences in theX-ray spectral characteristics of classical and weak-linedT Tauri stars (CTTS and WTTS). Both results wereobtained in a deep XMM-Newton observation of thenearby L1551 star-forming region in Taurus.

Polar jets are a relatively common feature in very youngstars, and jets frequently feature shocked regions, asevidenced by, for example, their emission lines in the

optical and UV. Favata et al. (2002) for the first timedetected X-ray emission from a protostellar jet: HH 154.The jet originated from the highly embedded binaryprotostar IRS 5 in L1551. The high sensitivity of XMM-Newton allowed the spectrum of the X-ray source to bestudied, and its temperature to be determined. AtT ~ 4 MK, the plasma responsible for the X-ray emissionis hotter than expected from the known characteristics ofthe jet’s working surface.

Later Chandra observations (Bally et al., 2003) showedthat the X-ray emission is not from the working surface,but is displaced by about 7 arcsec. A small knot is presentin the jet near this position, which new spectroscopicobservations by Fridlund show to have a velocity a factorof 2 higher than the working surface. This, together witha lower degree of ionisation, can explain the observedhigh temperature. The X-ray luminosity of the jet sourceis, at Lx ~ 3 x 1029 erg s–1, moderate. However, as theX-rays are emitted well above the accretion disc, theycan illuminate it from above, at a high incidence angle(something which the coronal emission from the youngstar cannot do), and thus penetrate and ionise the discmaterial at significant distance from the star. Ifprotostellar jet emission turns out to be common, it couldhave a significant role in determining the accretion disc’sionisation and thus the accretion rate.

Marginal detection of some other objects of this class asX-ray sources in the Rosat database has led to aprogramme of XMM-Newton and Chandra observationsto search for X-ray emission from other HH objects (PIF. Favata), which has been approved for both missions atthe last AO round.

Whether the presence of dense discs (as in the CTTS) hasan influence on the X-ray emission of young stars hasbeen a matter of debate since Einstein observations in1981. The high XMM-Newton sensitivity has allowedfor the first time the X-ray spectral characteristics ofT Tauri stars to be studied. Favata et al. (2003) haveshown that CTTS and WTTS in L1551 have differentX-ray spectral and temporal behaviours, suggesting thatdifferent mechanisms are responsible for the dominantparts of the X-ray emission. CTTS in L1551 have a muchhigher temporal variability than do WTTS, and theircoronal abundances show a large spread of almost threeorders of magnitudes, while the coronal abundances ofWTTS are narrowly clustered around a mean valueZ ~ ZSun (even though the photospheric abundances ofthe two groups are most probably identical). Also, theWTTS show a characteristic coronal abundance pattern(with the noble gases, notably Ne, enhanced over Fe)typical of older very active stars, which the CTTS do notshare. The X-ray emission mechanism of WTTS appearsto be purely coronal in nature, while in CTTS additionalmechanisms are likely to be at play.

A clue to the nature of the X-ray emission from CTTS is

Figure 2.2.1/3: The 5.5-8.5 keV residuals from thebest-fit continuum model of X 1624-490 observedwith EPIC. A broad emission feature at 6.58 keV andtwo narrow features identified with Fe XXV K alphaand Fe XXVI K alpha absorption at 6.72 keV and7.00 keV are clearly evident. Fainter features at7.83 keV and 8.28 keV might be present and aretentatively identified with Ni XXVII K alpha andFe XXVI K beta absorption.

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provided by the very peculiar behaviour shown by theyoung CTTS XZ Tau, whose X-ray emission increasedlinearly by a factor of ~ 4 during a 50 ks XMM-Newtonobservation (Fig. 2.2.2). At the same time, the absorbingcolumn density (N(H)) decreases by a comparable factor,pointing to the modulation being dominated by ashadowing effect. The peak N(H) value is compatiblewith the typical optical thickness of the accretion stream,suggesting that the X-ray emission is probably beingconcentrated at the accretion spot and shadowed by theaccretion stream rotating in and out of the line of sight.This implies that the X-ray source is spatially compact,and it could also imply that a non-negligible fraction ofthe X-ray emission is accretion-dominated. While Favataet al. (2001) had shown that the flaring emission ofT Tauri stars is confined in relatively compact regions,this is the first evidence that the quiescent emission fromCTTS is also confined in small spatial regions.

References Bally, J., Feigelson, E.D., Reipurth, B., 2003, ApJ, in press.Favata, F., Micela, G., Reale, F., 2001, A&A 375, 485.Favata, F., Fridlund, C.V.M., Micela, G., Sciortino, S.,

Kaas, A.A., 2002, A&A 386, 204.Favata, F., Giardino, G., Micela, G., Sciortino, S., Dami-

ani, F., 2003, A&A, in press.

2.2.3 X-ray background and large scale structure

Resulting from calibration work on XMM-Newton,detailed analysis of internal EPIC instrument back-grounds was undertaken, including the effects ofmagnetospheric soft protons scattered through the mirrorsystem. The Science Operations Centre (SOC) teamproduced a compilation of ‘blank field’ high galacticlatitude pointings that have been widely used in theanalysis of extended diffuse objects. The data were alsoused in their own right to constrain the contribution ofthe cosmic diffuse X-ray background. The study offereda high-sensitivity measurement which, for the first time,transcended the energy band at ~1 keV where thegalactic and extragalactic components cross over inintensity, and concluded that the normalisation is towardsthe higher end of previously claimed results. This hasimplications for the necessity of future long-durationexposures of deep XMM-Newton and Chandra fields(Lumb et al., 2002).

D. Lumb is leading the data analysis effort in a long-termprogramme with several institutions to determine the Ωmparameter from measurements of a flux-limited sampleof high-redshift clusters. Data from the first eight clusters(median z = 0.54) have been analysed, and a luminosity-temperature function established. In comparison withlow redshift samples, the results suggest a mild evolutionin cluster parameters, leading to interesting constraintson cosmological parameters and the evolution of intra-cluster gas physics (Lumb et al., 2003). Results on thespectroscopic analysis of XMM-Newton data of thecentral 0.5/h50 Mpc regions of the clusters of galaxiesComa, A1795 and A3112, were presented in collabora-tion with the University of Alabama (Nevalainen et al.,2003). A significant warm emission component at a levelabove the systematic uncertainties is evident, and the softX-ray (0.2-2.0 keV) luminosity is 10-30% of that of thehot gas. The best-fit temperatures (0.6-1.3 keV),overdensities (200-1000) and metal abundances (0-0.15of solar) of the warm component inside the central0.5/h50 Mpc are consistent with the results of recentcosmological simulations. These results offer observa-tional support to the theories that predict a large fractionof the current epoch’s baryons are located in a warm-hotintergalactic medium.

References Lumb, D.H., Warwick, R.S., Page, M., De Luca, A.,

2002, A&A 389, 93.

Figure 2.2.2: The X-ray light curves of two X-raybright pre-main sequence stars in the L1551 cloud, asobserved by XMM-Newton. The top panel is from theWTTS V826 Tau, showing little temporal variation.The bottom panel is from the young CTTS XZ Tau,showing the steady increase in X-ray luminositydiscussed in the text.

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Lumb, D.H., Bartlett, J., Blanchard, A. et al., 2003,A&A, submitted.

Nevalainen, J., Lieu, R., Bonamente, M., Lumb, D.H.,2003, ApJ, in press.

2.2.4 Deep XMM-Newton survey of the galaxy M33

XMM-Newton performed raster observations of thebright Local Group spiral galaxy M33 as part of theTelescope Scientist’s guaranteed time and open guestobserver’s time. Being a collaboration betweenscientists at MPE Garching (D), the OsservatorioAstronomico di Brera (I) and M. Ehle, this project hadthe goal of studying the population of X-ray sourcesdown to a 0.5-10 keV luminosity of 1035 erg s–1, morethan a factor of 10 deeper than earlier Rosatobservations. EPIC spectra and hardness ratios wereused to distinguish between different source classes.Light curves confirmed the 3.45 d period of the X-raybinary X-7, led to the detection of a transient super-softsource (Xn2) and were used to search for short-termvariability. Diffuse soft X-ray emission due to very hotgas was detected in the central disc of M33 and fromthe regions of the optical bright inner spiral arms(Fig. 2.2.4).

2.2.5 The starburst-AGN connection

The analysis of Chandra data on the low-luminosityAGN in NGC 4303 gives for the first time hints on theco-existence of an intermediate to high-mass black holetogether with a young super stellar cluster in the threecentral parsecs of the galaxy. These results are the maintopic of the Ph.D. work of graduate student E. Jimenez-Bailon, supervised by M. Santos-Lleo and M. Mas-Hesse(Laeff, Spain). The study is being complemented withthe analysis of XMM-Newton data for a similar AGN,NGC 1808.

Reference Jimenez-Bailon, E., Santos-Lleo, M., Mas-Hesse, M., et

al., 2003, ApJ, submitted.

2.2.6 The revival of fossil AGN

An XMM-Newton SOC-led group (Guainazzi, 2002;Guainazzi et al., 2002) has discovered transitionsbetween states where the nuclear X-ray emission isvisible through a photo-electric screen and states wherethe X-spectrum is dominated by Compton reflection.This result suggests that at least 10% of the local AGNmay undergo quiescence phases on timescales of theorder of several years. This discovery also suggests thatX-ray obscuration in type 2 AGN occurs on a wide rangeof spatial scales, from the innermost parsec to the hostgalaxy.

References Guainazzi, M., 2002, MNRAS 329, L13.Guainazzi, M., Matt, G., Fiore, F., Perola, G.C., 2002,

A&A 388, 787.

2.2.7 X-ray spectroscopy of general relativisticeffects in AGN

The unprecedented combination of photon-collectingarea and energy resolution allows XMM-Newton tomeasure directly general relativistic effects in nearbyAGN. The emission-line profiles of photons, which areemitted in X-ray-illuminated relativistic accretion discsaround a super-massive black hole, are distorted byDoppler shift and gravitational redshifts. Guainazzi(2003) discovered the typical ‘double-horned’ relativisticprofile of the iron K-alpha fluorescence line in thebrightest Seyfert galaxy so far, ESO198-G24. Theintensity of the red peak is comparable with the intensityof the blue peak, almost at odds with standard models.The author suggests that this line originates in a single‘flare’ above the surface of the disc at about 25Schwarzschild radii from the nuclear engine.

Reference Guainazzi, M., 2003, A&A, submitted.

Figure 2.2.4: A false-colour image of the XMM-Newton EPIC raster survey of M33. The opticalextent of M33 is marked by the white ellipse.Prominent in the soft-energy band (red) are diffusehot gas, HII regions (NGC 604), foreground stars andsuper-soft sources (e.g. Xn2), in the medium band(yellow) supernova remnants (X-3), and in the hardband (blue and white) the nucleus (X-8), X-raybinaries (X-7, X-2) and background AGN (Xn1).

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2.2.8 Discovery of an ionised Fe K edge in thez = 3.91 quasar APM 08279+5255

XMM-Newton observations of the high-redshift, broadabsorption line quasar APM 08279+5255 allowed thedetection of a high column density absorber (NH ~1023 atom cm–2) in the form of a K-shell absorption edgeof significantly ionised iron (Fe XV-Fe XVIII) andcorresponding ionised lower energy absorption(Fig. 2.2.8). The findings of Hasinger et al. (2002)confirm a basic prediction of phenomenological geom-etry models for the broad absorption line outflows andconstrain the size of the absorbing region. The Fe/Oabundance of the absorbing material is significantlyhigher than the solar value, giving interesting constraintson the gas enrichment history in the early Universe.

Reference Hasinger, G., Schartel, N., Komossa, S., 2002, ApJ 573,

L77.

2.2.9 The signature of SN ejecta in the X-rayafterglow of GRB011211

The XMM-Newton observations of the gamma-ray burst(GRB) afterglow of GRB011211 were analysed by acollaboration of scientists from the University ofLeicester (UK), MSSL University College London (UK),M. Ehle and N. Schartel from the XMM-Newton SOC. Amixture of elements including magnesium, silicon,sulphur, argon and calcium was seen as X-ray emissionlines. Such elements are typical of a supernova. With amean outflow velocity of about 0.1 c, the estimatedradius of the gas shell illuminated by the GRB andglowing in X-rays of ~1015 cm implies a time delay

between the supernova and the GRB of about 4 d. Thenew results add support to one prominent model for theorigin of GRBs, that at least some GRBs are associatedwith very recent supernova. The supernova ejects asubstantial quantity of enriched material at high velocityinto the surrounding medium, which is subsequentlyilluminated by the GRB.

Figure 2.2.8: The X-ray spectrum of broad absorp-tion line quasar APM 08279+5255 at a redshift of 3.91taken with the XMM-Newton pn camera. The fit iswith a power-law model absorbed by neutral gas.

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2.3 Optical/UV Astrophysics

2.3.1 Stars and stellar systems

The mysterious outburst of the star V838 Monocerotis

The previously unknown variable star V838 Monocerotiserupted in early 2002, brightening suddenly by a factorof almost 10 000 at visual wavelengths. An expandinglight echo appeared around the star shortly afterward, asillumination from the outburst propagated into asurrounding, pre-existing circumstellar dust cloud. Thisis the first light echo seen in the Milky Way since 1936.The star and its surrounding medium have been studiedby N. Panagia and collaborators, obtaining a series ofhigh-resolution images and polarimetry of the light echowith the Hubble Space Telescope and its newly installedAdvanced Camera for Surveys (ACS).

The echo exhibits a series of arcs, whose angularexpansion rates show that the distance is greater than2 kpc. The polarimetric imaging implies an even greaterlower limit to the distance as high as 6 kpc. Both limitsmark the first time that these phenomena have been usedto constrain an astronomical distance in the Milky Way.At maximum light, the object was extremely luminous, atleast as bright as visual absolute magnitude –9.6. Thespectrum of the star during the outburst remained that ofa cool stellar photosphere, but a composite spectrumappeared as the outburst subsided. V838 Mon thusappears to represent a new class of stellar outbursts,occurring in binary systems containing a relatively hot

main-sequence star and a companion that erupts tobecome a cool supergiant. A remarkably similar eventwas seen in the Andromeda Galaxy in the late 1980s.

Stellar segregation and the dynamics of stellar clusters

G. De Marchi has studied how dynamics change thedistribution of masses in stellar clusters over time. Incollaboration with G. Andreuzzi and others, he hasprobed the globular cluster NGC 6712 and shown that itsmass function has been severely modified by the tidalfield of the Galaxy in the course of the cluster’s lifetime,to the point that the number of stars presently decreaseswith mass, in marked contrast with any known globularclusters. The study of the nucleus of this object, done incollaboration with Paltrinieri et al., has revealed a largenumber of blue straggler stars, suggesting that the clusterwas originally much more massive and that most of itsstars have been dispersed into the Galactic halo.

In collaboration with Albrow et al., G. De Marchi hasused the HST to obtain a detailed and uniform mappingof mass segregation in the globular cluster M22. Thedegree of mass segregation observed in M22 can beaccounted for by relaxation processes within the cluster,whose global mass function is flatter than the Salpeterinitial mass function and cannot be represented by asingle power law. In collaboration with Sirianni et al.(2002), De Marchi found evidence for mass segregationin a much younger cluster, NGC 330 in the SmallMagellanic Cloud. While low-mass stars are uniformly

Figure 2.3.1/1: Comparison of ACS images obtained on 20 May 2002 (left) and 28 October 2002 (right). Thestructure is dominated by a series of near-circular arcs and rings, centred on the variable star, but there are cavitiesthat become progressively asymmetric with time.

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distributed throughout the cluster, more massive objectstend to be preferentially located in the central regions.Since the age of NGC 330 is 10 times shorter than theexpected relaxation time, the observed mass segregationmust be of a primordial nature rather than dynamical andtraces the locations where stars of different mass form.

ReferencesAlbrow, M., De Marchi, G., Sahu, K., 2002, ApJ 579,

660.Sirianni, M. et al. (incl. G. De Marchi), 2002, ApJ 579, 275.

Massive stars and their environments

J. Maíz-Apellániz has studied different aspects ofmassive stars and their interaction with theirenvironment, ranging from the nearest stars to severalMpc away. The most precise measurement to date of thescale height of the early-type stellar component of theGalactic disc and of the relative position of the Sun withrespect to its midplane was produced. A new theory forthe origin of the Local Bubble was proposed andelaborated for its possible consequences on Earth. Theinteraction of two dwarf starbursts, 30 Doradus and NGC4214, with their environment was analysed and the firstreliable distance to the latter was provided. Finally, thestructural properties of the nearest massive youngclusters was analysed, a new classification scheme forthem provided, and new evidence obtained for their roleas progenitors of globular clusters.

ReferencesMaíz-Apellániz, J., Cieza, L., McKinty, J.W., 2002, AJ

123, 1307.

Mayall II = G1 in M31: giant globular cluster or coreof a dwarf elliptical galaxy?

Mayall II = G1 is one of the brightest globular clustersbelonging to M31, the Andromeda Galaxy. G. Meylan, incollaboration with Sarajedini (UFL), Jablonka (Obs.Paris), Djorgovski (Caltech), Bridges (AAO) and Rich(UCLA), obtained multicolour photometry with the WideField and Planetary camera (WFPC2) of G1 (Meylan etal., 2001). From model fitting, they determined its meanmetallicity as [Fe/H] = –0.95±0.09, which is rather highand is somewhat similar to that of 47 Tucanae. By meansof artificial star experiments, they determined that mostof the observed spread in V-I colour is due to an intrinsicmetallicity dispersion amongst the stars of G1, possiblyas a consequence of self-enrichment during the earlystellar/dynamical evolutionary phases of this cluster. Sofar, only Omega Centauri, the giant Galactic globularcluster, has been known to exhibit such an intrinsicmetallicity dispersion, a phenomenon certainly related tothe deep potential wells of these two star clusters.

The total mass of this globular cluster has been estimatedto be about 10 million solar masses or higher, whichmakes G1 more than twice as massive as OmegaCentauri, the most massive Galactic globular cluster.

Figure 2.3.1/2: The core of the stellar clusterNGC 330 in the Small Magellanic Cloud. Massivestars are found almost exclusively near the centre,where they have probably formed.

Figure 2.3.1/3: This five-WFPC2-field mosaic of 30Doradus is the most detailed ever optical image of anstarburst region. Three line-subtracted continuumfilters (F336W, WFPC2 U; F555W, WFPC2 V;F814W, WFPC2 I) are combined in chromatic orderwith two narrow-band filters (F673N, [S II]6717+6731 in the red and F656N, H-alpha in thegreen channels). The mosaic shows the central70 x 45 pc of the 30 Doradus nebula at a resolution of0.1 arcsec (0.025 pc).

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Large masses appear to correlate with conspicuousmetallicity spreads, whose origin is still unknown. In thediagnostic defined by Kormendy, G1 always falls on thesequence defined by globular clusters, and definitelyaway from the sequences defined by elliptical galaxies,bulges and dwarf spheroidal galaxies. The same is truefor Omega Centauri.

ReferencesMeylan, G. et al., 2003, AJ 122, 830.

2.3.2 Galaxies

The nuclei of late-type spiral galaxies

Boeker and collaborators continued an ongoing study ofthe central morphology of spiral galaxies. Using theWFPC2 camera aboard HST, they completed an imagingsurvey of a large and unbiased sample of late-type,bulge-less spirals. The survey established that about 75%of the observed galaxies harbour a compact and luminousstar cluster in their nuclei. The formation mechanism ofsuch clusters is unclear, especially in galaxies of lateHubble type. In these bulge-less, disc-dominatedgalaxies, the gravitational potential in the nuclear regionis nearly flat, and gravity is a very inefficient mechanismfor gas infall towards the centre. It is therefore puzzlinghow the high star-formation efficiency needed to buildsuch massive clusters can be explained. The team iscurrently deriving stellar population ages and dynamicalmasses for a large number of nuclear clusters in order tobetter constrain their star-formation history. Early resultsfrom this spectroscopic follow-up programme indicatethat many clusters are relatively young, i.e. a few100 Myr. Since this is much shorter than the timescalesfor dynamical friction processes, this is evidence that theclusters have indeed formed where they are observedtoday.

The most powerful objects in the local Universe

Ultraluminous Infrared Galaxies (ULIRGs), withbolometric luminosities Lbol ~ LIR = 1012 LSun, are themost luminous objects in the local Universe. ULIRGsshow signs of strong interactions and mergers, and theyhave large amounts of gas and dust that significantlyobscure their ionising sources. They might be the precur-sors of optical quasars, and their properties are believedto be similar to those of high redshift galaxies. Theclosest ULIRGs offer the possibility of studying in detailhow the different physical processes interplay in thesespectacular objects. They are indeed exceptional naturallaboratories. S. Arribas, in collaboration with L. Colina(CSIC) and STScI colleagues, is carrying out a prog-ramme using integral field spectroscopy combined withhigh-resolution HST imaging to obtain complete datasets for a representative sample of low-redshift ULIRGs.

During the last 2 years, they have analysed in detailseveral objects in the sample, such as Arp220 and IRAS15206+3342 (Arribas & Colina, 2002). The velocityfield and the velocity dispersion map of the warm(ionised) gas of IRAS 15206+3342 show that the optical(or infrared) nucleus is clearly offset about 5 kpc relativeto the centre of symmetry. This result could be explainedin terms of a strong inflow of gas along a tidal tail, whichis feeding the nuclear regions where young stellarclusters are forming stars at a rate of about 150 MSun/yr.The two characteristics of strong inflows and massivestarbursts are expected during the final coalescencephase of two disc galaxies with bulges.

ReferencesArribas, S., Colina, L., 2002, ApJ 573, 576.

2.3.3 High-energy activity of radio galaxies andblazars

Studies of radio galaxies

As part of a large research project aimed at investigatingthe nuclear regions of radio galaxies, Chiaberge et al.(2002) have studied UV-band HST/STIS images of 28sources from the 3CR sample. Unresolved nuclei areobserved in 10 of the 13 low-power sources (belongingto the Fanaroff-Riley I class, FR I), and in five of the 15more powerful Fanaroff-Riley II. Broad-line radiogalaxies are found to have the flattest spectral indicessimilar to those of quasars and are confined within a very

Figure 2.3.3: The central regions of 3C 270 as theyappear in the UV band HST/STIS MAMA image.Note the small (0.3 arcsec) jet-like feature emergingfrom the nucleus, projected on to the large (~100 pcscale) dusty disc.

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narrow range. This is consistent with radiation producedin a geometrically thin, optically thick accretion disc. Onthe other hand, FR I nuclei show a wide range of spectralindices. Also, a clear trend with orientation is found:sources observed almost edge-on, or with clear signs ofdust absorption, have the steepest spectra. These resultsimply that obscuration in FR I can be present, but theobscuring material is not in a ‘standard’ geometricallythick torus. The major difference between theseabsorbing structures and the classic AGN ‘tori’ resides inthe lower optical depth of the FR I obscuring material.

UV observations of the FR I radio galaxy 3C 270 withHST/STIS permitted Chiaberge et al. (2003) to discovera jet-like structure that is aligned with the jet observed inthe radio and X-ray domains. This is the first jet-likecomponent ever detected in the UV in a radio galaxywith jets lying almost on the plane of the sky. In addition,Chandra X-ray data (image and spectrum) of this sourcehave shown the presence of a faint counter-jet. Themoderate obscuration inferred from an analysis of theHST images and Chandra X-ray spectrum stronglyfavours the scenario in which a standard geometricallyand optically thick torus is not present in FR I radiogalaxies, contrary to the basic expectations from theunification scheme of AGN.

ReferencesChiaberge, M., Macchetto, F.D. et al., 2002, ApJ 571,

247.Chiaberge, M. et al. (incl. Macchetto, F.D.), 2003, ApJ

582 (2), in press.

Studies of blazars

P. Padovani, in collaboration with H. Landt (STScI),E. Perlman (UMBC), P. Giommi (BeppoSAX/ASDC)and others, has continued his work on the DeepX-ray/Radio Blazar Survey (DXRBS). DXRBS is a largeblazar sample, deeper by a factor ~20 than previouslyavailable samples. DXRBS is now ~95% identified andincludes ~350 sources. By sampling for the first time thefaint end of the radio and X-ray luminosity functions, theDXRBS blazar sample allows us to investigate the blazarphenomenon and the validity of unified schemes down torelatively low powers. Work is in progress on theevolutionary properties of the DXRBS sample.Preliminary results on the luminosity functions show aremarkable agreement with the predictions of unifiedschemes. Work is on-going on other aspects of thesurvey, particularly on the definition of a BL Lacertaeobject.

P. Padovani has also continued his work on BeppoSAXdata of blazars. Padovani et al. (2003) presented newBeppoSAX observations of four flat-spectrum radioquasars (FSRQs) having effective spectral indices typicalof high-energy peaked BL Lacs. The BeppoSAX band in

one of the sources, RGB J1629+4008, is dominated bysynchrotron emission peaking at ~ 2 x 1016 Hz, as alsoshown by its steep (energy index alphax ~ 1.5) spectrum.This makes this object the first known FSRQ whoseX-ray emission is not due to inverse Compton radiation.Two other sources display a flat BeppoSAX spectrum(alphax ~ 0.7) but with indications of steepening at lowX-ray energies. This is also supported by Rosat andmultifrequency data and a synchrotron inverse Comptonmodel, which suggests synchrotron peak frequencies~1015 Hz, typical of ‘intermediate’ BL Lacs for which thesynchrotron and inverse Compton components overlap inthe BeppoSAX band.

ReferencePadovani, P. et al., 2003, ApJ, in press.

2.3.4 Cosmological studies

Highest resolution spectroscopy of a distant galaxy

P. Padovani has worked on a high-redshift Lyman Breakgalaxy with S. Savaglio (JHU) and N. Panagia(ESA/STScI). Very Large Telescope (VLT) high-resolution observations of MS 1512-cB58 (z = 2.724,V = 20.64) have revealed, with unprecedented detailalong a galaxy sight line, the Ly-alpha forest due tointervening clouds in the intergalactic medium (IGM),with indications of a possible excess of absorption closeto the galaxy. This high-density region is at least60/h65 Mpc comoving wide, but the large Ly-alphaabsorption of the galaxy itself prevents the detection of apossible structure extending down to the galaxy. Thisexcess of Ly-alpha clouds is suggestive of two possible

Figure 2.3.4: The image of a galaxy acquired by theHST/ACS Pure Parallel Ly-alpha Emission Survey(APPLES) (upper right) is shown together with thecorresponding extracted and calibrated spectrum.

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scenarios: the presence of a supercluster of Ly-alphaclouds not associated with MS 1512-cB58 or a highdensity of gas associated with the environment ofMS 1512-cB58.

Cosmological APPLES: the ACS Pure Parallel Ly-alpha Emission Survey

In collaboration with J. Rhoads (STScI; PI) and others,Pasquali, Pirzkal, Walsh and Cristiani have started anambitious survey of high redshift Ly-alpha emitters withthe HST-ACS. The project APPLES, the ACS PureParallel Ly-alpha Emission Survey, is one of the fourapproved ACS parallel programmes for Cycle 11 thatdirectly involves ST-ECF. Its aim is to exploit thecapabilities of the grism coupled with the ACS WideField Channel, by acquiring deep spectroscopicexposures of fields at high Galactic latitude. It also takesadvantage of the spectra extraction software andwavelength/flux calibrations that have been developed atST-ECF for grism slitless spectra. The scientific return ofAPPLES (which was granted 173 HST orbits) is to studygalaxy evolution and morphology at low-to-intermediateredshifts, and to perform a census of Ly-alpha galaxies,which will be used to constrain hierarchical galaxyformation models at high redshifts. An example ofAPPLES data being taken is given in Fig 2.3.4.

GOODS at ESO/ECF

GOODS, the Great Observatories Origins Deep Survey,is an international project that aims to unite extremelydeep observations from NASA’s Great Observatories(SIRTF, Hubble, Chandra), XMM-Newton and the mostpowerful ground-based facilities, to survey the distantUniverse to the faintest flux limits across the broadestrange of wavelengths. Astronomers at ESO/ECF areputting a major effort into the ground-based optical/near-IR imaging and spectroscopy of the southern GOODSfield, the CDF-S. Large programmes have started usingthe ISAAC, FORS2 and VIMOS instruments on the VLTto obtain deep J, H and Ks images and complete,magnitude limited (R < 25) low-resolution spectroscopyof sources in the field. These data, together withsubstantial earlier data on the field, are being madepublicly available at the ESO GOODS website.

2.4 Infrared/Submillimetre Astrophysics

2.4.1 ISO data exploitation

A. Salama, in collaboration with B. Schulz and S. Ott, ina team led by Coustenis (Observatoire de Paris)continued the analysis of the ISO Titan data taken by theSWS, ISOPHOT-S and ISOCAM instruments. Thecombination of these data provides Titan’s spectrum at2.5-17 µm with resolving powers of up to 3000. Theauthors were able to detect and separate the contributionsof most of the atmospheric gases present on Titan and todetermine disc-average mole fractions. For the first time,the ν5 band of HC3N was observed and a tentativedetection of benzene was obtained (Coutenis et al.,2003).

In a project led by Mueller (MPE), and involving S. Ottand R. Siebenmorgen (ESO), Solar System objectsserendipitously observed in the ISOCAM Parallel Modeare being extracted. Many asteroids and comets havealready been found. Publications are in preparation,including the scientific interpretation of the images andthe photometry.

Figure 2.4.1/1: The proposed evolutionary sequencefor O-rich AGB stars in their way to becomePlanetary Nebulae (PN). In the left panel the wholespectral range covered by SWS (2-45 µm) is shownwhile in the right panel just the short wavelengthregion is presented, in order to show in detail the mostimportant features used in the analysis in this spectralrange.

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Based on the detailed analysis of more than 300 low-resolution IR SWS spectra at 2-45 µm in the ISO DataArchive, P. Garcia-Lario, in collaboration withJ.W. Perea Calderon (VILSPA) proposed a classificationscheme for stars evolving from the Asymptotic GiantBranch (AGB) to the Planetary Nebula (PN) stage(Garcia-Lario & Perea Calderon, 2003). The classifica-tion was made on the basis of the detection and analysisof: (i) gas phase features in the extended atmospheres ofthe AGB stars; (ii) solid-state features in the neutralcircumstellar shells surrounding the transition objects;and (iii) nebular emission lines in the ionised PN. Thisinformation, combined with the observed overall IRenergy distribution in the spectral range covered by ISOSWS, was used to determine the evolutionary stage ofeach of the sources in the sample. The results obtainedprovide a complete view of the spectroscopic evolutionexpected in this short transition phase as a function of themass of the progenitor star as the starting point for futurespectroscopic research on this field in the IR range. Thefinal goal of this research is to determine quantitativelythe effective contribution of low-mass and intermediate-mass stars to the chemical enrichment of our Galaxy.

R.J. Laureijs, in collaboration with scientists from theISO Data Centre and others, performed a 25 µmphotometric survey with ISO of a sample of 81 nearbymain-sequence stars in order to determine the incidenceof ‘warm’ discs (Laureijs et al., 2002). All stars in thesample were detected by ISO. An empirical relation toestimate the photospheric flux of the stars at 25 µm was

used. Only five stars were found (6%) with excess abovethe photospheric flux attributed to a Vega-like disc. Thelow fraction and the fact that the discs have already beenidentified at 60 µm indicate that the bulk emission comesfrom cool dust (Tdust < 120K). The study shows thatwarm debris discs (warmer than 120K) are relativelyrare. Not a single star in our sample older than 400 Myrhas a warm disc, confirming earlier results that debrisdiscs are dissipated in the first few hundred million yearsof the main-sequence. An upper limit of 2 x 10–5 Earthmasses was derived for the mass of the discs that are notdetected.

R. Siebenmorgen, E. Kruegel and R.J. Laureijs (2001)have analysed photometry, spectro-photometry andpolarisation data from ISO of NGC 1808 to understandthe IR emission of nuclear regions in galaxies. The mid-IR polarisation map is the first of its kind of anextragalactic source. To explain the mid-IR and far-IRpolarisation synchrotron radiation and scattering fromlarge grains, PAH (Polycyclic Aromatic Hydrocarbon),or small grain emission are ruled out. Emission by large(>10 nm), non-spherical grains, aligned on large scales(500 pc) by uniform magnetic fields is proposed as themajor mid-IR and far-IR polarisation driver. Mid-IRspectroscopy revealed a multitude of emission bands.PAH features longward of 13 µm are detected for the firsttime in a galaxy. The integrated absorption cross sectionsof astronomical PAH are derived which can be used forfuture dust studies. The observations are consistentlyexplained by a radiative transfer model which considers

Figure 2.4.1/2: All-sky view of ISOCAM parallel pointings in galactic coordinates. The different symbols denotedifferent instrumental configurations.

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small localised regions of warm dust in the immediatevicinity of early-type stars (hot spots). This local heatinggives rise to a significant contribution to the mid-IRcontinuum by large grains, whereas the emission of smallgraphites or small silicates is negligible. The modelindicates that NGC 1808 is not a starburst since only10% of the total luminosity comes from OB stars. This issupported by the observation that the optical depth inNGC 1808 is more than a factor 5 lower than in genuinestarbursts like M82 or NGC 253.

S. Ott, together with N. Schartel and R. Siebenmorgencontinued to exploit the ISOCAM Parallel Modeobservations. In this mode, ISOCAM observed the skyclose to the primary target of one of the three other ISOinstruments, returning one image every 25 s with 1/24thof the normal telemetry rate. Over 9000 h of such datawere taken, covering 42 square degree of the sky, with upto 500 times higher sensitivity and up to 50 times higherspatial resolution than IRAS. Sample themes forscientific exploitation are: Cosmology (7 µm galaxycounts), starburst and AGN, stellar populations, discs andasteroid thermo-physical models. A catalogue of about16 500 mid-IR objects observed with the broadband filterLW2 (centred around 6.7 µm) will be published soon.

In another collaboration, Derriere, Ott and Gastaud (2003)used a novel approach for cross-identification of ISOCAMsources with reference catalogues in the optical and in thenear-IR via a probability pattern was developed.Compared with a classical nearest-neighbour-based cross-identification, the completeness for the selected associa-tions is improved by 4%, while the reliability is boosted by10%. This method could be applied to all cross-identification problems where the probability distribution

of the observing instrument is not symmetrical, and willlead to an improvement compared with the resultsachieved by a classical nearest-neighbour approach.

ReferencesCoustenis, A., Salama, A., Schulz, B., Ott, S., Lell-

ouch, E., Encrenaz, Th., Gautier, D., Feuchtgruber, H.,2003, Icarus, in press.

Derriere, S., Ott, S., Gastaud, R., 2003, A&A submitted. Garcia-Lario, P., Perea Calderon, J.V., 2003, ESA SP-511

in press.Laureijs, R.J., Jourdin de Muizon, M., Leech, K., Sieben-

morgen, R., Dominik, C., Habing, H.J., Trams, N.,Kessler, M.F., 2002, A&A 387, 285.

Siebenmorgen, R., Kruegel, E., Laureijs, R.J., 2001,A&A 377, 735.

2.4.2 Preparations for Planck

With the support of a small team of in-house contractstaff, K. Bennett continued the development ofcomponents of the Planck Integrated Data and Informa-tion System (IDIS). This work was carried out in theframework of the Planck LFI and HFI consortia, ofwhich the Department is a member represented at Co-Ilevel by Bennett. IDIS is an infrastructure that providessoftware components for documentation, software devel-opment, process coordination (or pipeline processing)(under the responsibility of MPA, Garching) and datamanagement and access mechanisms (under the respons-ibility of OAT, Trieste). These are to be eventuallyfederated into a single entry-point system to facilitateprocessing and analysis of the Planck data (Hazell,Bennett & Williams, 2003).

The data analysis of the Planck mission is complicatedby the geographical spread of the analysis teams, which,in combination with the size and the complexity of thedata themselves, pose challenges to the consortia inanalysis of the data in a timely manner. The completeIDIS system will be available by 2004 to support thedevelopment of processing software by the Data Pro-cessing Centres (DPCs) located at many sites in Europe.

Prototypes of the major components have beendeveloped and tested. Several are in daily use and beingoperated and maintained at RSSD. Additionally, we havedeveloped several applications to exercise many aspectsof the IDIS concept ranging from data storage topixelisation methods. Prototyping of methods to use theIDIS infrastructure is key to the development of IDIS andseveral projects have been undertaken to explore andexercise both the algorithms and the IDIS concept.

RSSD has continued to participate in laying the founda-tions leading to the eventual analysis of the Planck dataset. For example, J. Tauber and K. Bennett, in collabora-tion with G. Giardino, have continued to model the

Figure 2.4.1/3: Cross-correlation of a sub-samplecovering 14 square degrees with the 2MASS PSC. Thequality enables immediate discrimination of popula-tions.

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galactic synchrotron emission and its polarisation.Giardino et al. (2002) have analysed the angular powerspectra of the Parkes radio continuum and polarisationsurvey of the southern galactic plane at 2.4 GHz. Theyfound that in the multipole range l = 40-250 the angularpower spectrum of the polarised intensity is welldescribed by a power-law spectrum with fitted spectralindex αE = 2.37±0.21. In the same multipole range theangular power spectra of the E and B components of thepolarised signal are significantly flatter, with fittedspectral indices respectively of αE = 1.57±0.12 andB = 1.45±0.12. Temperature fluctuations in the E and Bcomponents are mostly determined by variations inpolarisation angle. They combined these results withother data from available radio surveys in order toproduce a full-sky toy model of galactic synchrotronintensity and linear polarisation at high frequencies(ν ≥ 10 GHz). This can be used not only to study thefeasibility of measuring the Cosmic MicrowaveBackground polarisation with forthcoming experimentsand satellite missions, but it is also an input to thesimulations in use by the Planck teams.

G. Franco and J. Tauber, together with P. Fosabla (now atIAP, Paris), carried out detailed simulations of thepolarisation response of Planck in order to estimate theresponse to polarised signals (Franco, Fosalba & Tauber,2003). These estimates were based on a set of simulationusing a physical optics code (GRASP8) for linearlypolarised detectors at different frequencies and locationsin the Planck focal plane. They studied the inducedaberration on the sky polarisation signals as well ascalculating spurious polarisation introduced by thetelescope optics. For the Planck example, this was foundto be of the order of 0.2%.

References Franco, G., Fosalba, P., Tauber, J.A, 2003, A&A, in press.Giardino, G., Banday, A.J., Gorski, K.M., Bennett, K.,

Jonas, J.L., Tauber, J.A., 2002, A&A 387, 82.Hazell, A., Bennett, K., Williams, O., 2003, ADASS XI,

ASP Conference Proceedings Series, in press.

2.4.3 Sub-mm emission of extragalactic objects

P. Papadopoulos worked on sub-mm emission ofextragalactic objects, specifically on ‘Resolved nuclearCO(1-0) emission in APM 08279+5255: gravitationallensing by a naked cusp?’ (Lewis et al., 2002) and ‘low-excitation gas in HR 10: possible implications forestimates of metal-rich H2 mass at high redshifts’(Papadopoulos & Ivison, 2002). This work is in progress.

ReferencesLewis, G.F., Carilli, C., Papadopoulos, P., Ivison, R.J.,

2002, MNRAS 330, L15.Papadopoulos, P.P., Ivison, R.J., 2002, ApJ 564, L9.

2.5 Exoplanets and Stellar Environments

Several questions related to the existence or formation ofexoplanets have been addressed (see also Section 2.2.2).These include scientific activities in preparation forCOROT and Eddington, as well as prepatory studies tocarry out the required precursor science (e.g. studies ofexo-zodiacal dust) for Darwin. Research Group membersparticipated in the continued evaluation and developmentof the ground-based high-resolution echelle spectrographMUSICOS. They have also continued to plan work ondeveloping models regarding biomarkers on Earth-likeplanets. A large data set of HST images and spectracollected from ground exists, covering the objectsL1551, M16 (including HH216), S185 and IC1848. Anumber of publications are under preparation, but somedata still need to be reduced.

2.5.1 Study of outflows in star-forming regions

M. Fridlund continued his work in studying anddescribing, in as much detail as possible, the energeticprocesses taking place in the vicinity of forming stars.The activity occurring in the close environment of ayoung stellar object has consequences for the interactionbetween jets, outflows, small hot dusty discs and largercold (magnetised) molecular discs. This, in turn, has far-reaching implications for the formation of planetarysystems, including comets, debris discs and dust(zodiacal) clouds. A major study of the dynamicproperties of a molecular disc was published during thereporting period (Fridlund et al., 2002).

M. Fridlund continued work together with the Stockholmstar formation group. Observations were carried out withthe SEST/SIMBA (1.2 µm continuum) and with the VLT(UVES), both ESO facilities. The SEST data show aclear indication of large grains in the disc of Beta-Pictoris, indicative of large, colliding bodies in thesystem. The VLT data are being reduced and theinterpretation is starting. Atomic gas (resonance lines)have been detected in the whole 400 AU of the Beta-Pictoris disc. The velocity pattern shows considerablewarping, which could be indicative of planets. Thisresulted in one publication in conference proceedings sofar

Reference Fridlund, C.V.M., Bergman, P., White, G.J., Pilbratt, G.L.,

Tauber, J.A., 2002, A&A 382, 573.

2.5.2 Pulsations of Beta Cephei stars

A. Stankov and M. Fridlund analysed large high-resolution spectroscopic material on BW Vul, the largestamplitude Beta Cephei star known. These stars are B-type main sequence stars evolving off the main-sequence

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of the Hertzsprung-Russell diagram. The interestingthing about the pulsations seen in these stars (radialmodes) is that, in general and in this case in particular,the atmosphere pulsates with many different velocitiesand in dis-equilibrium (the van t’Hooft effect). Whilepart of the atmosphere is falling inwards, new layers areexpanding from below. As the most extreme case, BWVul shows atmospheric velocities of several hundredkm/s, an anomalous abundance of several elements(possibly indicative of a strong magnetic field). Thisanalysis is the first to include so many spectral lines, alsoleading to the best determination so far of the stellarrotational velocity. The resulting paper is beingsubmitted for publication (Stankov et al., 2003), Severalnew observing proposals have also been accepted.

ReferencesStankov, A., Fridlund, M., Ilyin, I., 2003, in Astero-

seismology across the HR Diagram, in press.Stankov, A., Handler, G., Hempel, M., Mittermayer, P.,

2002, MNRAS 336, 189.

2.5.3 Exploitation of MUSICOS

B.H. Foing and colleagues, in collaboration withmembers of the external community, published theresults of the 1998 MUSICOS campaign. For example,the non-radial pulsation, rotation and outburst in the Bestar omega Orionis were studied (Neiner et al., 2002).Foing also continued the exploitation and developmentof the MUSICOS collaboration. Use of the MUSICOSnetwork is foreseen in the areas of stellar activity,circumstellar environments, stellar pulsations andpreparatory activities for the COROT and Eddingtonmissions. Upgrading of MUSICOS/Pic du Midi(NARVAL) to same status as MUSICOS/Hawaii(ESPADON) and investigation of the possibility ofadding an IR channel to MUSICOS/La Palma (ESA-MUSICOS) are foreseen.

ReferencesNeiner, C. et al. (incl. Foing, B., Oliveira, J.,

Orlando, S.), 2002, A&A 388, 899.

2.5.4 Preparations for Eddington

One of the key goals of the Eddington mission is todetect habitable planets by the transit method. The weakand brief transit signal will be buried in a long-durationlight curve with significant noise, including the intrinsicphoton noise and astrophysical noise sources, the mostprominent being the noise from stellar activity. Aigrain &Favata (2002) developed a novel algorithm for transitdetection in light curves, based on a Bayesian approach.The algorithm has been tested (and shown to beeffective) using a solar light curve from SOHO. Carpano,Aigrain & Favata (2003) have further shown that the

activity-induced noise can be very effectively filteredfrom the light curves, so that the proposed transitdetection algorithm is quite robust, and stellar activitydoes not constitute a significant obstacle to detection ofhabitable planets. As a side product, it has also beenshown (Favata & Aigrain, 2002) that the white-lightcurves that Eddington will produce for a large number ofstars contain a wealth of information about stellaractivity, so a rich harvest of science will also be producedby Eddington in this field.

ReferencesAigrain, S., Favata, F., 2002, A&A 395, 625.Carpano, S., Aigrain, S., Favata, F., 2003, A&A in press.Favata, F., Aigrain, S., 2002, Astron. Nachr. 323, 283.

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2.6 Solar Physics and Seismology

2.6.1 The Phoebus group: the search for g modescontinues

Solar gravity oscillations (the g modes) provide essentialinformation on the physics of the solar core, wherethermonuclear reactions take place. After the launch ofSOHO in December 1995, it was quickly realised thatonly a concerted effort of the helioseismic instruments ofSOHO and of ground-based observatories might enablethe detection of the elusive g-mode. This considerationhas led to the creation of the Phoebus working groupwhich, coordinated by T. Appourchaux, involves variousinstitutes from Europe, Japan and the United States (seealso Section 4.1). The upper limit to g-mode amplitudeset in 2000 to 10 mm s–1 has now been lowered usinglonger time series and new detection techniques (Chaplinet al., 2002), and also through the formation of acollaboration with the Institut d’Astrophysique Spatiale(IAS, F), responsible for the GOLF instrument data(Gabriel et al., 2002) that was previously inaccessible tothe Phoebus group. Fig. 2.6.1 shows the new limit sets bythe Phoebus group, together with the ground-basednetwork BiSON and GOLF (Appourchaux, 2003). Thislatter limit of 3 mm s–1 is still somewhat too high for aproper detection of the g modes.

References Appourchaux, T., 2003, ESA SP-517, in press. Appourchaux, T., Andersen, B., Berthomieu, G. et al.,

2001, ESA SP-464, 467. Chaplin, W. et al. (incl. T. Appourchaux), 2002, MNRAS

336, 979. Gabriel, A. et al. (incl. T. Appourchaux), 2002, A&A

390, 1119.

2.6.2 Solar activity and p modes

Solar activity is known to affect the frequencies of the pmodes. Since this is a surface effect, the impact on the fre-

quencies is independent of the degree and of the modefrequency, provided that a proper scaling related to theinertia of the mode is performed (Chaplin et al., 2001).Solar activity also affects the linewidth and the amplitudeof the modes. Using 4 years of SOHO/LOI (LuminosityOscillations Imager) data, Appourchaux et al. (2001)showed that the linewidth increases with solar activity,while the mode amplitude decreases (Fig. 2.6.2); the totalenergy of the modes decreases with solar activity, imply-ing that the energy loss is used for generating magneticfield in active regions. With a longer data set, Appour-chaux et al. (2002) showed that surface magnetic fieldscould be directly detected in the splitting of the p modes(modes are split by rotation, advection, magnetic fieldsproducing a fine frequency structure in a mode peak).

ReferencesAppourchaux, T. et al., 2001, ESA SP-464, 71. Appourchaux, T., 2002, ESA SP-508, 47. Chaplin, W. et al. (including T. Appourchaux), 2001,

MNRAS 324, 910.

2.6.3 The SUMER spectral atlas of solar-discfeatures

A far-UV and extreme-UV (FUV, EUV) spectral atlas ofthe Sun between 670 Å and 1609 Å has been derivedfrom observations obtained with the SUMER (SolarUltraviolet Measurements of Emitted Radiation)spectrograph aboard SOHO (Curdt et al., 2001). Theatlas contains spectra of the average quiet Sun, a coronalhole and a sunspot on the disc. The spectra includeemissions from atoms and ions in the temperature range6 x 103K to 2 x 106K, i.e., continua and emission linesemitted from the lower chromosphere to the corona. Thespectral radiances are determined with a relativeuncertainty of 0.15-0.30 and the wavelength scale isaccurate to typically 10 mÅ. The atlas is also availableelectronically.

More than 1100 emission lines are available in the

Figure 2.6.1: Current upper limit for GOLF(diamond), BiSON (square) and MDI (upper twocurves) derived under the 10% probability limitdefined by the Phoebus group in 2000. The GOLFlimit is obtained by Gabriel et al. (2002) using almost6 years of data. The BiSON limit is derived for aquadruplet from Chaplin et al. (2002) using 9 years ofdata. The MDI limit is derived from Appourchaux etal. (2001) for 1 year of data; the upper curvecorresponds to the radial displacement and the lowercurve to the total displacement (radial andhorizontal). The two lines at lower right are twodifferent theoretical estimates of the g-modeamplitudes for l = 1.

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SUMER spectral range. These include resonance lines aswell as previously unobserved faint intersystem lines,which can be detected by SUMER because of its low-noise detectors. Thus, the SUMER spectral atlas providesa rich source of new diagnostic tools for probingessential physical properties of the emitting plasma andstudying electron densities, electron temperatures andelemental abundances throughout the solar atmosphere.In particular, the wavelength range below 1100 Å asobserved by SUMER represents a significant improve-ment over the spectra produced in the past.

The atlas also provides an excellent reference forastrophysical applications (Fig 2.6.3). The SUMERspectrograph permits the extensive use of spectroscopictechniques in determining temperatures, pressures,densities and velocities in the upper solar atmosphere.The atlas also presents a powerful tool for the planningof future observations.

ReferencesCurdt, W. et al. (incl. P. Brekke), 2001, A&A 375, 591.

Figure 2.6.2: Change of p-mode parameters as a function of mode frequency for various degrees of l obtainedduring the rising phase of the solar activity cycle (between 1999 and 1996). The parameters are: frequencies (top,left), linewidths (top, right), amplitudes (bottom, left), energy rates (bottom, right).

Figure 2.6.3: A close-up of a selected region of theSUMER spectral atlas, compared with the irradiancespectrum of Alpha Cen A from Hubble SpaceTelescope (HST-STIS).

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2.6.4 Oscillations above sunspots

E. O’Shea, B. Fleck and co-workers have carried out ananalysis of time-series data obtained in sunspot umbralregions. These data were obtained in the context of aSOHO Joint Observing Program (JOP 97) in September2000. This JOP included the Coronal DiagnosticSpectrometer (CDS) and the Michelson Doppler Imaging(MDI) instrument, both part of SOHO, the TRACEsatellite and various ground-based observatories. Thedata were analysed by both Fourier and wavelet time-series analysis techniques. The CDS lines used coveredthe temperature range between the low transition regionand the upper corona. From TRACE, they obtained datafrom the temperature minimum region to the lowchromosphere. MDI was used to give ‘background’magnetogram and white light context images. O’Shea etal. (2002) found that oscillations were present in theumbra at all temperatures investigated, from the tempera-ture minimum up to the upper corona. An example of the

oscillations they investigated can be seen in Fig. 2.6.4,for a single location in the sunspot umbra. Using cross-spectral analysis of Fourier spectra, time delays werefound between low- and high-temperature emission (e.g.between the TRACE 1700 emission and the CDS O Vemission). Umbral oscillations were found both insideand outside of sunspot plume locations, which indicatesthat umbral oscillations can be present irrespective of thepresence of these particular features. From a measure-ment of propagation speeds, obtained from the timedelay measurements, O’Shea and co-workers proposedthat the oscillations they observed are due to slowmagnetoacoustic waves propagating up along themagnetic field lines.

Reference O’Shea, E., Muglach, K., Fleck, B., 2002, A&A 387,

642.

Figure 2.6.4: Time series of TRACE and CDS data. Note that the factors by which each time series has been scaledare shown in the brackets to the right of the line identifications. Thick continuous line: bandpass filtered data (4-7 mHz); dot-dash line: original (unfiltered) data. The analysis concentrated on two time intervals, A and B.

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2.6.5 Self-organised criticality and solar flares

Over the last decade the paradigm of Self-OrganisedCriticality (SOC) has been considered a means ofqualitatively understanding the heating of the solarcorona through the statistics of solar flare occurrence andreleased energies (Charbonneau et al., 2001).

The slope, or index αE, of the flare energy-frequencydistribution determines the relevance of small and largeenergy events in the overall heating budget of the solarcorona. Only if its value is greater than 2 are small-scalemagnetic reconnection events (nanoflares) a viablemechanism to solve the longstanding coronal heatingproblem.

X-ray flare spectra provide values of αE, for spatiallyunresolved flares of larger energies; they typically lie inthe range ~1.5. Nanoflares are most likely to be observedas small, fast brightenings in sequences of UV/EUVimages (e.g. with SOHO’s Extreme-ultraviolet ImagingTelescope; EIT), and yield αE in the range (1.5-2.3). Thiswide range of values arises from the lack of knowledgeabout the emitting volume required to convert theobserved brightening into a measured energy.

S. McIntosh and collaborators found that the avalanchesin SOC models are fractal in nature with g ~ 1.41(McIntosh & Charbonneau, 2001; McIntosh et al., 2002).Using this, they computed a correction factor that couldbe applied to individual model-dependent observationalestimates of αE and found that the published UV/EUV-determined values of αE could be reconciled using thegeometric scaling of SOC avalanches as an adjustingparameter. They found that the adjusted values of αE liebelow, but close to, 2, in the range 1.70-1.95, and inbetter agreement with the spatially unresolved X-rayobservations.

References Charbonneau, P., McIntosh, S.W., Liu, H., Bogdan, T.J.,

2001, Sol. Phys. 203(2), 321. McIntosh, S.W., Charbonneau, P., 2001, Ap. J. Lett. 563,

165. McIntosh, S.W. et al., 2002, Phys. Rev. (E) 65, 46125.

2.6.6 Magnetic interaction of waves in thechromosphere

S. McIntosh and collaborators investigated the roleplayed by the solar magnetic field in the solarchromosphere on wave disturbances propagating throughthe atmosphere. Using data from SOHO/SUMER andSOHO/MDI, McIntosh & Judge (2001) studied a featuredubbed a ‘magnetic shadow’. They demonstrated that the‘shadow’ is co-spatial with a significant drop in emittedcontinuum intensity (~40%) and an almost completesuppression (~75%) of the characteristic 3-min oscilla-

tion of the chromosphere. This can most clearly be seenin Fig. 2.6.6 (p.32) , in about spatial position 80 at thedashed line. Their calculations, based on potential fieldextrapolations of the line-of-sight MDI magnetogram,showed that the ‘shadow’ is also co-spatial with a closedmagnetic field region that can rise to chromosphericheights (about 1 Mm and above) and thus appear in theSUMER observations. They hypothesised that themanifestation of this ‘shadow’ was due to a topologicalchange in the solar chromosphere and that the magneticconfiguration interfered with the signal formation and thepassage of chromospheric waves.

In collaboration with a group from the Institute ofTheoretical Astrophysics at the University of Oslo (N),McIntosh and colleagues used multi-dimensionalmagneto-hydrodynamic (MHD) simulations of stimula-ted oscillations in ‘realistic’ solar magnetic fieldtopologies (Bogdan et al., 2002; Rosenthal et al., 2002).They have specifically studied the role played by themagnetic field on the wave modes present in an effort toquantify the effects of the underlying magnetic topologyon mode conversion and mixing in a stratified atmos-phere like that of the Sun. The ultimate goal of thisresearch is to reproduce, by coupling the multi-dimensional MHD simulations with a detailed descrip-tion of the radiation field, the spectral signaturesobserved by SUMER (or in two-dimensions by TRACE)in order to understand features like the ‘shadow’ ofMcIntosh & Judge (2001).

References Bogdan, T.J. et al. (including McIntosh, S.W), 2002,

Astron. Nach. 323, 196.McIntosh, S.W., Judge, P.G., 2001, Ap.J. 561, 420.Rosenthal, C., et al. (including McIntosh, S.W), 2002,

Ap.J. 564, 508.

2.6.7 Asteroseismology

The use of helioseismology for inferring the internalstructure of the Sun is soon to be applied to other stars; itis in this case termed asteroseismology. RSSD has beeninvolved since the beginning in the definition of theCOROT asteroseismology mission. T. Appourchaux andB. Foing are Co-Is of COROT. This CNES-led mission,supported in part by ESA for launch in November 2005(see also Section 3.1.6) can be seen as precursor to ESA’sEddington. The prime scientific objectives of COROTare to perform asteroseismology and exoplanet detection.For asteroseismology, five stars of magnitude less than 6will be continuously observed for 150 d. The spectrum oflow-degree stellar p modes will be used for inferring theinternal structure and dynamics of these stars. In thisrespect, the scientific expertise provided by helio-seismology will be of great help to COROT for reliablefrequency determination (Appourchaux, 2003). Forexoplanet search, 5000 stars will be monitored, which

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Figure 2.6.6: The spectroscopic timeseries (space-time) provided by the MDI (panels A & B) and SUMER (panelsD-G) instruments on SOHO and TRACE (panel C). These panels are organised by the height at which the signalwas formed from top to bottom and from left to right. The location of the ‘shadow’ is shown by the dotted line(originating at spatial position x = 80). The extent of the shadow, and its effect on the signal observed, is seen inpanels (C-F) and varies dramatically as function of height in the atmosphere.

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may result in the detection of 40 planets in the range of2-5 times the size of Earth.

The RSSD contribution to COROT consists of the ModelData Processing Unit (MDPU) built in collaboration withObservatoire de Meudon (Fig. 2.6.7). The MDPU is thecentral brain of COROT, managing and massaging theoverall data stream coming from the four CCDs.

Reference Appourchaux, T., 2003, in Asteroseismology across the

HR Diagram, in press.

2.7 Heliospheric Physics

2.7.1 Composition measurements of energetic part-icles above the southern solar pole by theUlysses COSPIN/LET instrument

In November 2000, during the second southern solarpolar pass, the Ulysses spacecraft reached its highestheliographic latitude at 80.2º at a solar radial distance of~2.27 AU. In the top panel of Fig. 2.7.1, the elementalabundance ratios of carbon, nitrogen, neon and iron withrespect to oxygen observed during this polar pass, areshown. In the bottom panel of the figure, the sameelemental abundance ratios are plotted with respect toreference values for solar energetic particles (SEPs).These ratios cluster around 1, i.e. the the majority of theparticles observed at high heliographic latitudes had theirorigin in SEP events, which were found to be coronalmass ejection (CME)-driven shock accelerated (Hofer etal., 2001, 2002).

During the current, post-maximum, phase of its mission,Ulysses has encountered the return to more stable solarwind stream structures, leading to the formation ofStream and/or Corotating Interaction Regions (SIRs or

Figure 2.6.7: A COROT MDPU box. Two such boxesprovide the processing power for the scientificpayload. The MDPU will be qualified in 2003.

Figure 2.7.1: Daily averaged elemental abundanceratios (C/O, N/O, Ne/O, Fe/O) from day 250 in 2000 today 14 in 2001 as recorded by the UlyssesCOSPIN/LET instrument. Top: Absolute valuestogether with proton intensity profile (1.2-3.0 MeV).Bottom: values with respect to the reference SEPvalues together with oxygen intensity (4.25-5.25 MeV/n). The intensity profiles are represented bysolid lines. The plotted error bars in the lower paneltake the statistical error and the error of the SEPvalues into account. The triangles at the top of thepanels mark the times of the flare identification(upper panel: only X-class flares; lower: X- and M-class flares). The black arrows at the bottom of thepanels mark the times of the shock arrival at theUlysses spacecraft.

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CIRs), in addition to the CME-associated transients.During a few occasions the composition data showclearly the reoccurrence of compression regions, i.e.SIRs, which seem to accelerate interplanetary materialand do not reaccelerate the SEP particles present. Acloser analysis shows that some SIRs occur within thecharacteristic time delay of 26 d. These are thereforerecurrent SIRs, i.e. a CIR reappears around mid-2002.

ReferenceHofer M. et al., 2001, Proc.27th Int. Cosmic Ray Conf.,

8, 3116.Hofer M. et al., 2002, Geophys. Res. Lett. 29(16),

10.1029/2002GL014944.

2.7.2 Propagation of solar energetic particles;analysis of the events’ decay phase

The conditions in the interplanetary medium in theheliosphere change on large scales with the solar cycleand on small scales with the passage of transientphenomena, e.g. outward propagating modulationbarriers, and also with heliospheric distance. In order toachieve an insight in the changes in the interplanetarymedium, M. Hofer and colleagues analysed the variationof the decay phases of large SEP events that are directlyinfluenced by the conditions in space.

The intensity-time profile of an SEP event has an onset

phase and a decay phase. The analysis of Hofer et al.(2003) concentrates on the decay phase. The decay of themaximum amplitude can be described by an exponentialdecay function The time duration and the slopes of thedecay phases of different events and for different energyranges were derived. In Fig. 2.7.2 the estimated eventduration for the selected events recorded at Ulysses areplotted as a function of heliocentric distance. The eventduration increases from around 10 d to about 50 d withincreasing radial distances. This general trend isconfirmed by adding a value averaged over the sameevents observed with the Uleis instrument on ACEorbiting the L1 point (1 AU).

The authors conclude that events observed father out lastlonger. Furthermore, higher average energy means ashorter event duration. The slope of the decay phasedecreases with heliocentric distance.

The onset time interval of the SEP events, which wasusually shorter than the decay phase, has been the objectof another recent joint analysis led by S. Dalla ofImperial College, London (Dalla et al., 2003).

ReferenceDalla, S., Hofer, M.Y., Marsden, R.G., Sanderson, T.R.

et al., 2003, Proc. Solar Wind 10, in press.Hofer, M. et al., 2003, Proc. Solar Wind 10, in press.

2.7.3 3He-rich events

A systematic survey of Ulysses COSPIN/LET pulseheight data has identified 12 3He-rich events since thestart of the mission. These events have been defined byperiods during which the ratio of 3He to 4He issignificantly greater than the Solar System value of0.0004. The spatial distribution of the events spanheliocentric distances to 5 AU and helio-latitudes up to50º, providing the first in situ observations of non-ecliptic energetic 3He populations.

Figure 2.7.3 shows the Ulysses trajectory plotted as afunction of heliocentric distance and helio-latitude fromlaunch to May 2002. The second orbit is slightlydisplaced from the true orbit in order to separate it fromthe first pair of polar passages for clarity. Colour-codedalong the Ulysses trajectory is the pulse height derived 4-6 MeV/n helium intensity measured by COSPIN/LET.The 12 periods of 3He enrichments identified are labelledas events A to L. Events A-G took place during the in-ecliptic transfer to Jupiter (launch to February 1992), andthe remaining events (H-L) were seen during the high-latitude phase of the mission.

The 3He rich events are seen only during the active phaseof the solar cycle but are not associated with periods ofthe highest SEP intensities. There appears to be no directcorrelation between the occurrence of these events with

Figure 2.7.2: Duration of the MeV particle eventrecorded in the lower energy range (1.0-5.0 MeV/n)by Ulysses as a function of solar radial distance. Theaverage value based on ACE data (0.64-0.91 MeV/n)is added to the plot.

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any salient features in the magnetic field or solar wind,which (if present) might indicate particle confinement oran association with interplanetary travelling shocks.Association of the events with solar X-rays and radioemissions may provide direct evidence for a coronalorigin for the 3He ions.

2.7.4 Observations of the Sun’s magnetic fieldduring the recent solar maximum

T.R. Sanderson, T. Appourchaux and US colleagues haveanalysed a comprehensive set of solar data to show howthe magnetic field of the Sun and the associated coronalholes varied through the last two solar cycles, and inparticular the recent solar maximum (Sanderson et al.,2003).

The behaviour of the dipole term and the quadrupoleterm were analysed, and a new way of visualising themwas developed. This shows the manner in which thedipole rotates once every 22-year cycle, and also how thequadrupole varies around solar maximum.

Combining coronal hole outline data with the magneticfield data reveals that the sites of the coronal holes moveacross the Sun’s disc in sympathy with the motion of thepoles of the dipole, and also that when the poles of thequadrupole become apparent, the coronal holes break upinto smaller, like-polarity groups of holes.

The way in which this influences the distribution of high-speed solar wind flow in the heliosphere, how it

influences the location of the current sheet, how thestructure of the current sheet changes with time, and howall of this propagates into the heliosphere have importantimplications for the propagation and acceleration ofenergetic particles.

ReferenceSanderson, T.R., Appourchaux, T., Hoeksema, J.T.,

Harvey, K.L., 2003, J. Geophys. Res. in press.

2.7.5 The SEPT/IMPACT instrument on theSTEREO mission

The IMPACT (In-situ Measurements of Particles AndCME Transients) investigation forms part of the payloadof the two STEREO spacecraft. STEREO is a NASAmission of considerable interest to European scientists.Its prime science goals address the 3D corona and solarwind structure, CME origins, CME interplanetaryevolution, solar-terrestrial coupling, solar energeticparticle acceleration and the solar magnetic flux cycle.

The IMPACT investigation will perform comprehensivein situ measurements to complement the remote-sensingmeasurements. It will be provided by a large transatlanticinternational consortium under the leadership ofJ. Luhman (UCB, US). The Solar Energetic ParticleTelescope (SEPT) is being developed by RSSD in closecooperation with the University of Kiel (D).

SEPT consists of two identical units (SEPT-NS and

Figure 2.7.3: He intensity measured by COSPIN/LETalong the Ulysses trajectory.

Figure 2.7.5/1: The SEPT Engineering Model. Theanalogue board with two PDFE ASICs is shown atupper left. The board carries two additional ASICs onthe backside. The digital board with the FPGA (Actel54SX32) on its frontside is shown at lower right. Thetwo RAMs placed on the backside are not visible.

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SEPT-E). Four detectors are used in two oppositeoriented telescopes, either in north-south (NS) or ecliptic(E) orientation. SEPT uses a miniaturised electronicsbased on a Mixed Analogue/Digital Application SpecificIntegrated Circuit (ASIC) which has been developedunder the ESA General Support Technology Programme.Each telescope is made up of 300 µm-thick PIPSdetectors (D1 and D2 provided by the University of Kielas well as the housing) with guard rings and cross-talkrings. One Particle Detector Front-End (PDFE)integrated circuit is used to analyse the signal from D1,using the guard ring in anti-coincidence. A second PDFEis used to analyse the signal from D2 in anti-coincidencewith its guard ring. Furthermore, anti-coincidencesignals between D1 and D2 ensure that an exclusive‘OR’ function is performed, i. e. only stopping particlesare analysed. In a special calibration mode, this exclusive‘OR’ is inhibited in order to use minimum ionisingparticles for on-station calibration. The resolution on thefull range of energy (2.2 MeV for protons) is 8 bits,limited on board to 5 bits, logarithmically scaled fortelemetry reasons.

The development of the instrument is well underway(Figs. 2.7.5). The Critical Design Review was recentlyheld; the Engineering Model is being assembled inhouse. The critical ASIC has now been evaluated andshown to be capable of reaching the required noise level.

2.8 Plasma and Gas Environment of Solar SystemBodies

The structure and dynamics of the plasma environmentsof various bodies in the Solar System were investigatedby analysing measurements collected by instrumentsdeveloped with RSSD’s involvement. One of the mainresearch activities was related to Cluster data analysisand maintaining the ESA Cluster Data Centre. Thestructure and dynamics of atmospheres were alsoinvestigated, including the ionospheres of Earth, Mars,Venus, Titan and comets as well as electrical propertiesof planetary body surfaces and their coupling with theatmosphere (Mars, Titan, comets) or with the solar wind(Mercury, Moon). In the near future, we will look toparticipation in the challenging BepiColombo mission.

On the application side, the Group was concerned aboutinteractions between space vehicles and their environ-ments. The main issues studied were spacecraft-plasmainteraction and spacecraft charging; atmosphericelectricity, winds and interaction with descent probes;surface electrical properties, lander charging and lander/surface electrical interaction; effects of solar electricpropulsion.

2.8.1 Cluster-related research

Observations in the mid-altitude cusp

P. Escoubet, M. Fehringer, H. Laakso, A. Masson andexternal collaborators worked on Cluster observations inthe polar cusp. The polar cusp is a huge funnel in theEarth’s magnetic field where particles from the Sun canenter directly and reach the atmosphere. There istypically one cusp in each hemisphere. Some theoreticalstudies predicted a few years ago that the polar cuspcould sometimes split, giving rise to a double cusp. Suchan example was found and analysed by P. Escoubet andcollaborators.

When the Cluster orbit has its apogee on the nightside,the spacecraft cross the mid-altitude polar cuspsuccessively as a ‘string of pearls’ (left panel ofFig. 2.8.1/1) and therefore temporal changes can bemeasured, for the first time observed by spacecraft.During this cusp crossing three spacecraft (SC1, SC2,SC4) were a few minutes apart, while SC3 lagged byabout 45 min. The right panel of Fig. 2.8.1/1 shows theion precipitation in the cusp observed by three spacecraftat altitudes of 4-6 RE. The polar cusp is characterised bythe decrease of the energy of the ions as the spacecraftmoved poleward (typical for IMF Bz negative). SC4 andSC1 observed approximately the same ion dispersion,although it was seen longer by SC1, whereas SC3observed a double dispersion. First there was a decreasein energy of the ions for about 30 min and then a seconddecrease (starting around 1645 UT) lasting about 45 min.

Figure 2.7.5/2: Calibration spectra obtained with theSEPT breadboard model, using the electronconversion lines of a Bismuth 207 source. At top right,the position of the source with respect to the detectorsis represented. The green curve is related to CS1, thecentre segment of D1. The red curve shows the countrate observed in CS2, the centre segment of D2. Theblue curve is related to XT1, the cross-talk ring of D1.The K conversion lines are nicely resolved (FWHM~27 keV). The different lines are also visible in CS2,shifted by ~110 keV, the average energy deposited byelectrons that traverse D1.

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Since the four spacecraft were almost at the same localtime, this observation is clearly a temporal effect.Something changed around 1645 UT that reconfiguredthe polar cusp and moved it poleward. The IMF had anegative Bz component during the interval with a strongBy component. However, an excursion to Bz positive wasobserved around 1645 UT, which most likely producedthe motion of the cusp.

A simulation of the magnetosphere by a magneto-hydrodynamic code will be compared to the data to betterunderstand these temporal events in the cusp. Thisexample clearly demonstrates the Cluster capabilities toobserve how the polar cusp is moving and changingaccording to external solar wind changes.

VLF and ELF waves near the plasmasphere

The Earth’s plasmasphere is an inner magnetosphericregion located above the ionosphere, which typicallyextends out to L = 3-6, depending on the magnetosphericactivity. Its topology can be seen as a toroidal belt aroundthe Earth where the density is relatively high(>100 cm–3), compared to the outer tenuous magneto-spheric plasma (few cm–3). Near the outer region of the

plasmasphere, the plasma drift changes from co-rotationinto convection. The geomagnetic-field-aligned outerboundary of the plasmasphere, which separates these twoplasma regimes, is usually called the plasmapause.

Various Very Low Frequency (VLF, 3.0-30 kHz) andExtremely Low Frequency (ELF, 0.3-3.0 kHz) wavespropagate in the vicinity of the plasmapause, and inparticular near the geomagnetic equator, in a mode ofpropagation called the whistler mode (whistlers, hiss,chorus). These waves, through wave-particle inter-actions, can scatter radiation belt electrons from theirorbits. These electrons may precipitate in the upperatmosphere and create auroras. As a consequence, thelocalisation of their source regions, their propagation,occurrence and dependence upon the geomagneticactivity are fundamental issues. Moreover, these wavesare also observed in the plasmaspheric region of otherplanets of the Solar System (e.g. Jupiter, Saturn,Neptune).

The Cluster mission provides excellent opportunities tostudy whistler mode waves as the spacefleet crosses theequatorial plane, in the vicinity of the plasmapause, ateach perigee pass. Both the WBD and WHISPERexperiments show a variety of structured ELF and VLF

Figure 2.8.1/1: Crossing of the mid-altitude cusp (around 5 RE altitude) successively by the Cluster spacecraft on30 August 2001. The positions of the spacecraft are shown in the left panel and the ion precipitation measured byCIS on SC4, SC1 and SC3 are shown in the right panel.

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Figure 2.8.1/2: Top panel: plasma frequency deduced from WHISPER below 80 kHz and from the EFW spacecraftpotential measurements above 80 kHz on 5 June 2001 between 2145 UT and 2335 UT. Middle panel: WHISPERelectric field spectrogram. The hiss-like emissions are well ducted inside the electron cavities (see dotted lines).Bottom panel: high-resolution WBD data corresponding to a shorter time interval.

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emissions in this region. Research conducted at RSSD byO. Moullard, H. Laakso and A. Masson in collaborationwith external colleagues, allowed the identification of anew whistler mode wave called banded-hiss emission(BHE) at frequencies below the electron cyclotronfrequency but above the lower hybrid resonancefrequency (Moullard et al., 2002). The new methodemployed in this case study allows extraction of theelectron density from the spacecraft potential, measuredby the electric field instrument EFW, and the activemeasurement of the density by the WHISPER relaxationsounder. Results from this case study are displayed inFigure 2.8.1/2.

A statistical survey has since been conducted andidentified around 30 cases in Cluster data. This surveyshowed that 1) the location of these waves is stronglycorrelated with the position of the plasmapause, 2) theircentral frequency varies from 2 kHz to 10 kHz, with a 1-2 kHz bandwidth, depending on the geomagnetic activity(Kp), (3) their magnetic latitude is included in the [–20°,20°] range and 4) these waves are sometimes guided inlarge detached density structures. The unique Clusterfacility of multi-point measurements has beensystematically used to estimate the spatial extent and thetemporal behaviour of these waves. Moreover, whenthese waves reach frequencies below 4 kHz, the analysisof the STAFF experiment data reveals that they are of thewhistler mode type, escaping from the geomagneticequator.

ReferenceMoullard, O. et al., 2002, Geophys. Res. Lett. 29(20),

1975.

High time resolution measurements of electron densityby the EFW experiment

For accurate measurements of electric fields, the Cluster-EFW spherical double probes are electronicallycontrolled to be set at a positive potential ofapproximately 1 V relative to the ambient magneto-spheric plasma. The spacecraft itself acquires a potentialthat balances photoelectrons escaping to the plasma andthe electron flux collected from the plasma.

The probe-to-spacecraft potential difference can bemeasured with a time resolution of a fraction of a second.It provides information on the electron density over awide range from the lobes (~0.01 cm–3) to themagnetosheath (>10 cm–3) and the plasmasphere(>100 cm–3).

This technique has been calibrated against other densitymeasurements on GEOS, ISEE-1, CRRES, Geotail andPolar. The Cluster spacecraft potential measurements,open for new approaches, particularly near boundariesand gradients, provide information never obtained

before. Preliminary calibrations against other densitymeasurements on Cluster has been done and moredetailed investigations will be performed in the future.

Figure 2.8.1/3 presents Cluster measurements for theelectron density vs. spacecraft potential relationship. Thedata are collected in various magnetospheric regions, anda good relationship appears between these twoparameters.

ReferencePedersen, A. et al. (incl. Escoubet, C.P., Laakso, H.),

2001, Ann. Geophys. 19, 1483.

Spacecraft potential control with ASPOC

M. Fehringer and P. Escoubet were involved in theoperations of the ASPOC instrument on Cluster. Theobjective of this instrument is to move the spacecraftpotential near the plasma potential in order to performlow-energy ion and electron measurements. The Clusterspacecraft potential varies from a few volts positive inthe magnetosheath to 50-60 V in the tenuous magneto-spheric lobes. When the potential reaches high values,the ions below that energy can no longer be measuredand the low-energy electrons are accelerated to the valueof the spacecraft potential. ASPOC can reduce the

Figure 2.8.1/3: Electron density measured byWHISPER given as a function of the spacecraft toprobe potential difference, Vs-Vp, derived from EFWobservations. A similar relationship is shown forcomparison, from the Polar satellite (Pedersen et al.,2001).

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spacecraft potential typically to around 8 V or lower byemitting a beam of indium ions.

Under certain conditions, such as intense coldionospheric outflow events in the polar cap, a wakeparallel to the magnetic field can appear due to highspacecraft potential, which can perturb electric fieldmeasurements with wire booms. Fig. 2.8.1/4 shows theelectric field measurements by two complementarymethods: with wire booms (EFW) and an electron gun(EDI). The electron gun is not influenced by thespacecraft potential since electrons have a much higherenergy (1.5 keV) than the spacecraft potential, and thewake cannot affect the motion of the energetic electrons.It is clearly seen that the two methods agree very wellwhen ASPOC is turned on (after 04:23 UT on Cluster 3).The agreement is not good on Cluster 1, where ASPOCis not operated. In most regions, however, the agreementbetween the two methods is good even when ASPOC isoff. Further work is therefore needed to better understandthe situations where the wire boom measurements maynot be applicable.

ReferenceTorkar, K. et al. (incl. Escoubet, C.P., Fehringer, M.),

2001, Ann. Geophys. 19, 1289.

2.8.2 Electron density distribution in the Earth’smagnetosphere

The total electron number density is a key parameterneeded for both characterising and understanding thestructure and dynamics of the magnetosphere. Thespatial variation of the electron density and its temporalevolution during different geomagnetic conditions andseasons reveal numerous fundamental processes

concerning Earth’s space environment and how itresponds to energy and momentum transfer, both inresponse to the solar wind, as well as to internal sources,such as the ionosphere.

Although the electron density in the magnetosphere isknown in a general sense from case studies, large-scale,systematic studies of the electron density distribution inthe magnetosphere have been performed only a fewtimes in the past. Consequently, the models of themagnetospheric plasma density are much poorer thanthose for the magnetic field. The latter have been underdevelopment for many decades and have benefited fromthe fact that almost every scientific satellite in themagnetosphere has carried a magnetometer.

Plasma density measurements are more difficult to obtainin a systematic sense from a single instrument, since theplasma density and temperature might typically varyover several orders of magnitude. There are a number oftechniques for measuring the total plasma numberdensity, but each technique has its own limitations.Spacecraft charging seriously limits the direct detectionof low-energy charged particles and must be taken intoaccount for a variety of instruments. Furthermore,photoelectrons and secondary electrons can cause asignificant increase.

Using spacecraft potential measurements of the Polarelectric field experiment, H. Laakso and colleagues haveinvestigated electron density variations of key plasmaregions within the magnetosphere, including the polarcap, cusp, trough, plasmapause and auroral zone,attempting to model how the electron density varies inspace under various conditions. The research in this areahas been very active, which is reflected in a series ofpublications.

ReferencesJanhunen, P. et al., 2001, Adv. Space Res. 28 (11), 1575.Janhunen, P. et al., 2002, Ann. Geophys. 20, 1743.Laakso, H., 2002, J. Atmos. Sol. Terr. Phys. 64, 1735.Laakso, H. et al., 2001, J. Atmos. Sol. Terr. Phys. 63,

1171.Laakso, H., Grard, R., 2002, Space Weather Study Using

Multi-Point Techniques, COSPAR Coll. Ser., p.193.Laakso, H. et al., 2002a, Ann. Geophys. 20, 1711.Laakso, H. et al., 2002b, Ann. Geophys. 20, 1725.Palmroth, M. et al., 2001, J. Geophys. Res. 110, 21109.

2.8.3 Plasma and wave phenomena induced byneutral gas releases in the solar wind

H. Laakso and colleagues have investigated plasma andwave disturbances generated by nitrogen (N2) gasreleases from the cooling system of an IR-camera of theVega 1 and Vega 2 spacecraft, during their flybys ofComet Halley in March 1986. N2 molecules were ionised

Figure 2.8.1/4: X component of the electric field,measured by the EFW (red) and EDI (black)instruments on Cluster 1 and 3 (courtesy M. Andreand G. Paschmann).

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by solar UV radiation at a rate of ~7 x 10–7 s–1 and gaverise to a plasma cloud expanding around the spacecraft.Strong disturbances owing to the interaction of the solarwind with the N2

+ ion cloud were observed with theplasma and wave experiment (APV-V instrument).Fig. 2.8.3 summaries the plasma and wave phenomenaobserved by the Vega 1 spacecraft.

Three gas releases studied are accompanied by increasesin cold electron density and simultaneous decreases ofthe spacecraft potential. This study shows that thespacecraft potential can be monitored with a reference

sensor mounted on a short boom. The comparisonbetween the model and observations suggests that the gasexpanded as an exhaust plume, and approximately only1% of the ions could escape the beam within the first fewmetres. The releases were also associated withsignificant increases in wave electric field emission(8 Hz - 300 kHz); this phenomenon lasted for more than1 h after the end of the release, which was most likelydue to the temporary contamination of the spacecraftsurface by nitrogen gas. DC electric fields associatedwith the events were complex. No magnetic fieldperturbations were detected, suggesting that nosignificant diamagnetic effect (i.e. magnetic cavity) wereassociated with these events.

Similar measurements will be performed by the SPEDEexperiment on the SMART-1 satellite during theoperations of the solar electric propulsion thrusters (seeSection 2.8.5).

ReferenceLaakso, H. et al., 2002, Ann. Geophys. 20, 1.

2.8.4 Instrument developments

Rosetta Mutual Impedance Probe (MIP) and LangmuirProbe (LAP)

The scientific payload of the Rosetta Orbiter includes anintegrated plasma package (RPC) of six instruments.RSSD is collaborating on two of these instruments: theMutual Impedance Probe (hardware development,mission operations and data analysis), and the LangmuirProbe (data analysis). The performance of MIP and itspreamplifiers was characterised over the whole opera-tional expected temperature range (–120ºC to +120ºC) aspart of the calibration activities.

The objectives of MIP and LAP are to study the plasmaenvironment of the diamagnetic cavity surrounding thecomet nucleus. Both instruments will cover, in acomplementary way, the variation of the cold plasmapopulation in equilibrium with the neutrals.

MIP is a collaboration with LPCE, Orleans (PI: J.-G. Trotignon; RSSD Co-Is: J.-P. Lebreton, R. Grard,H. Laakso; technical support was provided byU. Telljohann and B. Johlander). LAP is a collaborationwith IRF, Uppsala (PI: A. Eriksson; RSSD Co-Is:J.-P. Lebreton and R. Grard).

The SESAME Permittivity Probe on the Rosetta Lander

The Permittivity Probe (PP) is part of the Surface Elec-trical, Seismic and Acoustic Experiment (SESAME).This experiment consists of a variety of sensors tomonitor electric, acoustic and seismic properties of the

Figure 2.8.3: Summary of the plasma and wavedisturbances observed during the gas releases byVega 1. The quantities are, from top to bottom, signalsmeasured with the electric antenna in the frequencyrange 8 Hz - 300 kHz, the square of the electric fieldintegrated over the whole frequency range, theelectron current collected by a Langmuir probe, DCelectric field, and potential difference between abiased electric field probe and the spacecraft (Laaksoet al., 2002).

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subsurface layers of Rosetta’s target comet nucleusin situ as well as the dust flux falling back to the surface.The PP instrument consists of six sensors. Five arededicated to measuring the permittivity properties: twoare receivers and three transmitters. Three sensors areplaced under the three Lander feet and the other two onthe MUPUS and APX sensors. The PP measurementswill be used to monitor the water-ice content andtemperature of the surface layer.

The sixth PP sensor is a simple Langmuir probe thatmonitors the electron flux variations just above thecomet’s surface. This measurement can be used tomonitor the level of nucleus activity. Similarly, theplasma wave activity can be observed with the tworeceivers placed on the Lander feet.

The responsibility of RSSD was to develop the sensorsfor the PP instrument as well to participate in thedetermination of the instrument specifications and thecalibration of the permittivity measurements. The PPhardware was delivered in the summer of 2002.

PP is a collaboration with the Finnish MeteorologicalInstitute (FMI; PI: W. Schmidt). RSSD Co-Is areR. Grard, H. Laakso and R. Trautner; engineeringsupport was provided by B. Johlander.

The Spacecraft Potential, Electron Flux and Dust(SPEDE) experiment on SMART-1

The SPEDE experiment consists of two Langmuir probesand an electronics unit. The experiment is designed tomonitor in real-time large ion flux variations expectedduring the operations of the solar electric propulsionthrusters on the SMART-1 spacecraft. In addition to ionand electron measurements, the experiment can alsomonitor low-frequency (10-1000 Hz) plasma waves firstaround the Earth and later around the Moon, the finaltarget of the SMART-1 mission.

The main responsibility of RSSD was to develop twolightweight carbon fibre booms for the experiment. Theelectric sensors are placed at the end of these 60 cmstationary (i.e. no deployment mechanism) booms.RSSD also participated in the calibration of theexperiment by running several tests in its plasmachamber. The SPEDE hardware was delivered in theautumn of 2002.

SPEDE is a collaboration with the Finnish Meteor-ological Institute (FMI; PI: A. Mälkki). RSSD Co-Is areR. Grard and H. Laakso; engineering support wasprovided by B. Johlander.

ReferencesLaakso, H., Foing, B., 2001, ESA SP-476, 601.Tajmar, M. et al., 2002, Planet. Space Sci. 50, 1355.

ASPOC on Double Star

RSSD contributes mechanisms, the box, harness andexpertise in ion emitter development and in-flightoperations to ASPOC on the equatorial satellite of theChinese Double Star mission for launch in December2003. Triggered by the experience gained during almost2 years of operating ASPOC on Cluster, the ion emittermodule was modified to improve protection againstemitter cross-contamination. The cover openingmechanism had to be redesigned to fit the change to aEuropean-supplied pyro-actuator. Fig. 2.8.4/1 shows acomputer-generated illustration of the ASPOC emitter onDouble Star.

ASPOC is a collaboration with the Space ResearchInstitute of the Austrian Academy of Sciences, Graz (PI:K. Torkar; RSSD Co-Is: M. Fehringer and P. Escoubet).

Segmented Langmuir Probe on Demeter

RSSD has developed a multi-collector SegmentedLangmuir Probe (SLP). This sensor will be flown for thefirst time in early 2004 on the French Demeter mission,the first in the CNES microsatellite programme.Demeter’s scientific objectives are to study the electro-magnetic emissions and the ionospheric perturbationsassociated earthquakes and volcanic activity. Themission is developed under the PI M. Parrot, CNRS/LPCE (Orleans, F).

The Demeter Langmuir Probe (ISL: Instrument Sonde deLangmuir) is a miniaturised 8-channel instrumentconsisting of a classical cylindrical Probe and a smallspherical Langmuir Probe (Fig. 2.8.5/3). Demeter willprovide an excellent opportunity to demonstrate the SLPconcept. The instrument was delivered for integration in

Figure 2.8.4/1: The ASPOC emitter on Double Star.

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the payload in May 2002. A preliminary version of thedata analysis software was delivered from IAP to RSSDin November 2002.

ISL is one of the five instruments of the scientificpayload. ISL is developed under RSSD responsibility(J.-P. Lebreton, Co-I; D. Klinge, Instrument Manager) incollaboration with the Institute of Atmospheric Physics(IAP of Prague, Czech Republic), LPCE (F) and theObservatoire de Paris (Meudon, F).

The Huygens radar altimeter

The radar altimeter on Huygens has a dual function.Firstly, it provides the instantaneous distance to the Titansurface during the descent, information used by severalinstruments to change modes during descent and as postflight reference for the data analysis. Secondly, its RFreturn signal from the surface contains scientificinformation on the topography and the permittivity of thesurface. This information is extracted by dedicatedelectronics, developed by RSSD, within the Permittivity,Wave and Altimetry (PWA) unit of the HASI instrument.To further enhance the confidence in the operation of theradar and to improve the understanding of the scientificapplications, preparations for further testing startedduring 2002. This will include the use of the SM2Huygens probe mock-up with the flight spare models ofthe radar altimeters for sky tests and interference checks.During 2003 and 2004, helicopter and/or a stratosphericballoon test may be carried out on the same combination.A previous balloon flight in Spain in 1995 and ahelicopter flight in Tucson in 1996 showed the greatpotential of these field tests. The results obtained led tosignificant improvements to the flight hardware. With thenew tests we want to study how the new flight-identical

equipment responds to real targets, even if at a differentcomposition and a lower temperature than on Titan.A. Piot, H. Svedhem and J.-P. Lebreton are taking part inthese activities.

Quadrupolar Probe development

The measurement of the electric properties of surfacematerials is an important issue for planetary spacemissions. RSSD has contributed to Quadrupolar Probes(QPs), which are part of the Huygens HASI instrumentand the Rosetta Lander PP instrument. The RSSD group(R. Grard, R. Trautner, F. Simões) is also investigatingfurther development of this sensor that may becomeubiquitous on future planetary lander/surface missions.New QP architectures may include subsurface instru-ments and the employment of mobile platforms, allowingnew applications such as the investigation of buriedstructures and the detection of subsurface water(Trautner & Simões, 2002). In order to meet the require-ments of future missions, RSSD is supporting prototypedevelopments and computer modelling of new QParchitectures.

ReferenceTrautner, R., Simões, F., (2002), ESA-SP 518, 319-322.

Figure 2.8.4/2: Demeter ISL in flight configurationwith the connector saver.

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2.9 Comparative Planetology and Astrobiology

2.9.1 Comparative planetology of Earth-like planetsand moons

Comparative planetology is a core study area and is partof the preparations for scientific exploitation of ESA’supcoming planetary missions. More fundamentally,comparative studies are key to the continuing advance ofour scientific knowledge of the Earth and Solar System.Studies of the Moon, Mars, Venus and Mercury provideunique opportunities to understand the processes andfactors that have shaped our own planet. Similarly, theprocesses involved in geological and climatic evolutionon a planetary scale can only be understood throughcomparisons of these features on all of the inner planets.SMART-1, Mars Express, Venus Express and Bepi-Colombo offer research opportunities for comparativeplanetology. This motivated the Department to organisein 2002 the 36th ESLAB Symposium on Earth-likePlanets and Moons (see Section 4.1). RSSD staffpresented review papers on the missions to differentplanetary targets and on scientific thematic topics.

ReferencesChicarro, A., 2002, ESA SP-514, 21.Foing, B.H., Battrick, B. (eds), 2002, ESA SP-514.Foing, B.H., ILEWG, 2002, ESA SP-514, 3.Foing, B.H. et al., 2002, ESA SP-514, 345.Grard, R., Laakso, H., Svedhem, H., 2002, ESA SP-514,

25.Koschny, D., Marini, A., Hoofs, R., Almeida, M., 2002,

ESA SP-514, 89.

2.9.2 Lunar research and SMART-1 exploitation

The Moon bears the scars of countless impact craters andholds the only accessible record of the conditions in theEarth-Moon system over the past 4.5 billion years. Theactive geology and climate have long since destroyed theearly record of these events on the Earth, so the Moon iscritical to our understanding of the early history of ourplanet. The recent Clementine and Lunar Prospectormissions to the Moon provided the first views of globalgeochemistry. The SMART-1 mission will add our firstglobal IR dataset on minerals olivine and pyroxenesacross the surface, and the first global measurements inX-ray fluorescence, which will allow for the mapping ofelemental Mg. These are critical to our understanding ofthe Moon’s crustal evolution and origin, which isintrinsically linked to the early evolution of the Earth(Foing et al., 2001).

Analysis of Clementine data

The lunar research performed by D. Heather andcollaborators had two primary applications: the study of

lunar volcanism related to the thermal and physicalevolution of the Moon, and the detailed geological studyof large impact craters and crustal stratigraphy. Bothapplications use the mineralogical and chemical data setsprovided by the Clementine and Lunar Prospectormissions.

For volcanic studies, large-scale mapping of the southernOceanus Procellarum region was completed (Heather &Dunkin, 2002a). In this work, techniques have beendeveloped from which spectrally distinct mare basaltscan be mapped, and estimates of basalt thicknessobtained. A total of 13 basalts was recognised in theregion, 10 of which are spectrally distinct, and three ofwhich represent previously unrecognised members of theOceanus Procellarum stratigraphic group. The averagethickness of the basalts is between 160 m and 625 m,ranging from tens to hundreds of metres near themare/highland boundaries and consistently greater thanseveral hundred metres closer to the centre of the mare.This represents 8-32% of the total volume of basalts inOceanus Procellarum (Fig. 2.9.2/1).

In addition to the large-scale study, special focus hasbeen applied to the Marius Hills region, for whichspectrally distinct flows have been mapped for the firsttime using photographic and Clementine multispectraldata (Heather et al., 2003). The basalts on the plateau arevaried in age and composition, but are dominated by ayoung high-titanium basalt.

Figure 2.9.1: Earth-like planets and moons, targetsfor comparative planetology (Chicarro, 2002).

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Impact crater studies have focused on King, a largeimpact structure on the lunar farside (120ºE, 5.5ºN). BothClementine multispectral and photographic data setshave been used to investigate the crustal stratigraphy andgeology in the region (Heather & Dunkin, 2003). Thesurrounding area of the lunar crust was also studied for amore regional perspective, including the Al-Khawrizmi-King/Tsiolkovsky-Stark region of the farside (Heather &Dunkin, 2002b). The Clementine data show a variedsurface composition between the two sites, highlightedby the FeO content of the highland soils, which contain arelatively high iron abundance at King in comparison toTsiolkovsky. Conversely, on a vertical scale, the highlandcrust appears to show a matching trend of increasingfeldspar content with depth.

ReferencesFoing, B.H. et al., 2001, Earth Moon & Planets 85, 523.Heather, D.J., Dunkin, S.K., 2002a, Planet Space Sci.

50(14-15), 1299.Heather, D.J., Dunkin, S.K., 2002b, Planet. Space Sci.

50(14-15), 1311.Heather, D.J., Dunkin, S.K., 2003, Icarus in press.Heather, D.J., Dunkin, S.K., Wilson, L., 2003, J. Geo-

phys. Res., in preparation.

The Asteroid Moon micro-Imager Experiment (AMIE)on SMART-1

AMIE, the imaging experiment of SMART-1, is builtaround a very compact camera cube featuring a 1024 x1024-pixel CCD, read out with 10-bit dynamical range.The camera has an f/10 objective lens with a focal lengthof 140 mm. A set of colour filters is hard-mounteddirectly to the CCD for mineralogical imaging. D. Kos-chny is Co-I of the investigation, led by J.L. Josset,Neuchatel (CH). RSSD was responsible for the environ-mental testing and the optical calibration of the camera.

A thorough optical calibration of the Flight Model wasperformed before delivery in the beginning of 2002. Thiscalibration included dark-current measurements, flat-fielding, geometrical distortion and straylight tests. Thecamera performs well. Absolute calibration is plannedduring the cruise phase using standard stars.

Following completion of the calibration report and of theinput to the PI team for the in-flight calibration, a set ofroutines using the software tool IDL will be provided tothe AMIE science team. The help of M. Almeida isgreatly acknowledged. The support of J. Zender, thePlanetary Data Archiving Manager, was essential toensure that the image format is compatible with thestandard of the Planetary Data System.

2.9.3 Mars research

Mars Express exploitation

A. Chicarro, B.H. Foing, P. Martin and H. Svedhem arepreparing for the participation in scientific exploitationof Mars Express. Much remains to be understood aboutthe precise identity and form of the surface constituentsand to constrain physical, weathering/alteration andclimatic processes on Mars. Analysis of data from theHigh Resolution Stereo Camera (HRSC) will allow forcomprehensive investigations of geological, atmosphericand topographic features on Mars. The analysis of radardata will allow for subsurface sounding and the detectionof liquid or water ice.

Martin et al. (2002) have prepared for this a programmethat will use data from the HRSC and from the OMEGAimaging spectrometer. This programme is to characterisethe full range of spectral, compositional and mineral-ogical diversity of Mars; to correlate mineralogical,compositional and geomorphological information; todefine the roles played by weathering, mixing andalteration of the soils; and to determine the implicationsfor future missions an landing sites.

Maps for the Beagle-2 Isidis landing site were producedfrom a compilation of existing scientific datasets(Fig. 2.9.3/1).

Figure 2.9.2: A TiO2 map of the southern OceanusProcellarum, constructed using multi-colour Clemen-tine data (Heather & Dunkin, 2002a).

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ReferencesChicarro, A., 2001, LPI 32, 1044.Martin, P. et al., 2001, LPI 32, 1575.Martin, P., Chicarro, A., 2002, LPI 33, 1495.Martin, P. et al., 2002, ESA SP-514, 73.

Mars meteoritic layer modelling

The meteoric influx into a planetary atmosphere depositsa metallic ion layer. In the context of the future Marsmissions, the influence of such a layer at Mars on the

attenuation of HF radio waves has been evaluated. Themodel predicts a layer of metallic ions and electrons ataround 80 km height. Typical densities are 104 cm–3

during the daytime (Molina-Cuberos et al., 2003). Theone-way attenuation can reach 50 dB for a 5 MHz radiowave (Witasse et al., 2001). Our work will be applied tothe interpretation of the Mars Express ionospheremeasurements. Fig. 2.9.3/2 shows an example ofmodelling results of the composition of the lowerionosphere of Mars.

ReferencesMolina-Cuberos, G.N. et al. (incl. O. Witasse, J.-P. Le-

breton), 2003, Planet. Space Sci. submitted.Witasse, O. et al., 2001, Geophys. Res. Lett. 28, 3039.

2.9.4 Impact cratering processes

A most common geological process in the Solar System isimpact cratering. Greater understanding of the impactprocess and the resulting crater’s morphology andgeological nature will enhance the science that can bederived from remote-sensing data on the depths, diametersand stratigraphy exposed by impact craters on otherterrestrial planets. A. Chicarro and collaborators (2003)

Figure 2.9.3/1: Topography of eastern Isidis Planitia highlighting the low relief features of the region. Beagle-2landing ellipse shown in white (MOLA data, detrended over 1°; G. Michael, private communication).

Figure 2.9.3/2: Modelling results of the compositionof the lower ionosphere of Mars (Witasse et al., 2001).

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have investigated statistics of Earth impact craters, andhave started using Envisat and other satellite data to lookfor new and catalogue known impact craters on preservedpaleo-surfaces on Earth. G. Michael (2003) has developedalgorithms to recognise crater structures on Mars withinthe Mars Global Surveyor MOLA altimetry data.

The Chicxulub crater in the Yucatan Peninsula, Mexico isamong the largest impact craters on our planet, with adiameter greater than 200 km. Owing to the pristine stateof its ejecta blanket, it presents a unique opportunity tostudy large impact craters processes in situ. A. Ocampoand collaborators have examined the evidence for fluid-ised ejecta emplacement by the Chicxulub impact (Popeet al., 2003). The Yucatan Peninsula was rich in volatilesat the time of impact (65 Myr ago). Models predict thatabout 2-4% of the impact vapour plume was composedof CO2, SO2, and H2O produced from the carbonate,sulphate and water in the target rocks. The impactoccurred in a shallow sea, hence there was abundantsurface water that may have mixed with the ejecta. Sincethe Earth has a thick atmosphere, ejecta emplacement,especially in the outer parts of the ejecta blanket andbeyond, was no doubt affected by atmospheric drag.

ReferencesChicarro, A., Michael, G. et al., 2003, ESA Bulletin,

submitted.Michael, G., 2003, Planet. Space Sci., submitted.Pope, K.O. et al. (incl. A. Ocampo), 2003, Science,

submitted.

2.9.5 Contributions to astrobiology

Dense interstellar clouds are the birth-sites of solar-massstars and their planetary systems. Interstellar moleculesand dust become the building blocks for protostellardiscs, from which planets, comets, asteroids and othermacroscopic bodies eventually form. Observations at IR,radio, mm and sub-mm ranges show that a large varietyof gas-phase organic molecules are present in the denseinterstellar medium. Organic molecules evolve fromtheir formation in molecular clouds to their incorporationinto the early Solar System. Large carbon-bearingspecies, such as polycyclic aromatic hydrocarbons(PAHs) and fullerenes as well as carbonaceous solidshave been identified in the interstellar medium, incomets, meteorites and planetary environments. Currentand future ESA space missions can make a keycontribution to astrobiology (Foing, 2002). Theknowledge of organic chemistry in molecular clouds,comets, meteorites and planets and their common linkprovides constraints for the processes that lead to theorigin, evolution and distribution of life in the Galaxy.

ReferenceFoing, B.H., 2002, in Astrobiology. The Quest for the

Conditions of Life, Springer, p.389

Search for large organics in space and diffuse inter-stellar bands

Polycyclic aromatic hydrocarbons (PAHs) are believedto be the most abundant free organic molecules andremarkably stable in space. PAH molecules are producedpartly in the outer atmospheres of carbon stars, or formedby shock fragmentation of carbonaceous solid material.PAHs are also identified in meteorites and interplanetarydust particles (IDPs). The polyhedral geometry of C60fullerene was discovered in 1985. The presence of sootmaterial in carbon-rich stars, the spontaneous formationand the remarkable stability of the fullerene cagesuggested the presence of fullerene compounds ininterstellar space. In the 1990s fingerprints of the C60+ion were confirmed in the near-IR which indicates thatfullerenes can play an important role in interstellarchemistry. B.H. Foing, N. Boudin and collaborators havesearched for other diagnostics of fullerenes or PAHmolecules (Ruiterkamp et al., 2002; Boudin, 2002). It isnow crucial to understand the formation, evolution oforganics and their transport to planetary surfaces asingredients for prebiotic chemistry (Ehrenfreund et al.,2001).

The problem of Diffuse Interstellar Bands (DIBs) is oneof the oldest unsolved of modern astronomy. Followingtheir very successful work in the 1990s, B. Foing andcollaborators have looked with an ESO-VLT observingrun (four nights in September 2001) at the Magellanicclouds (Fig. 2.9.5/1) to see the effect of low metallicity in

Figure 2.9.5/1: Discovery of Diffuse InterstellarBands in the Magellanic clouds (ESO-VLT data).

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the formation of complex organic compounds(Ehrenfreund et al., 2002). They are continuing theanalyses of the VLT data, and of the WHT, CFHT andISO spectroscopic data of PAH features. They havereviewed reasons why fullerenes could be detected,while PAH electronic absorption signatures in the DIBspectra have remained elusive.

ReferencesBoudin, N., 2002, ESA SP-518, 37.Ehrenfreund, P., O’Tuairisg, S., Foing, B.H. et al., 2001,

in The Bridge between Big-Bang & Biology, 150.Ehrenfreund, P. et al. (incl. B.H. Foing), 2002, ApJ Letts.

576, L117.Ruiterkamp, R. et al. (incl. B.H. Foing), 2002, A&A 390,

1153.

Survival and evolution of organics in space

B.H. Foing, in a collaboration led by Leiden Univ. (NL),will study the survival and evolution of large organicmolecules under space UV exposure within the EXPOSEexperiment on the International Space Station (ISS) witha 1-year exposure in 2005. A set of large organicmolecules has been defined: a) aliphatic and aromatichydrocarbons (5-20 carbon atoms per molecule) b)nitriles, ketones, aldehydes, organic acids; c) aminoacids; d) large PAHs; e) fullerenes C60, C70, C84 andtheir hydrogenated or exohedral compounds; f) kerogensand complex organic mixtures of 3-D networks ofaromatic and aliphatic structure, including a variety ofheteroatoms (also a reference material for meteorites); g)spores and living organisms. Before and after spaceexposure, the samples will be subjected in the differentCo-I institutes to various analysis methods, such as high-performance liquid chromatography, IR spectroscopy,gas chromatography, laser desorption mass spectrometryand secondary ion mass spectrometry .

As a precursor to the ISS-EXPOSE experiment, a spaceUV exposure experiment of a sample tray filled with 16samples of different organics was selected for aBiopan/Foton flight with a planned 1-week exposure(Ruiterkamp et al., 2001; 2002). The experiment sample-tray was integrated at ESTEC and launched fromPlesetsk aboard the Foton-M1 spacecraft on 15 October2002. Unfortunately, the Soyuz rocket failed 15 s afterlift-off and the experiment was lost in the explosion.

ReferencesRuiterkamp, R., Ehrenfreund, P., Foing, B.H., Salama, F.,

2001, ESA SP-496, 137.Ruiterkamp, R. et al. (incl. B.H. Foing), 2002, NASA

Laboratory Astrophysics Workshop, 77.

Exobiology preparation for Mars Express: Marssimulation chamber studies

B.H Foing and collaborators from Leiden Univ. (NL), inpreparation for the exploitation of data from the MarsExpress Beagle-2 exobiology lander and futureexobiology multi-user facilities on future Mars landers,were selected for an investigation to expose differentorganics, embedded in martian soil analogues, tosimulated martian atmospheres, UV radiation andoxidising agents in order to study the stability andevolution of organic molecules on the martian surfaceand their implications for extinct and extant life on Mars(ten Kate et al., 2003).

An atmospheric simulation chamber in combination witha UV lamp is being set up to obtain data on the combinedeffects of UV photo-processing, atmospheric conditionsand the presence/absence of oxidising agents on organicmolecules. The organic compounds represent analoguesfor abundant meteoritic and cometary molecules andentail aliphatic and aromatic hydrocarbons, fullerenes,amino acids and nuclear bases, carbonaceous solids andterrestrial analogues (i.e. kerogens). The simulationchamber is a refurbished vacuum chamber of 1 mdiameter and 1.2 m length. It offers thermal and pressurecontrol. A window allows the attachment of UV lampsand appropriate filters to simulate the variation of thesolar UV flux at 190-280 nm according to the O3 contentin the martian atmosphere. Compact martian soilanalogues (representing the sedimentary deposits) willallow less oxidation penetration and be representative ofmaterial present at the recommended landing sites.Among the oxidising agents, we intend to use mainlyH2O2 and O2. The chamber can be filled with gasessimulating the evolution of the martian atmosphere (CO2,

Figure 2.9.5/2: The Mars simulation chamber equip-ment, with controlled temperature and environment,solar radiation lamp, UV lamps, sample trays withmartian analogue soil, and gas chromatograph massspectrometer and other instruments to monitor theevolution of organics.

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N2 and Ar and traces of O2 and CO). H2O2 and O3 can beadded as gases in the chamber in order to study oxidationeffects. We shall reproduce the thermal (e.g. 180-280K)cycling and measure the evolution and thermaldegradation products of embedded organics, and thesublimation of the more volatile compounds. First opera-tions after the build-up phase will include: procurementand processing of Mars-like soils; simulations on surfacewater; experiments related to biological activity and darkspots; simulations of survival organics; and tests ofsensors for organics and life.

The research activities on large organics, and especiallythe simulations in the Mars chamber, will contribute tothe interpretation of measurements obtained by Beagle-2.We shall therefore focus our experiments on the mostabundant organic molecules identified in Solar Systembodies and beyond, which may have been exogenouslydelivered to the martian surface.

ReferenceTen Kate, I. et al. (incl. B.H. Foing), 2002, ESA SP-518,

81.Ten Kate, I. et al. (incl. B.H. Foing), 2003, Int. Astro-

biology J., in press.

2.10 Cosmic Dust and Comets

This research theme encompasses a wide range ofactivities performed by members of RSSD, mostly ininternational collaborations. Activities range fromanalysing data from dust detectors flown on spacecraft,ground-based observations of comets and interplanetarydust particles, preparations of flight instruments to thedevelopment of generic elements for future dustinstruments.

2.10.1 In situ measurements of cosmic dust

From April 1997 to July 2002 the impact detectorGORID on the Russian Express-II satellite collected dataon cosmic dust and space debris from its location ingeostationary orbit. The spacecraft was positioned at80°E until July 2000, after which it was moved to 103°E.

H. Svedhem and colleagues analysed the impact eventsto study the relation to interplanetary and interstellar dustand to the space debris population, taking into accountgeometrical and seasonal effects. Dust and debrisparticles can, in a first approximation, be separated byevaluating the velocity: particles in Earth orbit are relatedto space debris and particles with velocities above theEarth-escape velocity are cosmic dust. Data sets fromone or several full years are required to suppress possiblebiases that can result from spatial, temporal anddirectional variations in the flux and to reduce thestatistical errors. The results have been compared withand match well existing models of the interplanetary dustflux.

On a few occasions a flux increase has been observedduring the major known meteor showers. A number ofoccasions with clustered events that are very likely realparticle impacts have also been identified. Many of theseoccur at n:m resonance, where n ≥ 1 is the number of fullorbits of the satellite and m is the number of orbits of theclustered particles. This indicates that the clusters orclouds are fairly recent. A likely origin of these particleclouds is orbit circularisation burns from apogee boostmotors of geostationary spacecraft. Indeed, simulationsof the propagation of the dust clouds from a few knownrocket firings have shown that the particles should bepresent at the observed positions at the observed times.At other times/positions events are registered in everyorbit (n = 1). These events could be related to particleclouds that have been orbiting the Earth for a longer time.

The GORID detector has two different concentric fieldsof view, a narrow FOV with high sensitivity and a wide(almost 2π sr) FOV with lower sensitivity. Recentrecalibration of a spare model of the detector haveenabled a better separation of the two ranges and has alsoshown that the difference in sensitivity between the tworanges is less than has been previously thought.

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The instrument was built by MPI-K in Heidelberg (D) asan engineering model for the Ulysses Dust Experiment.It was subsequently refurbished by RSSD to suit the newenvironment in geostationary orbit.

The routine analysis of data from the Galileo, Ulyssesand Cassini dust detectors also continued in closecollaboration with the dust group at MPI-K.

To prepare for future mission opportunities, studies wereperformed to simulate the ion trajectories for a novel dustmass spectrometer design. To verify the simulationresults, a test set-up was prepared to study the ionresponse to hypervelocity impacts simulated by laserpulses.

2.10.2 Infrared investigations of interplanetary dustparticles

Interplanetary dust particles (IDPs, < 50 µm diameter)from comets and asteroids are collected in thestratosphere. Some of them are among the mostchemically and isotopically primitive meteoriticmaterials available for laboratory investigation. Studiesof IDPs provide insight about grain dynamics in the earlySolar System and presolar interstellar and circumstellarenvironments. Processes like grain condensation,chemical and physical evolution, and grain densitydistribution in the protoplanetary disc can be investigatedthrough studies of IDPs. It is now also possible tocompare the properties of IDPs directly with those ofdust around other young stars using their spectralproperties in the IR, where most of the translational andvibrational bands are also found.

In order to compare the spacecraft IR data withlaboratory IR data from IDPs, it is highly desirable toobtain the data over a similar spectral range. Essentiallyall of the existing IR spectroscopic data on IDPs has beencollected over the 2-25 µm wavelength range, in contrastto the ISO data that covers 2.4-200 µm. So far, twoproblems have hindered acquisition of spectral databeyond 25 µm from IDPs: the small size of individualIDPs relative to the wavelength of the incident radiation,and the lack of detectors sensitive beyond ~25 µm. Therecent upgrade of the National Synchrotron Light Source(NSLS) at Brookhaven National Laboratory (US)allowed us for the first time to take spectra of an IDPover the important ‘mineral fingerprint’ region of 2.5-50 µm.

Figure 2.10.2/1 shows an atomic force microscope(AFM) image of an IDP (diameter ~10 µm) pressed ontoa CsI window. The high IR transparency of CsI allows usto measure the IR absorption properties of L2036-V25out to extended wavelengths, but the small size of theIDP demands the use of a high-brightness synchrotronlight source. We acquired two IR spectra of L2036-V25

at NSLS: one covering the 2.5-28 µm range and the otherthe 22-60 µm range. The spectral overlap between thetwo measurements is such that only a very slightmultiplication factor was necessary to splice the tworegions together (Fig. 2.10.2/2). Beyond 50 µm, thesignal-to-noise becomes too low.

The absorption spectrum of L2036-V25 is similar to theemission spectrum of Comet Hale-Bopp obtained by ISO(Fig. 2.10.2/ 2). The similarity is not unexpected sincehighly porous, fragile IDPs like L2036-V25 aresuspected to be from comets or comet-like outerasteroids.

The strongest features in the spectrum of IDP L2036-

Figure 2.10.2/2: The IR absorption of IDP L2036-V25(black line) compared with the absorption profile offorsterite (green line) and enstatite (blue line). Alsoplotted is the emission spectrum of Comet Hale-Bopp(red line) taken with ISO (Crovisier et al., 1997,Science 275, 1904).

Figure 2.10.2/1: AFM image of IDP L2036 V25. Theimage size is 10x10 µm; maximum height difference is3 µm.

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V25 are due to olivine, while some weaker features ofpyroxene are also detected. The peak positions of thefeatures, especially the ones at the longer wavelengths(>20 µm), provide information about the Mg/Fe ratio ofthe minerals. The features suggest an Mg/Fe ratio ofabout 3:1 for both the olivines and pyroxenes. Note thatthe peak positions in the IR spectra of Hale-Bopp areconsistent with pure Mg-olivine and pyroxene, i.e.forsterite and enstatite. This difference gives some veryimportant clues about the formation history of thedifferent components.

F. Molster and colleagues have demonstrated that it isnow possible to obtain IR spectra of individual IDPs overa spectral range extending out to ~50 µm. Silicateminerals like olivine and pyroxene can beunambiguously distinguished and their Mg/Fe contentscan be estimated. The above results are encouragingbecause IDP L2036-V25 was prepared as a calibrationstandard for the AFM Micro Imaging Dust AnalysingSystem (MIDAS) onboard Rosetta and not as a sampleoptimised for IR spectroscopy.

2.10.3 Ground-based observations of comets

Comet C/1999 S4 (LINEAR)

One of the most spectacular cometary splitting eventsever observed was the complete disruption of the nucleusof Comet C/1999 S4 (LINEAR). HST/VLT observations

of the comet’s debris on 5/6 August 2000 revealed thatapart from the bright dust tail dominating its visualappearance, more than a dozen individual fragmentswere spread around the predicted position of the originalnucleus. All these fragments faded rapidly and were nolonger detected in any of the subsequent observations. Itbecame clear rather soon that the time of the outburst(22 July 2000) that produced the dust tail and resulted inthe complete disintegration of the comet did not coincidewith the separation times of some individual fragments.These fragments must have separated some time betweenlate June and mid-July, hence the true splitting eventmust have occurred some time before the finaldisintegration started. Indeed the analysis of imagingobservations of Comet C/1999 S4 (LINEAR) obtainedbetween 28 June and 1 July 2000 (Fig. 2.10.3) confirmedthat a splitting of the nucleus occurred on 28 June 2000,which produced at least one major fragment and anumber of small fragments drifting in the tail direction(Schulz & Stuewe, 2002). The fragments remained activeat least until 1 July 2000, producing further disintegra-ting dust particles.

Comet C/1996 Q1 (Tabur)

The spectrophotometric CCD observations of CometC/1996 Q1 (Tabur) (Lara et al., 2001) allowed for thefirst time detailed multi-colour photometry of cometarycontinuum in the near-nucleus region to be extracted.The change of the spectral properties of the cometarydust as a function of distance to the nucleus wastheoretically modelled to separate the influence ofparticle size and composition on the colour of cometarydust. The calculations provided important characteristicsof the dust in the coma of Comet Tabur as a function ofnucleus distance. These are the power of the power-lawsize distribution and the radius of the smallest particles inthe dust distribution (Kolokolova et al., 2001).

Comet 46P/Wirtanen

The observations of the nucleus of Comet 46P/Wirtanenobtained at the VLT were analysed. No coma wasdetected in May 1999 when the comet was at aheliocentric distance of 4.98 AU. The mean nucleusradius was confirmed to be 555±40 m (albedo 4%). Themeasured light curve was in agreement with a rotationperiod of 5-7.5 h and a ratio of the main nucleus axes ofat least 1.4. The non-detection of a coma allows us toapproximate the upper limit on the dust production rateto be 0.05 kg s–1. A weak and condensed coma appears tobe present in the seeing disc of the comet at 2.9 AUinbound (December 2001), causing a higher brightnessthan expected from previous size estimates of thenucleus. The comet was very red (V-R spectral gradient~47%/100 nm) and the dust production rate wasdetermined to be 1 kg s–1 (Boehnhardt et al., 2002).

Figure 2.10.3: Comet C/1999 S4 (LINEAR) imaged inblue continuum (BC) and red continuum (RC). On1 July 2000, the coma is much more elongated than on28 June 2000. The Sun is to the left in all images.

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ReferencesBoehnhardt, H. et al. (incl. Schulz, R. & Schwehm, G.),

2002, A& A 387, 1107.Kolokolova, L., Lara, L., Schulz, R. et al., 2001, Icarus

153, 197.Lara, L., Schulz, R. et al., 2001, Icarus 150, 124.Schulz, R., Stuewe, J.A., 2002, Earth, Moon and Planets

90, 195.

2.10.4 Leonid observations

As for 1999, theoreticians had predicated a meteor stormgenerated by the Leonid meteor stream in November2001 and 2002. The storm of 2001 was observable onlyfrom Asia and Australia, with a second peak in the US,the 2002 storm from Europe, and again a second peak inthe US.

In 2001, D. Koschny, J. Zender and R. Trautner success-fully observed the storm peak from Western Australia.A. Knöfel from the International Meteor Organisation(D) accompanied them. A number of image-intensifiedvideo cameras and a special sensor to record the electricfield changes in the atmosphere were operated. Meteorspectra together with precise altitude information wereobtained. Zender et al. (2002) have prepared a firstanalysis. The observers have also analysed the lightcurves of the meteors and compared them to afragmentation model developed at RSSD (Koschny et al.,2002). Indications for an inhomogeneous comet nucleushave been found: bright meteors appear to be frommaterial with higher strength. This can be explained by

an inhomogeneous comet nucleus, where there are areasof higher and of lower strength. Large particles from thelow-strength areas will break apart immediately atejection and never make it away from the comet. Thisassumption needs to be confirmed by further modelling.

As part of the Leonid campaigns of 2001 and 2002, theterrestrial electric field was monitored by an electric fieldsensor derived from the Rosetta SESAME QuadrupolarProbe sensors (Trautner et al., 2002). The electric fieldsensor showed a significant increase in the fieldfluctuations during the 2001 Leonid storm. The curvematches the activity profile of the Leonids very well(Fig. 2.10.4/1). The experiment was repeated during the2002 Leonids shower using a modified sensor setup andimproved recording equipment. The data analysis is inprogress. It is expected that the measurement data willprovide important information on the link betweenelectric field fluctuations and meteor impacts in theterrestrial atmosphere. The experiments in our terrestrialenvironment are also a preparation for future missions toMars.

For the Leonid storm in 2002, the same team repeated themeasurements from Southern Spain in a collaborationwith the Instituto Astrofisica de Andalucia (IAA) inGranada (E), from two stations close to Granada. Therewas clear sky for only half of the time. As in 1999, wealso had one camera flying aboard a DC-8 aircraft as partof a campaign organised by the NASA SETI institute. Itrecorded the very bright fireball shown in Fig. 2.10.4/2.A total of about 1000 meteors were recorded with thissystem alone in about 3 h around the peak. The analysisof the 2002 data has just started.

Figure 2.10.4/1: Comparison between the verticalelectric field in arbitrary units and the ZenithalHourly Rate (ZHR) of the Leonid meteors asrecorded by the International Meteor Organisation,versus time on 18 November 2001.

Figure 2.10.4/2: A very bright fireball recorded by theairborne camera operated by R. Jehn (ESOC). Itappeared at 05:10:38 UT on 19 November 2002.Clouds are visible in the lower part of the image.

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ReferencesKoschny, D., Reissaus, P., Knöfel, A, Trautner, R.,

Zender, J., 2002, ESA SP-500, 157.Trautner, R., Koschny, D. Witasse, O., Zender, J.,

Knöfel, A., 2002, ESA SP-500, 161.Zender, J., Witasse, O., Koschny, D, Trautner, R.,

Knöfel, A., 2002, ESA SP-500, 121.

2.10.5 The Rosetta Imaging System (OSIRIS)

OSIRIS is the scientific imaging system of the Rosettamission (Keller et al., 2003). It will address key problemsin understanding the properties and behaviour of cometsby investigating the physical and chemical processes thatoccur on the nucleus and in the coma. OSIRIS consists oftwo cameras: a narrow-angle camera (NAC) with a2.4 x 2.4° FOV and a wide-angle camera (WAC) with a12 x 12° FOV. Two identical full-frame CCDs with 2048x 2048 pixels are used in the cameras.

OSIRIS is provided by a European consortium under theleadership of H.U. Keller (MPAe Lindau, D). RSSD ispart of this consortium and responsible for the DataProcessing Unit (DPU; Fig. 2.10.5). It consists of twoDigital Signal Processor (DSP) boards, a mass memoryboard and the relevant interfaces.

The Flight Model was delivered to MPAe and integratedwith the Electronics Box in the first half of 2001. Aftersome required rework, it passed all environmental tests.The complete OSIRIS Flight Model was delivered to theRosetta Project in summer 2001 and mounted on thespacecraft on 11 December 2001. OSIRIS participated inthe extensive spacecraft-level test campaign and theoperational interface with ESOC was refined.

D. Koschny participated in the optical calibration atMPAe. A complete calibration including absoluteresponsivity measurements was performed.

D. Koschny and K.-P. Wenzel are OSIRIS Co-Is,U. Telljohann is Project Engineer and B. Johlander wasresponsible for parts procurement.

ReferenceKeller, H.U., et al. (incl. Koschny, D.V., Telljohann, U.,

Wenzel, K.-P.), 2003, ESA SP-1165, in preparation.

Figure 2.10.5: The DPU Interface Board of theOSIRIS Flight Model DPU.

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2.11 Development and Exploitation of Super-conducting Cameras for Astronomy

2.11.1 Overview of activities

The development and exploitation of superconductingcameras has concentrated on the application ofSuperconducting Tunnel Junctions (STJs) to the opticalpart of the spectrum. This region provides opportunitiesto develop the basic technology coupled to practicalfield-testing with rapid technical and scientific feedbackfrom ground-based optical telescopes – specifically theWilliam Herschel Telescope (WHT) in La Palmas (E).Such an approach also allows for parallel spin-offdevelopments at X-ray wavelengths for future high-energy astrophysics missions such as XEUS. This opticalprogram, known as the Superconducting CameraProgramme (SCAM), is broken into six phases, of whichtwo were completed between 1999 and 2001.Fig. 2.11.1/1 summarises the overall programme in termsof a provisional time-line and the key objectives.

The basic superconducting detector used within theSCAM programme is an STJ. Fig. 2.11.1/2 showsessentially the key characteristics of such a device.Incident photons break Cooper pairs responsible for thesuperconducting state. Since the energy gap between theground state and the excited state is only a few meV, eachphoton creates a large number of free electrons inproportion to its energy. Examining the photoabsorptionprocess in detail at optical wavelengths has been a keytheoretical effort in collaboration with the School ofPhysics and Chemistry at Lancaster Univ. (UK). Theabsorption of a photon of a wavelength λ (nm) in asuperconductor is followed by a series of fast processeswhich involve the breaking of Cooper pairs by energeticphonons created by the hot electrons produced as theatom relaxes after the initial photoabsorption. The

essential result of this cascade is that the photon’s energyis converted into a population of free charge carriers(quasiparticles) in excess of any thermal population. Fortypical transition metals, this conversion process rangesfrom nanoseconds (niobium) to microseconds (hafnium).At sufficiently low temperatures (typically about anorder of magnitude lower than the superconductorscritical temperature Tc), the number density of thermalcarriers is very small while the average number of excesscarriers No created as a result of the photoabsorptionprocess can be written as No(λ) ~ 7 x 105/λ ∆(T/Tc).Here, the wavelength is expressed in nm and thetemperature-dependent energy gap ∆(T/Tc) is in meV.Thus, in a superconductor such as tantalum, with T << Tc

(4.5K), the initial mean number of free charge carrierscreated No(λ) is ~ 106 (103/eV).

The variance of No(λ) depends on the variance in thepartition of the photon’s energy between productivephonons (phonons with an energy Ω > 2∆ which canbreak Cooper pairs) and phonons which are essentiallylost from the system (Ω < 2∆). The population of Ω < 2∆phonons evolves with time as the average energy of theincreasing quasiparticle population relaxes, throughquasiparticle phonon emission, towards the bandgap. Thevariance <No> depends on the superconductors bandgap∆ and its Fano factor F such that <No>~ 7 x 10–4 F/[λ(nm) ∆(T/Tc)]. Expressing this variance interms of the wavelength resolution, we have dλF (nm) ~2.8 x 10–3 λ3/2 [F ∆(T/Tc)]

1/2. It has been shown thatF ~ 0.2 for elemental superconductors such as niobiumand tin (Kurakado, 1982; Rando et al., 1992). Thistherefore represents the fundamental Fano limitedresolution of any superconductor. Thus a superconductorsuch as tantalum, with T << Tc), irradiated with photonsof wavelengths covering the X-ray to the near IRλ ~ 1,10,100, 1000 nm, then dλF ~ 0.001,0.033,1.07,34 nm, respectively (Peacock et al., 1997; 1998).

Figure 2.11.1/1: The overall SuperconductingCamera Programme (SCAM) for ground-basedoptical astronomy.

Figure 2.11.1/2: A cross-section showing the basiccharacteristics of an STJ sensitive to optical photons.

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The quasiparticles produced through photoabsorptioncan be detected by applying a DC potential across twosuch films separated by a thin insulating barrier, formingan STJ (c.f. Fig. 2.11.1/2). The bias favours the transferof quasiparticles from one film to the other throughquantum mechanical tunnelling across the barrier. Thecurrent developed by this tunnel process thereforerepresents the detector signal. After initial tunnelling, aquasiparticle can tunnel back, therefore contributingmany times to the overall signal (Grey, 1978). Onaverage, each quasiparticle will contribute <n> times tothe signal through an average of <n> tunnels before it islost from the system through traps etc. Hence the meannumber of effective charge carriers N = n No. Themultiple tunnel process leading to n, the average numberof tunnels per quasiparticle, is of course subject also tostatistical fluctuation (Goldie et al., 1994). Thefluctuations due to the Fano process and that arisingfrom the tunnel process can be added in quadrature suchthat the overall limiting resolution for a perfectlysymmetrical superconducting tunnel junction can bewritten as: dλT (nm) ~ 2.8 x 10–3 λ3/2∆(T/Tc)

1/2

[F+1+1/n]1/2. Fig. 2.12.1/3 illustrates this tunneljunction-limited resolution for a number of elementalsuperconductors for the case when n ≥ 2. Note thisexpression for the tunnel-limited resolution dλT can befurther generalised to any superconductor compound orproximised bilayer through the use of the approximateBCS relation in the weak coupling limit of2∆ = 3.5 k Tc, where k is Boltzmann’s constant.Deviations from this relation are small even for stronglycoupled superconductors such as niobium. Thus in termsof the critical temperature we can write dλT (nm)~ 1.1 x 10–3 λ3/2 Tc

1/2 [F+1+1/n]1/2 (n ≥ 2). Typically, n isof order 10-100 and depends on the size and nature ofthe STJ. Of course, in optical and UV spectroscopy, highresolution normally implies a resolving powerλ/δλ > 104. From Fig. 2.11.1/3 it is clear that none of theclassical superconductors forming the basis of current

STJs under development (those based on Nb,Ta, Al, Moor Hf ) could achieve such a resolving power. In fact, asuperconducting critical temperature Tc << 100 mK isimplied to achieve a resolving power of 104 leading tothe development of STJs based on such elementalsuperconductors as rhodium. Of course, things are notquite this simple with the temporal characteristicsassociated with the production of the free excess chargecarriers being a function of the critical temperature,while the phonons with Ω > 2∆ have wavelengthssignificantly larger than the thickness of the film. Thussuch low temperature superconductors may well besignificantly slower in their overall response.

Given that the resolution of a typical STJ based ontantalum is not appropriate for high- or even medium-resolution spectroscopy, what are the alternative keyattributes that such a device can bring to the field ofoptical/UV astronomy? Two features are important: (a)the timing characteristics (≤ 10 µs) coupled to thebroadband spectral capability may make this the idealspectrophotometer. Objects such as pulsars and flarestars may be important objects with which to observewith narrow field small arrays; (b) the efficiency at UVwavelengths which, if coupled to a large-format array (apanoramic detector), may allow for the development ofan efficient broadband imaging spectrometer with whichto determine the low-resolution spectra of very faintobjects, allowing very deep-field surveys. Such surveyscould allow the determination in a single exposure of thebroadband spectra and possibly therefore the redshift z(and therefore age) of all objects in the field through themeasurement of the Lyman edge and the Lyman emissionlines (the Lyman forest). Note that the observedwavelength λo = λR (z+1), where λR is the rest wave-length. Thus the classical Lyman edge would appear at~ 400 nm at z ~ 3. This is close to the optimumperformance for a tantalum-based STJ, where it has anintrinsic efficiency of ~70% and a resolution of ~20 nm.It is, however, clear that STJ devices based on lowertemperature superconductors such as hafnium wouldallow the clear evaluation of redshift. This, therefore, isone of the key goals of the SCAM programme: todevelop a large-format (FOV ~1 arcmin), high-resolution, multi-object imaging instrument capable ofmeasuring with reasonable resolution (~1 nm) thespectra of deep field extragalactic objects so as todetermine their redshift.

ReferencesGoldie, D., et. al., 1994, Appl. Phys. Lett. 64, 3169.Grey, K., 1978, Appl. Phys. Lett. 32, 392.Kurakado, M., 1982, Nucl. Instr. & Meth. 196, 275. Rando, N., et al., 1992, Nucl. Instr. & Meth. A313,

173.Peacock, A., et. al., 1997, Astron. & Astrophys. Sup. 123,

581.Peacock, A., et. al., 1998, Astron. & Astrophys. Sup.,

127, 497.

Figure 2.11.1/3: The tunnel-limited resolution of sometypes of STJs under development as a function ofwavelength.

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2.11.2 The SCAM-1 programme

The SCAM-1 instrument represented the firstdemonstration of a superconducting camera developedspecifically for integration onto the WHT telescope. Inthis technology programme, all the basic key elements ofsuch an instrument were brought together into a singleinstrument:

— STJ array;— STJ multi-pixel bias system;— STJ readout electronics;— cryogenic system;— diagnostic test software;— real-time quick-look analysis.

SCAM-1 can therefore be considered as a technologydemonstrator rather than a scientific astronomicalinstrument. Fig. 2.11.2/1 shows the basic 6 x 6-pixel STJarray prior to its integration into the cryogenic coolingsystem. The array fabricated in tantalum with each pixel25 µm square covered a FOV of only 3.6 arcsec. ThisFOV is a critical issue since it only allows for effectivesingle-object studies when the telescope ‘seeing’ isreasonable (typically < 2 arcsec).

Each device had its own bias, amplification and signalprocessing circuitry outside of the cryostat and operatedat room temperature. The cryostat was a pumped He4

system with an internal closed-cycle He3 sorption pumpwhich brought the base temperature from ~1K to~300mK, the operating temperature of the tantalumarray. The instrument was integrated onto the Nasmythfocus of the WHT in February 1999 and after systemtesting was able to record individual photons fromspecific targets with a temporal accuracy of 5 µs whilemeasuring the photon colour over the wavelength range310-610 nm with a resolution of 100 nm at 500 nm.

A crucial technical demonstration of the systemperformance was the detection and measurement of

photons from the 33 ms Crab pulsar. Here we demon-strate with this single observation the power of the newinstrument allowing for detailed pulse phase spectro-scopy at high temporal resolution (Perryman et al.,1999). This celestial clock’s speed is so well establishedthat we can literally calibrate the complete system – endto end. Fig. 2.11.2/2 shoes the observed pulse profile as afunction of pulse phase.

ReferencePerryman, M.A.C., Favata, F., Peacock et al., 1999, A&A

346, L30.


SCAM-2 covered a series of three campaigns at theWHT over the period December 1999 until October2000. A significant number of improvements on theSCAM-1 design were introduced to ensure thisprogramme was orientated to astronomical exploitationeven if still centred on the 6 x 6 pixel tantalum array. Inparticular, the resolving power and photon event ratewere improved. The campaigns highlighted three areaswhere the SCAM can make a serious astronomicalcontribution:

— spectro-photometry of variable stars;— stellar temperature measurements; — quasar redshifts.

Fig. 2.11.3/1-3 show data referring to all three types ofastronomical observations.

Referencesde Bruijn, J.H.J. et al., 2002, A&A 381, 57.Reynolds, A.P., de Bruijne, J.H.J., Perryman, M.A.C.,

Figure 2.11.2/1: The original SCAM-1 6 x 6 array.

Figure 2.11.2/2: Pulse profile of the Crab pulsar asobserved by SCAM-1 in February 1999.

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Ramsay, G., Cropper, M., Bridge, C.M., 2002, A&A inpress.


It is clear from these results that the SCAM instrumentcan be a powerful tool for observational astronomy

provided weaker areas can be further developed. Inparticular these weaker areas are considered to be:

— the field coverage (field of view);— the long wavelength limit;— the resolving power;— the count rate limits.

Figure 2.11.4: The SCAM-3 array prior to instrumentsystem tests. Each device is still biased and read outindividually.

Figure 2.11.3/1: The light curve of the eclipsingAM Her system V2301 Ophiuchi during the eclipseingress. Spectra, with high time resolution throughthe eclipse, allow the separation of the accretionstream component from the white dwarf, therebyconstraining the system geometry. Figure 2.11.3/3: The redshift of a number of quasars

as measured by SCAM-2 versus the actual knownliterature redshift as determined through high-resolution spectroscopy (de Bruijn et al., 2002).

Figure 2.11.3/2: The observed stellar temperatureversus the literature temperatures for eight stellarobjects in the SCAM-2 sample (Reynolds et al., 2002).

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The SCAM-3 programme is based on the SCAM-2campaigns. SCAM-3 is therefore built around a 10 x 12-pixel array of tantalum-based STJs each 33 µm square(c.f. Fig. 2.11.4) covering a field of ~10 x 12 arcsec.

The IR rejection has also been improved with theintroduction of new filters allowing an increase inefficiency and resolving power to 34% and 13respectively, compared with 22% and 8 at 500 nm forSCAM-2. In addition, the red response has beenextended to 750 nm compared with 650 nm. Finally, theelectronics have been dramatically improved, withmodules operating in banks of 32 pixels. With such anapproach, single pixel rates of 8 kHz and 250 kHz perbank (i.e. a MHz for the whole array) has been achieved.This will allow SCAM-3 to take real advantage of the5 µs intrinsic timing ability to study short timescalephenomena.


While the SCAM-3 programme, about to enter itsoperational phase, will increase the field coverage so thatsingle objects can be observed in reasonable or even poor‘seeing’, while still being able to observe the surroundingsky background, the single-pixel approach will be alwayslimited. Clearly with each pixel requiring its own wiringand readout electronics, an expanded array can neverhope to be able to cover a significant field(~1 x 1 arcmin). In addition, larger pixels introduceserious degradation in performance. The solution that has

been introduced is the Distributed Readout OpticalImaging Detector (DROID). Fig. 2.12.5/1 shows thebasic principle of the DROID.

Essentially, photons are not absorbed directly in the STJbut in a superconducting absorber strip. The resultantcharge carriers diffuse along the strip until they reacheach end, where they are trapped by a lower bandgapmaterial and enter the STJs. The sum of the two STJsignals provides the energy of the photon, while theirratio is a measure of the position in one-dimension, thesecond dimension being simply the width of the strip.Such systems have been tested successfully at optical andX-ray wavelengths. Clearly packaging such individualdetectors into arrays as shown in Fig. 2.11.5/2 will allowlarge field coverage.


For observing at very remote sites, the general use of aSCAM instrument will be limited by the requirement tocool a tantalum detector to ~300mK by liquid helium.The availability of helium, coupled with complex fillingand cool-down procedure, could possibly precludeSCAM-type cameras becoming available as general userinstruments. Therefore it is the aim of the SCAM-5technology demonstration programme to provide atantalum-based SCAM camera cooled to 300mK by afully closed-cycle refrigeration system. This is achievedthrough the use of a Pulse Tube Refrigerator (PTR)coupled to a He4 sorption pump, which is then coupled to

Figure 2.11.5/2: The field coverage envisaged in theSCAM-4 programme. A deep field exposure from aCCD camera at the WHT prime focus is used asbackground.

Figure 2.11.5/1: The basic concept of the DROID.

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a second He3 sorption pump. The PTR provides a basetemperature of 4K from which the closed-cycle He4

pump takes the temperature to ~1K, from which the He3

pump provides the final base temperature of 300mK.Currently the system is under test and has achieved therequired base temperature. EMC and acoustic issues arenow being addressed prior to the start of device testing.


From Fig. 2.11.1/3 it is clear that STJs or DROIDS basedon tantalum will be limited in their resolving power to atbest ~25 at 500 nm. The purpose of the SCAM-6programme is to develop STJs and DROIDs based onlower bandgap materials. Two materials are currently indevelopment at the device level for the STJ”molybdenum and aluminium. Since aluminium (Tc ~ 1K,compared with 4.5K for Ta) is a basic building block ofTa-based STJs, it is natural to develop devices based onthis material as a precursor to developments in otherlower Tc materials. Aluminium devices, whichtheoretically should have a resolving power twice asgood as tantalum, have been developed to a level wherethey are now sensitive to optical photons. Fig. 2.11.7/1shows the spectrum from such a single STJ deviceilluminated by monochromatic 500 nm light.

In parallel with the developments in aluminium, devicesin Mo-Al have also been fabricated. Fig. 2.11.7/2 showsa large-format array of Mo prior to such STJs undergoingbasic junction tests such as current leakage andJosephson current suppression.

2.11.8 SCAM programme conclusion

The SCAM programme seeks to develop a new class ofinstrument for use by general astronomers, both forground-based and space-based platforms. The heart ofthe programme is the material science associated withsuperconductors. These materials offer for the first timethe technique of single photon counting coupled tomedium-resolution imaging-spectroscopy (Peacock etal., 1996). Design issues derived from the SCAMground-based observing runs will feed into future space-based spectrometers for applications in wavelength fromthe near-IR to the soft X-ray.

ReferencePeacock, A. et al., 1996, Nature 381,135.

Figure 2.11.7/2: A 32 x 10-pixel molybdenum testarray prior to such Mo-based devices undergoingtesting at 40mK in a cryostat.

Figure 2.11.7/1: The optical spectrum from 500 nmphotons recorded by a pure aluminium-based STJoperated at 40mK.

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2.12 Advanced sensor, optics and instrumentdevelopment research

X-ray optics and detectors are being developed for space-based astrophysics observatories and planetary missions.In the area of semiconductor-based photon detectors,compounds like gallium arsenide (GaAs), thalliumbromide (TlBr), indium phosphide (InP) and narrowbandgap materials are the focus of the research.

2.12.1 Compound semiconductor photon detectors

GaAs has attracted considerable interest as a viablealternative to Si or Ge for the detection of X-rays abovea few keV. It has a simple cubic lattice structure and isone of the high group compound semiconductors with abandgap sufficiently wide (1.42 eV) to permit room-temperature operation but small enough so that its Fano-limited spectroscopic resolution is close to that of Si.

A small GaAs array was produced by growing an ultra-pure 325 µm epitaxial layer onto an n+ semi-insulatingsubstrate using chemical vapour phase depositiontechniques. To reduce leakage currents, a 10 µm thick p+

layer was then deposited onto the epi-layer, forming a p-i-n structure. This layer was then patterned by etching, tocreate a 4 x 4-pixel structure surrounded by a guard ring(Fig. 2.12.1/1). The pixel sizes are 350 x 350 µm with aninter-pixel gap of 50 µm. Contact with the pixels isachieved by wire bonding. In this configuration, biasingthe n+ side and collecting off the p+ side utilises holecharge collection, preamplified by low capacitance FETs.The array uses resistive feedback preamplifiers in theform of hybrids, also mounted directly on the substrate.The leakage currents were low enough to permit room-

temperature operation, with typical FWHM energyresolutions of 600 eV at 5.9 keV and 0.7 keV at59.54 keV (pulse width 550 eV).

The spatial uniformity of the array was evaluated onbeamline X1 using a 15 keV pencil beam of size20 x 20 µm, normally incident on the pixels. Thedetector is very uniform over the surface of each pixeland the array, as shown in Fig. 2.12.1/2.

Wide-gap compound semiconductors offer thepossibility of room-temperature operation, whilemaintaining sub-keV spectral resolution at hard X-raywavelengths. The ability to mix and match availableband-gaps and stopping powers is commerciallyattractive, since it suggests that materials can be tailored

Figure 2.12.1/1: Left: photomicrograph of the 4 x 4 GaAs detector assembly used in the present study. The deviceis die-attached to the substrate, which in turn is mounted on a 2-stage Peltier cooler. Right: the completed GaAsarray/hybrid/substrate assembly.

Figure 2.12.1/2. A surface plot of the spatial variationof the gain (i.e., the fitted centroid position) across the4 x 4 GaAs array measured at HASYLAB using a15 keV, 20 x 20 µm pencil beam. The spatial samplingin X and Y was 10 µm.

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for specific applications and wavelengths. Of availablematerials, TlBr and InP are two of the least studied.

TlBr has emerged as a particularly interesting materialfor room-temperature hard X-rays and gamma-rayapplications, in view of its wide band-gap (2.5 times thatof Si) and high atomic numbers (Tl = 81, Br = 35) of itsconstituent atoms. In fact, its density (7.5 g cm–3) iscomparable to bismuth germanate and thus it hasexcellent stopping power for hard X-rays and gamma-rays. Prototype detectors have been fabricated from athermally grown mono-crystal, produced by theBridgeman-Stockbarger technique and tested on the X-1beamline at HASYLAB. Measurements were carried outover the energy range 10.5-100 keV. We have produced athird generation of detectors making severalmodifications in material production and detector design.Several new devices have been fabricated, including aprototype 3 x 3 array, shown in Fig. 2.12.1/3.

InP is a group III-V direct band-gap material whoseresistivity and mobilities are intermediate between Si andGaAs. While the rest of its properties are similar toGaAs, it is potentially a more attractive material becauseof its larger stopping power (2-3 times that of GaAs), andhigher drift velocities (again, 2-3 times that of GaAs).

InP was synthesised from solution and purified byvacuum distillation. Semi-insulating material wasproduced by doping with Fe and a monocrystal grown byliquid-encapsulated Czochralski. Wafers were slicedfrom the boule along the <100> direction and detectorplatelets diced from the wafer. These were lapped andpolished by chemical and mechanical processing to a

thickness of 180 µm. A p+ layer was then deposited onone side of the plate by vapour-phase epitaxy using Zn asa dopant. Circular Au/Ti contacts of diameter 2 mm weredeposited on the top and the bottom of the plate. Thecompleted detector and its response is shown inFig. 2.12/.14. The device is clearly spectroscopic and, infact, these data represent the best spectroscopicperformance yet reported for an InP detector.

Figure 2.12.1/4: Top: the first prototype 3.14 mm2

180 µm-thick InP detector. Centre: the detector’sresponse to a 40 keV, 20 x 20 µm X-ray beam. Bottom:a composite of energy-loss spectra recorded atHASYLAB.

Figure 2.12.1/3: Left: the world’s first 3 x 3, 1 mm thick TlBr array. The array has a pixel size of 350 x 350 µm withan interpixel gap of 100 µm. Right: spatial response of the array to a 15 keV, 20 x 20 µm X-ray pencil beam.

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2.12.2 Low-mass X-ray optics

ESA, together with European industry, is exploring theX-ray optics technologies for the next generation ofspace astrophysics and planetary missions currentlyunder design. A number of technologies are under study,ranging from low-mass replication processes builtaround conventional Wolter-I nested geometries as wellas radically different approaches. In the later case, e.g.the technology used to produce glass micro-channelplates (MCPs) is used to produce X-ray optics with verythin reflecting surfaces, of the order of only a fewmicrometers.

Note that a Wolter-1 configuration comprises, as a basicelement, a paraboloid (P) coupled to a hyperboloid (H)and is shown schematically in the left side ofFig. 2.12.2/1. To achieve a reasonably large collectingarea, pairs of shells (P+H) are stacked inside each other.To ensure an adequate imaging resolution, these shellsmust be stiff and well aligned, leading to bulky andheavy optics. On the right side of Fig. 2.12.2/1 theimplementation of a conical approximation to a Wolter-1 system based on MCPs is shown. Such a systemallows the substantial reduction of the mirror wallthickness, due to an additional radial structure. Such asystem can therefore be made very much lighter thancurrent state-of-the art optics, maintaining the requiredmechanical stiffness of the reflecting surfaces. Themirror plate thickness can be reduced by a factor of afew 100.

The conical approximation to the Wolter-1 geometry isacceptable, if the length of the reflecting surfaces(indicated as ‘L’ in Fig. 2.12.2/1) is small compared withthe focal length of the system (‘F’ in the figure).

Such a compact and light lens has been made for the firsttime in a geometry that produces true X-ray imaging.This lens has been manufactures under ESA contract byPhotonis (F) with support from Leicester UniversitySpace Centre (UK). Testing has been performed by ESAstaff in collaboration with the Bessy PTB synchrotronfacility in Berlin (D) and at the European SynchrotronRadiation Facility in Grenoble (F), with support providedby personnel of the the Univ. of Leicester.

MCPs have been developed for image intensifiers andphoton-counting detectors, and their mass production hasreached a high level of optimisation. Inherent to theproduction process, which involves severe stretching ofthe glass fibres, very smooth walls are obtained, whichare arranged in a regular geometry. Starting with a slab ofmaterial, the glass is drawn into long and thin fibres,which are then grouped into multi-fibres and drawnagain. Finally the multi-fibres are stacked to the desiredgeometry, and then fused to form a monolithic block. Theblock is then cut into slices, which are then slumped tothe required radius and finally etched to form pores byremoving the core glass. To adapt the MCPs for use asX-ray optics, it was necessary to change and improve themicro-fibre geometry and reduce the surface roughness.The resulting optics are, however, very rigid andextremely light. In fact, the optics are also very robust,since the specific mass and the corresponding forcesduring vibration are low.

A prototype X-ray optics consisting of two circular platesof 60 mm diameter, each plate being 5 mm thick, wasproduced, and is shown in the left part of Fig. 2.12.2/2.Each plate contains 20 million almost perfectly squareholes, each 10 µm in diameter with a wall thickness of amicron (right part of Fig. 2.12.2/2). The MCP plates are

Figure 2.12.2/1: A Wolter-1 X-ray telescope showingthe key parameters, left. Only grazing incidencereflections are used. Concentric stacking is essentialfor achieving a practical effective area for the system.By implementing the concentric mirrors in twoMCPs, as shown on the right side, the packing densityincreases and the mirror thickness can besubstantially reduced owing to the radial wallsstabilising the optics.

Figure 2.12.2/2: SEM micrograph of the hierarchicalstructure of the prototype MCP X-ray ‘lens’.

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made of glass with a high bismuth content, to increasethe X-ray reflectivity and improve the processing of theglass. To achieve the conical approximation to a Wolter-1geometry, one plate is slumped to a spherical profile witha radius of curvature of 20 m, the other to a radius ofcurvature of 6.7 m. In combination, this doublet has afocal length of 5 m, which was chosen to facilitate X-raytesting. Fig. 2.12.2/2 shows the hierarchical structure ofthe radially packed square micro-fibres in the MCPs ofthese optics. The RMS surface roughness is 10 Å(measured 20-2000 mm–1), which is sufficiently smoothto reflect medium-energy X-rays.

This X-ray optic behaves in the same way as a normalbiconvex lens in the visible range. It is effectively anX-ray lens. The mass of the 60 mm diameter prototype is28.5 g (10 kg m–2, in comparison with ~900 kg m–2 forXMM-Newton). Half the focused radiation of theseoptics falls within a circle with a diameter of 1.0 arcmin.This is only a factor of 4 larger than the imagingresolution of XMM-Newton, with a much larger specificmass (with 350 kg at a diameter of 700 mm, i.e.910 kg m–2). If this imaging quality were to be furtherimproved, it might be possible to build a comparablemirror system for under 10 kg with accompanyingsavings on mission costs, as illustrated in Fig. 2.12.2/3.

An alternative technology to produce MCPs ismicromachining of silicon. Silicon of very high quality isavailable on the market today, and the methods andprocesses to structure it have been developed in recentdecades with enormous efforts by the electronicsindustry. Silicon also very good thermal and mechanicalproperties:

— good thermal conductivity;

— good stiffness;— low specific mass;— high uniformity (monocrystalinity).

The main advantage of this approach is, next to thesuperior material qualities of silicon over glass, theintrinsically excellent alignment of the individual porewalls owing to the crystalline structure of the material.By using lithographic techniques to pattern the surface ofsilicon wafers and applying standard industrialprocesses, very accurate geometries can be realised witha significant freedom in the design.

The main development is concentrated on the processesnecessary to produce deep structures in the Si wafers,with very smooth surfaces. The later is difficult, withoutdestroying the general surface geometry or figure.

The crystalline structure of Si and the associated etchingprocesses permit only the fabrication of squarestructures, but not radial ones, which are in principlerequired for the X-ray optics. The solution to thisproblem is the division of the optics into narrow strips,arranged in concentric circles and covering the completeaperture. The individual strips are limited in width by thesize of the angular resolution element in the focal plane(e.g. in the case of XEUS the plate scale is 250 µm perarcsec, and therefore the angular resolution element isabout 1 mm in the focal plane, corresponding to 4 arcsec,and therefore the silicon strips would be limited in theirwidth to about 1 mm). The length of the strips would belimited by the size of available silicon wafers used asstarting material, nowadays 300 mm in diameter. Inpractice, the MCP strips would therefore be about 1 mm

Figure 2.12.2/4: Si MCP optics architecture. TheX-ray optics are composed of strips of Si grids(MCPs) of width W, arranged concentrically aroundthe optical axis. The strips are deformed elastically intheir mounting structure, which, for thermal reasons,is also Si.

Figure 2.12.2/3: Mass density comparison of thenickel-based XMM optics and a glass-based MCPoptics prototype. The angular resolution of the XMMoptics is only a factor of 4 better than that of this firstradially-packed doublet MCP X-ray optics prototypeever produced.

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wide and 200 mm long, slightly trapezoidal to bettercover the aperture in the radial arrangement, asschematically shown in Fig. 2.12.2/4. Note that theeffective area of each strip is highly comparable to thearea covered by each shell in a traditional nested systembased on electroformed nickel or bent aluminium foils.

The MCP strips are assembled into the X-ray optics usingvery stiff support structures, made also of Si andproduced by either traditional and/or micromachiningtechniques. The geometry of the support structure ischosen to produce a rigid body and at the same timeminimise the projected area in the optical axis. The MCPstrips are elastically formed into the required figure.

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65

3.1 Astrophysics Missions Division3.1.1 Herschel3.1.2 Planck3.1.3 Eddington3.1.4 James Webb Space Telescope3.1.5 Gaia3.1.6 COROT3.1.7 Darwin3.1.8 DTP on SMART-2-Plus3.1.9 XEUS3.1.9 ISS payloads: Lobster-ISS, EUSO, ROSITA

3.2 Solar and Solar-Terrestrial Missions Division3.2.1 Introduction and overview3.2.2 Ulysses3.2.3 SOHO3.2.4 Cluster3.2.5 Double Star3.2.6 Solar Orbiter3.2.7 Solar-B

3.3 Planetary Missions Division3.3.1 Introduction and overview3.3.2 Cassini/Huygens3.3.3 Rosetta3.3.4 Mars Express3.3.5 SMART-13.3.6 BepiColombo3.3.7 Venus Express3.3.8 The Cosmic DUNE mission definition study

3.4 Fundamental Physics Missions Division3.4.1 Introduction3.4.2 LISA3.4.3 SMART-23.4.4 STEP3.4.5 Hyper3.4.6 Microscope

3.5 Space Telescope Operations Division

3.6 Science Operations and Data SystemsDivision

3.6.1 Overview and general activities3.6.2 ISO3.6.3 XMM-Newton3.6.4 Integral3.6.5 Astro-F3.6.6 Herschel science operations development

3.7 Science Payloads Technology Division /Science Payload and Advanced ConceptsOffice

3.7.1 Overview of activities3.7.2 Assessment phase of future missions

BepiColomboSolar OrbiterDarwin/SMART-3XEUSInternational Space Station (ISS) payloads

3.7.3 Towards a strategic approach to future missiondevelopment

3.7.4 Coordination and development of new payloadtechnologies

3.7.5 Payload support to ESA science projects3.7.6 Technical infrastructure support to RSSD

research programme

3. SCIENTIFIC SUPPORT ACTIVITIES

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scientific support activities 67

Chapter 3 addresses the contributions of RSSD ProjectScientists and covers the mission–related activities of theDepartment. These encompass ESA’s science missions intheir orbital and post-operations phases, the approvedmissions under or awaiting development, and missionsunder study. ‘Europeanised’ missions led by a nationalagency and potential International Space Station (ISS)payload elements are included.

The chapter is structured by Division, reflecting theRSSD organisation at the end of the reporting period (seeTable 3). As stated in Chapter 1, RSSD has four MissionsDivisions (Sections 3.1 to 3.4) and two OperationsDivisions (Sections 3.5 and 3.6). The responsibilities andactivities of the former Science Payloads TechnologyDivision (now the Science Payload and AdvancedConcepts Office) are summarised in Section 3.7.

For astronomy missions (excluding HST), the Astro-physics Missions Division has responsibility for Project

and Study Scientist support until in-orbit commissioning.Responsibility for the development and execution ofscience operations and, after completion of the in-orbitcommissioning phase, for the mission management restswith the Science Operations and Data Systems Division.The Space Telescope Operations Divisions hosts theESA staff supporting the Hubble Space TelescopeScience Institute (STScI) in Baltimore (US) and theEuropean Coordinating Facility (ST-ECF) in Garching(D).

For the sake of brevity, the instruments, PrincipalInvestigators, mission or interdisciplinary scientists,science team members etc. of the missions described arenot tabulated here. Such information may be found inESA’s report to COSPAR, the most recent being beingESA SP-1259 (August 2002), produced by the RSSDProject Scientists, and in the relevant Web pages (theaddresses are included here as footnotes with eachmission description).

Table 2: Research and Scientific Support Department 2002 – Projects and Studies.

Division Astrophysics Solar Planetary Fundamental Space Science Ops.Missions Missions Missions Physics Telescope & Data

Opserations Systems

Missions in Ulysses Cassini/ HST ISOOperation or SOHO Huygens XMMPost-Operation/ Cluster -NewtonArchive Phase Integral

Missions in or Herschel Double Star Rosetta LISA Astro-Fawaiting Planck Solar Orbiter Mars Express Microscope Herscheldevelopment Eddington SMART-1 science ops.

JWST Venus ExpressGaia BepiColomboCOROT

Mission and Darwin ILWS SMART-2ISS Payload XEUS Solar-B HyperStudies ISS*

* Lobster-ISS, EUSO, ROSITA

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68 scientific support activities

3.1 Astrophysics Missions Division

3.1.1 HerschelG. Pilbratt

The ‘Herschel Space Observatory’ (formerly known asthe ‘Far InfraRed and Submillimetre Telescope’, orFIRST) is a multi-user observatory-type mission thattargets approximately the 57-670 µm wavelength rangein the far-IR and submillimetre spectrum, providingobservation opportunities for the entire astronomicalcommunity. Herschel is now being implemented as anelement of the next major astronomy mission set in‘Cosmic Vision’, the new ESA Space ScienceProgramme, with a planned launch in 2007.Herschel is designed to address the ‘cool’ Universe. Ithas the potential of discovering the earliest epoch proto-galaxies, revealing the cosmologically evolving AGN-starburst symbiosis, and unravelling the mechanismsinvolved in the formation of stars and planetary systembodies.

Herschel will complement other facilities by offeringspace observatory capabilities in the far-IR and sub-millimetre for the first time, extending the wavelengthcoverage longwards from that of, for example, IRAS,ISO, SIRTF and Astro-F, and shortwards of SWAS andOdin. A major strength of Herschel is its photometricmapping capability for performing unbiased surveysrelated to galaxy and star formation. Redshiftedultraluminous IRAS galaxies peak in their spectralenergy distributions (SEDs) around 50-100 µm (in theirrest frames). Similarly, class 0 proto-star and pre-stellarobjects also have SEDs that peak in the Herschel primeband. Herschel is also well equipped to performspectroscopic follow-up observations to further charac-terise particularly interesting individual objects.

In order to fully exploit the favourable conditions offeredby being in space, Herschel needs a precise, stable andvery low-background telescope and a complement ofvery sensitive scientific instruments. The Herscheltelescope will be be passively cooled (to maximise size)while the instruments will be housed inside a superfluidhelium cryostat, on top of which the telescope ismounted. The three instruments, provided by consortialed by PIs in return for guaranteed observing time, are:

— the Photodetector Array Camera and Spectrometer(PACS) is a camera and low- to medium-resolutionspectrometer for wavelengths up to 210 µm;

— the Spectral and Photometric Imaging REceiver(SPIRE) is a camera and low- to medium-resolutionspectrometer for wavelengths longer than 200 µm;

— the Heterodyne Instrument for the Far Infrared(HIFI) is a heterodyne spectrometer. It offers veryhigh velocity resolution for a single pixel on the sky.

The spacecraft has a modular design:

— the extended payload module with a superfluidhelium cryostat housing the instrument focal planeunits, and supporting the telescope, the sun-shield/shade and payload-associated equipment;

— the service module, providing the infrastructure andresources such as power, attitude and orbit control,onboard data handling and command execution,communications, and safety.

Herschel will be launched by an Ariane-5 shared withPlanck (see 3.1.2), and will operate from the vicinity ofL2, 1.5 million km away from the Earth in the anti-sunward direction. L2 offers a stable thermalenvironment with good sky visibility. Commissioningand performance verification will take place enroutetowards L2. Once these crucial mission phases arecompleted, Herschel will go into routine scienceoperations for a minimum duration of 3 years.

The scientific operations will be conducted in a noveldecentralised manner. The operational ground segmentcomprises six elements:

— the Herschel Science Centre (HSC), provided byESA;

— three dedicated Instrument Control Centres (ICCs),one for each instrument, provided by their PIs;

— the Mission Operations Centre (MOC), provided byESA;

— the NASA Herschel Science Center (NHSC),provided by NASA.

The HSC acts as the interface to the science communityand outside world in general, supported by NHSC for theUS science community. The HSC/NHSC providesinformation and user support related to the entire life-cycle of an observation, from calls for observing time, todata processing, archiving and distribution to theirowners. The Science Operations and Data SystemsDivision is responsible for the implementation of thescience operations (Section 3.6.6).

3.1.2 PlanckJ. Tauber

The Planck mission is designed to image the anisotropiesof the Cosmic Background Radiation Field (CBRF) overthe whole sky, with unprecedented sensitivity(∆T/T ~ 2 x 10–6) and angular resolution (better than10 arcmin). Planck will allow the testing of currenttheories of the early Universe and of the origin of cosmicstructure.

The ability to measure the angular power spectrum of theCBRF fluctuations to high accuracy will allow thedetermination of fundamental cosmological parameterssuch as the density parameter and the Hubble constant,with a few percent uncertainty. In addition to the main

http://astro.esa.int/herschel/ http://astro.esa.int/planck/

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cosmological goals of the mission, the Planck sky surveywill produce a wealth of information on the properties ofextragalactic sources, and on the dust and gas in ourGalaxy. For instance, Planck will measure the Sunyaev-Zeldovich effect in many thousands of Galaxy clusters.

Planck comprises three basic components:

— a telescope and baffle system, providing the angularresolution and rejection of straylight;

— a Low Frequency Instrument (LFI), an array of tunedradio receivers, based on HEMT amplifiers,covering the frequency range 30-100 GHz andoperated at 20K;

— a High Frequency Instrument ( HFI), consisting of anarray of bolometers operated at 0.1K and covering100-857 GHz.

Planck will be launched together with the Herschelobservatory (see 3.1.1). It will be placed into a Lissajousorbit around the L2 Lagrange point of the Earth-Sunsystem. At this location, the payload can be continuouslypointed in the anti-Sun direction, thus minimisingparasitic signals induced by thermal fluctuations andstraylight entering the detectors through far sidelobe. Thespacecraft is spin-stabilised at 1 rpm and the viewingdirection of the telescope is offset by 85º from the spinaxis, so that the observed sky patch traces a great circleon the sky. Planck will carry out two complete surveys ofthe full sky in about 15 months.

Planck is a survey-type project which is being developed

and operated as a PI mission. The instruments are beingprovided by two PI teams, who will also man and operatetwo Data Processing Centres responsible for theprocessing of all Planck data. All-sky maps in 10frequency bands will be made publicly available a yearafter completion of the mission, as well as a firstgeneration set of maps of the CBRF, Sunyaev-Zeldovicheffect, dust, free-free and synchrotron emission. The timeseries of observations (after calibration and positionreconstruction) will also be made available on-line.

In early 1999, ESA selected two Consortia of scientificinstitutes to provide the two Planck instruments. LFI isbeing developed by a Consortium led by R. Mandolesi ofthe Istituto TeSRE (CNR) in Bologna (I). HFI is beingdeveloped by a Consortium led by J.-L. Puget of theInstitut d’Astrophysique Spatiale (CNRS) in Orsay (F).In total, more than 40 European and US institutes arecollaborating on the development, testing and operationof the Planck instruments and the final data analysis.

In early 2000, ESA and the Danish Space ResearchInstitute (DSRI, Copenhagen) signed an Agreement forthe provision of the two reflectors that constitute thePlanck telescope. DSRI leads a Consortium of Danishinstitutes. In late 2000, it issued an Invitation to Tender(ITT) to industry for the development of the Planckreflectors. The winning bid was by Astrium GmbH(Friedrichshafen, D), who will manufacture the reflectorsusing state-of-the-art carbon fibre technology. At the endof 2002, the design of the reflectors was finished, themoulds needed for the layout of the facesheets wereadvanced, and all was proceeding according to plan.

In early 1999, ESA selected Alcatel Space (F) to carryout a detailed study of the architecture of the Planckpayload. This study was completed in early 2000, andlaid the basis for the issue in September 2000 of an ITTto industry for the procurement of the Herschel andPlanck spacecraft. From the submitted proposals, a singleprime contractor, Alcatel Space, was selected in early2001. Alcatel Space is supported by two majorsubcontractors: Alenia Spazio (Torino, I) for the ServiceModule, and Astrium GmbH (Friedrichshafen, D) for theHerschel Payload Module; and by many other industrialsubcontractors from all ESA member states. The detaileddefinition work (Phase-B) began in June 2001, and iswell advanced. The Preliminary Design Review wascompleted in December 2002. The current design ofPlanck is shown in Fig. 3.1.2.

In parallel, instrument development is proceeding largelyaccording to schedule, in spite of a number of financialdifficulties during 2002. Some hardware subsystems arealready being manufactured and tested. The firstdeliveries of instrument qualification models areexpected in late 2003, with the flight models due in early2005. The development of the spacecraft and payload ison track for a launch in February 2007.

Figure 3.1.2: Planck in orbit. (Alcatel Space)

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3.1.3 Eddington F. Favata

The two key science goals of the Eddington mission are:

— to map the interior structure of stars spanning a rangeof mass, age and chemical composition;

— to detect a significant number of planetary systemsspanning a range of planetary sizes and orbitalperiods, with an emphasis on the detection ofhabitable planets.

While the stellar structure will be investigated by meansof asteroseismology, planetary systems will be detectedthrough the transit method, looking for the minute dips inthe starlight caused by a transiting planetary body. Bothgoals require high-precision, wide-field, long-durationoptical photometry, and therefore can be effectivelyimplemented in a single space observatory.

The accurate asteroseismic investigations performed byEddington will bring stellar astrophysics to new,quantitative grounds, allowing, for example, the accuratedating of individual stars and stellar populations. Openclusters are expected to be among Eddington’s keytargets, as are old, Population-II stars. Nucleosynthesiswill be studied in detail by mapping the interior structureof massive stars, which are the precursors of type-IIsupernovae.

Eddington’s goal of finding habitable planets (planetswith a rocky surface, sufficient gravity to hold anatmosphere and a temperature compatible with thepresence of liquid water) will have a clear impact on thepublic at large. At the same time, Eddington will providea large, statistically significant database on thecharacteristics of planetary systems spanning a broadrange of parameters (e.g. mass, orbital period,eccentricity), supplying the data needed for acomprehensive theory of the formation and evolution ofplanetary systems.

Long-duration, accurate space-based photometry willalso permit a number of additional scientificinvestigations to be carried out, including the study oflong-term variability from, for example, AGN andcompact binaries, or the detection of transientphenomena, such as novae and supernovae.

Eddington was originally proposed to ESA in 2000 inthe framework of the ‘F2/F3’ call for proposals, and itwas then selected with a ‘reserve’ status. In May 2002,the SPC formally approved it for implementation in thecontext of the Herschel/Planck project. The targetlaunch date is 2007. The baseline configuration forEddington (subject to confirmation from the ongoingfinal study) is a split-aperture four-telescope systemwith a mosaic of CCD camera (six chips per camera), acollecting area equivalent to that of a 1.2 m monolithic

telescope and a FOV 5º in diameter. The payload will bemounted on top of a copy of the platform used for theHerschel mission. Eddington will be placed into an L2orbit by a Soyuz-Fregat vehicle, for 5 years of opera-tions. For 3 years, planet finding will be the primaryscience goals, while 2 years will be dedicated to astero-seismologic observations of typically 1-2 monthsduration. The planet-finding programme will consist ofa single, 3-year observation of the same field, allowingthe detection of repeated transits of planets with periodsup to a year.

Eddington will be implemented as a facility-typemission, fostering a wide involvement of the scientificcommunity. The observing programme will be subject toa broad community consultation. The area to be searchedfor habitable planets will be selected during an openworkshop to be held in Palermo (I) in April 2003. Thepointing directions for the asteroseismic observationswill be subject to an AO. All Eddington data will be madeimmediately accessible to the entire European scientificcommunity, without any proprietary period. Eddington’sscientific operations will be carried out by the EddingtonScience Centre (ESC), provided by ESA under theresponsibility of RSSD. The ESC will be the interface tothe external scientific community, and will ensure thatEddington data are properly calibrated before beingdistributed.

3.1.4 James Webb Space Telescope P. Jakobsen

NASA, ESA and the Canadian Space Agency (CSA)have since 1996 collaborated on a worthy successor tothe Hubble Space Telescope, the so-called NextGeneration Space Telescope. The observatory, which isscheduled for launch in the 2010-2012 time frame, wasin 2002 renamed the James Webb Space Telescope(JWST; Fig. 3.1.4), in honour of NASA’s secondadministrator. ESA’s participation in the mission wasformally approved as a Flexi-mission by the ScienceProgramme Committee in October 2000.

JWST is to consist of a passively cooled, 6 m-classtelescope, optimised for diffraction-limited performancein the near-IR (1-5 µm) region, but with extensions toeither side into the visible (0.6-1 µm) and mid-IR (5-28 µm) regions.

The large aperture and shift to the IR embodied by JWSTis, first and foremost, driven scientifically by the desireto follow the contents of the faint extragalactic Universeback in time and redshift to the epoch of ‘First Light’ andthe ignition of the first stars. Nonetheless, like itspredecessor, JWST will be a general-purpose observa-tory capable of addressing a very broad spectrum ofoutstanding problems in galactic and extragalacticastronomy.

http://sci.esa.int/home/eddington http://astro.estec.esa.nl/NGST/

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JWST will carry the following complement of threeinstruments:

— Near-IR Wide Field Camera covering 0.6-5 µm;— Near-IR Multi Object Spectrograph covering 1-

5 µm;— Mid-IR combined Camera/Spectrograph covering 5-

28 µm.

In contrast to HST, JWST will be placed into a Sun-EarthL2 halo orbit and will not be serviceable after launch. Itwill therefore not be possible to repair or replace theseinstruments over the lifetime of the observatory.

The JWST telescope proper and its three instruments areto be cooled in bulk to < 50K, a temperature determinedby the operating temperature of the (InSb and HgCdTe)detector arrays covering the prime near-IR 1-5 µm range.Cooling is passive by placing the observatory at L2 andkeeping the telescope and its instrumentation in perpetualshadow by means of a large deployable sunshade.

In order to fit into the shrouds of suitable launchers, it isnecessary to fold the primary mirror during launch. Thefine pointing required to exploit the telescope spatialresolution will be achieved by deflecting the telescopeimage by means of a fast steering mirror controlled by afine guidance sensor located in the telescope focal plane.

ESA’s participation in JWST will follow closely thesuccessful HST model, and consist of three mainelements:

— Scientific instrumentation. ESA will provide theNear-IR Multi-Object Spectrograph. In addition,through special contributions from its member

states, Europe will provide the Optics Module for theMid-IR Camera/Spectrograph to be developedjointly by NASA and ESA. Both instruments arepresently undergoing definition studies in industryand the scientific community;

— Non-instrument flight hardware. ESA’s non-instrument contribution to JWST is being negotiated.The possibility of ESA providing the launcher forJWST is being explored;

— Contributions to operations. ESA will participate inJWST operations in a similar manner as on HST.

Through its contributions, ESA will gain a ~15%partnership in JWST and secure for astronomers from itsmember states full access to the observatory on identicalterms to those enjoyed today on HST. They will haverepresentation on all advisory bodies of the project andwill win observing time through a joint peer-reviewprocess, backed by a guarantee of a minimum ESA shareof 15%.

3.1.5 Gaia M. Perryman

By extending the successful Hipparcos concept to faintermagnitudes and higher accuracies, Gaia will provideunprecedented positional and radial velocity measure-ments with the precision needed to produce a stereo-scopic and kinematic census of about a billion stars inour Galaxy and throughout the local group. Combinedwith on-board multicolour photometry, these data willallow us to quantify the early formation and subsequentdynamical, chemical evolution of the Milky Way.Additional scientific output includes the detection andorbital classification of tens of thousands of extra-solarplanetary systems, a comprehensive survey of manydifferent astrophysical sources, from huge numbers ofminor Solar System bodies to some 500 000 distantquasars. Gaia will also provide a number of stringentnew tests of general relativity and cosmology.

Approval of a Concept and Technology Study for Gaiawas given in 1996. A 1-year industrial study took placebetween mid-1997 and mid-1998, with the support of anad hoc scientific advisory group. The resulting report,ESA-SCI(2000)4, July 2000, presented the scientificcase, a technical design, the mission performanceassessment and a description of the proposed approach tothe data analysis and mission management. On the basisof this study, Gaia was selected as one of the nextCornerstone missions of the ESA science programme bythe SPC in September 2000. The design included twoseparate astrometric telescopes (viewing directions) eachwith its own focal plane, and a dedicated telescope forradial velocity and medium-band photometry. Launchwas foreseen by Ariane-5, with operation at the L2Lagrange point. Through on-board object detection, allbillion objects down to 20 mag would be observed, with

Figure 3.1.4: JWST concept. (TRW/Ball)

http://astro.estec.esa.nl/gaia

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resulting astrometric accuracies of about 10 microarcsecat 15 mag.

At the end of 2001, as a result of the Council Meeting atMinisterial Level, the revised ESA science programmefunding suggested that the high costs of the majorCornerstone missions could not be supported, and amajor review of the overall ESA science programme wasundertaken by the agency’s advisory bodies, with a targetdate for completion of the review of June 2002. The Gaiaproject initiated a rapid technical reassessment study,starting in December 2001 and with a duration of6 months. The constraints on the launch vehicle wererelaxed, and the detailed industrial reassessment study,again supported by the Gaia Science Team, identified apayload design compatible with the smaller and cheaperSoyuz launch vehicle, but otherwise maintaining all ofthe primary scientific goals. Gaia was confirmed withinthe ESA programme by the SPC in June 2002, with atarget launch date in mid-2010.

The redesigned mission is now being subjected tointensive technical and scientific optimisation andinvestigation, in which the Gaia Science Team issupported by 15 scientific working groups focused onparticular aspects of the overall design and optimisation.On the technical side, all of the major industrialdevelopment activities related to the advanced technicalactivities (focal plane, on-board data handling, siliconcarbide mirror manufacture, etc), including two majorindustrial technical assistance contracts, started during2002. On the scientific side, working groups devoted tothe satellite design (accuracy, on-board detection,calibration, etc), to the treatment of specific objects(double stars, variable stars, Solar System objects, etc),and to the data analysis activities have made considerableprogress. A highlight has been the completion of the firstprototype of the data analysis environment for Gaia,which is successfully handling the ingestion of simulatedsatellite telemetry, and which will form the basis formore extensive development of the data analysis systemover the coming years.

The immediate goal is to complete all technicaldevelopment activities, and the associated scientificdesign, by the end of 2004, allowing for the detaileddefinition and Phase-C/D of the mission to begin in2005, consistent with a launch date in early 2010.

3.1.6 COROT F. Favata

COROT (COnvection, ROtation and planetary Transits)is a CNES-led mission that will perform astero-seismology and planet-finding using the transit method.The mission will be based on a Proteus platform. Thepayload of COROT consists of a 27 cm-diametertelescope and a mosaic CCD camera (of four chips) with

a 2.8 x 2.8º FOV at its focal plane. The polar orbit ofCOROT allows it to observe two sky directions for6 months at a time. The long observations imply thatvery high precision will be reached on the oscillationfrequencies, allowing, for example, the mapping of theinterior rotation of the target stars.

COROT will be the first space-based search for extra-solar planets using the transit method. Its performancewill allow it to find large rocky planets in near orbits.While limited to planets significantly larger than theEarth, COROT is thus well-placed to discover the firstextra-solar planets around normal stars that are not gasgiants (like all those discovered to date via the radialvelocity method). In addition, the COROT data willallow us to study a number of additional science topics,including stellar activity and surface rotation.

Originally proposed in 1996 as a CNES-only mission, anumber of European partners joined the programme inthe course of 1999 and 2000. In particular, the COROTproject applied for ESA support in 2000 in the context ofthe F2/F3 call for proposals. As a result, a €2 millioncontribution was approved by ESA’s advisory bodies.Under this scheme, ESA is contributing the telescopeoptics and the payload environmental tests. In return,scientists in ESA member countries will have access toCOROT data. The satellite is planned for launch at theend of 2005.

3.1.7 Darwin M. Fridlund

Darwin is ESA’s mission to search for terrestrialexoplanets, i.e. worlds like our own orbiting other stars,with the explicit purpose of determining their ability tohost life as we know it. Darwin is baselined as a space-deployed interferometer, operating in the mid-IR andconsisting of six free-flying telescope units and aseparate beam-combiner unit and a communications andcontrol spacecraft. Planned for a launch after 2013, andpossibly in a joint mission with NASA, the Europeanroadmap leading to a Darwin mission is following threeparallel paths:

— a phase of intensive technology development,mainly through Technology Research Programme(TRP) activities with industry and laboratories;

— the definition of a ground-based precursor instru-ment (GENIE: Ground-based European NullingInterferometer Experiment), in close collaborationwith ESO. This instrument is being developed with atwo-fold purpose. It is primarily to gain theexperience in building and operating such aninstrument, including the development of therequired technology. Secondly, it will carry out therequired precursor science. A major disturbing factorin obtaining exoplanetary data in the mid-IR will be

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the large amount of zodiacal dust in the targetsystems, the so-called exo-zodi emission. All Darwintargets will have to be screened in advance in orderto select only those where a planetary signal can beobtained in a reasonable time. This will be done withGENIE;

— the third avenue is the definition of ways ofcooperation between Darwin and its NASAcounterpart, the Terrestrial Planet Finder (TPF). Anagreement has been made with NASA for a first3-year phase of scientific cooperation andtechnological coordination. The study scientists andmanagers on both sides participate in both studies.ESA is also represented in the TPF team by twoexternal scientists, while two US scientists aremembers of the Darwin study team. The aim of thisfirst phase of collaboration is for ESA and NASA todefine, by 2007, the final architecture of a jointmission.

3.1.8 DTP on SMART-2-Plus M. Fridlund

For SMART-2 (see 3.4.3), the option of including aDarwin Technology Package (DTP) to verify thetechnology required for formation flying, was alsoactively studied. This necessitated two spacecraft andwas referred to as ‘SMART-2-Plus’.The DTP packageconsisted of the following elements: Formation Flying(deployment, collision avoidance and RF metrology witha precision of about 1 cm), Precision Formation Flyingalong one axis (High Precision Optical Metrology withan accuracy of about 1 µm), and verifying the need for anoptical delay line in the Guidance, Navigation andControl (GNC) system. The actual hardware consisted ofa set of RF antennas, an optical metrology bench, alateral sensor, a fine longitudinal sensor and an opticaldelay line. All components were to be interfaced into theGNC.

3.1.9 XEUS A. Parmar

The X-ray Evolving Universe Spectroscopy mission(XEUS) has been under study as part of ESA’s long-termHorizons 2000 science programme. The key goal is theX-ray spectroscopic study of the first massive blackholes. By studying how black hole masses and spin ratesevolve with cosmic time, astronomers will be able toinvestigate how they grow and the role they play in theevolution of the galaxies.

XEUS will consist of separate detector and mirrorspacecraft flying in formation, 50 m apart. XEUS will belaunched by an Ariane-5 rocket after 2012 and have aninitial mirror diameter of 4.5 m. XEUS requires arevolutionary extension of the X-ray mirror technology

used by XMM-Newton. Narrow- and wide-field imagerswill provide energy resolutions of 500-1000 and 20 at1 keV, respectively. The detector spacecraft willmanoeuvre to remain at the focus of the optics. Afterusing most of its propellant, the detector spacecraft willdock with the mirror spacecraft and the pair will transferto the same orbit as the ISS. The mirror spacecraft willthen dock with the ISS and additional mirror segmentswill be attached around the outside of the spacecraft. Thisincreases the mirror diameter to 10 m and the effectivearea at 1 keV from 6 m2 to 30 m2. An 18-month SystemStudy addressing the critical issues identified in anearlier feasibility study is imminent.

3.1.10 ISS payloads: Lobster-ISS, EUSO, ROSITA A. Parmar

Lobster-ISS

A new X-ray source may suddenly appear, shine brightly,and then disappear a few days later. A highly sensitiveX-ray mission such as XMM-Newton observes only asmall region of sky at any one time and could easily misssuch unpredictable events. This is where an all-sky X-raymonitor, such as Lobster-ISS, can play a vital role. Byalerting astronomers to important events occurringanywhere in the sky, powerful observatories can berapidly repointed to take advantage of new opportunities.

Lobster-ISS is a proposal to fly an extremely sensitiveall-sky monitor on the International Space Station (ISS)around 2009. It was submitted to ESA in response to the‘F2/F3’ call for proposals, issued in October 1999.Lobster-ISS will use a novel form of micro-channel plateX-ray optics. It will be the first true imaging X-ray all-sky monitor and will be able to locate X-ray sources towithin 1 arcmin. Lobster-ISS will produce a catalogue of200 000 X-ray sources every 2 months which will bemade available via the Internet. As well as providing analert facility, the high sensitivity will allow many topicsto be studied using Lobster-ISS data alone. A 12-monthPhase-A study started in 2002 is progressing smoothly.

EUSO

The Earth is being continuously bombarded by high-energy cosmic rays. While those with energies up to1015 eV almost certainly originate from well-understoodobjects, understanding the origin of cosmic rays withenergies >5 x 1019 eV is one of the current challenges inastrophysics. At such extreme energies, cosmic raysinteract with the cosmic microwave background and thedistance that a cosmic ray can travel is limited to ourgalactic neighbourhood. Intriguingly, all the astro-nomical objects that could produce such cosmic rays liemuch further away than this. Using double Fresnel lensoptics, EUSO will observe the flash of UV fluorescence

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light and the reflected Cerenkov light produced whensuch a cosmic ray interacts with Earth’s atmosphere. Bylooking down from the ISS with a 60º FOV, EUSO willdetect around 1000 events per year, compared to thehandful seen so far with ground-based experiments.

The EUSO proposal was submitted to ESA in response tothe F2/F3 call for proposals. Following an initialfeasibility study, the best way of accommodating such alarge (2.5 m-diameter) and heavy (1.4 t) payload on theISS around 2009 is one of the key topics of the 12-monthPhase-A study that began in March 2002.

ROSITA

ROSITA (ROentgen Survey with an Imaging TelescopeArray) is a proposal received by ESA to perform the firstimaging all-sky survey in the medium-energy X-rayrange using an array of telescopes aboard the ISS. Themain scientific goals are to detect all obscured accretingblack holes in nearby galaxies and many new, distant,active galactic nuclei, to detect the hot intergalacticmedium in many galaxy clusters and groups and the hotgas in filaments between clusters, to find massive distantclusters of galaxies and to study the physics of galacticX-ray source populations, such as pre-main sequencestars, supernova remnants and X-ray binaries. Above2 keV, the proposed ROSITA survey will have 100 timesthe sensitivity and better angular resolution than the lastall-sky survey in this band, which was performed about25 years ago. In the 0.5-2 keV, band the ROSITA surveywill be more sensitive and have substantially betterenergy and angular resolutions than the previous (Rosat)all-sky survey. An initial feasibility study using ESA’sConcurrent Design Facility did not reveal anyshowstoppers and preparations are underway for aPhase-A study.

3.2 Solar and Solar-Terrestrial Missions Division

3.2.1 Introduction and overview

The Solar and Solar-Terrestrial Mission Divisionemerged in February 2002 as one of two branches of theprevious Solar System Division. It provides scientificsupport for all ESA missions in solar, heliospheric andsolar-terrestrial science. This encompasses Ulysses,SOHO and Cluster in their operational phases, DoubleStar under development and Solar Orbiter in theassessment phase. The Division also has responsibilityfor the management of the missions in the exploitationphase.

Divisional staff is located at ESTEC, Noordwijk (NL)and at the SOHO Experiment Operations Facility at theNASA Goddard Space Flight Center, Greenbelt (USA),where the SOHO Project Scientist Team resides.

Ulysses has completed its 12th year in orbit and hascontinued to unveil striking differences in high-latitudeheliosphere during its second solar maximum orbit incomparison to the data from its first, solar minimumorbit. In 2001, NASA approved funding for Ulyssesoperations until September 2004, in line with the earlierSPC decision. As in the past, Ulysses results featuredprominently at international meetings and in thescientific literature. In addition, two books focusing onthe science output of Ulysses, co-edited by the ProjectScientist, were published in 2001.

The SOHO scientific operations, conducted at theExperiment Operations Facility at GSFC, continuedsmoothly throughout 2001 and 2002. SOHO remained atworld centre stage in solar physics, with numerouscoordinated observations with ground observations andother spacecraft. Science communications and outreachactivities were given specific attention by the SOHOProject Scientist Team, contributing to a high visibility ofthis mission with its spectacular images of the dynamicSun at solar maximum and with its unique discoveries ofprocesses in the solar interior. A particular milestone wasreached in February 2002 when the SPC approvedextension of the mission to March 2007. This will ensureobservations of the Sun’s evolution over a full solaractivity cycle.

A wealth of new scientific results on small-scalestructures of magnetospheric boundaries in 3-D isemerging from the Cluster mission. The operations of thespacecraft quartet in its first 2 years in orbit wentsmoothly and as planned. The scientific value of beingable to adjust the spacecraft separation to the appropriatestructure size of the region to be studied was clearlyproved. A major milestone was reached in February 2002when the SPC approved both the extension of themission until December 2005 and the full data coveragealong the Cluster orbit.

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ESA’s collaboration with China on the two-spacecraftmagnetospheric Double Star Programme was approvedin mid-2001. The activities mostly related to the supportof European space-plasma scientists with Cluster-typeinstruments on the Chinese spacecraft had a slower startthan expected, but are now progressing well. Delivery ofmost of the European instrument flight models to Chinafor the first (equatorial) spacecraft is planned for mid-2003 for launch in December 2003.

Following confirmation the Solar Orbiter mission as partof the ‘Cosmic Vision’ programme, activities havefocused on the detailed definition of the model payload.A Payload Working Group comprising experts of thescientific community, was established in 2002. It hasworked closely with the Divisional Study Scientists andmembers of the Directorate’s Science Payload andAdvanced Concept Office to provide input to a PayloadDefinition Document and to define potential payloadtechnology developments.

It is very rewarding to note the continued goodperformance in-orbit of several instruments built inprevious years by members of the Solar System Division,including the COSPIN investigation on Ulysses, the LOIinstruments on SOHO, the GORID dust instrument ingeostationary orbit on the Russian Express-II spacecraft,the MDC dust instrument on the Japanese Nozomispacecraft, as well as the electric field (EFW) andpotential control (ASPOC) instruments on Cluster.

Divisional staff also continued to undertake scientificresearch. This encompasses, in line with the previousactivities of the Solar System Division, both thedevelopment of scientific instrumentation and analysis ofscientific data, mostly from instrumentation previouslybuilt.

In line with the modified role of the Department,hardware development concentrated on the completionof commitments; no new hardware commitments weretaken on during the reporting period. The development ofall flight instrumentation for Rosetta (now under theresponsibility of the Planetary Missions Division) wascompleted. A prototype of the SEPT/IMPACT instrumentwas successfully tested, being developed for flight onNASA’s STEREO mission. The SEPT instrument is themost recent link in the very successful series of energeticparticle instrumentation built for previous missions.

On the data analysis side, Divisional staff were involvedin work on solar physics (see Section 2.6), heliosphericphysics (2.7) and space plasma physics (2.8). Thecontinued presence of Research Fellows has been animportant prerequisite for maintaining these researchactivities.

3.2.2 UlyssesR.G. Marsden

Ulysses is an exploratory mission carried out jointly byESA and NASA to study the properties of the inter-planetary medium and solar wind in the inner heliosphereas a function of heliographic latitude and solar activity.The mission also focuses on the dust and gas componentsof the local interstellar medium that gain access to theheliosphere inside the orbit of Jupiter. The European-built Ulysses spacecraft was launched by the SpaceShuttle on 6 October 1990 and a Jupiter gravity-assistmanoeuvre, executed in February 1992, deflected theprobe into its final high-inclination heliocentric orbit.Major milestones of the mission to date include the solarminimum traversal of the polar regions in September1994 (south) and July/August 1995 (north), and thereturn to high heliographic latitudes, this time near solarmaximum, in 2000 and 2001. Ulysses is presentlyengaged in the exploration of the high-latitudeheliosphere in the declining phase of solar cycle 23,focusing in particular on the effects of the polarityreversal of the large-scale solar magnetic field.

Scientific highlights during the reporting period includedthe first complete characterisation of the high-latitudesolar wind at solar maximum, the first in situobservations of CMEs over the solar poles, the firstobservations of solar energetic particle events at highheliographic latitudes, and the first definitive in situmeasurement of the flow direction, speed and tempera-ture of interstellar neutral helium in the heliosphere.

A joint ESA-NASA Mission Operations Team located atthe Jet Propulsion Laboratory in Pasadena conductsspacecraft operations. The spacecraft and its scientificpayload encountered very few problems during theperiod covered by this report, and remain in excellenthealth. As predicted, December 2000 saw the return ofthe nutation-like disturbance to the spacecraft motionthat is caused by non-symmetric heating of the axialboom by incident sunlight. Operational proceduresdeveloped prior to the 1994/95 build-up proved highlyeffective in once again controlling the level of nutation toa point that scientific operations were generallyunaffected. In recognition of the excellent job done incontrolling nutation throughout the period, the membersof the Mission Operations Team were awarded both aNASA Group Achievement Award, and a special ESACertificate.

On the programmatic side, the outcome of the 2001NASA Sun-Earth Connection Missions Senior Review,held in July 2001, was generally positive for Ulysses.NASA approved funding for Ulysses operations until2004, in line with the earlier SPC decision.

During the reporting period, the ESA Project Scientist,together with his JPL counterpart, E. Smith, provided

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scientific advice to the operations team on all missionaspects, and co-chaired the Science Working Team(SWT) meetings. Four SWT meetings were held in2001/2002, two at ESA establishments (ESOC in2001 and ESTEC in 2002) and two in the USA. InJuly 2002, the responsibilities for all aspects of theESA project, including those that were formerlyhandled by K.-P. Wenzel, were transferred to theProject Scientist.

As in the past, the Project Scientist was involved in theorganisation of a number of special sessions at interna-tional scientific meetings that focused on Ulysses resultsand the study of the heliosphere. In keeping withUlysses’ key role as a member of the international flotillaof solar and heliospheric missions currently in operation,the project was the focal point of a very successfulUlysses-ACE-Voyager joint workshop held in Oxnard,CA (USA), in October 2001. Ulysses investigators havecontinued to publish prolifically, with more than 140papers appearing in 2001-2002. In addition, two majorbooks focusing on the science output of Ulysses,

co-edited by the Project Scientist, were published in2001.

The ESA Ulysses Data Archive is maintained at ESTECand is mirrored at JPL. Ulysses data are also archived byNASA at the National Space Science Data Center(NSSDC), and form part of the Planetary Data System(PDS) archive. The Ulysses Science Working Team, at itsmeeting in October 2002, agreed to waive the proprietary1-year period for exclusive rights to analyse and publishtheir measurements. The most recent Ulysses data (in themajority of cases to mid-2002) are therefore nowavailable in the public domain from dedicated missionarchives. Efforts have also focused on securing new datasubmissions, where appropriate, to bring the mostcomplete and highest time resolution data into theUlysses data archives. The CD-ROM archive of the SolarWind Ion Composition experiment (SWICS) thatprovides all the instrument matrix rates at the highesttime resolution available is a good example of this. AllUlysses data can be accessed at http://helio.estec.esa.nl/ulysses/archive

Figure 3.2.2: A comparison of solar wind observations during the pole-to-pole transits near solar minimum (leftpanel) and around solar maximum (right panel). (Courtesy D.J. McComas, SWRI, San Antonio, US).

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3.2.3 SOHO B. Fleck

Since its launch on 2 December 1995, SOHO hasprovided a wealth of information about the Sun, from theinterior, through the atmosphere, and out to the solarwind. Helioseismology data from SOHO have shed newlight on a number of structural and dynamic phenomenain the solar interior. The imagers and spectrometers haverevealed an extremely dynamic solar surface andatmosphere. Together with the in situ particle experi-ments and sky mappers, they have greatly expanded ourknowledge of conditions in the interplanetary space andhow it is affected by the Sun.

At its meeting in February 2002, the SPC approvedanother mission extension of 4 years through March2007, allowing SOHO to cover a full 11-year solar cycle.

SOHO remains a busy observatory, with a high numberof coordinated observations involving differentinstruments as well as ground-based observatories andother spacecraft, mostly with TRACE, RHESSI andUlysses. The coordinated observing time has increasedslightly, and is now at over 12 h per day.

Science operations coordination focuses on maximisingthe science output of the mission on both short- and long-time scales. Current interests in joint observations areserved by facilitating requested joint observingcampaigns; possibilities for future analysis is furtherenhanced by initiating ad hoc collaborations based onindividual instrument plans.

Science operations coordination also involvesidentifying and resolving technical conflicts betweendifferent instruments and between instrument andspacecraft operations. During exceptional operations,such as Emergency Sun Reacquisition and spacecraftmanoeuvres, instrument activities are scheduled in closecontact with the Flight Operations Team. In particular,two offpoint manoeuvres and a 360º +90º roll manoeuvrefor instrument calibration and special scienceobservations were planned and executed.

The Internet-based approach to science operationscoordination and data dissemination that SOHOpioneered since 1994 is still the cornerstone of the SOHOinformation and data system, and continues to grow. Anaverage of almost 7 million requests were received, andmore than 950 GB of data were transferred from theSOHO servers every month during the last 2 years (upfrom 3.3 million requests and 287 GB during theprevious period). The increase is in large part due to arevamping of the SOHO web pages, and new featuressuch as the ‘SOHO Hot Shots’ and ‘SOHO WeeklyPicks’.

Another key development during the reporting period

was the replacement of NASA’s SOHO Command andData Handling Facility with a highly automated systemdeveloped by the ESA SOHO Science Data Coordinator.The new service, using primary and backup serversprovided by NASA, has taken over the followingfunctions:

— level-0 telemetry processing. Reception of level-0telemetry from the NASA ground segment,automated distribution of telemetry to the PI teamswith standing requests, and archiving of telemetryfor on-demand retrieval at a later time;

— ancillary data processing: Processing of telemetryand flight dynamics orbit inputs to create anddistribute the SOHO ancillary data sets.

Thanks to special efforts and a network of personalmedia contacts, SOHO keeps a high profile in the media.For instance, SOHO observations were featured in 18stories on CNN.com and five stories on BBCi in thereporting period. On 27/28 April 2001 we celebratedSun-Earth Day and SOHO’s 5th anniversary with specialevents in 47 cities in 14 European countries, and 12events in the US and Canada. Building on the successfrom the 5-year celebrations, we supported the EUinitiative ‘Space Weather and Europe’, part of theEuropean Science and Technology Week (4-10November 2002).

We have established an active dialogue with the ESAEducation Office, providing support for variousinitiatives (e.g. the Nuna solar car tour, screenings of theIMAX movie SolarMax, Space Weather and Europe).

http://soho.estec.esa.nl

Figure 3.2.3: SOHO has provided an unparalleledbreadth and depth of information about the Sun.

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3.2.4 Cluster C.P. Escoubet and M. Fehringer

The aim of the Cluster mission is to study small-scalestructures of the magnetosphere and its environment inthree dimensions. To achieve this, Cluster comprises fouridentical spacecraft flying in a tetrahedral formation. Theseparation distances vary between 600 km and20 000 km, according to the scientific objectives.

During the reporting period, the Project Scientist and hisdeputy have devoted a large part of their time to thescientific operations of the Cluster mission. Thesestarted, after a 5-month commissioning and verificationphase, on 1 February 2001. The excellent status of thespacecraft and instruments soon suggested a missionextension beyond the planned 2 years. It was also quicklyrealised that the data coverage of about 50% of the timewas not fully satisfactory. Abrupt events like solar stormsor geomagnetic substorms were missed or not fullyrecorded. Large regions of the magnetosphere such as theplasmasheet could not be fully covered. Thus, the SPCagreed in February 2002 both to extend the missionoperations for three more years up to December 2005 andto acquire data over 100% of each orbit. This increasecould be implemented as early as June 2002 by adding asecond ground station and with the very good supportfrom ESOC, the Joint Science Operation Centre (JSOC)and the PI teams.

The Cluster Science Data System (CSDS), which wasspecially developed to allow for an easy and fast accessto the Cluster physical parameters measured by theinstruments, has been running smoothly since February2001. All instruments are routinely providing data andthe PI teams verify and validate them before makingthem available to the community. Nine national datacentres from Austria, China, France, Germany, Hungary,Netherlands, Sweden, United Kingdom and the UnitedStates constitute the CSDS. These national data centresare funded by their national agencies. ESA coordinatesthe system and provides the user interface to allow ascientific user to query, retrieve and manipulate the datacoming from all instruments. User access to the datasystem is gradually increasing every month. The averagedownload by scientific users over the last 3 months of2002 was above 3.5 GB/month. The physical parametersdatabase contains about 14 GB at the end of 2002.

The CSDS parameters take a few weeks to be generatedafter data acquisition owing to the distribution of data onCD-Roms and to the time needed by the PIs to validatethe data. For faster access to data, the CSDSweb wascreated. These web pages show data from one spacecraftand are produced as soon as the data arrive at ESOC,which may vary from a few hours to a few days,depending on the ground station visibility, and are thenmade available to the public. CSDSweb software isunder the responsibility of JSOC.

JSOC, located at Rutherford Appleton Laboratory (UK),was established to support the Cluster Project Scientist incoordinating the complex science operations of theCluster mission. Its five main tasks are payloadcommanding, payload health monitoring, planning andinformation dissemination, delivery and maintenance ofthe command data management system and of theCSDSweb. JSOC has operated successfully for 1.5 years.

Cluster, with four identical spacecraft, can for the firsttime measure physical quantities that cannot be measuredwith single- or double-spacecraft missions. For instance,the electric current, which is a source of energy thatdeforms the Earth’s magnetic field, can be measured forthe first time with Cluster without any assumptions. Bycombining the measurements of the magnetic field at thefour spacecraft and using Ampere’s law, we obtain thecurrent flowing through the volume of space enclosed bythe four spacecraft. Fig. 3.2.4 shows the currentmeasured in a flux transfer event (FTE) formed by thereconnection of a flux tube from the Sun and from theEarth. The direction (away from Earth) as well as thevalue (50 mA km–2 maximum) are obtained without anyassumptions. It is also seen that the maximum current isobserved on the edge of the flux tube and mainly parallelto the magnetic field (J// dominates). This new findinghas important implications for modelling these structuresand, furthermore, our understanding of energy transferfrom the solar wind to the magnetosphere.

Figure 3.2.4: Cluster orbit (upper) and electriccurrent in the FTE (lower panel). In red is the currentparallel to the magnetic field and in greenperpendicular to the magnetic field. (Courtesy ofRobert & Roux, CETP, F)

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3.2.5 Double StarC.P. Escoubet and M. Fehringer

The Chinese Double Star Programme of two satelliteswill study the effect of the Sun on the Earth’senvironment. The equatorial spacecraft (DSP-1) willinvestigate substorm processes as well as the entry ofsolar particles on the front-side of the magnetosphere.The polar spacecraft (DSP-2) will monitor the energyinput from the solar wind into the polar ionosphere. Thetwo spacecraft will be launched in December 2003 andJune 2004, respectively, into orbits to maximise theconjunctions with Cluster. Half of the payload consists ofEuropean instruments (spares or duplicates of the Clusterinstruments); the other half are built by the Chinese.

In July 2001, ESA and the Chinese National SpaceAdministration (CNSA) signed the DSP cooperationagreement. ESA’s goal in this first collaboration withChina is to provide unique opportunities for Europeanspace plasma scientists. To this end, ESA has beensupporting the refurbishment/rebuilding of the Europeaninstruments, helped in the pre-integration of theEuropean instruments in Europe, will advise China onbuilding magnetically clean spacecraft, will increase thescientific return of DSP by acquiring 4 h of data per daywith a European ground station and will coordinate thescientific operations of the European instruments.

In the last 2 years, the Project Scientist and his deputy, inaddition to their prime duties on Cluster, have devoted alarge part of their time, first in preparing the approval ofthe collaboration agreement with China by SPC in May2001 and by Council in June 2001 and then in theimplementation of several of the ESA responsibilities.

Regular meetings with the Chinese and the European PIshave been arranged and supported to define the interfacesand to verify that the Cluster spare models can beintegrated on the spacecraft. In order to keep theEuropean cost to a minimum, the Chinese partners builta special data handling system to match the ‘Clusterinterfaces’. This system was successfully tested with allEuropean instruments in September 2002.

It was also decided to reuse as much as possible theground data system developed for Cluster. The EuropeanPayload Operation Centre (adapted from Cluster’sJSOC) will coordinate the commanding of the Europeanpayload and update the Data Management System forDouble Star. Similarly the Double Star Data System(DSDS), a subset of the Cluster data system, will be usedto distribute the data to the user community.

3.2.6 Solar OrbiterR.G. Marsden and B. Fleck

The key mission objectives of the Solar Orbiter are: tostudy the Sun from close up (45 solar radii, or 0.21 AU),permitting investigation of the solar surface at highspatial resolution; to study the links between the solarsurface, the corona and inner heliosphere duringperihelion passes that are matched to the Sun’s rotationspeed; to provide images of the Sun’s polar regions fromheliographic latitudes in excess of 30º. The mission wasoriginally approved for implementation as a Flexi-mission by the SPC in October 2000. Following thereevaluation of the Science Programme in the aftermathof the November 2001 Council Meeting at Ministeriallevel, Solar Orbiter will now be implemented togetherwith the BepiColombo mission as a common project.Launch of all elements of the two missions is foreseenfor 2010-2012.

Solar Orbiter’s model payload currently comprises twosophisticated instrument packages: Heliospheric in situinstruments: solar wind analyser, radio and plasma waveanalyser, magnetometer, energetic particle detector, dustdetector, neutral particle detector, gamma-ray detector,solar neutron detector. Solar remote-sensing instrumentsare: EUV imager, EUV spectrometer, visible-lightimager and magnetograph, EUV and visible-lightcoronagraph, radiometer, X-ray imager and heliosphericimager.

Activities during the reporting period focused on thedetailed definition of the above model payloadinstruments. To this end, a Payload Working Group(PWG) was established in 2002, comprising members ofthe scientific community with expertise in instrument-ation of the kind envisaged for the Solar Orbiter. ThePWG, which has sub-groups for the In-Situ and Remote-Sensing packages, has worked closely with the Study

Figure 3.2.6: Artist’s view of the Solar Orbiter,showing the operational orbit with its progressivelyincreasing inclination.

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Scientists and members of the SCI-A Office to provideinput to the Payload Definition Document, and to definepotential payload technology developments. AnotherPWG task has been the identification of problems to beexpected as a result of the extreme thermal and radiationenvironment to which the Orbiter will be exposed.Meetings of the PWG were held in ESTEC in May andNovember 2002. In addition to supporting the PWG, theStudy Scientists have presented the mission at a numberof international meetings addressing the future of solarand heliospheric physics. In this regard, Solar Orbiterenjoys broad international support, and is seen as a keycontribution to the International Living With a Star(ILWS) programme.

3.2.7 Solar-BB. Fleck

Solar-B is an ISAS-led solar physics mission planned asthe follow-on to the highly successful Yohkoh (Solar-A).The Solar-B payload consists of a coordinated set ofoptical, EUV and X-ray instruments to investigate theinteraction between the Sun’s magnetic field and corona.The result will be an improved understanding of themechanisms that give rise to solar magnetic variabilityand how this variability modulates the total solar outputand creates the driving force behind space weather.Solar-B is scheduled for launch in August 2005.

ESA has been invited to collaborate on Solar-B,particularly in data analysis systems and operationalground support from a polar station. ESA will seek SPCapproval to accept this invitation. If endorsed, ESAwould provide funds for the use of a Norwegian groundstation, which, owing to its high-latitude location, canprovide downlink on all passes of Solar-B in its Sun-synchronous polar orbit. This collaboration wouldprovide the European solar physics community withrapid access to the Solar-B data.

ESA envisages its involvement in Solar-B as an elementof its contribution to the International Living with a Star(ILWS) programme. The ultimate goal of thisprogramme is to increase our understanding of how thevariability of the Sun affects the terrestrial and otherplanetary environments, both in the short- and long-terms, and in particular how mankind and society may beaffected by the solar variability and its consequences.

B. Fleck acted as the prime ESA contact person withISAS. R. Marsden was recently appointed as ESArepresentative on the ILWS Steering Committee.

3.3 Planetary Missions Division

3.3.1 Introduction and overview

The Planetary Missions Division is the second branch thatemerged from the Solar System Division after thereorganisation of the Department in February 2002. TheDivision provides scientific support for all ESA missionsin planetary science: Huygens, the Titan Probe contributedby ESA to the joint NASA/ESA Cassini/Huygens missionon course to the Saturnian System; three missions in theirfinal stages of implementation for launch in 2003-2004,Rosetta, the comet rendezvous mission, SMART-1 andMars Express. Venus Express was approved in late 2002with a very ambitious schedule to be launched by end-2005. The mission to Mercury, BepiColombo, is underreassessment. Huygens is the first mission for which theDivision took over responsibility for the missionmanagement in its exploitation phase.

Cassini/Huygens completed its 6-month Jupiter flybycampaign very successfully, providing unique scienceobservations.It is now en route for Saturn arrival in lateJune 2004. The Huygens mission trajectory was changedin 2001 to accommodate a new geometry requirementduring the Probe relay phase that will reduce the Dopplershift received by the Orbiter. This change was necessaryto cope with a design flaw of the Huygens radio receiverdiscovered during inflight testing in 2000. In this newscenario, the Probe will be released in late December2004 to enter Titan’s atmosphere on 14 January 2005.

For both Rosetta and Mars Express, the reporting periodwas very busy, with the flight payloads being completedand delivered for integration into the spacecraft and theextensive environmental test programmes. The activitiesof the Project Scientist Teams focused on monitoring ofthe instrument development, supporting the regularprogress meetings with the experiment teams and theESA review cycle, e.g. Experiment Flight OperationsReview, Flight Acceptance Review, and Flight andMission Readiness Reviews. In addition, thedevelopment for both the Rosetta and the Mars Express/Beagle-2 Landers required dedicated coordinationsupport. It was rewarding to see that the payloads forboth missions was delivered on time and met thespecified performance criteria. Specific efforts were alsodeployed towards the preparations for the scienceoperations of these missions.

SMART-1, the first in the SMART (Small Missions forAdvanced Research In Technology) series, will preparethe use of Solar Electric Primary Propulsion for futuredeep-space missions. SMART-1 hosts seven instruments,some with novel technologies that will be tested duringthe mission. All instruments were delivered at the end of2002. In close collaboration with the ProjectsDepartment, the Division prepared the science operationsactivities for the cruise and lunar orbit phase.

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The activities for BepiColombo focused on the detaileddefinition of a baseline mission scenario. Twocompetitive industrial definition studies were carried out,based on the separate launches of the Mercury PlanetaryOrbiter (MPO), to be provided by ESA, and the MercuryMagnetospheric Orbiter (MMO), to be provided byJapan, with two Soyuz-Fregat launchers in 2011-2012.Extensive efforts were mounted to include a MercurySurface Element (MSE) in the mission scenario throughan enlarged international cooperative approach. TheDirectorate’s Science Payload and Advanced ConceptOffice, supported by the Project Scientist Team from theDivision, is reassessing the mission scenario and themodel payload in order to optimise the mission and toenable the implementation of all three elements, MPO,MMO and MSE, within the programmatic constraints(see Section 3.7.2).

Flight instruments involving Division hardwarecontributions continued to provide excellent data,especially the MDC dust detector on the JapaneseNozomi spacecraft and the GORID dust instrument ingeostationary orbit on the Russian Express-II spacecraft.The GORID instrument was eventually switched off inmid-2002, after it had worked well for many years.

Research in the Division concentrated on the analysis ofdata from flight instruments where either hardware hadbeen provided or members of the Division participated asCo-investigators based on their expertise in specific areasof planetary research. A number of activities have beendirectly related to supporting the implementation ofspecific missions.

Flight hardware development concentrated on thecompletion of the instrumentation for Rosetta, aresponsibility taken over from the former Solar SystemDivision, and on support to instrument development forSMART-1. In expectation of the AO for BepiColombo,no new commitments were taken on in the reportingperiod. Instrument pre-development concentrated on thestudy of key elements for a generic dust detector and thesupport to feasibility studies for miniaturised in situcomposition analysers for planetary landers.

With regard to data analysis, Divisional staff wereinvolved in cometary physics and studies of theproperties of interplanetary and interstellar dust grains,comparative planetology and exobiology, the study ofterrestrial impact craters, and the study of meteorstreams. The excellent work of the Research Fellows inthe Division must be acknowledged as a key factor formaintaining these research activities at a high standard.

3.3.2 Cassini/Huygens J.-P. Lebreton

The Cassini/Huygens mission carried out jointly byNASA and ESA is designed to explore the Saturniansystem and all its elements: the planet and itsatmosphere, rings and magnetosphere, and a largenumber of its moons, particular Titan and the icysatellites. The Cassini/Huygens spacecraft was launchedin October 1997. The interplanetary voyage of about 6.7years included gravity-assist manoeuvres at Venus (April1998 and June 1999), at Earth (August 1999) and atJupiter (December 2000) (Fig. 3.3.2/1). After completionof the scientifically successful Jupiter 6-month flybycampaign, the spacecraft is now on a direct trajectory toSaturn, where it will arrive in late June 2004. The SaturnOrbit Insertion manoeuvre will be executed while thespacecraft is crossing the ring plane on 1 July 2004. Thismanoeuvre will place the spacecraft in a 90-day orbit,which includes the first targeted Titan flyby. The second(48-day) orbit, which also includes a targeted Titan flyby,will shape the trajectory so that the Huygens mission canbe carried out on the third (32-day) orbit using an Orbiterflyby altitude of 60 000 km (Fig. 3.3.2/2). The Probe willbe released on 24 December 2004, 22 days before Titanencounter. Five days after the release, the Orbiter willperform a deflection manoeuvre to avoid impactingTitan. This manoeuvre will also set up the Probe-Orbiterradio communication geometry for the Probe descentphase. Huygens’ entry into Titan’s atmosphere is plannedfor 14 January 2005.

During the reporting period, the Project Scientist had toinvest a major effort to coordinate and support theactivities to recover the Huygens scientific mission. Thiswas done in close collaboration with the Directorate’s

Figure 3.3.2/1: The Cassini/Huygens trajectory uponarrival at Saturn. The Huygens mission trajectorywas changed in 2001 to accommodate a new geometryrequirement during the Probe relay phase thatreduces the Doppler shift of the radio signal receivedby the Orbiter.

http://sci.esa.int/huygens/

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Projects Department, the Huygens Operations Team atESOC, the Huygens team collocated at JPL in 2002, andthe JPL Cassini Project. The Project Scientist chaired theHuygens Science Working Team meetings and co-chaired with his JPL counterpart the Cassini/HuygensProject Science Group meetings. In late 2002 the ProjectScientist took on the additional responsibility of MissionManager when the responsibility for the overallmanagement of the mission was transferred from theProjects Department to RSSD.

3.3.3 RosettaG. Schwehm

The main goal of the Rosetta mission was a rendezvouswith Comet 46P/Wirtanen and included the study of twoasteroids during close flybys en route to the comet.Launch was set for 13 January 2003. Following thefailure of the new Ariane-5 ECA version during its firstlaunch in December 2002, the vheicle was grounded andthe Rosetta launch had to be postponed. Studies havebeen initiated to work out in detail alternative missionscenarios that will preserve the scientific objectives ofthe mission and minimise technical risks and thefinancial impact on the overall Science Programme.

Rosetta will rendezvous with a comet, follow it along itsorbit and study the nucleus and its environment in greatdetail over a heliocentric distance between 4.5 AU andthe perihelion passage of the comet. A Lander will bedeployed on to the nucleus early in the near-nucleusobservation phase.

The Project Scientist and his team closely monitored theflight hardware development by supporting regularProgress Meetings and the Project Reviews. During theextensive environmental test period at ESTEC theyparticipated in the flight instrument check-out to fillmanpower gaps in some Experiment Teams.

The team will be responsible for the Rosetta ScienceOperations Centre (RSOC), especially for the consoli-

Figure 3.3.2/2: The revised approach strategy forHuygens at Titan.

http://sci.esa.int/rosetta/

Figure 3.3.3: The elements of the Rosetta ground system.

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dation of the command sequences for the operation of thescience payload. These command files will be submittedto the Rosetta Mission Operations Centre (RMOC) atESOC (Fig. 3.3.3). The development of the tools forpayload operations planning progressed well in thereporting period. In close cooperation with the MissionOperations Team at ESOC, the RSOC interfaces with theRMOC were tested. The RSOC was ready to support thein-orbit payload commissioning phase.

In parallel, the preparatory work for the Rosetta ScienceData Archive was initiated as part of a general ESAScience Data Archive in close collaboration with RSSD’sScience Operations and Data Handling Division. Thelong mission duration of Rosetta with the prime sciencephase starting only long after launch, makes it mandatorythat a complete, easily accessible database anddocumentation for both spacecraft and the payload isestablished. Knowledge management and its practicalimplementation was therefore brought up as a major newtopic for the Project Scientist Team. In close cooperationwith the Experimenter Teams, a prototype of aknowledge database, including documentation, dailycorrespondence and video-taped interviews with teammembers involved in instrument design, manufacturingand calibration has been produced.

3.3.4 Mars ExpressA. Chicarro

The Mars Express mission will be launched in May 2003from Baikonur aboard a Russian Soyuz-Fregat launcher.The mission comprises an Orbiter to be placed in a quasi-polar martian orbit, with closest approach at 250 km anda mission lifetime of one martian year (687 days), and thesmall Beagle-2 probe. Beagle-2 will land at IsidisPlanitia in December 2003 and operate on the martiansurface for about 6 months. In addition to studying thesurface, subsurface and atmosphere of Mars, the mainthemes of the mission are the search for water at presentand the search for possible signs of life in the history ofthe planet. The specific scientific objectives of the orbiterare: global high-resolution imaging and imaging ofselected areas with super-resolution, global IRmineralogical mapping, sounding of the subsurfacestructure down to a few km, global atmosphericcirculation study and mapping of the atmosphericcomposition, study of the interaction of the inter-planetary medium with the upper atmosphere, as well asradio science. The goals of the Beagle-2 lander are:geology, geochemistry, meteorology and exobiology ofthe landing site. Beagle-2 will use a suite of imagers,organic and mineral chemistry analysers, environmentalsensors and robotic devices to sample soil and rocks onand below the surface. Collaboration with the JapaneseNozomi mission will diversify the scope and enhance thescientific return of both missions, as they arecomplementary in terms of orbits and science goals.

The Project Scientist Team (PST) organised a series ofmeetings with the Mars Express PI teams at ESTEC andESOC throughout the reporting period, under theumbrella of the Mars Express Science Working Team.This included two working groups on Science Operationsand Data Archiving. The PST has monitored thescientific performance of the instruments during theirdevelopment phase. It has responsibility for planning thescientific operations, including commissioning, incoordination with the Mars Express Payload OperationsService (POS), located at the Rutherford AppletonLaboratory (UK).

3.3.5 SMART- 1 B.H. Foing

SMART-1 is the first of the SMART mission seriesintroduced in the ESA Scientific Programme to preparethe technology for future major missions. SMART-1 willdemonstrate the use of Solar Electric Primary Propulsion(SEPP) for future deep-space missions like Bepi-Colombo and Solar Orbiter. The SMART-1 scenario aimsat a transfer of the spacecraft to the Moon. It willdemonstrate the use and navigation of SEPP with aStationary Plasma Thruster throughout the cruise phasefrom geostationary transfer orbit into lunar orbit.SMART-1 will reach the Moon in 15-17 months, enteringa polar orbit of 300 x 10 000 km for lunar observations.Science operations in lunar orbit are baselined for6 months, with a possible extension. The mission was tobe launched nominally in March 2003 as an Ariane-5piggyback payload into geostationary transfer orbit.

During the reporting period, the Project Scientist devoteda large fraction of his time to monitoring thedevelopment of the payload, which includes seven highlyminaturised instruments incorporating a number of noveltechnologies. He organised the preparation of the scienceoperations activity in close cooperation with the ProjectTeam and members of the Rosetta Science OperationsCentre. He also initated and carried out a very broadrange outreach programme to promote lunar science witha number of symposia and student workshops.

3.3.6 BepiColombo R. Grard and H. Laakso

The BepiColombo mission to Mercury was selected as aninterdisciplinary mission in October 2000. The proposedspace segment consists of three components: a MercuryPlanetary Orbiter (MPO) mostly dedicated to remotesensing, a Mercury Magnetospheric Orbiter (MMO)accommodating field and particle instruments, and aMercury Surface Element (MSE) for in situ observa-tions. MPO is a nadir-pointing platform that orbits theplanet at 400 x 1500 km, whereas MMO is a spinner onan eccentric orbit (400 x 12 000 km) (Fig. 3.3.6). The

http://sci.esa.int/marsexpress/ http://www.beagle2.com http://sci.esa.int/smart-1/ http://sci.esa.int/bepicolombo/

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interplanetary transfer is to be performed with a SolarElectric Propulsion Module (SEPM) and gravity assist;the orbit insertion and landing are ensured with aChemical Propulsion Module (CPM). The MPO, MSE,SEPM, CPM, launch service segment and cruiseoperations are to be provided by ESA, the MMO elementbeing contributed by Japan’s Institute of Space andAstronautical Science (ISAS). Launch is foreseen in the20011/2012 time frame.

Two competing industrial definition studies wereconducted from May 2001 to early 2003. A single launchof the three scientific modules, MPO, MMO and MSEwith an Ariane-5 was used as the initial baseline.Budgetary constraints imposed on the ESA ScientificProgramme at the November 2001 ESA Council atMinisterial Level dictated a redirection to a split launchon two smaller Soyuz-Fregat rockets. In order tomaintain the full scientific goals of BepiColombo,including the MSE segment, additional partners willingto join in this international cooperative effort are beingidentified. In September 2002 the mission moved intoreassessment phase, where the payload design andmission implementation profile are being reevaluated fortechnical and financial feasibility (see Section 3.7.2).This phase is expected to end in July 2003.

In the reporting period, the Division’s involvement inBepiColombo was primarily in support of a variety ofscientific and payload issues. This included participationin the definition of an overall strategy for the mission;definition of the model payload, based on the scientificobjectives and together with the external ScienceAdvisory Group; preparation of a draft sciencemanagement plan; preparation of the Payload DefinitionDocument, and contributions to the Payload InterfaceDocument.

Additional activities included scientific assessment ofthe synergies and complementarity of BepiColombo andNASA’s Messenger mission; support to Mercury surfaceand environment modelling; follow-up of the industrial

definition studies; interfacing with technological studiesand developments, and development of science operationtools.

3.3.7 Venus ExpressH. Svedhem

Venus Express was proposed to ESA in response to theMarch 2001 Call for Ideas for reuse of the Mars Expressplatform. The mission was approved by the SPC inNovember 2002 for a launch on Soyuz in November2005, thereby making it the fastest-ever developed ESAscientific project. This will be possible due to the rebuild,with only minor modifications, of the Mars Expressspacecraft, the availability of scientific instruments andthe use of experienced teams from industry and ESA.The scientific payload includes three original MarsExpress instruments and two original Rosettainstruments. During the definition study it was found tobe scientifically valuable and technically feasible toreplace the standard Mars Express engineering VideoMonitoring Camera by a scientific instrument, the VenusMonitoring Camera (VMC). A magnetometer was addedto further enhance the payload.

The Venus Express mission will study the atmosphereand plasma environment of Venus on global and detailedregional levels. Venus orbit insertion will take place inApril 2006, followed by a nominal operational phase oftwo Venus days (~500 Earth days) and a possibleextension of another two Venus days. The highlyelliptical polar orbit will have a pericentre altitude ofabout 250 km and an apocentre altitude of 66 000 km.The pericentre will be located at about 70ºN latitude.This orbit is well-suited to remote observations at a

Figure 3.3.6: The BepiColombo MPO orbiter (left)and MMO magnetospheric orbiter (right).

Figure 3.3.7: Venus Express in orbit at its targetplanet.

http://sci.esa.int/venus express

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global level from high altitude, for detailed studies of thenorthern hemisphere from low altitude and for in situmeasurements covering a large range of distances fromthe planet, at varying solar aspect angles. The selectedpayload will allow studies of the physics and chemistryof the atmosphere and clouds and the related circulationat an unprecedented level. In particular, the poorlystudied lower atmosphere will be probed through the‘windows’ in the near-IR wavelengths. The interaction ofthe upper atmosphere with the solar wind will beinvestigated by dedicated instruments.

The tasks of the Project Scientist, who took overresponsibilities from the Study Scientist in October 2002,include the coordination of all scientific aspects of themission and the harmonisation of the requirements of thedifferent experiments, in order to maximise the scientificoutput from the mission under the given constraints. Thepreparation for the mission science operations will be animportant part of the activities taking into considerationthe very short preparation time until launch.

3.3.8 The Cosmic DUNE mission definition studyH. Svedhem

The Cosmic DUNE (Cosmic Dust Near Earth) missionwas submitted to ESA in March 2001 in response to theCall for Ideas for a low-cost mission based on the reflightof the Mars Express platform. It was proposed as anobservatory for the investigation of interstellar dust, animportant but little-studied component of the interstellarmedium. It also addressed many questions concerningthe interplanetary dust complex that has only beenpartially studied. Galactic interstellar dust constitutes thesolid phase of matter from which stars and planetarysystems form. Interplanetary dust from comets andasteroids represents remnant material from bodies ofdifferent stages of early Solar System formation. Datafrom this mission would enable comparison between thecomposition of the interstellar medium and primitiveplanetary objects and so provide insights into thephysical conditions during the planetary systemformation.

The proposed payload consisted of four co-alignedinstruments for in situ measurements, addressingdifferent aspects of the dust particles encountered, suchas composition, mass and dynamical properties. TheMars Express spacecraft was found to be very well-suited for the payload and for the desired position foroperation, the Lagrangian L2 point.

Cosmic DUNE received a ‘high’ scientific rating and wasfound to be both technically and programmaticallyfeasible, but was not included in the Agency’s ScienceProgramme. The RSSD Study Scientist coordinated thework of the Cosmic DUNE definition study team in2001.

3.4 Fundamental Physics Missions Division

3.4.1 Introduction

In September 2001, the Fundamental Physics Office,which had been set up in 1997 following a recommen-dation by the SSD Advisory Committee, became theFundamental Physics Missions Division. Unlike theother divisions in RSSD, this change had no conse-quences for the functional tasks, manpower allocationand assignment of staff in the Division. During the 2001-2002 reporting period, the Office/Division supported theactivities described below.

For the ESA/NASA collaborative LISA mission, a studyon laser ranging with centimetre precision, a study on theinitial acquisition procedure, the LISA ObservatoryArchitecture Team (co-chaired by the Project Scientist)as a scientific advisory group to the Joint SystemEngineering Board (since October 2002), organising aworkshop on Time-Delayed Interferometry for LISA,organising the 5th Science & Engineering Workshop andsupporting the compilation of the Technology Readinessand Implementation Plan (TRIP) for NASA.

For the SMART-2 mission, two parallel industrialsystem-level studies (September 2001 to July 2002), twoparallel industrial studies in an extended definition phase(activities started in October 2002 and will continue untilthe foreseen start of the implementation phase in July2003) and the activities of the LTP (LISA TechnologyPackage) Architect, particularly the design of the inter-ferometer for the LTP.

For the NASA/ESA collaborative STEP mission, apre-Phase-B study (January to October 2002) of theSTEP Service Module, an industrial study on the drag-free control subsystem (April 2001 to October 2002),various technical development studies of Europeanpayload elements, preparation of the Science Manage-ment Plan, and a Phase-A Concept Study in NASA’sSmall Explorer (SMEX) programme (October 2001 toApril 2002). Unfortunately, NASA’s Office of SpaceScience in July 2002 announced the non-selection ofSTEP; all STEP-related activities in ESA were brought toa close shortly thereafter.

For the CNES/ESA collaborative Microscope mission, aPhase-A study (mid-2001 to January 2003), preparationof the Letter of Agreement between CNES and ESA, andpreparation of the AO and subsequent selection ofexperiments.

For the Hyper mission, an industrial system-level Phase-Astudy (June 2002 to February 2003) and preparation forpayload development in ESA’s Technological ResearchProgramme in the 2004-2006 time frame.

The Division provided the Study Scientists for these

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studies and the Study Manager for the STEP industrialstudies. A senior LISA Mission Scientist from thescientific community has been associated with theDivision since August 2001. A LISA Project Scientist inRSSD, who also serves as SMART-2 Study Scientist, hasbeen in post since May 2002. A Microscope ProjectScientist, with prime duties in another Division, wasappointed in October 2001.

With the recruitment of a new staff member (the LISAProject Scientist) the Office/Division is now for the firsttime in the position to start up a research programme infundamental physics. However, it is too early to reportany results.

3.4.2 LISA O. Jennrich

The objective of the Laser Interferometer Space Antenna(LISA) mission is the detection and observation ofgravitational waves from massive black holes andgalactic binaries in the low-frequency range 10–4-10–1 Hz,inaccessible to ground-based interferometers. The LISAmission comprises three identical spacecraft, located atthe vertices of an equilateral triangle with a baseline of5 million km. The centre of the triangular formation is inthe plane of the ecliptic, 1 AU from the Sun and trailingthe Earth by approximately 20º (Fig. 3.4.2/1). LISA’sworking principle is that of a Michelson interferometer,obtaining information about amplitude, direction andpolarisation of gravitational waves and providing someredundancy via the third arm.

LISA is an ESA/NASA collaborative mission with anominal launch in 2011. To develop the requirements and

design for the mission and oversee the definition anddevelopment, helping to make trade-offs and missiondesign choices, NASA and ESA formed a LISAInternational Science Team (LIST) in early 2001. LISThas 11 US and 11 European members, including the USand European Mission and Project Scientists. The day-to-day scientific work is organised in six working groups.In October 2002, a meeting of the InterferometryWorking Group was held at ESTEC to discuss TimeDelay Interferometry. To employ this technique, thedistance between the spacecraft has to be known to betterthan 30 m. Recent studies supported by the LISA ProjectScientist showed laser ranging to be suitable.

The last two meetings of LIST (in July 2002 at Penn.State University and in December 2002 at the AEI inHannover) brought forward the potential change of thelauncher from the Delta-II 7925H to the more powerfulDelta-IV, an identification of items to be included in anindustrial rider study, and a preliminary concept for a‘minimum mission’.

As LISA presents new challenges to scientists andengineers alike, regular meetings between both groups aretaking place. The 5th Science & Engineering Workshopwas held at ESTEC in October 2002, supported by theProject Scientist. The meeting dealt in large parts with thepreparation of the Technology Readiness andImplementation Plan (TRIP) report, requested by NASAHeadquarters. This report will be reviewed in Februaryand March 2003 and is supposed to support NASA’sdecision in prioritising either LISA or Constellation-X inthe proposed ‘Beyond Einstein’ theme of NASA.

Every 2 years, typically in July, the LISA Team organisesa major LISA Symposium, with the venue alternatingbetween the US and Europe. The 4th Int. LISASymposium was held on 20-24 July 2002 at Penn. StateUniversity. The fifth will be held on 12-16 July 2004 atESTEC, to be organised by the Project Scientist.

3.4.3 SMART-2 O. Jennrich

SMART-2 is primarily intended to demonstrate the keytechnologies for the LISA mission. To this end,SMART-2 will accommodate a LISA TechnologyPackage (LTP), provided by European institutes andindustry, and a Disturbance Reduction System (DRS)that is very similar to the LTP and has the same goals butis provided by US institutes and industry. The LTP andthe DRS can be accommodated on a single spacecraft.The mission goals for the LTP are:

— demonstrating drag-free and attitude control in aspacecraft with two proof masses in order to isolatethe masses from inertial disturbances. The aim willbe to demonstrate the drag-free system with a

Figure 3.4.2/1: Orbital configuration of the threeLISA spacecraft.

http://sci.esa.int/lisa http://sci.esa.int/home/smart-2

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performance on the order of 10–14 m s–2 Hz–1/2 in thebandwidth 10–3-10–1 Hz. The LISA requirement in thesame band is 10–15 m s–2 Hz–1/2;

— demonstrating the feasibility of performing laserinterferometry in the required low-frequency regimewith a performance as close as possible to10–12 m Hz–1/2in the frequency band of 10–3-10–1 Hz, asrequired for the LISA mission;

— assessing the longevity and reliability of thecapacitive sensors, thrusters, lasers and optics in thespace environment.

As the environment on the SMART-2 spacecraft will becomparatively noisy (in terms of temperaturefluctuations and residual forces), the technologydemonstrator is aimed at meeting specifications that areabout a factor 10 more relaxed than necessary for LISA.

The LTP represents one arm of the LISA interferometer;the distance between the two proof masses is reducedfrom 5 million km to 20 cm. As in LISA, the proofmasses fulfil a double role: they serve as opticalreferences (‘mirrors’) for the interferometer and asinertial references for the drag-free control system. Thedrag-free control system onboard the LTP consists of anaccelerometer (or inertial sensor), a propulsion system(Field Emission Electric Propulsion) and a control loopusing capacitive sensing in three dimensions. Thedistance between the proof masses is obtained by aninterferometric measurement system.

Two parallel industrial system-level studies were carriedout from September 2001 to July 2002. These definitionstudies investigated several mission scenarios involvingone or two spacecraft. In December 2002, it was decidedthat SMART-2 will consist of only one spacecrafthousing the LTP and the DRS. The mission is currentlyundergoing an extended definition phase that allows us toreinvestigate issues specific to the one-spacecraftscenario. This phase will run from October 2002 until thestart of the Implementation Phase in July 2003. Adviceon the LTP requirements and specifications is providedby the Project Scientist.

The SMART-2 launch is currently scheduled for August2006. Following the commissioning phase, the in-flightdemonstration of the LISA technology will take place inthe second half of 2006, providing timely feedback for thedevelopment of the LISA mission to be launched in 2011.

3.4.4 STEP R. Reinhard

The Satellite Test of the Equivalence Principle (STEP) isa NASA/ESA collaborative project to test theEquivalence Principle to a precision of 1 part in 1018, animprovement of five orders of magnitude over presentknowledge. In this collaboration, ESA would procure the

Service Module and a Rockot launch vehicle, whileNASA would procure the dewar and the ground segmentand be responsible for overall project management,integration, testing and pre-launch, mission and scienceoperations. The payload sharing ratio is 50/50. TheEuropean payload elements are assumed to be nationallyfunded. STEP was planned for launch in February 2006into a Sun-synchronous, circular orbit at 550 km altitude.

From July 1999 to April 2000, ESA carried out anindustrial study of the Service Module at Phase-A level.This was followed by a pre-Phase-B study from January2002 to October 2002. An industrial study on drag-freecontrol and algorithm design was started in April 2001and ended in October 2002. On the US side, STEP wasselected for a Phase-A Concept Study in NASA’s SmallExplorer (SMEX) programme. This study was carriedout from May to November 2001. ESA’s share in theproject (Service Module, launch vehicle) was provision-ally approved by the SPC in December 2001, subject tolater approval by NASA of its share.

On 2 July 2002, NASA announced the non-selection ofSTEP as a SMEX. It is clear that the continued technicalproblems and consequent delay of Gravity Probe-B had anegative influence on the STEP non-selection. If GP-B islaunched successfully in 2003 and the experiment worksproperly in orbit, STEP would have a better chance ifreproposed to NASA.

The various ESA industrial studies were carried outunder the technical, programmatic and budgetaryresponsibility of the STEP Study Manager in theDivision. He worked closely with the US Study Managerat JPL and with the Science Team at Stanford andsupported the SMEX review at Stanford by a NASAReview Committee with a presentation on ESA’scontributions. He was supported in these activities by theStudy Scientist in the Division. The Study Scientist alsoinitiated and monitored various technical developmentstudies of European payload elements (completed inOctober 2002), prepared the Science Management Planand organised a Working Group on test mass materialselection, design, fabrication, metrology and verificationin the first half of 2002.

3.4.5 Hyper R. Reinhard

Hyper (hyper-precision cold atom interferometry inspace) carries four cold-atom interferometers that can beoperated either in the Mach-Zehnder mode to measurerotations and accelerations or in the Ramsey-Bordé modeto measure frequencies. The primary scientific objectivesof the Hyper mission are:

— to test General Relativity by mapping for the firsttime the spatial (latitudinal) structure (magnitude

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and sign) of the gravitomagnetic (frame-dragging orLense-Thirring) effect of the Earth with about 10%precision;

— to determine independently from QuantumElectrodynamics (QED) theories the fine structureconstant α by measuring the ratio of Planck’sconstant to the atomic mass one to two orders ofmagnitude more precise than present knowledge;

— as a secondary objective, to investigate matter-wavedecoherence to set an upper bound for quantumgravity models.

Atom interferometry also allows us to test theEquivalence Principle with quantum particles bycomparing the free fall of two distinct atomic species(rubidium and caesium). This measurement is comple-mentary to the Microscope and STEP missions, whichinvestigate the free fall of macroscopic objects. Hyper’satom interferometer should reach an accuracy of aboutone part in 1016. The constraints in mass and powerimposed by the satellite make it difficult to pursue boththe measurement of the Lense-Thirring effect and the EPtest. The EP test is therefore considered as an alternativeobjective. For the measurement of the gravitomagneticeffect of the Earth, the four atom interferometers areoperated in the Mach-Zehnder mode; for the measure-ment of the fine structure constant, they are operated inthe Ramsey-Bordé mode.

Hyper was proposed to ESA in January 2000 in responseto ESA’s Call for Mission Proposals for the second andthird Flexi-missions (F2/F3). It was selected for a studyat assessment level, which was carried out from March toJuly 2000 by the Concurrent Design Facility Team atESTEC. This was followed by a system-level industrialstudy with Astrium (D) as prime contractor. The studywas kicked-off in June 2002 and is expected to finish inMarch 2003.

A Hyper Symposium was held on 4-6 November 2002 atCNES HQ, Paris. The Study Scientist supported theindustrial study and the preparation of the Symposium.He was also actively involved in the discussions onHyper’s scientific objectives.

3.4.6 Microscope M. Fehringer

Microscope (MICROSatellite à traînée Compensée pourl’Observation du Principe d’Equivalence) is aCNES/ESA collaborative mission to test the EquivalencePrinciple in space to a precision of 1 part in 1015. It is alow-cost, room-temperature experiment in low-Earthorbit with a total mission cost to CNES of about€15 million. ESA’s share in this collaboration is theprovision of the Field Emission Electric Propulsion(FEEP) thrusters for drag-free and fine attitude control ofthe satellite. This contribution is of particular interest to

ESA as the FEEP technology is currently foreseen to flylater on the SMART-2, LISA, Gaia, Darwin, Hyper andGOCE missions.

A joint CNES/ESA AO was prepared by the ProjectScientist and released in December 2001 with the aim ofEuropeanising the payload. Two proposals were receivedfrom European institutes and, after careful review byESA’s advisory bodies and the Microscope Project Team,accepted by the SPC in May 2002. ZARM (Bremen, D)proposes to perform free-fall tests of the Microscopeaccelerometers and to do end-to-end simulations of theEP measurement. The second proposal was submitted bythe ESA Project Scientist and deals with extended FEEPtesting in orbit in view of the importance of FEEPs forESA’s space science programme.

CNES is currently performing the Phase-A study of themission; the Phase-A review will be held in May 2003.The payload has already passed this review and is now inits detailed design phase. A contract for the procurementof the complete FEEP micropropulsion system has beenawarded to Alta (Pisa, I). The Project Scientist has beennominated as ESA’s Directorate of Science represent-ative for the FEEP development and is monitoring thiscontract in close coordination with ESA’s Directorate ofTechnical and Operational Support. During thedevelopment phase, a 1-year endurance test of a flight-representative thruster will be carried out. The date forthe delivery of the flight propulsion system is set for late2005; launch is planned for late 2006.

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3.5 Space Telescope Operations Division

The Hubble Space Telescope (HST) programme is theenvy of every science facility in the world: it has one ofthe most recognised names, it is considered as one of themost effective science mission ever as rated by citationsin the science news media, and it is routinely cited as amajor reason for increased world-wide interest inastronomy. The demand for telescope time is at a recordhigh: more than eight times as much time was requestedin Cycle 11 than was available.

The Space Telescope Science Institute (STScI) isresponsible for all aspects of HST operations and inparticular for its scientific productivity. ESA contributesto this effort with the assignment of 15 scientists andengineers who are fully integrated into the organisationalstructure of the Institute. Some of the senior staffmembers have achieved significant leadership roleswithin the Institute’s structure and are influential in keyareas of the decision-making process.

Highlights of the HST programme include notableenhancements in Hubble’s ability to produce world-classscience, along with several achievements that gainedworldwide attention. By every measure, HST has morescience capability now than at any time in its lifetime. Ithas achieved a discovery power 10 times greater than atthe beginning of the reporting period. Institute staffcontributed to all phases of this improvement.

Some of the most important achievements were thesupport for a highly successful SM-3B servicing mission,with the installation of a new camera, the AdvancedCamera for Surveys (ACS), and the revival of NICMOSthrough the installation of the NICMOS Cooling System(NCS). Institute personnel provided key support for thismission at the technical, scientific and programmaticlevels. The Institute carried out the Servicing MissionOrbital Verification flawlessly despite having to modifythe work plan when it became apparent that the NCScooling was proceeding much slower than expected.

Following the SM-3B mission, Early ReleaseObservations were obtained with the new instruments.ACS produced some spectacular images, both of nearbyobjects (e.g. the Cone Nebula) and of the distantUniverse (e.g. in the background of the Tadpoleinteracting galaxies, where some 6000 galaxies can beseen). These observations were presented in a pressconference on 30 April 2002, and resulted in anunprecedented worldwide media coverage. The EarlyRelease Observations of the resurrected NICMOScamera (e.g. of the dusty disc of the galaxy NGC 4013)demonstrated the camera’s power to peer through thedust all the way into the galaxy’s core. The results werepresented at a press conference on 5 June 2002.

Observatory operations continued at high efficiency,

despite the downtime associated with servicing. The netefficiency for HST from 3 July 2001 to 2 July 2002 was43.6% for prime observations and 51.0% for prime plussnap exposures. The science data rate increased by morethan a factor of two following the installation of the newinstruments, and the Institute supported this increases.

HST is also becoming easier to use, thanks to the newtools produced at the Institute. Migration of the archivedata to magneto-optical media was completed lastautumn. Several new software tools in support of HSToperations were released: the Astronomer’s ProposalTool (APT), StarView and the Space Telescope GrantManagement System (STGMS).

The Institute, and in particular the ESA staff, has providedleadership in several important science policy issues. Twonew programmes, the Treasury and Theory programmes,added to the opportunities for scientists to do researchwith Hubble and its data archives. With Cycle 11 we havestarted the Hubble Treasury Program, which had beenrecommended by the Hubble Second Decade Committeeto stimulate science that might not naturally beencouraged by the existing process, and, in particular, topromote the creation of important data sets that one wouldregret not having obtained when Hubble is ultimatelydecommissioned. Treasury programmes address multiplescientific problems with a single, coherent data set. Thedata sets carry no proprietary rights.

There were other novelties in Cycle 11. Given the rate ofincrease in the size of the Hubble data archive and thevalue of large, homogeneous data sets, we wished tostimulate more ambitious Archival Research (AR) bycreating the new AR Legacy Programme. SelectedLegacy programmes will perform a homogeneousanalysis of a well-defined data set in the Hubble archiveand will generate data products of use to the scientificcommunity (catalogues, software tools, web interfaces,etc.), which will allow a variety of new investigations.

Another important change in Cycle 11 was the start of theHubble Theory Programme, funded as part of the HubbleAR programme. The Theory Programme stressed theimportance of promoting theoretical research inconjunction with major observing facilities, in order toimprove the interpretation and understanding of the datafrom these facilities.

Another policy-related topic has been theimplementation of the project to trade observing timebetween Chandra and HST. This initiative came tofruition in Cycle 10 and was also advertised in Cycle 11.Both the HST and Chandra Time Allocation Committees(TACs) and users are very supportive of the concept andwe expect that we will soon see the published resultsfrom these joint efforts.

All of these initiatives were extremely well received and

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Cycle 11 was the most oversubscribed Cycle yet, by afactor of 8.5! As judged by an external review committeeof the TAC process, the STScI ran the Cycle 11 timeallocation process ‘in an exemplary fashion’.

The On-The-Fly Recalibration (OTFR) capability forWFPC-2 and STIS was implemented in 2001. This workwas originally pioneered by the European CoordinationFacility (ECF) staff in Garching and later adopted at theSTScI. Implementation of this capability enables STScIto provide better service to the user community byproviding science data products using the latestcalibration reference files. With OTFR implementation,we are now only storing the raw science data. Byeliminating the archiving of calibrated data sets, we havereduced the media requirements and since August 2001we are able to provide on-line access to the entire Hubblearchive. New agreements with the ST-ECF werenegotiated to implement the changes arising from OTFRoperations. The migration of the HST archive from Sonyplatters to magneto-optical media was completed aheadof schedule, before the end of 2001.

In summary, these have been two highly productive yearsfor the Institute and the Hubble programme.

3.6 Science Operations and Data Systems Division

3.6.1 Overview and general activities

The Science Operations and Data Systems Division wasformed in early 2001 as part of the reorganisation of theDepartment into a more matrix-based structure. It isresponsible for the development and execution of scienceoperations for astronomy missions and, after completionof the in-orbit commissioning phase, takes over overallproject management responsibility. Currently, for SolarSystem missions, the Division provides support andplays an oversight role. The Division also providessupport in data systems to the entire Department. Thestaff of the Division are located in VILSPA (Villafranca,near Madrid, E), in ESTEC and currently also has onestaff member collocated with the Integral Science DataCentre in Versoix (near Geneva, CH).

The key goals of the Division are to:

— improve the efficiency with which payloadoperations are prepared, executed and the resultingdata captured, distributed and archived;

— provide (and ensure) continuity of expertise not onlyfrom concept to conclusion but also from mission tomission’

— streamline RSSD-internal information technologysupport and usage.

To achieve these goals, the approach includes startingwork on defining science operations requirements andtheir associated costs as early as possible in the mission,looking for maximum commonality between in-orbitoperations and pre-launch testing and calibration,maximising the reuse of experience, techniques and (ifpossible) tools between projects, and designing anddeveloping the system in very close contact with theeventual users. The Herschel development (see Section3.6.6) embodies these principles. Support has been givento early definition of Eddington science operations tohelp establish realistic costs. The Division has alsoorganised reviews of the science operations of Herschel,Planck, Integral, Rosetta and SMART-1 and supportedreviews of Mars Express; these not only establish thecurrent status of the individual project but also help in thetransfer of experience.

Archives provide a good current example of cross-project developments reducing costs and reusingexpertise and code. A small archive-development grouphas been set up at VILSPA to provide horizontal supportto various missions’ archive projects. A flexible multi-tier architecture and modern technology (Java, XML) isbeing used to enable reuse of design and code fromearlier projects, thereby bringing down bothdevelopment and maintenance costs, while speeding updevelopment timescales. The modular approachfacilitates evolution and port of subsystems without

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affecting other systems, thus assisting in preservingefficient long-term access to the data from ESA’s sciencemissions. Furthermore, the openness of this model allowsESA science archives to interface easily with externalarchives and applications, thus ensuring their early andfull integration in the Virtual Observatory initiativesworldwide.

People in this archive team developed the ISO DataArchive (first public release in December 1998,www.iso.vilspa.esa.es/ida) and then reengineered thesystem to produce the XMM-Newton Science Archive(April 2002, xmm.vilspa.esa.es/xsa) in about half thetime and at one-third the cost. Current activities includemaintenance of the ISO and XMM-Newton archives aswell as the development of a general ESA PlanetaryScience Archive and a browser for the Integral archive.The Planetary Archive is being designed for general-purpose use (International Halley Watch campaign, MarsExpress, Rosetta, SMART-1, etc); the first release withIHW Giotto data is planned for mid-2003.

During the reporting period, the Division has managedall of RSSD’s computer systems. The work has beenorganised by platform, namely: the Unix environment(mainly Solaris but also LINUX and some Mac OS Xsystems), primarily orientated towards scienceoperations and data analysis; the Windows environment,including laboratory control, data analysis and officeautomation systems; and a small VMS environment fordata analysis. In addition to maintaining and wheneverpossible improving services for users (such asavailability, reliability, connectivity, back-up, e-mail,WWW, print-sharing, file-sharing, licence serving, etc), afocus has been placed on merging and streamlining theoriginally separate systems that were a legacy from thelong-standing two-division structure of the Department.Significant progress has been made in 2001-2002 and themerger is expected to be completed during 2003.

Other information technology services provided by theDivision include a document management system(Livelink), a hierarchical storage management system(presently scalable up to 38 TB), the DepartmentalWWW site, development of a publications-trackingdatabase, maintenance of a personnel database andassociated mailing lists, various database services(LDAP), helpdesk applications and various majorsoftware packages (including user support) such as theOracle database and the Concurrent Versioning Systemfor software development. Additionally, the Divisionmanages the human resources needed to provide dataprocessing support to the various research topics.

3.6.2 ISO A. Salama

The Infrared Space Observatory was the world’s first trueorbiting IR observatory. With a pointing accuracy at thearcsec level and four highly-sophisticated scientificinstruments, ISO provided a facility of unprecedentedsensitivity and capabilities for exploring the Universe at2.5-240 µm. During its highly-successful in-orbit opera-tional phase from November 1995 to April 1998, ISOmade some 30 000 individual scientific observations ofall types of astronomical objects. All the data areavailable to the community via the ISO Data Archive(follow the links from the ISO home page atwww.iso.vilspa.esa.es).

The ISO project is now in its Active Archive Phase,which will run until December 2006. This final phase isdesigned to maximise the scientific exploitation of ISO’sextensive IR database and to leave behind ahomogeneous archive with refined data products, as alegacy to future generations of astronomers.

For ISO, RSSD has the cradle-to-grave responsibility forISO’s scientific operations and, from the end of thecommissioning phase, overall responsibility for theproject. Currently, the Division has a team of staff andcontractors, led by the Project Scientist, in Villafranca,comprising the ISO Data Centre, whose activities includemaintaining the central data archive and providing expertsupport to the community across all instruments. TheISO Data Centre collaborates with National Data Centresat MPIA (Heidelberg, D), SRON (Groningen, NL), MPE(Garching, D) and RAL (Chilton, UK). Until the end of2001, there was also a formal involvement of centres inSaclay/Orsay (F) and IPAC (USA).

During 2001, the automatic processing pipeline andassociated calibration (used to generate the products forthe archive) continued to be refined. Then, all data werereprocessed with the final version of the pipeline toproduce the Legacy Archive. This was released at the endof February 2002 and represents the best set of productsthat can be generated by automatic processing. The ISOData Centre is now stimulating and coordinatingactivities to reduce selected data sets systematically byhand so as to obtain the ultimate quality data productsand to capture these into the archive (the Expert-ReducedData).

Regular archive maintenance and improvement activitieshave continued. Refereed ISO publications have beentracked and the resulting information incorporated. NewISO catalogues and atlases have been ingested. First setsof expert-reduced data were captured. In addition topreviously-existing links to SIMBAD, NED, IPAC/IRASand ADS, the ISO archive now interacts withCDS/Vizier, HEASARC, ADS and IRSA for display anddirect retrieval of ISO data products.

http://www.iso.vilspa.esa.es

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The ISO archive remains intensively used by theastronomical community. There are now over 1300registered users, who in the first 4 years of use havedownloaded the equivalent of seven times the totalnumber of scientific observations in the archive, amonthly retrieval rate of around 15%.

A major element of the ISO Data Centre’s activities isproviding support to the general community on allmatters regarding ISO data. The deep expertise of thestaff across all four instruments is used in a variety ofways: answering questions sent to the helpdesk facility(one per day on average); assisting visitors (28 visits inthe reporting period); and organising dedicated meetings.During 2001/2, two large conferences were organised.These were ‘ISO’s Calibration Legacy’ in February 2001and ‘Exploiting the ISO Data Archive’ in June 2002 (seeSection 4.1). Each attracted about 100 participants. Also,three small workshops (each with about a dozen people)were held; these gave an intensive 1-week course on aspecific aspects of ISO data processing, namely PHT32Oversampled Mapping. The proceedings are published inthe ESA SP series.

Another major activity is documentation. Variousreleases of a 5-volume ISO Handbook were made. Thisis the definitive standalone guide to the ISO mission andto its data products. Volume I gives an overview of themission and the spacecraft and volumes II-V cover thefour instruments. The legacy version is under preparationand will be released in early 2003. Regular summaryreports on the recent advances in ISO calibration werereleased. These summarised the activities of allparticipants, including various working groups and thenational ISO centres, and made the results easilyaccessible to the community. The WWW continues to bewidely used to disseminate information, with an averageof three postings per month being made on the ISOserver, with about one every 2 months being dedicated tooutreach.

ISO’s scientific results, impacting astronomical researchfields from comets to cosmology, continue to consolidatethe earlier technical and operational success of themission. In the 2001-2002 period, around 300 papersappeared in the major refereed journals and many morein the conference literature. With the ISO data archivehaving establishing itself as a general astronomicalresearch resource and also as an important tool forplanning future missions, with activities continuing onenhancing its contents and functionality, many moreastronomical surprises and discoveries from ISO are stillexpected.

3.6.3 XMM-Newton F.A. Jansen

The XMM-Newton X-ray astrophysics observatoryenables astronomers to conduct sensitive X-ray spectro-scopic observations (with simultaneous monitoring atoptical wavelengths) of a wide variety of cosmic sources.It was launched in December 1999 and has an expectedlifetime of over 10 years. Full information is available viathe WWW at http://xmm.vilspa.esa.es/.

Its three telescopes and suite of complementaryinstruments (EPIC, RGS and OM, used simultaneously)are designed to investigate in detail the spectra of cosmicX-ray sources down to a limiting flux of 10–15 erg cm–2 s–1.Sources down to a few times 10–16 erg cm–2 s–1 can bedetected; however, at these low flux levels, sourceconfusion starts to play a role. The principal character-istics of XMM-Newton are:

— effective aperture of 4500 cm2 at 1 keV (12.4 Å) and1000 cm2 at 10 keV (1.24 Å);

— almost constant angular resolution of ~15 arcsecHEW across the full waveband;

— X-ray FOV ~30 arcmin;— capability of performing sensitive medium-resolution

spectroscopy with resolving powers between 100 and700 over the wavelength band 5-35 Å (350-2500 eV);

— broadband imaging spectroscopy from 100 eV to15 keV (0.8-120 Å);

— simultaneous sensitive coverage of 1600-6000 Å(~17 arcmin FOV) through a dedicated opticalmonitor, co-aligned with the X-ray telescopes;

— continuous coverage of a source for up to 42 h.

The Division has overall management responsibility forthe project and is directly responsible for the execution ofthe science operations.

Mission operations for XMM-Newton are conductedfrom ESOC (Darmstadt, D), while science operations areconducted from VILSPA (Villafranca del Castillo, E). Themain tasks of the Science Operations Centre are:

— monitoring payload operations in real time;— performing mission planning and maintaining all

contacts with the observers necessary to construct anoptimally efficient schedule. This includes issuingand processing announcements of opportunity, aswell as handling Targets of Opportunity;

— maintaining a variety of XMM-Newton handbooks,including the XMM-Newton users handbook, theusers guide to the interactive analysis software, etc;

— tracking the maintenance of and implementation ofchange requests to its operations subsystems byexternal contractors;

— providing the archive containing all science data;— defining, implementing and tracking procedures for

operating the scientific instruments;

http://xmm.vilspa.esa.es/

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— implementing instrument calibration observations,coordinating and participating in their analysis, anddelivering finalised calibration files to thecommunity;

— pre-release checking of scientific validity of theScience Analysis Software (SAS) and the associateddata products.

During the first half of 2001, the emphasis was onensuring smooth and fast data delivery to the end-users.The mission met with considerable problems in this area,which resulted in unacceptable delays in data delivery.Numerous changes were implemented and additionalprocessing power was made available to the SurveyScience Consortium (SSC, PI: M. Watson, LeicesterUniv., UK) to cope with the backlog. One of theremaining problems, the generation of science data filesfor all observations performed before end-2000, wassolved by the installation of a separate processing chain,which could regenerate these data by bulk reprocessingof the raw telemetry stream. By August 2001, most of thebacklog processing had been executed and a moreroutine way of working could be adopted. The timebetween execution of an observation and delivery of thedata is now the nominal 3 weeks.

Work continued at ESTEC on developing and enhancingthe SciSIM (Science SIMulator) and the ScienceAnalysis Software (SAS). Robustness of the SAS, acollaborative development between ESA and the SSC, isa crucial factor in the success of any XMM-Newton dataprocessing. The latest SAS release is capable of routinelyprocessing >98% of all data. SAS and SciSIM work willbe transferred to VILSPA by mid-2003.

In close collaboration with a considerable number ofindependent external advisers, requirements weredefined for the XMM-Newton Science Archive. This isthe final, public repository of all XMM-Newton data.Following the definition of these user requirements, animplementation study concluded that the best option forimplementing the archive would be reuse of the highly-successful ISO Data Archive software and expertise.This was done and resulted in a well-received firstrelease of the XMM-Newton Science Archive (XSA) inMarch 2002, with additional functionality added in asecond release in November 2002.

ESA took a more active role in defining changes toonboard software in response to two anomalies. Anautonomous switch-off of the EPIC PN thermal controllerled to the definition and implementation of new softwareonboard XMM-Newton that will ensure proper remedialaction should such an event ever occur again. The EPIConboard software was modified to ensure filter wheelclosure of the instruments should ground contact be lostshortly before entering the radiation belts.

In orbit, the X-ray detectors are subjected to bombard-

ment by energetic particles, which causes degradation inperformance. Measured in-orbit results match pre-launchpredictions quite well. In order to ameliorate most of thedegradation incurred to date, it was agreed with the EPICand RGS PIs to cool the detectors by an additional 20-30ºC to around –120ºC. This action began in November2002 and will be completed in early 2003. An indicationof the effect of cooling the XMM-Newton detectors canbe seen in Fig. 3.6.3.

The second Call for Observing Proposals (AO-2) wasissued in August 2001 and some 860 proposals werereceived. The selection of the AO-2 observingprogramme met with some delays and was finallyannounced in July 2002. Priority was given tocompletion of the guaranteed time programme so theAO-2 observations started in September 2002.

In November 2001 a highly successful meeting, ‘NewVisions of the X-Ray Universe in the XMM-Newton andChandra Era’, attended by over 300 participants, washeld at ESTEC. The proceedings are being issued as anESA SP publication.

An XMM-Newton Users’ Group, to advise the Project

Figure 3.6.3: These pictures illustrate the enormouseffect that detector cooling has on the amelioration ofradiation induced damage. Panel (a) with detectors at–80ºC clearly shows many ‘hot pixels’ as artefacts,whereas they are completely absent at –110ºC (panel(b).

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Scientist on all matters relevant to optimising the scienceoutput of the mission, was appointed. The chairman isProf. J. Schmitt (Hamburger Sternwarte, Hamburg, D).The group met in March and September 2002 inVILSPA.

Despite its 10-year potential lifetime, only 2 years ofoperations were initially included in the overall cost. InDecember 2001, the SPC unanimously approved a 4-yearextension until March 2006 and agreed the budget for thefirst two of those years. Future extension requests willalso be based on this rolling 4-year horizon, whichenables making longer-term investments aimed atreducing future costs for mission operations, such asporting the operations systems from SCOS-1b to SCOS-2000.

With a very strong demand for observing time and arapidly increasing number of XMM-Newton papersappearing in the refereed literature, it is evident that theobservatory is fulfilling the scientific expectations of thecommunity. Results from XMM-Newton have alreadychallenged and invalidated some hitherto broadly-accepted theories and and have provided the basis fornew and refined models. Further exciting science isconfidently expected.

3.6.4 IntegralC. Winkler, A. Parmar and L. Hanson

Integral is dedicated to the fine spectroscopy and fineimaging of celestial gamma-ray sources in the energyrange from 15 keV to 10 Mev, with concurrent sourcemonitoring in the X-ray and optical bands. It waslaunched on 17 October 2002 from the BaikonurCosmodrome by a Russian Proton. The Launch and EarlyOperations Phase was completed 2 weeks after launch,with all nominal spacecraft functions having beenverified, and with all subsystems working nominally.Further information is available via the WWW athttp://astro.estec.esa.nl/Integral/isoc/.

Integral has two main gamma-ray instruments: aspectrometer (SPI) and an imager (IBIS). Both use codedaperture masks for gamma-ray imaging. Developed by aFranco-German-led team, SPI is performing spectralinvestigations of point-like and extended gamma-raysources with unprecedented energy resolution(E/∆E = 500) and sensitivity using Ge detectors cooledto 85K. SPI provides images of the gamma-ray sky with2.5º FWHM spatial resolution. IBIS, designed by anItalian-French-led team, is the perfect partner for SPI. Ithas lower energy resolution (E/∆E = 10) but is able toproduce the finest images ever of the gamma-ray skyowing to its good sensitivity and unprecedented spatialresolution of 12 arcmin FWHM. To supplement theobservations by SPI and IBIS, Integral also carries aDanish-led X-ray imager (JEM-X) with two detectors

each fitted with coded masks, and a Spanish-led CCDimager (OMC) operating in the Johnson V-band.Figs. 3.6.4/1 and /2 show first-light images from IBISand SPI.

The Division provides the Project Scientist, who chairsthe Integral Science Working Team. It has directresponsibility for the development, operations andmaintenance of the Integral Science Operations Centre(ISOC) as well as for coordination of the overall ScienceGround Segment. As of the formal end of the commiss-ioning phase on 13 December 2002, the Division hastaken over the overall management responsibility for theproject.

During 2001-2002, the main activities of the IntegralScience Working Team focused on finalisation of theCore Programme observation planning, reviewing thepre-launch calibration results, participating in major ESAprogramme reviews (flight acceptance, ground segmentreadiness) and scientific support for the planning of theperformance and verification phase that was conductedduring the 2-month commissioning phase after launch.Further activities concentrated on the preparation of thenext (5th) Integral scientific workshop.

The Integral Science Ground Segment (SGS) formallyconsists of the ESA-provided ISOC, located at ESTECduring the nominal mission phase (until December2004), and the nationally-funded Integral Science DataCentre (ISDC), located in Versoix (CH). The main inter-

Figure 3.6.4/1: A first light ISGRI image of Cyg X-1(centre) and Cyg X-3 (upper right) from 16 Novem-ber 2002. Energy range 14-60 keV, exposure 4 h.(Courtesy IBIS team).

http://astro.estec.esa.nl/Integral/isoc/

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faces and information flows are shown schematically inFig. 3.6.4/3. The instrument teams also contribute to theSGS. To support the community, ISOC and ISDC jointlyoperate a web-based helpdesk system.

The first Call for Observation Proposals (AO-1) was

issued by ISOC in November 2000 with proposals duefrom the scientific community by 16 February 2001. Theresponse was overwhelming, with 291 proposalsrequesting more than 19 times the open observing timeavailable. This remarkable over-subscription is testamentto the scientific capabilities of the mission and to the

Figure 3.6.4/3: The blue boxes show the two parts of the Integral science ground segment (ISOC and ISDC) togetherwith the main interfaces and information flows to ESOC.s Mission Operations Centre (MOC), the scientificcommunity and the satellite.

Figure 3.6.4/2: A SPI spectrum obtained during the solar flare of 10 November 2002 showing gamma-ray lines fromactivation of local detector material due to solar flare protons and demonstrating the spectroscopic quality of SPI.(Courtesy SPI team).

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interest of the astronomical community in the topics thatIntegral addresses.

All proposals were scientifically assessed by anindependent Time Allocation Committee (TAC), chairedby Prof. E. van den Heuvel (Univ. Amsterdam, NL).Based on scientific merit, the proposals selected by theTAC still oversubscribe the available time for 1 year by afactor of ~2. ISOC checked for targets close together inthe sky that can be observed in a single pointing, sosaving observing time through the amalgamation ofseveral independent research proposals. This isparticularly important for Integral where theobservations are generally long and the fields of view ofthe gamma-ray instruments are very large – the fullycoded fields of view are 16º (SPI) and 9 x 9º (IBIS). Anyscientifically outstanding proposals (grade A) that cannotbe scheduled during the first year will be carried over tothe AO-2 cycle.

The accepted proposals were processed at ISOC into anoptimised observing plan consisting of a timeline oftarget positions, together with the corresponding instru-ment configurations. Optimised observing plans are thenforwarded to the ESOC MOC for the creation of thecorresponding commands to be sent to the spacecraftwhich is, routinely, commanded using a pre-plannedautomatic command sequence.

The gamma-ray sky is very variable and interesting newtargets may appear unexpectedly anywhere in the sky.The Integral ground segment is designed to react rapidlyto these Targets of Opportunity. Observations withIntegral may be requested via the ISOC WWW pages.Following a positive decision by the Project Scientist,ISOC will generate a new observing programme, forwardit to the MOC, and make it available on the WWW so thatother coordinated observations can be planned.

Related to the core tasks of ISOC of processingobserving proposals and creating observing schedules,ISOC staff, in close collaboration with the Integralscience working team, were involved in a number ofactivities including:

— finalising the Core Programme of guaranteed timeobservations;

— preparation and management of the initial in-flightcalibration for the instruments during thePerformance and Verification Phase;

— various case studies to assess in-orbit performance.An example is the prediction that the IBIS detectorplane is sensitive to gamma-ray radiation passingthrough the SPI coded mask at ~45º off-axis. Thiseffect can be used to localise strong sources (e.g.GRBs) outside IBIS’ FOV but also imposesconstraints on the scheduling of some observationsso as to minimise the contribution from the fewstrong ‘contaminating’ sources like the Crab Nebula;

— supporting the instrument teams in instrumentconfiguration and operations (e.g. telemetryallocation).

On the technical side, 2001-2002 marked the comingtogether of all the ISOC software systems shown in theleft-hand side of Fig. 3.6.4/3. A first release of theoperational system was available for AO-1 and thesubsequent TAC process. It included a proposalgeneration tool (PGT) plus proposal handling softwarerunning in ISOC. The PGT is a Java application that isdownloaded via the Web by a proposer and run locally athis premises. In addition to capturing the incomingproposals, the proposal handling system also includescapabilities for printing, sorting, viewing and amalga-mating proposals. After the proposal process was over,the observation scheduling system was brought on line.ISOC’s system is largely implemented in Java and anORACLE database. The majority of the code wasdeveloped in-house but it includes pieces of softwarefrom ESOC/Flight Dynamics and software from theOMC PI. The complete ISOC system was used to supportinterface tests and end-to-end tests with the entire groundsegment and the satellite or an overall simulator. Beforelaunch, the system was also used to support activities likefuel budget assessment and long-term planning. It has, ofcourse, also been used extensively to support thepreparation and execution of the PV phase as well aslately the routine phase mission planning.

With the start of the routine operations phase in lateDecember 2002, the community is looking forward to anew view on the variable gamma-ray sky.

3.6.5 Astro-F M.F. Kessler

Astro-F is a Japanese mission with the prime goal ofmaking a second-generation IR all-sky survey with highersensitivity and longer wavelength coverage than IRAS.Launch is scheduled for 2004. ESA is collaborating withISAS to provide tracking support (use of a second groundstation) and assistance with the survey data reduction(pointing reconstruction) in return for 10% of theobserving opportunities during the non-survey parts of themission, to distribute to the ESA community. The SPCapproved this collaboration in autumn 2000.

Regarding tracking support, ESOC, in cooperation withISAS and with support from the Division, has drafted the‘Mission Implementation Requirements Document’ and‘Mission Implementation Plan’. For the pointingreconstruction and community support activities, whichwill be carried out in VILSPA sharing staff with the ISOData Centre, a plan has been made covering details of thenecessary software development.

In August 2001, the community in Europe was contacted

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to find research groups interested in participating in, andcontributing their own resources to, the catalogueproduction in return for scientific access prior to publicdata release. Some dozen responses were received whichwere processed with ISAS. As a result, ISAS are enteringinto collaborations with a few European institutes.

In summary, activities during the reporting period have,in general, been preparatory awaiting completion of theformal agreement between ESA and Japan for thecollaboration. This was achieved in December 2002, sothe pace of activities will sharply increase.

3.6.6 Herschel science operations development J.R. Riedinger

The Herschel Space Observatory is scheduled for launchin 2007 (see Section 3.1.1). Its science ground segment isbeing implemented in a distributed architecture with thescience community being supported by an ESA-providedHerschel Science Centre (HSC) located at VILSPA,Spain (US astronomers supported by the NASA HerschelScience Center at IPAC at CalTech) and instrumentoperations being carried out from three InstrumentControl Centres at MPE (Garching, D), RAL (Chilton,UK) and SRON (Groningen, NL).

Within RSSD, the Astrophysics Missions Division hasoverall responsibility for the scientific integrity of themission and for providing many of the requirements forscience operations. The Science Operations and DataSystems Division is responsible for implementing thescience operations, in close collaboration with theinstrument teams, and will take over overall projectmanagement responsibility from the end of the in-orbitcommissioning phase.

HSC development started in February 2000. Thisdevelopment will reuse many of the key operationalconcepts from previous, successful ESA astrophysicsmissions (ISO, XMM-Newton, Integral). However,based not only on progress in software technology andcomputer hardware but also on lessons learned fromprevious missions, several changes in ESA’s approach tosuch a Science Centre development are being made.

As part of the increasing acceptance of object-orientedsoftware development, the HSC software is beingdeveloped in Java. For HSC, this gives the advantages ofa large degree of platform independence and increasesthe possibility of reusing software components from oneproject to another.

The traditional single ‘waterfall’ development (with allcomponents coming together only at the end ) has beenreplaced by an incremental development with frequentintermediate releases that can be used, and commentedon, by end users. The benefits of this approach include

greatly increased interactions between end users andsystem implementers and reduction of the problemsinherent in bulk integration of a software system ofsignificant size.

Previously, the development of systems for operationshas been separated from facilities developed and used forinstrument development, test and integration on theground. To overcome this, the HSC developmentsupports the concept of ‘smooth transition’. A kernelsystem is rolled out to the instrument teams early(5 years before launch) for use in tests at instrumentlevel. Then, in parallel with instrument and satellitedevelopment, this kernel system is expanded infunctionality, used at system level and carried forward tooperations. The possible disadvantage of continuallyexpanding a system while it is already in use to archiveand analyse vital data is believed to be more than offsetby the advantages of this approach. Benefits of thisextensive pre-launch use include much more thoroughvalidation of the flight software, essential for a time-limited mission, and early detection of inconsistenciesbetween different parts of the overall space-groundsystem.

Almost from the beginning of this development, ESAand the PI Teams have made a conscious decision todevelop the Herschel Science System as a joint effort. Allbelieve that this is the best way of producing a systemthat best meets the needs of its end users, despite the factthat it cannot be completely specified at the start ofdevelopment.

Two years into this development, very significantprogress has been made:

— the user requirements have been consolidated; — the system has passed a System Requirements

Review, a Preliminary Design Review, and a CriticalDesign Review for the kernel system that is to bedelivered to the instrument teams for the start of theirinstrument-level tests at the beginning of 2003;

— the kernel system has been integrated and is beingprepared for System and Acceptance Tests;

— the infrastructure to further control and coordinatethis development is in place, and it seems that thedevelopment of Herschel science operations is wellon track.

http://astro.esa.int/herschel/

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3.7 Science Payloads Technology Division / SciencePayload and Advanced Concepts Office

3.7.1 Overview of activities

The overall responsibilities of the Science PayloadsTechnology Division, which in July 2002 evolved andexpanded into the Directorate’s Science Payload andAdvanced Concepts Office (hereafter ‘the Office’) canbe summarised as follows:

— support and manage the assessment phase of futuremissions;

— develop a strategic approach to future missiondevelopment;

— coordinate and develop new payload technologies insupport of the longer-term ESA science programme;

— provide scientific and technical support to ESAscience mission payloads and to the ESA scienceproject teams;

— provide the technical infrastructure in support of theRSSD research programme.

3.7.2 Assessment phase of future missions

The new Science Payload and Advanced TechnologiesConcepts Office has taken over responsibilities forperforming the assessment phase of future missions priorto a mission entering the definition and developmentphases. The current missions under assessment are:BepiColombo, Solar Orbiter, Darwin/SMART-3, XEUSand ISS payloads.

BepiColombo

The scientific objectives of the BepiColombo mission(see also Section 3.3.6) to Mercury are summarised inFig. 3.7.2/1, while the specific aims of the reassessmentphase can be summarised as follows:

— to reassess in detail the payload design;— to examine the potential for new technology to be

applied to individual instruments. Optimisation ofpayload resources through the introduction ofadvanced technologies and levels of integration;

— to reassess a range of mission implementationprofiles with a view to maximising the scientificreturn, within the associated technical and fiscalconstraints;

— to provide a basic mission design that can achievethe scientific objects and is technically andfinancially feasible for all the parties involved.

There are three core elements to the mission, which areshown schematically in Fig. 3.7.2/2: Mercury PolarOrbiter (MPO), Mercury Magnetospheric Orbiter(MMO), provided by ISAS/Japan, Mercury SurfaceElement (MSE), essentially the lander spacecraft.

The reassessment has been restricted to MPO and MSEand, in particular, the optimisation of the payloadthrough the use of advanced technologies to improvescientific performance while reducing resourcerequirements (mass, volume, power etc.). With such anapproach, the mission profile can be modified in such amanner as to provide an improved performance andtechnical feasibility while reducing overall costs. The

Figure 3.7.2/1: The overall science goals of the Bepi-Colombo mission to Mercury.

Figure 3.7.2/2: The three key BepiColombo missionelements.

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BepiColombo mission should enter the definition/development phase after the completion of thisreassessment, which is envisaged to be completed in July2003.

Solar Orbiter

The scientific objectives of the Solar Orbiter mission (seealso Section 3.2.6) are summarised in Fig. 3.7.2/3. It willform part of the BepiColombo mission group from thedevelopment phase onwards since many of thetechnologies required for both missions are common.Technologies such as high temperature solar-arrays,antennae and Solar Electric Propulsion (SEP) arepossibly common to both missions so close to the Sun (~0.2 AU). The Science Payload and Advanced ConceptsOffice has, and will continue, this mission assessment,through the conduct of the following key activities:

— detailed evaluation of the proposed model payload inclose cooperation with an external Payload WorkingGroup (PWG);

— optimisation of payload resources through theintroduction of advanced technologies and levels ofintegration;

— development and implementation of a payloadtechnology plan;

— industrial study of the mission profile options andspacecraft design, making full use of the heritage andtechnologies of the BepiColombo mission.

The overall schedule related to the assessment activitiesis summarised in Fig. 3.7.2/4. Solar Orbiter would be ready to enter its development phase by March 2004. The

basic configuration is illustrated in Fig. 3.7.2/5 togetherwith the mission’s currently established characteristics.

Darwin/SMART-3

The scientific objectives of the Darwin mission (see alsoSection 3.1.7) are summarised in Fig. 3.7.2/6. Darwinhas four core building blocks, which the Office isdeveloping so as to be able to move the missioneventually into its definition/development phase. Thesecan be summarised as follows:

— development and implementation of a payloadtechnology plan;

— study and implementation of a ground-based nullinginterferometer at the ESO-VLTI in collaborationwith ESO. This is a key project teaming with thecommunity and is known as GENIE;

— study and assessment through the SMART-3programme of the required in-orbit demonstrationtechnologies such as formation flying;

— industrial study of the mission profile options andspacecraft design, making full use of the heritagefrom SMART-3.

Figure 3.7.2/3: The basic scientific objectives of theSolar Orbiter mission.

Figure 3.7.2/5: The Solar Orbiter overall configura-tion and current characteristics.

Figure 3.7.2/4: The Solar Orbiter near-term schedule.PDD: Payload Definition Document.

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Darwin is a very complex and technically demandingmission that needs to be developed in a careful and step-wise manner on a number of fronts. Only with thisapproach can a technically feasible and financially well-bounded mission be able to enter the development phase.The current configuration featuring six spacecraftcontaining 1.5 m-diameter telescopes covering 5-20 µmand a seventh acting as the beam combiner form the fullnulling interferometer operated at 40K is illustrated inFig. 3.7.2/7. An eighth spacecraft handling communica-tions and data processing is also shown.

GENIE represents the demonstration in the near-IR ofthe basic nulling interferometer concept using some ofthe telescopes at the ESO VLTI. The technologydevelopments focus on many of the technical problemsassociated with combining the light with the appropriatedelays and phase-shifts from the various apertures.

XEUS

The scientific objectives of the XEUS mission (see alsoSection 3.1.9) are summarised in Fig. 3.7.2/8. XEUS hastwo key building blocks, which the Office is engaged so

as to be able to move the mission into the developmentphase. These are:

— development of a large-aperture segmented high-resolution X-ray mirror;

— integration and expansion of the mirror system usingthe International Space Station in-orbit infra-structure.

The key technology is, of course, the mirror and itsrequirement to provide high resolution (~2 arcsec) with alarge aperture (>10 m2). In addition, it needs to bemodular, segmented and low-mass, all of which challengethe basic heritage associated with X-ray mirror tech-nology. The problems – difficult but not insurmountable –are being handled in the Office through a number ofindustrial technology development contracts to demon-strate at breadboard level the required characteristics andperformance needed in the flight model.

Figure 3.7.2/6: The basic scientific objectives of theDarwin mission.

Figure 3.7.2/7: In-orbit configuration of Darwin.

Figure 3.7.2/9: XEUS docked at the ISS undergoingexpansion of the mirror from the initial 4.5 m to 10 mdiameter.

Figure 3.7.2/8: The XEUS science objectives.

Original Science Case• to detect the Earth orbiting a G2V star at 1 AU at r = 10 pc in a

reasonable time

Darwin Mission Development Science Case• to detect the Earth in the habitable zone around a large enough

(>500) sample of F, G, K & M-type stars

Secondary Scientific Objective• astrophysical interferometry imaging in the near-IR

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A single Ariane-5 launch could not lift and deploy inorbit a mirror of diameter ~10 m. XEUS overcomes thislimitation by making use of the in-orbit infrastructurecurrently being developed in low Earth orbit, namely theISS. This requires not only XEUS to be launched into afellow-traveller Orbit to the ISS but it must also be ableto dock with the ISS so as to grow the mirror from aninitial 4.5 m diameter to the final 10 m. Fig. 3.7.2/9illustrates XEUS docked to the ISS undergoing themirror expansion through the use of ISS robots.

International Space Station (ISS) payloads

Three science payloads are being studied within the Officeat Phase-A level towards a possible phased integration onto the ISS (see also Section 3.1.10). These studies arebeing conducted in close cooperation with external scienceteams as well as the Directorate of Human Spaceflight,responsible for ESA’s ISS development. These threepayloads are: EUSO (a high-energy cosmic ray observa-tory); Lobster (a medium-energy X-ray transient monitorusing novel X-ray optics); ROSITA (a medium-energy X-ray all-sky survey, essentially a replacement for the failedAbrixas German national mission).

While the scientific community would develop thepayloads, the uplift, integration and operation would bepart of ESA’s responsibility. Figure 3.7.2/10 summarisesthe overall objectives and characteristics of these threesignificant astrophysics ISS payloads.

It is clear that as the ISS infrastructure capabilitiesdevelop and mature in-orbit the demand in particularareas such as astrophysics and solar physics willincrease. Additionally, the modalities of studying futurepayloads and the clarification of responsibilities betweenthe various partners will also need to develop.

3.7.3 Towards a strategic approach to future missiondevelopment

Future missions proposed through the normal Call forIdeas and selected for assessment through theconsultative process with the appropriate working groupsand advisory committees need to be strengthenedthrough active preparatory work by ESA. To this end, theOffice has embarked on the study of a number ofTechnology Reference Missions (TRMs) with the aim of:

— studying potential future mission profiles;— identifying key technology areas needing develop-

ment in a longer-term strategic technology plan;— providing early mission support to the scientific

community to help in developing ‘new ideas’.

A number of TRMs are under study of which a subset,providing the overall flavour, is:

— a sample and return mission from a low-gravityenvironment, specifically the martian moon Deimos;

— a number of jovian system explorer missions to anumber of Jupiter’s moons, in particular Europa;

— Venus Aerobot explorers;— gamma-ray astrophysics imaging telescope.

Such missions should allow mission drivers, missionfeasibility and technological developments to be identi-fied and provided as input into the wider deliberations ofthe scientific community.

3.7.4 Coordination and development of new payloadtechnologies

The TRMs described above allow for the longer-termplanning of strategic technologies at both payload and

Figure 3.7.2/10: The ISS payload objectives andcharacteristics.

Figure 3.7.4: The overall flow of the technology plan-ning and implementation process.

ISS Science Payload ObjectivesEUSO

• space-based detection of extremely energetic cosmic rays and neutrinos(> 5x1019 ev)

• what are the limits to high-energy cosmic-ray processes, how do theypropagate, where do they come from?

• open up new channels such as high-energy neutrino astronomy• uses Earth’s atmosphere as a fluorescent detector of cosmic-ray showers

Lobster• continual all-sky coverage in the energy band 0.2-3 keV, with new Lobster-

eye optics• order-of-magnitude increase in sensitivity cf. previous missions allows

first opportunity to achieve long-term coverage of AGN light curves• breakthrough capability in monitoring energetic events such as X-ray

bursters, relationships to gamma-ray bursts, supernova shock breakouts,super transients, etc.

ROSITA• all-sky survey in energy band 2-10 keV, extending the sensitivity of Rosat

to higher energies and bringing higher angular resolution than previousmissions at high energies

• discover the rare brightest QSO type-2 objects, determine the obscurationbudget to black holes in the Universe, and map structure in the Universe

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spacecraft level. This allows therefore long-term needs tobe built into overall Science Directorate and Agency-wide technology plans. In addition, the assessmentphases of missions described in Section 3.7.2 allow for adetailed assessment of the instruments forming the modelpayload. This assessment not only allows the develop-ment of a Payload Definition Document (PDD), whichforms the backbone of any industrial assessment study,but is the basis for the payload technology plan. TheScience Payload and Advanced Concepts Office,supported by other parts of the Science Directorate andESA, particularly the Directorate of Technology andOperations Support, has tried to bring together thesemany strands of the long-term and medium-termtechnologies necessary for ESA’s future sciencemissions. This whole process involves identification,management, coordination and finally implementation,which are summarised in Fig. 3.7.4.

3.7.5 Payload support to ESA science projects

The Office provides support to ESA science missions,specifically payload support for missions in-orbit andpayloads for missions under development.

In the first case there are several areas where effort isprovided:

— instruments undergoing problems where instrumentphysics and engineering expertise can be utilisedoften in support of a PI team;

— instrument performance monitoring to develop adatabase of instrument heritage and problems, whichmay be useful in the design of future instruments;

— collation of instrument development costs includingin-orbit support in order to mature the instrumentdevelopment cost models.

In the case of missions under development the followingadditional activities are undertaken:

— reviews of instruments during the development cyclein support of the ESA project team as well as the PI-team;

— support to PI-teams in problem-solving and testing.An example here would be the extensive supportgiven to the Rosetta COSIMA instrument;

— specific payload technology development such asthose required for Eddington and Gaia. In the case ofEddington, both the telescope design and the CCDdesign and procurement for the focal plane camerasare technically coordinated through the Office insupport of the project and project scientist. For Gaia,the Office experts also support the focal planetechnology in cooperation with the Project Scientist;

— cost analysis of payloads under development, both atthe start and end of the cycle, followed by thematuring of instrument cost models.

3.7.6 Technical infrastructure support to RSSDresearch programme

The Office also provides the technical infrastructure insupport of RSSD’s research programme. In this regard,the Department’s laboratories, test facilities and technicalsupport fall within the responsibility of the Office ofScience Payload and Advanced Concepts. The Officesupports the development both of flight instrumentation,generally in collaboration with external institutes, as wellas applied physics/technology development for longer-term potential ESA science missions. The core supportprovided can be summarised as follows:

— maintenance of the laboratory infrastructure;— planning of the laboratories’ evolution in terms of

internal test facilities, support skills;— provision of technical and scientific support to

research projects involving flight and technologydevelopment hardware;

— management of all flight hardware and technologydevelopment projects.

Some of the key flight programme instrumentdevelopments underway or nearing completion are:

— the MIDAS Atomic Force Microscope for Rosetta(Fig. 3.7.6/1). This extremely challenging dust-analysis instrument is now integrated on thespacecraft. A spare unit will soon be integratedwithin the laboratory to support calibration, dataanalysis and cruise phase diagnostics;

— the impedance probes for the Rosetta Lander;— the Data Processing Unit for the Rosetta OSIRIS

camera, which is now integrated and fully tested onthe spacecraft (see Section 2.10.5);

— the SPEDE instrument on SMART-1, whichmonitors the electromagnetic environment aroundthe spacecraft resulting from the Solar ElectricPropulsion Module (see Section 2.8.4);

— the detector electronics for the electron and protontelescopes on-board the NASA STEREO spacecraft(see Section 2.7.5);

— the Data Processing Unit for the CNES/ESACOROT mission (see Section 2.6.7). COROT is animportant precursor mission to ESA’s Eddingtonmission now entering development as part of theHerschel-Planck-Eddington mission group, basedaround the common Herschel spacecraft bus.

In addition to these flight instrument units, a significanteffort is underway in support of the research andtechnology development in the following (non-exhaustive) areas:

— semiconductor sensors from the UV to the gamma-ray part of the spectrum;

— superconducting sensors from the near-IR to the softX-ray part of the spectrum;

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— low-mass X-ray optics for planetary exploration andastrophysics;

— in situ planetary instrumentation;— gamma-ray astrophysics developments in the field of

optics and sensors;— highly integrated analogue and digital electronics;— integrated payload suites for planetary orbiters;— biosensors.

Many of these laboratory developments are carried out inclose collaboration with industry and the scientificcommunity. In particular they are generally orientated tothe establishment of enabling technologies for thescientific community as building blocks for instrumentsexpected to be required in the long-term on futurescience missions.

The overall infrastructure support is summarised inFig. 3.7.6/2. Note that both technical and scientificmanpower support (technicians, engineers and appliedphysicists) are involved. In conclusion, the Office ofScience Payload and Advanced Concepts provides broadtechnical support to the Science Directorate’s instrumentand payload developments while assisting in theplanning, moulding and assessment of future missions.

Figure 3.7.6/1: The Rosetta MIDAS Atomic ForceMicroscope.

Figure 3.7.6/2: The overall infrastructure supportprovided by the Science Payload and AdvancedConcepts Office.

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symposia and workshops 105

4. OTHER ACTIVITIES

4.1 Symposia and Workshops organised by RSSD

‘The Calibration Legacy of the ISO Mission’, ISO DataCentre, ESA-VILSPA, Spain, 5-9 February 2001

This conference, organised by the ISO Data Centre, tookplace shortly after the ISO Calibration Working Groupshad completed their synthesis of the results of ISOinstrument calibration work. The meeting’s aim was tofocus the memory of the community of involved andinterested experts and to gather in one place the legacy ofthe ISO calibration work, with emphasis on clear andthorough exposition of the experience gained and of thelessons learned. Particular emphasis was placed on therelevance of the ISO experience to the calibration offuture space missions.

The conference attracted almost 100 participants frominstitutes all over the world involved in a wide range ofcurrent and planned Earth- and space-based astronomyprojects. The participants shared their extensiveexperience of calibration through 65 oral and 33 posterpresentations that captured the full range of calibrationexperience, and much of the mission operationalexperience, gained through the decades of the ISOmission. Topics addressed included instrument pre-launch and in-flight calibration, the challenges posed bythe space environment, detector physics, optical design,the establishment of reference source databases, and dataprocessing, and concluded with a session gatheringtogether lessons of importance for future missions.

The proceedings were published as ESA SP-481.

‘The Dark Universe: Matter, Energy, and Gravity’,STScI, Baltimore, Maryland, USA, 2-5 April 2001

The goal of this symposium was to bring togetherphysicists and astronomers working on all aspects ofdark matter and theories of gravity. The topics coveredinclude: nucleosynthesis, hot gas in clusters, MACHOs,WIMPs, rotation curves, gravitational lensing neutrinos,large-scale flows, dwarf spheroidals, cosmologicalparameters from supernovae, the cosmic microwavebackground, the cosmological constant and theories ofgravity.

The symposium was organised by S. Casertano andM. Stiavelli, together with other colleagues from STScI.

The First Eddington Workshop, ‘Stellar Structure and Habi-table Planet Finding’, Cordoba, Spain, 11-15 June 2001

The first Eddington workshop was the first occasion forthe wide community interested in the Eddington mission

to discuss the mission science and implementation,following the decision, in September 2000, to includeEddington in the scientific programme of ESA (although,at the time, with a ‘reserve’ status). About 100participants discussed the scientific goals of Eddingtonand the various options for the mission’s payload. Theworkshop attracted a broad variety of scientists,reflecting Eddington’s broad scientific goals. Experts inextrasolar planetary astronomy and in stellar structureand evolution featured prominently, reflecting the twokey scientific goals of the mission. In addition, scientistswhose main field is galactic structure, supernovae andgamma-ray bursts, were present. Scientists active in theother high-accuracy space photometry missions(COROT, MOST, MONS and Kepler), played a veryimportant role at the workshop.

The Scientific Organising Committee was co-chaired byI.W. Roxburgh of Queen Mary & Westfield College,University of London (UK) and by F. Favata. The localorganisation was performed by colleagues at the Institutode Astrophysics de Andalucia and Cordoba University.

The proceedings of the workshop were published as ESASP-485.

35th ESLAB Symposium, ‘Stellar Coronae in theChandra and XMM Era’, ESTEC, 25-29 June 2001

The symposium covered all aspects of high-energyphenomena in normal stars, ranging from the solarcorona to the coronae of active stars to the role of X-raysin star formation. More than 100 participants fromEurope, US and Japan attended the event.

Recent observational results from both Chandra andXMM-Newton obviously featured prominently amongthe presentations at the meeting, as did solar resultsbased on SOHO and TRACE. These were complementedwith a number of presentations about key (and yetunsolved) theoretical issues, such as the coronal heatingmechanism, the physics of flares, the spatial distributionof stellar coronal plasma, and the nature and presence ofelemental fractionation and abundance anomalies.Observational results from previous missions, such asEUVE, Rosat and SAX were also presented, showing thelasting legacy of these past observatories.

The Scientific Organising Committee was co-chaired byF. Favata (who was also responsible for the localorganisation) and by J. Drake from the Harvard-Smithsonian Center from Astrophysics in Cambridge(Massachussets, USA). The 600-pp proceedings of theSymposium (edited by F. Favata and J. Drake) werepublished in the Astronomical Society of the PacificConference Series, as Volume 27.

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106 symposia and workshops

‘New Visions of the X-ray Universe in the XMM-Newtonand Chandra Era’, ESTEC, 26-30 November 2001

This symposium focused on those areas in astrophysicswhere the results obtained by XMM-Newton and/orChandra invalidated current models and allowed thecreation of much more detailed ones. Examples were theLog N - Log S in deep fields at high energies (6-10 keV),which now largely explains the X-ray background atthose energies, and the cooling flow model for AGN,which was invalidated by the new observations. Thehighly successful meeting was attended by over 300registered participants, who were very enthusiastic aboutthe meeting and the results presented.


Phoebus Workshops on ‘g-mode Detection Techniques’,ESTEC, May 2001 and June 2002

In 1997, the Phoebus group was formed on the initiativeof T. Appourchaux. The aim is to detect low-frequency,low-degree g modes. The group is composed ofB. Andersen (Norwegian Space Center); G. Berthomieu,J. Provost and T. Toutain (Observatoire de Nice);W. Chaplin, Y. Elsworth and G. Isaak (University ofBirmingham); C. Fröhlich and R. Wachter (WorldRadiation Center); D.O. Gough (University ofCambridge); T. Sekii (National Astronomical Observa-tory of Japan); T. Hoeksema, A. Kosovichev andP. Scherrer (Stanford University); A .Jiménez (Institutode Astrofisica de Canarias) and T. Appourchaux.

The 4th and 5th workshops were held in May 2001 andJune 2002, leading to the production of three papersrelated to g-mode detection (Chaplin et al., 2002, MNRS,324, 910; Gabriel et al., 2002, A&A, 390, 1119; Wachteret al., 2003, ApJ). These workshops focused on usingadditional information on the internal structure of theSun (rotational splitting) and on novel statisticaltechniques for lowering the upper limit set by thePhoebus group in 2000. These new findings led to areview talk presented by T. Appourchaux on behalf ofthe group at the 12th SOHO workshop. A new researchdirection has been set that may lead the group to proposenew instrumentation and/or new space missions.

‘Cluster Workshops’, ESTEC, 3-5 October 2001;ESTEC, 5-8 March 2002; RAL, 18-20 September 2002

The Cluster mission has now been operating for almost2 years. An efficient data analysis phase requiresexchange of data among the 11 instrument teams aswell as discussions on the scientific topics. To this end,Cluster workshops have been organised by RSSD staff(specifically C.P. Escoubet, H. Laakso and A. Masson)once every 6 months since the start of operations with

the support of the scientific community. Threeworkshops, each attended by more than 120 scientists,were conducted with two or three parallel sessions,chaired by scientists from RSSD and the community.Each session concentrated on a theme or a scientificregion. The chairmen had pre-selected a list of eventsfor discussion. At the end of each workshop, the mostpromising events were selected for further study, withan assigned coordinator to lead the preparation of apublication.

The first workshop covered Cluster observations in thedayside of the magnetosphere, made about 6 monthsearlier. Specific attention was given to the bow shock,magnetopause, polar cusp, auroral region and plasma-sphere. One of the main results of the workshop was thepublication of a paper on the black aurora in Nature a fewmonths later.

The second workshop emphasised the magnetotail andmid-altitude polar cusp. It was also the first workshopinitiating a collaboration with the NASA IMAGE team.Both the IMAGE PI and several Co-Is participated. Twohighlights were the results on thinning and oscillation ofthe plasma sheet and the observation of double cusps.

The third workshop concentrated again on the daysidemagnetosphere and inner magnetosphere. This time,however, the discussions focused on the small spacecraftseparations (100 km) that were achieved at the beginningof 2002. Highlights of this workshop were the firstidentification of the various waves present in themagnetosheath, using the k-filtering method, and the firstmulti-point observations of the magnetic reconnection inthe magnetotail.

More information about the workshops can be found athttp://solarsystem.estec.esa.nl/~hlaakso/Cluster/

IAU Colloquium 186, ‘Cometary Science after Hale-Bopp’, Puerto de la Cruz, Tenerife, Spain, 21-25 January2002

The Colloquium, dedicated to the memory of the lateProf. Mayo Greenberg, was a follow-up of ‘The FirstInternational Conference on Comet Hale-Bopp’ held in1998. Its aim was to cover the progress in cometaryscience made since 1998. The scientific sessions coveredthe following topics:

— Hale-Bopp, what makes a big comet different; — split comets; — physical properties of cometary nuclei;— the relationship between coma abundances and

nuclear composition;— dust observations and models; — what we can learn from space missions;— origin and dynamical evolution of comets;

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symposia and workshops 107

— a roundtable discussion on how to benefit optimallyfrom the new 8-10 m telescopes and spaceobservations.

About 100 participants from 22 countries took part,presenting a total of 111 papers (18 invited and 93contributed oral and poster presentations).

The colloquium also looked into the relationship betweencomets and the interstellar medium, where comparisonbetween the chemical compositions of the gas and dust ofboth was a key issue.

R. Schulz chaired the Scientific Organising Committeeand is Co-Editor of the proceedings, which will bepublished as a special issue of Earth, Moon and Planets.

11th SOHO Workshop, ‘From Solar Min to Max: Half aSolar Cycle with SOHO’, Davos, Switzerland, 11-15March 2002

The 11th SOHO Workshop, dedicated to Roger M.Bonnet, covered the whole field of SOHO science, fromthe deep solar interior out to the solar wind andheliosphere, with special emphasis on solar cyclevariations. More than 160 participants from all over theworld discussed the current knowledge about our varyingstar in over 180 papers. It was organised around eightsessions:

— Solar Interior and Dynamo Theories;— Subsurface/Surface Dynamics and Magnetic Fields;— Total and Spectral Irradiance;— Magnetic Coupling and Dynamics of the Transition

Region and Corona;— Coronal Holes and Large-Scale Structures;— Transient Events: CMEs, Flares, Energetic Particles;— Solar Wind and Heliosphere;— Is Cycle 23 Normal, Abnormal or a Sign of Long-

Term Changes?

B. Fleck was a member of the Scientific OrganisationCommittee, chaired by C. Froehlich. The proceedingswere published as ESA SP-508.

‘Astrophysics of Life’, STScI, Baltimore, Maryland, USA,6-9 May 2002

The aim of this symposium was to understand the astro-nomical and astrophysical foundations upon whichsearches for life in the Universe must be based, andwhich bear on the nature and origin of life. Topicsincluded extrasolar planet searches and properties, thehistory of the Solar System, emergence, dust discs, starand planet formation, interstellar and Solar Systemchemistry, the habitability of planets, satellites and theGalaxy, strategies for searches, and cosmological

considerations. The aim was to lay the astrophysicalgroundwork for locating habitable places in theUniverse. New astronomical mission concepts were alsoan important element of the conference.

This symposium was organised by A. Clampin-Nota andcolleagues.

36th ESLAB Symposium, ‘Earth-Like Planets andMoons’, ESTEC, 3-8 June 2002

The 36th ESLAB Symposium covered comparativestudies of the Earth, Mercury, Venus, Mars, Moon,Galilean moons, Titan and terrestrial exoplanets. Thegoal was to review the understanding of their observedsimilarities and differences, and to give both an Earth-oriented and a cosmic perspective.

The Symposium had the following sessions:

— a family portrait of Earth-like planets and moons;— the contribution of space missions for understanding

Earth-like planets and moons;— Earth as a planet;— methods for comparative planetology;— interiors, surfaces, exospheres and impact processes; — comparing atmospheres and fluids (with emphasis

on Earth, Mars, Venus, Titan, Europa);— Earth-like planets and moons in the Galaxy;— habitable Earth-like planets and moons;— perspectives for future robotic and human exploration;— Young Planetary Explorers Special Session.

The programme was based on comprehensive invitedreviews, supported by interdisciplinary contributedpapers and a large body of posters on specific results,methods and planetary objects. Lectures by J. Head andApollo 17 astronaut H.H. Schmitt, open to all ESTECstaff, were well attended.

The organisation of the Symposium was led byB.H. Foing, supported by several other RSSD staff. Theproceedings were published as ESA SP-514. Moreinformation can be found at http://www.rssd.esa.int/Resources/conferences/eslab36/index.htm

‘Exploiting the ISO Data Archive – Infrared Astronomyin the Internet Age’, Parador of Siguenza, Spain, 24-27June 2002

The symposium, organised by the ISO Data Centre,VILSPA (SOC Chair: C. Gry; LOC Chair: P. Garcia-Lario), had a number of objectives, including offering theopportunity to present new results obtained with ISO,with special emphasis given to the generation ofcatalogues, to projects involving large datasets orsystematic data reduction, or any project making use of

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the data with a different purpose to that planned in theoriginal proposal, as well as offering new ideas andcollaborations for such projects. Another objective wasto encourage new projects by providing inventories ofthe scientific content of the archive and to advertise therelevance of the ISO Data Archive for the use of futureinfrared science facilities (Herschel, SIRTF, Astro-F,SOFIA, etc.) and solicit suggestions to make the archivemore useful in this respect. A final objective was tofacilitate the use of the archive by offering informationon the different tools available to work with ISO data andby addressing the relationship of the archive to otherdatabases and virtual observatories.

All these points were covered by the active participationof close to 100 scientists from 13 countries, who gave anequal number of contributions and data-handlingdemonstrations. The presentations revealed the existenceof many systematic data-reduction projects andhighlighted the interest of the participants for theingestion of expert-reduced data into the archive as oneof the main goals of the ISO Active Archive Phase(running until 2006). The high scientific quality of thepresentations emphasised the continuing avid interest ofthe community in ISO data and in mining the wealth ofits archive in particular.


‘Astronomical Data Analysis Software & Systems XII’,STScI, Baltimore, Maryland, USA, 13-16 October 2002

The ADASS conferences provide a forum for scientistsand programmers concerned with algorithms, softwareand software systems employed in the reduction andanalysis of astronomical data. An important element ofthe programme is to foster communication betweendevelopers and users with a range of expertise in theproduction and use of software and systems. Theprogramme consisted of invited talks, contributed papersand poster sessions. A number of user group meetingsand special interest group meetings were also held duringthe conference.

The proceedings will be published by ASP. The editorsare H. Payne, R. Jedrzejewski and R. Hook.

The 2002 HST Calibration Workshop’, STScI, Baltimore,Maryland, USA, 17-18 October 2002

The workshop featured reports from the commissioningof ACS and the recommissioning of NICMOS. Newcalibrations and advances in the understanding of STIS,WFPC2, FOS and FGSs were also presented, as well aspreviews of calibration plans for COS and WFC3, whichare planned to be launched during HST ServicingMission 4 in 2004 or 2005. The workshop was designed

to foster the sharing of information and techniquesbetween observers, instrument developers, andinstrument support teams. About 130 astronomersattended the workshop, which included approximately 30invited talks, 40 posters and time for demonstrations andsplinter groups on various topics.

The proceedings will be published by the USGovernment Printing Office, NASA and STScI in 2003(Eds. S. Arribas et al.).

12th SOHO Workshop, ‘Local and Global Helio-seismology: The Present and Future’, Big Bear Lake,CA, USA, 27 October - 1 November 2002

The 12th SOHO Workshop was held jointly with theannual meeting of the Global Oscillation Network Group(GONG). It focused on the study of the interior of theSun from a seismic perspective and the prospects forsimilar study of Sun-like stars. The workshop providedan excellent opportunity for the scientific community topause and reflect on the status of this fertile field, withmore than half a solar cycle of SOHO and GONGobservations. More than 120 participants discussed over100 papers addressing a wide variety of topics, includingthe observational status of low-, medium- and high-degree p-mode characterisation, low-frequency g-modedetection, solar structure and dynamics, mode excitationand damping, and advances in local helioseismology.There were seven sessions:

— Local and Global Helioseismology;— Helioseismic Imaging;— Temporal Variations in the Solar Interior;— Irradiance and Helioseismology;— From Solar to Stellar Seismology;— Structure of the Solar Interior;— Prospects for the Future.

The proceedings will be published as ESA SP-517.

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4.2 Science Communications

The prime responsibility for disseminating knowledgeand information about the goals and achievements of theESA Science Programme to the general public rests withthe Science Communications Service. However, RSSDProject Scientists and staff provide scientific expertisespecifically related to their project or discipline insupport of this responsibility. In the reporting period, thisincluded providing text and images for leaflets, posters,brochures, press releases and media interviews, as wellas validated background information on ESA sciencemissions, space topics and special features for the ESAScience public website (http://sci.esa.int). For the latterpurpose, RSSD staff contributed to 187 web stories in2001 and to 115 stories in 2002.

Of the 90 and 93 ESA press releases issued in 2001 and2002, respectively, 10 and 16 were related to science(somewhat less than 27 and 17 in 1999 and 2000). Inaddition, there were more than 10 press releases issuedby the STScI over the 2 years. ESA staff of the SOHOProject Scientist Team also made major contributions,together with their NASA colleagues, to keep the highprofile of solar science in the media.

Supporting the Science Communications Service towardsthe general public

RSSD staff supported a Science Media day on 18 June2002 at ESTEC, when the Integral and Rosetta spacecraftwere being prepared for shipping to their launch sites.RSSD Project Scientists, together with ESA projectmanagers and industry representatives, gave present-ations and interviews. Visits to the spacecraft in their testenvironment were included.

The highlight for ESA science in 2002 was the successfullaunch of Integral on 17 October. The mission was aprime topic for ESA public relations and sciencecommunication activities, with seven ESA press releasesand 10 web stories in 2002. Emphasis was placed on thepreparations of the spacecraft and the Proton launchcampaign from August to October, on the launch and,finally, on the first light from the different instruments atthe end of 2002. The public appeal of Integral wasconcentrated along the following lines: it will give newviews of the most extreme environments and from themost violent events far away in the Universe, and willdetect radiation from processes that created heavychemical elements necessary for life. Media represent-atives in Europe could follow the video transmission ofthe launch at ESOC (the main European press centre),ESTEC, ESRIN and VILSPA. RSSD experts wereavailable at each site for interviews.

There was also a high level of public-relations activitiesin 2002 on Rosetta (18 web stories). Emphasis was

placed on spacecraft ground tests as well as on theplanned science (origins of Solar System; Rosetta – acomet ride to solve planetary mysteries; life ingredientsfrom comets), and on the technological challenge oflong-duration survival. The Project Scientist participatedin a press event at Kourou after the Mission FlightReadiness Review Board on 13 November 2002. RSSDstaff also supported national media events in Munich,Berlin and London.

Both Mars Express and science from Mars attractedmajor media attention in 2002. They were the subject of11 web stories, building on the Mars Odyssey scienceresults on Mars water ice and weather, and theperspective of the ESA Mars Express mission. RSSDstaff also supported the ‘Red Encounter’ initiative of theScience Communications Service.

Communication activities in the reporting periodincluded the promotion of lunar and planetary science,new technologies, ESA horizons and new methods forsmall space missions and international space exploration.Project Scientists gave interviews to various mediarepresentatives on ESA planetary missions. On theoccasion of the ESLAB Symposium on ‘Earth-likePlanets and Moons’ in June 2002, several outreach eventswere organised. For example, the SMART-1 ProjectScientist supported interviews on lunar exploration andfilming of the spacecraft. A Lunar Base DesignWorkshop, attended by young scientists, engineers andarchitects, held after the Symposium, attracted theinterest of the public and media. The Apollo 17 AstronautH.H. Schmitt served as a lecturer.

The Lunar Explorers Society (LUNEX), created in 2000,is a bridge between space agencies and the public inter-ested in lunar, planetary and space exploration, empha-sising public outreach and education aspects. At its FirstLunar Explorers Convention at Palais de la Découverte,Paris in March 2001, the SMART-1 mission and otherESA planetary missions were highlighted by present-ations, models, computer simulations, leaflets, posters andinformation for the public. A press conference attracted 70journalists and resulted in good media coverage.

The often spectacular observations and discoveries madewith SOHO continued to make news headlines, oftentriggered by CNN news stories. Articles about SOHOappeared in several popular magazines. Several film andTV crews visited the SOHO Experiment OperationsFacility and SOHO has featured in a number of scienceTV stories. SOHO observations and images also play aprominent role in the 40-min giant-screen IMAXdocumentary ‘SOLARMAX’ (see www.solarmovie.com).

The international Sun-Earth Day on 27-28 April 2001provided an exciting opportunity to ponder our links withour nearest star and to celebrate the discoveries of ESA’sSOHO, Cluster and Ulysses solar observatories. This

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event, held on the 5th anniversary of the SOHO mission,was an opportunity to promote public awareness of thedynamics of our Sun and its influence on the Earth. Itwas shown how solar physics research, both from spaceand from the ground, contributes valuable informationthat can affect our daily lives. RSSD staff supportedevents (in local languages) at more than 40 locationsthroughout Europe.

RSSD scientists also supported a large number of othercommunication activities in 2001-2002, including theParis Salon at Le Bourget in June 2001, which included arealtime broadcast of the 21 June total solar eclipse fromAfrica, in coordination with SOHO coronal observations.Animations included presentations on space science andtechnology for the press and public, and a simulatedmartian landscape featuring a Beagle2 lander.

RSSD support to ESA corporate public relations activities

RSSD staff supported the ESA TV Service in theproduction of material related to ESA science missions,in a variety of formats covering missions such asIntegral, Mars Express and HST.

Support to other outreach initiatives

RSSD staff supported science communications events forthe science community at large. These took place, forexample, during sessions at IAF, COSPAR and EGSassemblies, where a network of space sciencecommunications partners was further developed.

Collaborative science communications events withmuseums, planetaria and educational institutions indifferent Member States were supported. Assistance wasgiven in organising exhibition events co-sponsored byESA featuring ESA space science missions.

Public outreach activities were conducted during theLeonid meteor campaigns in 2001 (from Australia) and2002 (from Calar Alto observatory, Spain). RSSD staffalso served as experts for the ‘Life in the Universe‘programme, when secondary school students preparedprojects on science and art. National winners werepresented at a central event at CERN, Geneva inNovember 2001. The EU Commission programmeNetdays to promote the use of new media in educationand culture was also supported.

Finally, RSSD staff also served as lecturers or expertreviewers in projects coordinated by the ESA Outreachand Education Office, such as:

— ‘Physics on Stage’ event for teachers in April 2002 atESTEC, bringing together hundreds of teachers for aweek;

— lectures and tutoring in support of the ESA/IAFinitiative, arranging the participation of about 200European students at IAF Toulouse in October 2001,and at the World Space Congress Houston in October2002;

— reviews for the SSETI workshop project, wherestudent teams all over Europe built a satellite via theWeb.

ESA Space Science public web site (missions and news):

http://sci.esa.intSOHO site: http://sohowww.estec.esa.nl/Lunar Explorers Society: http://www.lunarexplorer.orgLife in the Universe: http://www.lifeinuniverse.org/

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4.3 Other Coordination and Support Activities

EIROFORUM

Since the early 1950s, a number of powerful researchinfrastructures and laboratories used by an extensivenetwork of scientists have been developed and deployedwithin Europe by the European IntergovernmentalResearch Organisation (EIRO). These organisations(including CERN, EMBL, ESA and ESO) have set up acoordination and collaboration group (EIROFORUM),with their Directors General or equivalent as members. Aprimary goal of EIROFORUM is to play an active role inpromoting the quality and impact of European researchthrough effective high-level inter-organisational inter-action and coordination. This is possible by exploitingthe existing intimate links between the memberorganisations and their respective European researchcommunities. EIROFORUM encourages and facilitatesdiscussion on issues of common interest, relevant toresearch and development, to maximise the scientificreturn and optimise use of resources and facilities bysharing developments and results whenever feasible. Itcoordinates the outreach activities, including technologytransfer and public education, and simplifies high-levelinteractions with the European Commission and otherorgans of the European Union (EU).

A. Gimenez is a member of the ESA EIROFORUMdelegation. During the reporting period, a number ofjoint projects have been presented to the EC for fundingincluding, for example, the European Excellence Fellow-ship Programme (EEFP) and the European ScienceTeachers Initiative (ESTI). A number of ThematicWorking Groups have also been set up, including thoseon Instrumentation and Grid.

Astrovirtel/AVO

The ST-ECF, on behalf of ESA/RSSD, is involved intwo Programmes, co-funded by the EC, that aim toimplement in two steps a European AstrophysicalVirtual Observatory. The Virtual Observatory is aninternational astronomical community-based initiative.Its goal is to allow global electronic access to theavailable astronomical data archives of space- andground-based observatories and sky survey databases. Italso aims to enable data analysis techniques through acoordinating entity that provides common standards,wide-network bandwidth and state-of-the-art analysistools.

In this context, the ST-ECF is responsible for theprecursor Astrovirtel programme, which providesspecific scientific and technical support to selectedproposals based on the exploitation of existing digitalarchives of astronomical data, in particular thoseobtained with the Hubble Space Telescope and the ESO

Telescopes. The proposals are selected by a peer-reviewprocess on a yearly basis. The programme started in 2000and will finish at the end of 2003. During the threeCycles, some 15 proposals were supported at variouslevels. The outcome of the Astrovirtel programme hasbeen very positive because it not only produced novelscientific results, such as discovering new asteroids andstudying supernovae progenitors, but also stimulated theattention of the community on the huge scientificpotential of digital on-line archives. Astrovirtel was alsoinstrumental in providing actual science requirements forthe design and implementation of a fully-fledgedAstrophysical Virtual Observatory (AVO).

Opticon

The ST-ECF, on behalf of ESA/RSSD, participated in theOpticon Network, an EC-supported forum for thediscussion of initiatives in optical and infrared Europeanastronomy. The ST-ECF completed a feasibility study(fully funded by the EC) on the possible implementationin Europe of an ‘Elite Fellowship Programme’, similar tothe Hubble Fellowship Program in the US. The study waswell received by the EC and will be considered forimplementation in the 7th Framework Plan.

External Research Fellows

In addition to the internal Research FellowshipProgramme, there are about 20 External ResearchFellows, funded to work 1 or 2 years in ESA MemberState institutions outside of their own countries. TheseFellows contribute to research networking in support ofESA missions. Research Fellows working with the ESASOHO team at NASA/GSFC or at the STScI are alsorecruited via this scheme. During the reporting period,both R. Grard and B.H. Foing were members of the ESAinter-Directorate selection board.

General Scientific Support

The existence of an RSSD laboratory with experience inthe construction of flight instrumentation (now part ofthe Science Payload and Advanced Concepts Office)proved valuable for several external groups. SeveralRosetta and SMART-1 experiments that required in-house support during test programmes conducted atESTEC could be supported on short notice.

RSSD staff provided scientific advice and support to andparticipated in committee and working groups notdirectly within the purview of the Scientific Directorateand of ESA. These included:

— G. Schwehm continued to provide support to theAgency’s Space Debris Working Group. He was also

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nominated as coordinator for all Planetary Protectionactivities in the Agency. He represents ESA in theCOSPAR Planetary Protection Panel and is anobserver on NASA’s Planetary Protection AdvisoryCommittee. In April 2002, G. Schwehm participatedin the COSPAR/IAU Workshop on PlanetaryProtection in Williamsburg, Virginia, USA, whichwas convened to organise, update and consolidateCOSPAR’s Planetary Protection Policy;

— W. Wamsteker and the Department’s Operationsstaff at VILSPA, in coordination with ESA's Inter-national Affairs Department, have continued toprovide support to the organisation and programmedevelopment of the UN/ESA Workshops. This seriesof workshops has found a special niche in identify-ing opportunities to use space science in the develop-ing world. Special support was given to the 2001Workshop in Reduit, Mauritius, where a full sessionwas dedicated to the possibilities for the utilisationof data from SOHO. Also, at a workshop on SpaceData Utilization, the possibilities of using thearchival data of the ISO and IUE missions wereexplained. The 10th UN/ESA workshop was held inCordoba, Argentina. One of the concepts that hasarisen out of the deliberations of these workshops isthe general model of a World Space Observatory asan effective means of stimulating space science indeveloping countries, and to generate better oppor-tunities for participation of scientists from develop-ing countries in space science and education. Theimplementation of this is being studied by anInternational Committee, the World Space Observ-atory Implementation Committee (WIC), with amembership of scientists from 20 countries;

— B.H. Foing supported, as ESA representative,activities of the International Lunar ExplorationWorking Group (ILEWG), a body charged withdeveloping an international strategy for theexploration of the Moon. He also assisted as anexpert the United Nations Space GenerationAdvisory Council (UNSGAC), in particular for theSpace Generation Summit held at the World SpaceCongress 2002 in Houston;

— RSSD staff were active in numerous scientificsocieties (EAS, EGS, EPS) and some of theScientific Unions (COSPAR, IAU, URSI, IUPAP),where they contributed to scientific meetings (e.g.EGS, COSPAR) by organising special sessions anddiscussions, and, in some cases, holding electiveoffices. For example, W. Wamsteker is a member ofthe Executive Working Group of the IAU for FutureLarge Scale Facilities, and K.-P. Wenzel is Chairmanof COSPAR Scientific Commission D on SpacePlasmas in the Solar System, and Chairman ofIUPAP Commission C4 on Cosmic Rays;

— RSSD staff also taught space sciences and relatedtopics in Member State universities and in severalinstances were also appointed as jury members forPh.D. theses. The direct contact between ESA staffand students and staff at the universities continues tobe mutually rewarding;

— M.F. Kessler and K.P. Wenzel were invited to co-author review papers in fields of their scientificexpertise for the book The Century of Space Science,which appeared in 2002.

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ANNEX 1Manpower Deployment

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Department Office, ESTEC

Head of DepartmentGimenez, A. (from July 2001).

Chief ScientistFoing, B.H., SMART-1 Project Scientist, comparative

planetary and astrobiology, solar-stellar physics.

Administrative staffBingham, C., Departmental Administrative Assistant.Fontaine, R., RSSD Project Controller.Ihaddadene, S., Divisional Secretary and Administrative

Assistant.Nilsson, C. (to July 2002), Divisional Secretary and

Administrative Assistant.Schroeder, B., Divisional Secretary and Administrative

Assistant.Villien, C. (from November 2002), Divisional Secretary

and Administrative Assistant.

Astrophysics Missions Division

Clavel, J., Head of Division (from April 2002),Multiwavelength Observational Astronomy.

De Bruin, J., (from October 2002), Support Scientist onGaia.

Favata, F., Eddington Study Scientist, COROT ProjectScientist, support to GAIA studies, cool stars andstellar activity, X-ray astronomy.

Fridlund, M., IRSI/Darwin Study Scientist, astrophysicsof star formation.

Heras, A., Herschel scientist, infrared astronomy.Jakobsen, P., JWST Study Scientist, optical/UV astron-

omy with HST and ground-based astronomy.Laureijs, R.J. (from December 2001), Planck Deputy

Project Scientist, interstellar medium, dust properties.Parmar, A., Acting Integral Project Scientist, XEUS,

Lobster, ROSITA and EUSO Study Scientist, Leaderfor SAX LEGSPC, X-ray astronomy (X-ray binariesand AGN).

Perryman, M.A.C., Hipparcos Project Scientist, GaiaProject Scientist, exploitation of Hipparcos data.

Pilbratt, G.L., Herschel Project Scientist, IR and sub-mmastronomy.

Prusti, T., Herschel Scientist, infrared astronomy.Tauber, J., Planck Project Scientist, sub-mm astronomy.

ESA Research FellowsBocchino, F. (to September 2001), X-ray astronomy.Boirin, L. (from October 2001), X-ray astronomy.Del Burgo, C. (from October 2002), Modelling of sky as

seen by Planck.Dupac, X. (from October 2002), Planck-related science

on cosmic background and interstellar dust.

Giardino, G. (to January 2001), Cosmology studies.Jansen, R. (to December 2001), Optical/UV astronomy.Katz, D. (to Septermber 2001), Optical astronomy.Nevalainen, J. (to August 2001), X-ray astronomy.Papadopolous, P., Interstellar medium.Sidoli, L. (to June 2001), X-ray astronomy.Stankov, A. (from February 2002), Analysis of stellar

seismology.

Young Graduate TraineesAigrain, S. (to September 2001), Algorithm for exo-

planet transit detection.Carpano, S. (to September 2002), Exoplanet transits with

Eddington.

StagiairesChico, A. (March-August 2001), GENIE configuration.Drummond, R. (July-September 2002), Spacecraft jitter

simulations for Eddington.Hijmering, R. (May-September 2002), Quicklook data

analysis software for STJs.

Portuguese/Spanish TraineesFranco, G. (to October 2002), Planck/XMM.Perez Ramirez, D. (from May 2002), XMM data

analysis.Silva, B. (from November 2002), Eddington data

analysis.

Contractor Staff (full- or part-time during the reportingperiod)Bremer, M., Planck ground segment system engineering

and web support.

Solar and Solar-Terrestrial Missions Division

Wenzel, K-P., Head of Division, Deputy Head ofDepartment, energetic particles studies.

Brekke, P., Support to SOHO Project Scientist, solarphysics, science communications.

Escoubet, C.P., Cluster and Double Star Project Scientist,magnetospheric physics.

Fehringer, M., Support to Cluster and Double StarProject Scientist, Microscope Study Scientist (sinceSeptember 2001, 25% under the Fundamental PhysicsMissions Division).

Fleck, B., SOHO Project Scientist, Solar Orbiter StudyScientist, solar physics.

Haugan, S., SOHO Science Operations Coordinator,solar physics.

Marsden, R.G., Ulysses Project Scientist and ProjectManager, Solar Orbiter Study Scientist, ILWSsupport, energetic particle data interpretation.

Sanchez, L., SOHO Science Data Ordinator, SOHOarchive.

ANNEX 1: MANPOWER DEPLOYMENT

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Sanderson, T.R., Cluster Archive Scientist, energeticparticle instrument development and datainterpretation.

ESA Research FellowsBerghmans, D. (to June 2002), develop image recognition

software tools for detection of major solar events inSOHO data.

Fierry-Fraillon, D. (to January 2002), Helioseismology.Hofer, M. (to December 2002), Energetic particle data

analysis.Masson, A. (to October 2002), Cluster data analysis.Moullard, O. (to January 2002), Plasma and particles

studies.O’Shea, E. (to September 2002), Solar magnetic field

studies, ESMN Fellowship.Trautner, R. (to October 2001), Instrument development.

ESA External FellowMcIntosh, S. (from February 2001), Criticality of solar

flares and chromospheric dynamics.

TraineesWinston, E. (June-August 2001), Solar events.

Contract staff Mann, I. (to August 2002), Cosmic dust studies and

IRSI/Darwin support.Masson, A. (from November 2002), Cluster data

analysis.Tranquille, C., Ulysses data archive.

Planetary Missions Division

Schwehm, G., Head of Division (from February 2002),Rosetta Project Scientist.

Chicarro, A., Mars Express Project Scientist, planetarygeology.

Grard, R.J.L., BepiColombo Project Scientist, modellingand instrument development.

Koschny, D.V., Support to Rosetta Project Scientist,Science operations planning, meteor research,planetary cameras.

Laakso, H., Support to BepiColombo, magnetosphericplasma research.

Lebreton, J.-P., Huygens Project Scientist and MissionManager, Solar System technology support, plasmaphysics instrument development.

Martin, P., Mars Express Operations Scientist.Ocampo, A. (from February 2002), Support to Mars

Express and BepiColombo.Schulz, R.M., Support to Rosetta Project Scientist,

Rosetta Lander, cometary studies.Svedhem, L.H., Venus Express Project Scientist,

development of planetary instrumentation, cosmicdust studies.

Research FellowsBoudin, N. (from March 2002), Astrochemistry (for B.H.

Foing).Heather, D. (to June 2002), Lunar studies.Michael, G. (from March 2002), Comparative

planetology.Piot, A. (from March 2002), Exploitation of Huygens test

balloon data.Witasse, O. (to September 2002), Planetary atmospheres.

Young Gradutate TraineesHoofs, R. (to June 2001), Science operations planning

tool development.Kazeminejad, B. (to June 2002), Huygens mission

analysis studies.O’Sullivan, J. (to September 2002), Development of

Dust Mass Spectrometer for BepiColombo.

StagiairesAlmeida, M. (February-June/August-September 2002),

SMART-1 AMIE calibration, science operationssupport.

Diaz, J. (March-July 2002), Meteor research. Dages, O. (March-August 2001), SMART-1 risk analysis.Firre, D. (March-May 2001), Huygens mission scenario.Larfors, K. (April-July 2002), Instrumentation develop-

ment on dust spectrometer.Lefevre, F. (March-August 2001), Payload operations.Manaud, N. (March-August 2002), Planetary operations. Martinez, S. (October 2001-January 2002), Rosetta

science operations.Riesen, T. (March-May 2002), Rosetta science archive. Reissaus, P. (to December 2001), Meteor simulations.Samaine, T. (March-August 2002), Laboratory testing of

multi-channel I-V converter ASIC chip.Uberia, M. (March-June 2002), Rosetta knowledge

management.Vasquez, B. (October 2001-January 2002), Planetary

science data archives.Vilar, E. (April-August 2002), SMART-1 and Rosetta

operations and data simulation.

PhD/MS StudentsRuiterkamp, R. (from 2001), BioPAN and organics in

space.Ten Kate, I. (from 2002), Mars simulations chamber.Zijlstra, A. (September-December 2002), Lunar lander

design thesis (MS).

Spanish/Portuguese TraineesPerez Ayucar, M. (from June 2002), Huygens telecomm-

unications engineering (E)Simoes, F., (from April 2002), Water on Mars (PT).Vazquez Garcia, J. (June 2002), SMART-1 telecommuni-

cations engineering (E).

ContractorsHeather, D. (from July 2002), Support to planetary data

analysis.

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Hoofs, R. (from July 2001), Rosetta science operationsengineer.

Trautner, R. (from November 2002), Mars Expressengineer.

Fundamental Physics Missions Division

Reinhard, R., Head of Division, Study Scientist for LISA(until April 2002), STEP, Hyper and Microscope (untilSeptember 2001).

Jafry, Y., STEP Study Manager (until October 2002), drag-free control expert for fundamental physics missions.

Jennrich, O. (from May 2002), LISA and SMART-2Study Scientist.

Space Telescope Operations Division

Macchetto, D., Head of Division, AGN, ellipticalgalaxies, gamma ray bursts.

ST-ECF, GarchingESA scientific staffBenvenuti, P., Head of ECF, HST Project Scientist,

extragalactic HII regions, SNRs.Albrecht, R., Deputy Head ECF, Head of Science Data

and Software Group, minor bodies of the SolarSystem, computer science.

Dolensky, M., Science archive and WWW softwarespecialist.

Fosbury, R.A.E., Head of HST User Support Group,galaxies and AGN.

Micol, A., Science archive software specialist, imageprocessing techniques and information systems.

Rosa, M.R., Head Post-operational Archive Group, HIIregions, star formation, supernovae, evolution ofgalaxies.

ESO staff (included here to give the full picture of ST-ECF team staffing)Cristiani, S. (to July 2002), Instrument Scientist, obser-

vational cosmology, galaxy evolution.Freudling, W., Instrument Scientist, observational cos-

mology, peculiar motion of galaxies.Haase, J. (from June 2002), Astronomical data archive

and pipeline software specialist.Hook, R.N., HST Data Analysis Scientist, scientific

software support, image restoration applications.Kuntschner, H. (from November 2002), Instrument

Scientist, galaxy formation and evolution.Pierfederici, F., Astrovirtel support scientist.Pirenne, B., HST Archive Scientist, data storage tech-

nology, gravitational lenses.Pirzkal, N., Scientific analyst/programmer, pre-main-

sequence stars.Sjöberg, B., ST-ECF administrative assistant/secretary.Walsh, J.R., Instrument Scientist, planetary nebulae, HII

regions.

ESO staff under ESA contractAlexov, A., Post-operation instrument scientific

programmer.Bristow, P., Post-operation instrument scientific

programmer.Christensen, L., HST Outreach Astronomer.Fourniol, N., Archive operator.Kerber, F., Post-operation Instrument Scientist, early-

type stars.Kornmesser, M., HST Outreach Technical Editor.Pasquali, A., Instrument Scientist, stellar winds, nebulae.

Contract staff Pettefar, N. (from August 2002), ST-ECF systems

administrator.

STScI, BaltimoreArribas, S., NICMOS Instrument Scientist, AGN, high-

redshift galaxies, cosmology.Boeker, T., NICMOS Instrument Scientist, galaxy

formation and evolution, in particular gas dynamics inthe central regions.

Clampin-Nota, A., Deputy Head, Science Division,massive stars, late stages of stellar evolution, IMFstudies.

De Marchi, G., ACS Instrument Scientist, initial massfunction, globular clusters, dark matter haloes.

Espey, B. (to April 2002), STIS Instrument Scientist,emission line diagnostics, symbiotic binary stars,QSO emission and absorption lines, HDF South.

Goudfrooij, P. (to October 2002), STIS InstrumentScientist, interstellar matter and stellar populations inearly-type galaxies.

Jenkner, H., HST Mission Deputy, Guide Star Catalog II,microvariability studies using FGS photometry.

Mais-Appellaniz, J. (from July 2002), SpectrographsInstrument Scientist, HII regions, young clusters.

Meylan, G., Proposal Scientist, gravitational lensing andcosmology, stellar dynamics, photometry.

Miebach, M., Lead Engineer for scientific instruments.Mobasher, B. (from April 2000), STIS Instrument

Scientist, Galaxy surveys, dwarf galaxies, ellipticalgalaxies.

Padovani, P., Multi-Mission Archive Scientist, AGN:unified schemes, evolution, X-ray spectra, blazars.

Panagia, N., NGST Science Lead, stars, interstellarmedium, supernovae, galaxies, cosmology.

Robberto, M., WFC3 Instrument Scientist, star forma-tion, massive stars, IR instrumentation.

Stanghellini, L., Proposal Scientist, planetary nebulaeand their central stars, extragalactic distance scale.

Stiavelli, M. (to September 2001), ACS InstrumentScientist and Integrated Product Team Member forWFC3, formation and evolution of galaxies.

Wiklund, T. (from September 2002), NICMOSInstrument Scientist, AGN, starburst galaxies.

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ESA External Research FellowsChiaberge, M. (from 2001), AGN, FRI and FRII

unification, BL Lacs.

Science Operations and Data Systems Division

Kessler, M.F., Head of Division (from April 2001),Infrared Astronomy.

Bennett, K., Gamma-ray astronomy, Planck (Co-I).Jansen, F., XMM-Newton Project Scientist, X-ray

astronomy. Szumlas, M., Technical coordination, data bank

maintenance.Thoerner, G., Divisional system analyst/computer

manager, SAX data analysis and cosmology studies.Toni, A., Computer administration.Winkler, C., Integral Project Scientist, gamma-ray

astronomy data analysis.Wamsteker, W., Multi-disciplinary scientist, active

galaxies, abundances at high redshifts (at VILSPA).Zender, J.J., Data handling/archiving management for

planetary science operations.

Contractor Staff (full- or part-time during the reportingperiod: ESTEC)Bowen, A., Data librarian.Bowen, H. (from December 2002), Solaris system

administration. Buggy, O. (from February 2001), Solaris system

admininstration plus HSM M&O. Cappa, F. (to October 2002), Computer system

administration.Esson, S., VMS system administration, Oracle and

Livelink support.Giardino, G., Planck IDIS Development: data layer.Hansen, J. (to December 2002), Solaris system

administration.Hazell, A., Planck IDIS Federation and system

engineering.Hulsbosch, A. (to December 2002), Ulysses research

support, Rosetta SOC development.Moser, F., Windows system administration.Phipps, K. (from March 2002), Planck IDIS develop-

ment: software repository, LDAP support. Planje, K., Graphics and printers support.Riemens, M., Administrative support and database

maintenance.Williams, O.R. (to July 2002), COMPTEL/Planck data-

base management and scientific operations.

Herschel Science Centre, ESTECRiedinger, J., Herschel Science Centre Development

Manager.Claes, P. (to February 2001), Herschel software engineer.Mathieu, J-J., Interactive analsysis (part-time, TOS

support).

Ott, S. (from July 2002), System analyst, interactiveanalysis coordinator.

Prades-Valls, R., Quality assurance (part-time, TOSsupport).

Veillat, S. (to June 2002), System engineer (integratedTOS support).

Contractor Staff (full- or part-time during the reportingperiod)Bakker, J. (from September 2002, shared with XMM),

interactive analysis. Bonfield, A. (from September 2002), Proposal handling,

(integrated TOS support).Brumfitt, J., System architect, core classes, scientific

mission planning.Candussio, N. de (from July 2002), Interactive analysis,

(integrated TOS support).Galloway, K., System engineer, telemetry ingestion,

documentation.Porrett, C. (from June 2001), Calibration uplink system,

testing, build scripts. Siddiqui, H., MIB interface, interactive analysis, SPR

system.Zondag, R. (from June 2001), Configuration control,

system builds, testing, installation, web.

Integral Science Operations Centre (ISOC), ESTECHansson, L., Integral Science Operations Manager.Barr, P., Operations scientist, mission planning.Breneol, C. (to July 2001), Computer software

development manager.Much, R., Operations scientist and Deputy Project

Scientist, observational astronomy.Orr, A. (from June 2002), Operations scientist, JEM-X

and OMC expert, helpdesk.Sternberg, J., System engineering, ISDC liaison.Trams, N. (to July 2001), Operations scientist.

Contractor staff (full- or part-time during the reportingperiod)Cruse, B. (to April 2001), Software engineer, PHS

development.Dean, N., Testing, OSS maintenance, backup software

librarian.Jacobs, F. (from January 2001), PHS maintenance

(JAVA), DB administrator. Jeanes, A. (25% since mid 2002), OSS development/

maintenance (JAVA).Greenwood, S. (from January to August 2002), OSS

development.Kuulkers, E. (from June 2002), Operations scientist,

backup mission planner, IBIS expert. Nolan, J., ISOC procedures, instrument and spacecraft

operations expert.Oosterbroek, T. (from August 2002), Operations

scientist, SPI expertise, local science analysissoftware expertise.

Orr, A. (to May 2002), Operations scientist.

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Treloar, J., Software librarian, PGT and associatedsoftware maintenance.

Williams, O.R. (from August 2002), Integral ScienceData Archive installation and maintenance.

Zondag, R. (to June 2001), Archive engineer, systemadministration.

Integral Science Data Centre (Geneva)Texier, D. (from June 2002), Resident engineer.

XMM-Newton Science Operations (ESTEC)Contractor staff (full- or part-time during the reportingperiod)Bakker, J., SAS/SciSIM GUI/cross platform develop-

ment.Lammers, U., CAL software/Event selection.

ISO Data Centre (IDC), (VILSPA)Blommaert, J. (to October 2001), ISO Resident

Astronomer, ISOCAM expert, ISOCAM Handbook,Handbook co-editor, AGB evolution and galacticstructure.

Burgdorf, M. (to November 2001), ISO ResidentAstronomer, LWS expert, Solar System, stellarstatistics.

Garcia-Lario, P., ISO Resident Astronomer, cross-calibration expert, Handbook co-editor, late stages ofstellar evolution.

Gry, C., ISO Resident Astronomer, LWS expert, LWSHandbook, interstellar medium.

Kessler, M.F. (to March 2001), ISO Project Scientist. Laureijs, R.J. (to December 2001), ISO Resident

Astronomer, PHT expert, ISM and dust.Leech, K. (to December 2001) ISO Resident Astron-

omer, SWS expert, SWS Handbook, infraredastronomy, brown dwarfs, Hale-Bopp.

Lorente, R. (from October 2002), ISO ResidentAstronomer, ISOCAM expert.

Metcalfe, L. (to July 2002), ISO Project Scientist,gravitational lensing.

Müller, T. (to December 2001) ISO ResidentAstronomer, Handbook co-editor, Solar Systemstudies, asteroids.

Ott, S. (to June 2002), ISOCAM expert, ISOCAMinteractive analysis lead, ISOCAM parallel mode.

Peschke, S., ISO Resident Astronomer, ISOPHOTexpert, comets.

Salama, A., ISO Project Scientist (from May 2002),SWS expert, Titan, novae and symbiotic stars.

Schulz, B. (to January 2002), ISO Resident Astronomer,ISOPHOT expert, AGN.

Verdugo, E. (from November 2002), Resident Astron-omer, ISOPHOT expert, ISO Data Archive productsquality.

Research FellowsSanchez Fernandez, C. (from April 2002), ISO and

XMM-Newton data analysis.

Contractor staff (full- or part-time during the reportingperiod)Martin, S. (from September 2001 to January 2002),

secretarial and administrative support. Matagne, J., ISO WWW master.Salomone, M. (to January 2002), Science journalist.Willis, A., Secretarial and administrative support.

XMM-Newton SOC (VILSPA)Clavel, J. (to March 2002), XMM-Newton Science

Operations Manager.Altieri, B., Software and payload support, observational

astronomy.Arpizou, M., Secretarial and administrative support.Ehle, M., XMM-Newton user support, observational

astronomy.Gabriel, C., XMM-Newton instrument support, super-

nova remnants, cosmology.Guainazzi, M., XMM-Newton user support, observa-

tional astronomy.Kirsch, M. (from February 2002), EPIC calibration

scientist. Metcalfe, L. (from July 2002), XMM-Newton Science

Support Manager.Munoz Peiro, J. (from May 2002), Instrument Operations

Manager.Pollock, M. (from February 2002), RGS calibration

scientist.Santos-Lleo, M., XMM-Newton user support, observa-

tional astronomy.Schartel, N., XMM-Newton User Support and Mission

Planning Group Team Leader, observationalastronomy.

Texier, D. (to March 2002), XMM-Newton InstrumentSupport Group Team Leader.

Contractor staff (full- and part-time during the reportingperiod)Alonso Martinez, E. (from July 2001), Computer

operator. Alvarez, R., Analyst.Bailey, R. (from September 2001), WWW creation/

maintenance and proposal handling tools. Breitfellner, M., Enhancement/mission/planning/ToO

on-call.Brenchley, M., Software engineer.Buenadicha, G., Instrument on-board software main-

tenance.Calderon Riano, P, Inscon.Cheek, N., Operations analyst, Operations database.Chen, B., OM calibration scientist.Delgado Rioja, J., Software maintenance: SGS/QLA.Diaz Rodriguez, D. (from March 2002), Software

maintenance: PHS-RPS.

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Djavidnia, S., Operations analyst.Fauste, J., Operations engineer.Fuente, A. de la, Analyst.Garcia Beteta, J.J., Software maintenance: ODS/PMS.Garcia Mandillo, A., Computer operator.Gilolmo Lobo, M. (from November 2001), Inscon. Gonzalez Garcia, B., Inscon.Gonzales Riestra, R., RGS calibration/community

support.Hoar, J. (to August 2002), Software engineer. Juarez Blanca, B., Inscon.Loiseau, N. (from March 2001), Inscon. Lorente, R. (to September 2002), Inscon.Martin, T., Analyst.Martos, A., Inscon.Ojero, E., Analyst.Olabarri, B., Operations engineer.Perea Calderon, P., Computer operator.Perez Martinez, R. (from June 2001), Inscon.Rives, S., Operations engineer.Rodriguez Duran, F. (from July, 2001), Computer

operator. Rodriguez Pascual, P., Community support scientist.Salgado, J. (to August 2002), Instrument controller.Sanchez-Beato, R., Software maintenance: PMS/ODS.Smith, M., EPIC calibration.Soriano Borrull, R., Software maintenance: AMS.Talavera, A., OM calibration scientist.Tomas, L., Mission planning.Vallejo, J.C., Managing software support team.Verdugo, E. (to December 2002), OM calibration/

community support.

Science Archives Group (VILSPA)StaffArviset, C., System engineering, archive group leader.

StagiairesMeddour, R. (from August 2002 to January 2003).Rodriguez, E. (from April to August 2001).

Contractor staff (full- and part-time during the reportingperiod)Dowson, J., Archives: database expert.Hernandez, J., Archives: JAVA/GUI expert.Ortiz, I. (from October 2002), Archives: database expert.Osuna, P., Archives: data distribution/virtual observatory.Salgado, J. (from August 2002), Archives: data distribu-

tion/virtual observatory.San Miguel, G. (from October 2002), Archives:

JAVA/GUI expert.Venet, A. (from November 2001), Archives: database

expert.

Science Payload and Advanced Concepts Office(formerly Science Payloads Technology Division)

Peacock, A., Head of Office, STJ Research Team Leader.Andersson, S., Electronics engineering for advanced

technologies for semiconductors sensors. Appourchaux, T., Solar Orbiter payload support, solar

research, COROT instrument Research Team Leader.Adriaens, M. (to June 2002), Mechnical engineer.Arends, H., Mechanical engineer and mechanical

laboratory coordinator.Bavdaz, M., Advanced technologies sensors and optics,

Sensors and Optics Research Team Leader, Head ofAdvanced Technology Section (p.i.).

Beaufort, T., Electronics engineer for COROT PDU.Biezen, J.F. van der, Electronics and laboratory

metrology support to advanced technologyprogramme.

Butler, B.A.C., Instrument development engineer.Dordrecht, A. van., Advanced Sensors electronics

engineer.Erd, C., Sensor research and development, ESA missions

support.Falkner, P., Electronics research and development, Head

of Planetary Exploration Section (p.i.).Gondoin, Ph., Darwin-Genie instrument manager, XMM

observational research.Heida, J., Instrument support engineer.Johlander, B., Head of Instrument Support Group,

instrument development engineer.Klinge, D., Instrument development engineer.Lumb, D., Advanced sensor research, XEUS an ISS

payload and mission support, XMM observationalresearch.

Martin, D., SCAM3 instrument manager, Head ofInfrastructure Section (p.i.).

Rando, N., Payload support and development engineer,Head of Missions Section (p.i.).

Romstedt, J., In-situ planetary instrument development,Rosetta-MIDAS (AFM) Lead Scientist.

Smit, L.C., Instrument development support engineer.Sunter, W., Mechanical design engineer (seconded from

D/TOS).Telljohann, U., Instrument electronics engineer.Verveer, J., Laboratory cryogenic systems support.

Research FellowsMolster, F., Rosetta-MIDAS AFM.

StagiairesBonal, L., Scientific Evaluation of MIDAS (April-July

2002).

TraineesMoreira, O. (Portuguese Trainee from April 2002),

Helioseismology.Pitcher, K. (June to August 2001), International law.

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Contractor staff (full- or part-time during the reportingperiod)Beijersbergen, M. (to December 2001), X-ray optics.Brammertz, G., Laboratory Cryogenic and solid-state

test support.Den Hartog, R., Cryogenic Optics and solid-state test

support.Duvet, L. (from July 2002), COROT and STEREO flight

instrument technical support.Hijmering, R. (from November 2002), Croygenic camera

sensor test data analysis.Jeanes, A., Payload databases and payload cost analysis

support.Kraft, S., Payload minaturisation technical support.Owens, A., Solid-state support and optics technical

support.Page, J. (to April 2002), Cryogenic engineering support.Reynolds, A., Laboratory data processing and test

analysis.Sirbi, G. (from October 2002), Laboratory cryogenic

technical support.Smit, H. (from January 2002), STEREO flight

instrument technical support.Verhoeve, P., Laboratory cryogenic and solid-state test

support.

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ANNEX 2Publications

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122 publications

ANNEX 2: PUBLICATIONS

Solar & Solar-Terrestrial Missions Divisionand Planetary Missions Division

Refereed Journals, 2001

Banerjee, D., E. O’Shea, J.G. Doyle and M. Goossens,The Nature of Network Oscillations, Astron.Astrophys., 371, 1137-1149, 2001.

Banerjee, D., E. O’Shea, J.G. Doyle and M. Goossens,Long Period Oscillations in the Inter-Plume Regionsof the Sun, Astron. Astrophys., 377, 691-700, 2001.

Banerjee, D., E. O’Shea, J.G. Doyle and M. Goossens,Signatures of Very Long Period Waves in the PolarCoronal Holes, Astron. Astrophys., 380, L39-L42,2001.

Bosqued, J.M., T.D. Phan, I. Dandouras, C.P. Escoubet,H. Reme et al., Cluster Observations of the High-Latitude Magnetopause and Cusp: Initial Results fromthe CIS Ion Instruments, Ann. Geophys., 19, 1545-1566, 2001.

Chaplin, W. J., T. Appourchaux, Y. Elsworth, G. R. Isaak,and R. New, The Phenomenology of Solar Cycle-Induced Acoustic Eigenfrequency Variations: AComparative and Complementary analysis of GONG,BISON and IRGO/:LOI data, MNRAS, 324, 910,2001.

Charbonneau, P., S.W. McIntosh, H.-L. Liu and T.J.Bogdan, Avalanche Models for Solar Flares (InvitedReview), Sol. Phys., 203 (2), 321-353, 2001.

Curdt, W., P. Brekke, U. Feldman, K. Wilhelm, B.N.Dwivedi, U. Schühle and P. Lemaire, The SUMERSpectral Atlas of Solar-Disk Features, A & A, 375,591-613, 2001.

Drolshagen, G., H. Svedhem, E. Gruen, K.D. Bunte,Measurements of Cosmic Dust and Micro-Debris inGeostationary Orbit, Adv. Space Res. 28(9), 1325-1333, 2001.

Escoubet, C.P., M. Fehringer and M. Goldstein, Intro-duction: The Cluster Mission, Ann. Geophys., 19,1197-1200, 2001.

Fierry-Fraillon, D. and T. Appourchaux, The Effects of aGap-Filling Method on P-Mode Parameters, MNRAS,324, 1159, 2001.

Gloeckler, G. and K.-P. Wenzel, Acceleration Processesof Heliospheric Particle Populations, In Century ofSpace Science, J.A.M. Bleeker, J. Geiss, M.C.E.Huber (eds), Kluwer Academic Publ., 963-1005,2001.

Grard, R. and A. Balogh, Returns to Mercury: Scienceand Mission Objectives, Planet. & Space Sci., 49(14-15), 1395-1407, 2001.

Gustafsson, G., M. André, T. Carozzi, A.I. Eriksson,C.-G. Fälthammar, R. Grard, G. Holmgren, J.A.Holtet, N. Ivchenko, T. Karlsson, Y. Khotyaintsev,S. Klimov, H. Laakso, P.-A. Lindqvist, B. Lybekk,G. Marklund, F. Mozer, K. Mursula, A. Pedersen,B. Popielawska, S. Savin, K. Stasiewicz, P. Tanskanen

and J.-E. Wahlund, First Results of Electric Field andDensity Observations by Cluster EFW Based onInitial Months of Operation, Densitites, Ann.Geophys., 19, 1219-1240, 2001.

Heber, B. and R.G. Marsden, Cosmic Ray ModulationOver the Poles at Solar Maximum: Observations,Space Sci. Rev., 97(1-4), 309-319, 2001.

Heber, B., E. Keppler, R.G. Marsden, C. Tranquille,B. Blake and M. Fraenz, The Evolution of theAnomalous Cosmic Ray Oxygen Spectra from 1995to 1998: Ulysses Observations, Space Sci. Rev., 97(1-4), 363-366, 2001.

Houdek, G., W.J. Chaplin, T. Appourchaux, J. Christ-ensen-Dalsgaard, J.W. Däppen, Y. Elsworth, D.O.Gough, G. Isaak, R. New and M.C. Rabello-Soares,Changes in Convective Properties over the SolarCycle: Effect on p-Mode Damping Rate, MNRAS,327, 483, 2001.

Janhunen, P., A. Olsson, W.K. Peterson, H. Laakso, J.S.Pickett, T.I. Pulkkinen and C.T. Russell, A Study ofInverted-V Auroral Acceleration Mechanisms UsingPolar/Fast Auroral Snapshot Conjunctions, J. Geo-phys. Res., 106, 18995-19012, 2001.

Keller, H.U., H. Hartwig, R. Kramm, D. Koschny, W.J.Markiewicz, N. Thomas, M. Fernandez, P.H. Smith,R.M.T. Reynolds, J. Weinberg, R. Marcialis,R. Tanner, B. J. Boss and C. Oquest, The MVACSRobotic Arm Camera, J. Geophys. Res., 106, 17609-17622, 2001.

Kolesnikova, E., C. Beghin, R. Grard and C.P. Escoubet,The Electrical Stability of the Electric Field Antennasin the Plasmasphere, J. of Atm. Sol. Terr. Phys., 63(11),1217-1224, 2001.

Kolokova, L., L.M. Lara, R. Schulz, J.A. Stuewe andG.P. Tozzi, Properties and Evolution of Dust in CometTabur (C/1996Q1) from the Color Maps, Icarus, 153,197-207, 2001.

Koschny, D. and E. Gruen, Impacts into Ice-SilicateMixtures: Crater Morphologies, Volumes, Depth-to-Diameter Ratios, and Yield, Icarus, 154, 391-401,2001.

Koschny, D., G. Kargl and M. Rott, ExperimentalStudies of the Cratering Process in Porous Ice Targets,Adv. Space Res., 28(10), 1533-1537, 2001.

Koschny, D.V. and E. Gruen, Impacts into Ice-SilicateMixtures: Ejecta Mass and Size Distributions, Icarus,154, 402-411, 2001.

Krueger, H., E. Gruen, A. Graps, D. Bindschadler,S. Dermott, H. Fechtig, B.A. Gustafsson, D.P.Hamilton, M.S. Hanner, M. Hoanyi, J. Kissel, B.A.Lindblad, D. linkert, G. Linkert, I. Mann, J.A.M.McDonnell, G.E. Morfill, C. Polanskey, G. Schwehm,R. Srama and H.A. Zook, One Year of Galileo DustData From the Jovian System: 1996, Planet. SpaceSci., 49, 1285-1301, 2001.

Krueger, H., E. Gruen, M. Landgraf, M. Baguhl,S. Dermott, H. Fechtig, B.A. Gustafson, D.P.Hamilton, M.S. Hanner, M. Horanyi, J. Kissel, B.A.Lindblad, D. Linkert, I. Mann, J.A.M. McDonnell,

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publications 123

G.E. Morfill, C. Polanskey, G. Schwehm, R. Sramaand H.A. Zook, Four Years of Ulysses Dust Data:1996-1999, Planet. Space Sci., 49, 1303-1324, 2001.

Laakso, H. and M. Jarva, Evolution of the PlasmapausePosition, J. of Atm. Sol. Terr. Phys., 63, 1171-1178,2001.

Lara, L.M., R. Schulz, J.A. Stuwe, and G.P. Tozzi,Activity of Comet Tabur (C/1996 Q1) During Sept.12-17, 1996, Icarus, 150, 124-139, 2001.

Mann, I. and H. Kimura, Dust Properties in the LocalInterstellar Medium, Space Sci. Rev., 97, 389-392,2001.

Marsden, R.G., The Heliosphere after Ulysses,Astrophys. & Space Sci., 277, 337-347, 2001.

Marsden, R.G., Highlight Results from Ulysses: InRecent Insights into the Physics of the Sun andHeliosphere : Highlights from SOHO and Other SpaceMissions, IAU Symposium 203, P. Brekke, B. Fleck,and J.B. Gurman (Eds), 525-532, 2001.

Masson, A., B.B. Shishkov and F. Lefeuvre, Use ofHigher-Order Statistical Tests in the Analysis of TimeSeries Associated with Space Data, Signal Processing,18, 59-78, 2001.

McIntosh, S. and P. Charbonneau, Geometrical Effects inAvalanche Models of Solar Flares: Implications forCoronal Heating, Astrophys. J. Lett., 563, L165-L168,2001.

McIntosh, S.W. and P.G. Judge, On the Nature ofMagnetic Shadows in the Solar Chromosphere,Astrophys. J., 561, 420-426, 2001.

Moullard, O., D. Burgess, C. Salem, A. Mangeney, D.E.Larson and S.D. Bale, Whistler Waves, LangmuirWaves and Single Loss Cone Electron DistributionsInside a Magnetic Cloud: Observations, J. Geophys.Res., 106(A5), 8301-8313, 2001.

Moullard, O., R.G. Marsden, T.R. Sanderson et al.,Energetic Ions Observed at Low to High Latitudes inthe Southern Heliosphere during Declining and RisingSolar Activity, Space Sci. Rev., 97(1-4), 289-292,2001.

Norman, J.P., P. Charbonneau, S.W. McIntosh, andH. Liu, Waiting-Time Distributions in Lattice Modelsof Solar Flares, Astrophys. J., 557, 891-896, 2001.

Opgenoorth, H.J., M. Lockwood, D. Alcayde,E. Donovan, M. J. Engebretson, A. P. van Eyken,K. Kauristie, M. Lester, J. Moen, J. Warterman,H. Alleyne, M. André, M. W. Dunlop, N. Cornilleau-Werhlin, A. Masson, A. Fazerkerley, H. Reme, et al.,Coordinated Ground-Based, Low Altitude Satelliteand Cluster Observations on Global and Local ScalesDuring a Transient Postnoon Sector Excursion of theMagnetospheric Cusp, Ann. Geophys., 19, 1367-1398,2001.

O’Shea, E., D. Banerjee, J.G. Doyle, B. Fleck andF. Murtaugh, Active Region Oscillations, A&A, 368,1095-1107, 2001.

Palmroth, M., H. Laakso and T. Pulkkinen, Location ofHigh-Altitude Cusp During Steady Solar WindConditions, J. Geophys. Res., 110, 21109-21122, 2001.

Pedersen, A., P. Decreau, C.P. Escoubet, G. Gustafsson,H. Laakso, P.A. Lindqvist, B. Lybekk, F. Mozer andA. Vaivads, Four-Point High Time ResolutionInformation on Electron Densities by the ElectricityField Experiments (EFW) on Cluster, Ann. Geophys.,19, 1483-1489, 2001.

Reme, H., C. Aoustin, J.M. Bosqued, I. Dandouras,B. Lavraud, J.A. Savaud, A. Barthe, J. Bouyssou,T. Camus et al. (incl. C.P. Escoubet), FirstMultispacecraft Ion Measurements In and Near theEarth’s Magnetosphere with the Identical Cluster IonSpectrometry (CIS) Experiment, Ann. Geophys., 19,1303-1354, 2001.

Sanderson, T.R., R.G. Marsden, C. Tranquille,A. Balogh, R.J. Forsyth, B.E. Goldstein, J.T. Goslingand K.L. Harvey, The Influence of the Sun’s MagneticField and the Heliosphere on Energetic Particles atHigh Heliospheric Latitudes, Geophys. Res. Lett.,28(24), 4525-4528, 2001.

Torkar, K., W. Riedler, C.P. Escoubet, M. Fehringer et al.,Active Spacecraft Potential Control for Cluster –Implementation and First Results, Ann. Geophys., 19,1289-1302, 2001.

Trotignon, J.G., H.C. Seran, R. Grard, H. Laakso,N. Meyer-Vernet and R. Manning, In Situ Observa-tions of the Ionized Environment of Mars: the AIMExperiment Proposed as Part of the MARSIS RadarOnboard Mars Express, Planet. Space Sci., 49, 155-164, 2001.

Witasse, O., J.-F. Nouvel, J.-P. Lebreton and W. Kofman,HF Radio Wave Attenuation Due to a Meteoric Layerin the Atmosphere of Mars, Geophys. Res. Lett.,28(15), 3039-3042, 2001.


Proceedings and other Publications, 2001

Appourchaux, T., Results from the LuminosityOscillations Imager on board SOHO: Low-Degreep-Mode Parameters for a 4-Year Data Set, ESA SP-464, 71-74, 2001.

Appourchaux, T., B. Andersen, G. Berthomieu et al., g-Mode Detection: Where do we Stand? ESA SP-464,467-471, 2001.

Arends, H., J. Gavira, J. Romstedt, B. Butler, K. Torkar,G. Coe and M. Yorck, The MIDAS Experiment for theRosetta Mission, Proc. of 9th Eur. Space Mech. &Tribology Symp. (ESMATS), ESA SP-480, 67-74,2001.

Banerjee, D., E. O’Shea, J. G. Doyle, and M. Goossens,Long Period Ocillations in Polar Plumes as Observedby CDS on SOHO In Recent Insights into the Physicsof the Sun and Heliosphere: Highlights from SOHOand Other Space Missions, Proceeding of IAUSymposium 203, P. Brekke, B. Fleck and J. B.Gurman (Eds), 244-246, 2001.

Banerjee, D., E. O’Shea, J.G. Doyle, M.Goosens and

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124 publications

B. Fleck, On the Nature of Network Oscillations, ESASP-464, 175-178, 2001.

Brekke, P., Impact of SOHO, TRACE and Yohkoh onSolar Physics, 11th Cambridge Workshop on CoolStars, Stellar Systems and the Sun, Garcia Lopez, R.J.et al (eds), PASP 223, 311, 2001.

Brekke, P., The Sun’s Role in Climate Changes, Proc. ofthe Int. Conf. On Global Warming and the Next Ice Age,19-24 August, Halifax, Nova Scotia, in press, 2001.

Brekke, P., Space Weather, Europhys. News 32(6), 232,2001.

Brekke, P., B. Fleck, S.V.H. Haugan, SOHO in its primeYears, Nordic Space Activities 9(2), 2001.

Chicarro, A.F., The Mars Express Mission and the Searchfor Life on Mars, Astronomicheski Vestnik 35(6), 1-6,2001.

Chicarro, A.F., The New Views of the Moon LunarInitiative, Rev. del IAA, 5, 11-12, 2001.

Donnelly, J., A. Thompson, D. O’Sullivan, A.J. Keane,L. O’C. Drury and K.-P. Wenzel, The Abundances ofActinide Nuclei in the Cosmic Radiation as Clues toCosmic-Ray Origin, Proc. of 27th ICRC (Hamburg),1715-1716, 2001.

Drolshagen, G., H. Svedhem, E. Gruen, Measurementsof Cosmic Dust and Micro-Debris with the GORIDImpact Detector, ESA SP-473, 177-184, 2001.

Escoubet, C.P., M. Fehringer and P. Bond, Rumba, Salsa,Samba and Tango in the Magnetosphere – the ClusterQuartet’s First Year in Space, ESA Bulletin, 107, 43-53, 2001.

Fleck, B., Highlights from SOHO and Future SpaceMissions in The Dynamic Sun, Proc. 1999Kanzelhoehe Summer School and Workshop (EdsA. Hanslmeier et al.) Kluwer Academic Publ., 1-41,2001.

Fleck, B. and the Solar Orbiter Study Team, Solar Orbiter– A High Resolution Mission to the Sun and InnerHeliosphere, SPIE Proc. Series, 4498, 1-15, 2001.

Fleck, B., R.G. Marsden and O. Pace, Solar Orbiter, ESABulletin, 105, 56-57, 2001.

Graps, A.L., E. Gruen, H. Krueger, M. Horanyi andH. Svedhem, Io Revealed in the Jovian Dust Streams,Meteorids 2001, ESA SP-495, 601-608, 2001.

Grard, R.J.L. and H. Laakso, The Plasma EnvironmentAround Mercury, in Proc. of the 7th SpacecraftCharging Technology Conf. ESA SP-476, 617-622,2001.

Grün, E., M. Baguhl, H. Svedhem and H.A. Zook, In Situmeasurements of Cosmic Dust, in Interplanetary DustE. Gruen, Guftafson, Dermott and Fechtig (eds), 295-346, 2001.

Haugan, S.V.H., Anomalous Line Shifts on theSOHO/CDS NIS Detector, In Recent Insights into thePhysics of the Sun and Heliosphere, ASP Conf. Ser.200, 396-400, 2001.

Hofer, M.Y., R.G. Marsden, T.R. Sanderson andC. Tranquille, Cosmic Ray and Solar ParticleComposition Measurements in the Southern SolarPolar Region, Proc. of 27th ICRC, 8, 3116, 2001.

Hofer, M.Y., R.G. Marsden, T.R. Sanderson and C. Tran-quille, Energetic Particle Composition Measurementsat High Heliographic Latitudes Around the SolarActivity Maximum, In Solar and GalacticComposition (ed. R.F. Wimmer-Schweingruber) AIPConf. 598, 189-193, 2001.

Huber, M.C.E., Roger Bonnet, The Scientist, ESASP-493, 81-94, 2001.

Kimura, H., I. Mann and E.K. Jessberger, Properties ofLocal Interstellar Dust derived from RemoteAstronomical Observations, Laboratory Analyses, andin Situ Measurements, Proc. Meteorids 2001 Conf.,Kiruna,, ESA SP-495, 633-642, 2001.

Klecker, B., V. Bothmer, A.C. Cummings, J.S. George,J.W. Keller, E. Salerno, u.J. Sofia, E.C. Stone, F.-K.Thielemann, M.E. Wiedenbeck, F. Buclin, E.R.Christian, E.O. Flückiger, M.Y. Hofer, F.C. Jones,D. Kirilova, H. Kunow, M. Laming, C. Tranquille andK.-P. Wenzel, Galactic Abundances: Report ofWorking Group 3, In Solar and Galactic CompositionR.F. Wimmer-Schweingruber (Ed), AIP Conf. Proc.598, 207-220, 2001.

Kuitunen, J., G. Drolshagen, J.A.M. McDonnell,H. Svedhem, M. Leese, H. Mannermaa, M. Kaipi-ainen and V. Sipinen, Debie – First In Situ DebrisMonitoring Instrument, Proc. 3rd European Conf. OnSpace Debris, Darmstadt, ESA SP-473, 185-190,2001.

Laakso, H. and B.H. Foing, Characteristics of the PlasmaEnvironment for the SMART-1 Mission, in Proc. ofthe 7th Spacecraft Charging Technology Conf.,ESTEC, ESA SP-476, 601-608, 2001.

Laakso, H., R. Grard, A. Masson, O. Moullard, S. Bale,F. Mozer, A. Pedersen, M. André, A. Eriksson,G. Gustaffson and P.-A. Lindqvist, Multi-PointElectric Field Observations in the High-LatitudeMagnetosphere, Proc. Sheffield Space PhysicsConference: Multipoint Measurements Versus Theory,ESA SP-492, 27-34, 2001.

Lanzerotti, L.J. and T.R. Sanderson, Energetic Particlesin the Heliosphere. In The Heliosphere Near SolarMinimum, Balogh. A. et al. (Eds), 259-286, 2001.

Lebreton, J.-P. and D.L. Matson, Cassini/HuygensMission, Encyclopeida of Astronomy and Astro-physics, Nature Publishing Group, Basingstoke, UK,37469, 2001.

Mann, I., Charging Effects on Cosmic Dust, ESA SP-476, 629-634, 2001.

Mann, I., H. Kimura, E. Jessberger, M. Fehringer andH. Svedhem, Dust in the Inner Solar System, Proc. FirstSolar Orbiter Workshop, ESA SP-493, 445-446, 2001.

Marsch, E., R. Harrison, O. Pace, E. Antonucci,P. Bochsler, J.-L. Bougeret, B. Fleck, Y. Langevin,R. Marsden, R. Schwenn and J.-C. Vial, SolarEncounter, a High Resolution Mission to the Sun andInner Heliosphere, ESA SP-493, XI-XXVI, 2001.

Marsden, R.G., The 3-D Heliosphere at Solar Maximum– Conference Highlights 34th ESLAB Symp., PASP113, 129-130, 2001.

sp1247s4.qxd 3/5/03 3:58 PM Page 124

publications 125

Marsden, R.G. and P. Bochsler, Particle and FieldInstruments – Report of Payload Splinter Group I,ESA SP-493, 143-144, 2001.

Marsden, R.G., T.R. Sanderson, C. Tranquille andM. Hofer, The Ulysses Fast Latitude Scan at SolarMaximum: COSPIN/LET Energetic Particle Observa-tions, Proc. of 27th Int. ICRC, 8, 3310-3313, 2001.

McKibben, R.B., J.J. Connell, C. Lopate, M. Zhang,A. Balogh, S. Dalla, R.G. Marsden, T.R. Sanderson,C. Tranquille, J.D. Anglin, H. Kunow, R. Mueller-Mellin, B. Heber, A. Raviart and C. Paizis, UlyssesCOSPIN Observations of the Energy and ChargeDependence of the Propagation of Solar EnergeticParticles to the Sun’s South Polar Regions, Proc. 27thICRC, 8, 3281, 2001.

O’Shea, E., D. Banerjee, J.G. Doyle, B. Fleck andF. Murtagh, Active Region Oscillations, 10th Proc.SOHO/GONG 2000 Workshop: Helio- andAsteroseismology at the Dawn of the Millenium, ESASP-464, 223-226, 2001.

Palumbo, P., L. Colangeli, V. della Corte, F. Esposito,L. Ferrini, S.F. Green, E. Gruen, S. Kempf, H. Kruger,N. McBride, J.A.M. McDonnell, G. Schwehm,R. Srama, H. Svedhem and J.C. Zarnecki, ScientificObjectives and Technologies for the Solar OrbiterDust Detector, Proc. First Solar Orbiter Workshop,ESA SP-493, 315-319, 2001.

Romstedt, J. and A. Jaeckel, Micro-Magnetic Propertiesof Selected Mineral Grains in Primitive Meteorites,Lunar and Planetary Sciences XXXII (CD ROM),1687, 2001.

Romstedt, J. and M. Novara, Master, ESA Bulletin, 105,52-53, 2001.

Sanderson, T.R. and O. Pace, Storms, ESA Bulletin, 105,58-59, 2001.

Sasaki, S., E. Igenbergs, H. Ohashi, G. Hofchuster,R. Muenzenmayer, W. Naumann, R. Senger, F. Fisher,A. Fujiwara, E. Grün, Y. Hamabe, T. Kawamura,I. Mann, H. Miyamoto, K. Nogami and H. Svedhem,Interplanetary Dust Observation in the Earth-Mars byMars Dust Counter (MDC) on Board NOZOMI:Three Year Results, Meteorids 2001, ESA SP-495,595-599, 2001.

Torkar, K., W. Riedler, M. Fehringer, K.R. Svenes andB. Narheim, Effects of Active Spacecraft PotentialControl on Cluster Plasma Measurements – FirstResults, Proc. 7th Spacecraft Charging TechnologyConf., ESA SP-476, 255-260, 2001.

Tranquille, C., R.G. Marsden and T.R. Sanderson, GalacticAbundances: Report of Working Group 3, In Solar andGalactic Composition R.F. Wimmer-Schweingruber,(ed.), AIP Conf. Proc. 598, 195-200, 2001.

von der Lühe, O. and B. Fleck, Visible Imager/Magnetograph: Summary of Splinter Session, ESASP-493, 149-150, 2001.

von Steiger, R., J.-C. Vial, P. Bochsler, M. Chaussidon,C.M.S. Cohen, B. Fleck, V.S. Heber, H Holweger,K. Issautier, A.J. Lazarus, K.W. Ogilvie, J.A.Paquette, D.B. Reisenfeld, L. Teriaca, K. Wilhelm,

S. Yusainee, J.M. Laming and R.C. Wiens, MeasuringSolar Abundances, In Solar and Galactic CompositionR.F. Wimmer-Schweingruber (Ed), AIP Conf. Proc.598, 13-22, 2001.



Bell, J.F. III, N.I. Izenberg, P.G. Lucey, B.E. Clark,C. Peterson, M.J. Gaffey, J. Joseph, B. Carcich,A. Harch, M.E. Bell, J. Warren, P.D. Martin,L.A. McFadden, D. Wellnitz, S. Murchie, M. Winter,J. Veverka, P. Thomas, M.S. Robinson, M. Malin andA. Cheng, Near-IR Reflectance Spectroscopy of 433Eros From the NIS Instrument on the NEAR Mission.1. Low Phase Angle Observations, Icarus, 155, 119-144, 2002.

Boehnhardt, H., C. Delahodde, T. Sekiguchi, O. Hainaut,J. Spyromilio, M. Tarenghi, R.M. West, R. Amestica,R. Schulz and G. Schwehm, VLT Kueyen Observa-tions of Rosetta Target Comet 46P/Wirtanen nearAphelion, Astron. Astrophys., 387, 1107-1113, 2002.

Bowey, J.E., M.J. Barlow, F.J. Molster, A.M. Hofmeister,C. Lee, C. Tucker, T. Lim, P.A.R. Ade and L.B.F.M.Waters, The 69-micron Forserite Band as a DustTemperature Indicator, MNRAS, 331, L1-L6, 2002.

Chaplin, W.J., T. Appourchaux, Y. Elsworth, G.R. Isaakand R. New, Variation of Acoustic Mode CentroidFrequencies over the Solar Cycle, Adv. Space Res.,29(12), 1881-1888, 2002.

Chaplin, W.J., Y. Elsworth, G.R. Isaak, K.I. Marchenkov,B.A. Miller, R. New, B. Pinter and T. Appourchaux,Peak Finding at Low Signal-to-Noise Ratio: Low-1Solar Acoustic Eignemodes at n < 9 from the Analysisof BISON Data, MNRAS, 336, 979, 2002.

Fredvik, T., O. Kjeldseth-Moe, S.V. Haugan, P. Brekke,J.B. Gurman, and K. Wilhelm,, Variability andDynamic State of Active Region Loops, Adv. SpaceRes., 30(3), 635-340, 2002.

Gabriel, A.H., F. Baudin, P. Boumier, R.A. Garcia, S.Turck-Chieze, T. Appourchaux, L. Bertello, G. Berth-omieu, J. Charra, D.O. Gough, P.I. Palle, J. Provost, C.Renaud, J.-M. Robillot, T. Roca-Cortes, S. Thiery andR.K. Ulrich, A Search for Solar g Modes in the GOLFData, Astron. Astrophys., 390, 1119, 2002.

Hofer, M.Y. and M. Storini, Peculiar Features in theCoronal Hole Occurrence, Sol. Phys., 207, 1-10, 2002.

Hofer, M.Y., R.G. Marsden, T.R. Sanderson andC. Tranquille, Composition Measurements Above theSouthern Solar Polar Region Around the SolarActivity Maximum by the Ulysses COSPIN/LETInstrument, Geophys. Res. Lett., 29(16), 10.1029/2002GL14944, 2002.

Hoogzaad, S.N., F.J. Molster, C. Dominik, L.B.F.M.Waters, M.J. Barlow and A. de Koter, The Circum-stellar Dust Shell of the Post-AGB Star HD 161796*,Astron. Astrophys., 389, 547-555, 2002.

sp1247s4.qxd 3/5/03 3:59 PM Page 125

126 publications

Keller, L.P., S. Hony, J.P. Bradley, F.J. Molster, L.B.F.M.Waters, J. Bouwman, A. de Koter, D.E. Brownlee,G.J. Flynn, T. Henning and H. Mutschke, Idenficationof Iron Sulphide Grains in Protoplanetary Disks,Nature, 417 (6884), 148-150, 2002.

Janhunen, P., A. Olsson and H. Laakso, AltitudeDependence of Plasma Density in the Auroral Zone,Ann. Geophys., 20, 1743-1750, 2002.

Kemper, F., C. Jäger, L.B.F.M. Waters, T. Henning, F.J.Molster, M.J. Barlow, T. Lim and A. de Koter,Detection of Carbonates in Dust Shells aroundEvolved Stars, Nature, 415, 295-297, 2002.

Kemper, F., F.J. Molster, Jäger and L.B.M. Waters, TheMineral Composition and Spatial Distribution of theDust Ejeta of NGC 6302, Astron. Astrophys., 394,679-690, 2002.

Kimura, H., I. Mann, D. A. Biesecker and E.K. Jess-berger, Dust Grains in the Comae and Tails of Sun-grazing Comets: Modeling of Their Mineralogical andMorphological Properties, Icarus, 159, 529-541,2002.

Laakso, H., Variation of the Spacecraft potential in theMagnetosphere, J. Atmos. Solar. Terr. Phys., 64, 1735-1744, 2002.

Laakso, H., R. Grard, P. Janhunen and J.-G. Trotignon,Plasma and Wave Phenomena Induced by Neutral GasReleases in the Solar Wind, Ann. Geophysicae, 20, 1-11, 2002.

Lavraud, B., M.W. Dunlop, T.D. Phan, H. Rème, J.-M.Bosqued, I. Dandouras, J.-A. Sauvaud, R. Lundin,M.G.G.T. Taylor, P.J. Cargill, C. Mazelle, C.P.Escoubet, C.W. Carlson, J.P. McFadden, G.K. Parks,E. Moebius, L.M. Kistler, M.-B. Bassavano-Cattaneo,A. Korth, B. Klecker, A. Balogh, Cluster Observationsof the Exterior Cusp and Its Surrounding Boundariesunder Northward IMF, Geophys. Res. Lett., 29(20),1995, 2002.

Liu, H., P. Charbonneau, A. Pouquet, T. J. Bogdan andS.W. McIntosh, Continuum Analysis of an AvalancheModel for Solar Flares, Phys. Review E, 66, 056111,2002.

Marsch, E., E. Antonucci, P. Bochsler, J.-L. Bougeret,B. Fleck, R. Harrison, Y. Langevin, R. Marsden,O. Pace, R. Schwenn and J.-C. Vial, The Solar Orbiter– A High Resolution Mission to the Sun and InnerHeliosphere, Adv. Space Res., 29(12), 2027-2040,2002.

Marsden, R.G., The Rising Phase of Solar Cycle 23 asseen by Ulysses, Adv. Space Res., 29(3), 401-409,2002.

McIntosh, S., P. Charbonneau, H. Liu and T.J. Bogdan,Geometrical Properties of Avalanches in Self-Organized Critical Models of Solar Flares, Phys.Rev. E, 65, 46125, 2002.

Moullard, O., A. Masson, H. Laakso, M. Parrot,P. Décréau, O. Santolik and M. André, DensityModulated Whistler Mode Emissions Observed Nearthe Plasmapause, Geophys. Res. Lett., 29(20), 1975,2002.

Müller, M., S.F. Green, N. McBride, D. Koschny, J.C.Zarnecki and M.S. Bentley, Estimation of the Dust FluxNear Mercury, Planet Space Sci., 50, 1001-1115, 2002.

O’Shea, E., K. Muglach and B. Fleck, OscillationsAbove Sunspots: Evidence for Propagating Waves?,Astron. Astrophys., 387, 642-664, 2002.

Romstedt, J., A. Jaeckel, W. Kloeck, K. Nakamura,H. Arends, K. Torkar, W. Riedler, In situ Imaging ofMicron and Sub-Micron Sized Grains in a CometaryEnvironment by Atomic Force Microscopy, Planet.Space Sci. 50(3), 347-350, 2002.

Sasaki, S., E. Igenbergs, H. Ohashi, R. Muenzenmayer,W. Naumann, G. Hofschuster, M. Born, G. Färber,A. Fujiward, A. Glasmachers, E. Grün, Y. Hamabe,H. Igleseder, T. Kawamura, H. Miyamoto, K. Morish-ige, T. Mukai, T. Naoi, K. Nogami, G. Schwehm andH. Svedhem, Observation of Interplanetary andInterstellar Dust Particles by Mars Dust Counter(MDC) on Board Nozomi, Adv. Space Res., 29(8),1145-1153, 2002.

Schulz, R. Trans-Neptunian Objects, Astron. &Astrophys. Rev., 11, 1-31, 2002.

Schulz, R. and J. A. Stuewe, The Dust Coma of CometC/1999 S4 (LINEAR), Earth, Moon and Planets, 90,195-203, 2002.

Schulz, R., Comets: Relics of the Early Solar System,Journal de Physique IV, 12(10), 293-305, 2002.

Settele, A., M. Sigwarth and K. Muglach, Temporal andSpatiall Variations of the Magnetic Field Vector inSunspots, Astron. Astrophys., 392, 1095-1104, 2002

Tajmar, M., J. Gonzales, G. Saccoccia, G. Noci andH. Laakso, Plasma Diagnostics and Simulation for theSMART-1 Mission, Planet. Space Sci., 50, 1355-1360, 2002.

Wilber, M., G.K. Parks, C.W. Carlson, S. Bale, J.M.Fadden, F. Mozer et al. (incl. C.P. Escoubet), Multi-Spacecraft Observations of Magnetospheric ParticleBoundaries by Cluster, J. Geophys. Res., submitted,2002.



Appourchaux, T., B. Andersen and T. Sekii, What HaveWe Learnt With the Luminosity Oscillations ImagerOver the Past 6 Years? , ESA SP-508, 47-50, 2002.

Banerjee, D., E. O’Shea, J.G. Doyle and M. Goossens,Long Period Oscillations in Polar Coronal Holes asobserved by CDS on SOHO, In Multi-WavelengthObservations of Coronal Structure and Dynamics,Yokkoh 10th Anniversary Meeting, Martens., P.C.H.and D. Cauffman (Eds), COSPAR Colloqu. Series, 13,19-22, 2002.

Berner, C., L. Bourillet, J. van Casteren, J. Ellwood,M. Kasper, P. Kletzine, R. Schulz and G. Schwehm,Rosetta: ESA’s Comet Chaser, ESA Bulletin, 112, 10-37, 2002.

sp1247s4.qxd 3/5/03 3:59 PM Page 126

publications 127

Bogdan, T.J., C.S. Rosenthal, M. Carlsson, V.H. Han-steen, A. McMurry, E.J. Zita, M. Johnson, S.J. Petty-Powell, S.W. McIntosh, A. Nordlund, R.F. Stein andS.B.F. Dorch, Waves in Magnetic Field Concen-trations: The Critical Role of Mode Mixing and Inter-ference, Astronomische Nachrichten, 323, 196, 2002.

Brekke, P., Space Weather Effects and How SOHO hasImproved the Warnings, In Solar-Terrestrial MagneticActivity and Space Environment, H.N. Wang and R.L.Xu (eds), COSPAR Colloquia Ser. 14, 385-392, 2002.

Brekke, P., Solar Eruptions – the Effects on the EarthEnvironment, In IAU Highlights of Astronomy, Publ.ASP, Hans Rickmann (ed.), 12, 384-388, 2002.

Brekke, P., Solens innnvrikning på Jordens Klima,kunnskapsforlagets Leksikon, 243, 2002.

Brekke, P. and B. Fleck, From Solar Min to Solar Max:Half a Solar Cycle of SOHO Observations, Proc. of27th ICRC (Hamburg), Invited, Rapporteur andHighlight Papers (CDROM), 21-40, 2002.

Chicarro, A., Missions to Mars, ESA SP-514, 21-24,2002.

Eberhard, G., H. Krüger, R. Srama, S. Kempf, S. Auer,L. Colangeli, M. Horanyi, P. Withnell, J. Kissel,M. Landgraf and H. Svedhem, Dust Telescope: A NewTool for Dust Research, In Dust in the Solar Systemand Other Planetary Systems, Proc. of IAU Colloq.181, Canterbury, UK, 2000, Eds Greens, Williams,McDonnell and McBride, 15, 181-194, 2002.

Farquhar, R., J. Kawaguchi, C. Russell, G. Schwehm,J. Veverka and D. Yeomans, Spacecraft Exploration ofAsteroids: The 2001 Perspective, In Asteroids IIIAsteroids 2001 Conf. (Bottke, W.F. et al. Eds), SpaceSci. Series, Arizona Press, USA, 2002.

Fleck, B., Prospects of Future Solar Space Missions, InMagnetic Coupling of the Solar Atmosphere, Proc.IAU Colloq. 188 (Ed. H. Sawaya), ESA SP-505, 311-318, 2002.

Fleck, B. and P. Brekke, SOHO Onthult de GeheimenVan de Zon, Ruimtevaart, 5, 14 August 2002, 2002.

Fleck, B. and R. G. Marsden, Solar Orbiter: A MissionOverview and Status Update. In Solar Variability:From Core to Outer Frontiers, Proc. 10th ESPmeeting, ESA SP-506, 919-922, 2002.

Grard, R., H. Laakso and H. Svedhem, Missions toMercury, ESA SP-514, 25-30, 2002.

Gruen, E., H. Krüger, R. Srama, S. Kempf, S. Auer,L. Colangeli, M. Horanyi, P. Withnell, J. Kissel,M. Landgraf and H. Svedhem, Dust Telescope: A NewTool for Dust Research, In Dust in the Solar Systemand Other Planetary Systems, Proc. of IAU Colloq.181, Canterbury, UK, 2000, Eds Greens, Williams,McDonnell and McBride, 15, 181-194, 2002.

Hochedez, J. F., J. Alvarez, F. D. Auret, P. Bergonzo, M.-C. Castex, A. Deneuville, J. M. Defise, Fleck, B. et al.,Recent Progress of the Bold Investigation towards UVdetectors for the ESA Solar Orbiter, Diamond & Re.Mat., 11(3-6), 427-432, 2002.

Kazeminejad, B., J.-P. Lebreton, M.K. Bird andD.H. Atkinson, Titan Wind Effects on the Descent

Trajectory of the ESA Huygens Probe, ESA SP-514,191-200, 2002.

Koschny, D., A. Marini, R. Hoofs and M. Almeida,Science Operations of ESA Planetary Missions, ESASP-514, 89-94, 2002.

Koschny, D.V. and J. Diaz del Rio, Meteor Orbit andTrajectory Software (MOTS) – Determining thePosition of a Meteor with Respect to the Earth UsingData Collected with the Software MetRec, WGN, TheJournal of the IMO, 4, 87-1001, 2002.

Koschny, D.V., P. Ferri, E. Montagnon, R. Hoofs andP. Van der Plas, Science Operations Planning andImplementation for Rosetta, Acta Astron., 51(1-9),601-608, 2002.

Koschny, D.V., P. Reissaus, P. Knöfel, R. Trautner andJ. Zender, Modeling the Fragmentation of MeteroidsUsing Poisson Statistics and Application to theLeonids 2001, ESA SP-500, 157-160, 2002.

Koschny, D.V., P. Reissaus, P. Knöfel, R. Trautner and O.Witasse, The ESA Leonids 2001 Expedition toAustralia, ESA SP-500, 185-188, 2002.

Laakso, H., Earth’s Ionosphere and Magnetosphere, ESASP-514, 41-50, 2002.

Laakso, H. and R. Grard, The Electron Density Distribu-tion in the Polar Cap: Its Variability with Season, andits Response to Magnetic Activity, In: Space WeatherStudy Using Multi-Point Techniques, COSPARColloquia Series, 12, 193-202, 2002.

Marsden, R.G. and B. Fleck, Space Weather Aspects ofthe ESA Solar Orbiter Mission, In Solar-TerrestrialMagnetic Activity and Space Environment, H.N. Wangand R.L. Xu (eds), COSPAR Colloquia Ser. 14, 443-445, 2002.

Marsden, R.G. and B. Fleck, Space Weather Aspects ofthe ESA Solar Orbiter Mission, In Solar Cycle andSpace Weather, Proc. SOLSPA Euroconf., ESA SP-477, 359-361, 2002.

Martin, P.D., T.B. McCord, P.C. Pinet, M.S. Robinson andG. Schwehm, Surface Mineralogy of Earth-LikePlanets, Moons, and Small Bodies, ESA-SP 514, 73-80,2002.

Masson, A. and H. J. Opgenoorth, Eveningside DiscreteArcs in Electrodynamics of Auroral Forms, AuroralPlasma Physics Book, ISSI, Kluwer, 259-270, 2002.

McIntosh, S., Conduction in the Transition Region:Interpretation of Dems Using SOHO/SUMER Obser-vations. In From Solar Min to Max: Half a Solar Cyclewith SOHO, ESA SP-508, 271-274, 2002.

Parrot, M. et al., Martina Ionospheric Study with theCNES Orbiter PREMIER, ESA SP-514, 109-114,2002.

Romstedt, J., K. Torkar, W. Riedler, H. Arends,R. Kassing, F. Rüdenauer, L. Abelamn, W. Barth,B. Butler, J. Gavira, H. Jeszensky and M. Siekman,An Instrument for In-Situ High Resolution Imaging ofCometary Dust Particles, Lunar and PlanetaryConference Science XXXIII, #1515, Abstract (CD-ROM), 2002.

Sasaki, S., E. Igenbergs, H. Ohashi, R. Muenzenmayer,

sp1247s4.qxd 3/5/03 3:59 PM Page 127

128 publications

W. Naumann, R. Senger, F. Fisher, A. Fujiward,E. Grün, Y. Hamabe, H. Igleseder, T. Kawamura,I. Mann, H. Miyamoto, K. Nogami and H. Svedhem,Observation of Interplanetary and Interstellar DustParticles by Mars Dust Counter (MDC) on BoardNozomi: Three-Year Results, Lunar and PlanetaryScience Conference XXXIII, #1167, Abstract (CD-ROM), 2002.

Sasaki, S., E. Igenbergs, R. Münzenmayer, H. Ohashi,G. Hofschuster,W. Naumann, G. Färber, F. Fisher,A. Fujiwara, A. Glasmachers, E. Gruen, Y. Hamabe, H.Iglseder, H. Miyamoto, T. Mukai, K. Nogami,G. Schwehm, H. Svedhem, M. Born, T. Kawamura,D. Klinge, K. Morishige, T. Naoi, R. Peeks, H. Yanoand K. Yamakoshi, Mars Dust Counter (MDC) onBoard NOZOMI: Initial Results, In Dust in the SolarSystem and Other Planetary Systems, Proc. of IAUColloq. 181, Canterbury, UK, 2000, Eds Greens,Williams, McDonnell and McBride, 15, 176-180, 2002.

Sasaki, S., E. Igenbergs, H. Ohashi, R. Senger,G. Hopfsschuster, R. Muenzenmayer, W. Naumann,A. Fujiward, E. Grün, Y. Hamabe, T. Mukai, I. Mann,H. Miyamoto, K. Nogami, S. Shoji and H. Svedhem,Interplanetary and Interstellar Dust Observation byMars Dust Counter on Board NOZOMI: Four-YearOperation, ESA SP-500, 79-82, 2002.

Schulz, R., Review of Target Comets for Space Missions,Conf. Ser. of the Astron. Soc. of the Pacific (ASP), inpress, 2002.

Schulz, R., Dust and Gas in Cometary Comae, Habilit-ationsschrift, Georg-August-Universitaet Goettingen,2002.

Schulz, R., Comparative Study of Gas ComaMorphologies, ESA-SP 500, 553-556, 2002.

Svedhem, H., Cosmic Dune, ESA Bulletin, 109, 82-84,2002.

Tozzi, G.P., H. Boehnhardt, M. Delbo, H. Campins,M. Di Martino, L. Kolokolova, L. M. Lara Lopez,J. Licandro, R. Schulz and T. Sekiguchi, MultibandObservations of the Comet C/200 WM1 (LINEAR) atits Closest Approach to the Earth, ESA SP-500, 593-596, 2002.

Trautner, R. and R. Grard, Measuring the ElectricProperties of Planetary Environments with MutualImpedance (MI) Probes, ESA SP-514, 105-108, 2002.

Trautner, R. et al., Coordination of Mars Express andBeagle 2 Science Operations, ESA SP-514, 67-72,2002.

Trautner, R., D. Koschny, O. Witasse, J. Zender andJ. Knöfel, ULF-VLF Electric Field MeasurementsDuring the 2001 Leonid Storm, ESA SP-500, 161-164, 2002.

Vilar, E., M. Almeida, D. Koschny, B.H. Foing, LunarData Simulation for SMART-1, ESA SP-514, 101-104, 2002.

Wenzel, K.-P. and B. Fleck, Prospects in ESA for YoungResearchers in Solar Physics, In Solar Variability:From Core to Outer Frontiers, ESA SP-506, 1001-1003, 2002.

Zender, J., O. Witassse, D. Koschny, R. Trautner andJ. Knöfel, First Results of Spectroscopic Measure-ments during the ESA Leonids Campaign 2001, ESASP-500, 121-126, 2002.


Editorial Work, 2001

Balogh, A, R.G. Marsden and E.J. Smith (eds), TheHeliosphere Near Solar Minimum: The UlyssesPerspective, Springer-Praxis Publ., 411pp, 2001.

Brekke, P., B. Fleck and J.B. Gurman (eds), RecentInsights into the Physics of the Sun and Heliosphere –Highlights from SOHO and other Space Missions,IAU Symposium 203, Manchester, ISBN 1-58381-069-2, 612pp, 2001.

Escoubet, C.P, (ed.), Cluster First Results, Ann.Geophys., 19(10-12), 533pp, 2001.

Grard, R., A. Balogh (eds), Returns to Mercury, PlanetSpace Sci., 49(14-15), 297pp, 2001.

Marsch, E., V. Martinez Pillet, B. Fleck and R. Marsden(eds), Solar Encounter, Proc. First Solar OrbiterWorkshop, ESA SP-493, 476pp, 2001.

Marsden, R.G. (ed), The 3-D Heliosphere at SolarMaximum, Space Sci. Rev., 97(1-4), 431pp, 2001.

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Astrophysics Missions Division, Science Operations& Data Systems Division and Science Payload &Advanced Concepts Office (formerly SciencePayload & Technology Division)


Alard, C., Blommaert, J.A.D.L., Cesarsky, C., Epchtein, N.,Felli, M., Fouque, P., Ganesh, S., Genzel, R., Gilmore,G., Glass, I.S., Habing, H., Omont, A., Perault, M.,Price, S., Robin, A., Schultheis, M., Simon, G., VanLoon, J., Th., Alcock, C., Allsman, R.A., Alves, D.R.,Axelrod, T.S., Becker, A.C., Bennet, D.P., Cook, K.H.,Drake, A.J., Freeman, K.C., Geha, M., Griest, K.,Lehner, M.J., Marshall, S.L., Minniti, D., Nelson, C.,Peterson, B.A., Popowski, P., Pratt, M.R., Quinn, P.J.,Sutherland, W., Tomaney, A.B., Vandehei, T., Welch,D.L., 2001, Mass-losing Semiregular Variable Stars inBaade’s Windows, ApJ, 552, 289, 2001.

Arnaud, M., Aghanim, N., Gastaud, R., Neumann, D.,Lumb, D., Briel, U., Altieri, B., Ghizzardi, S.,Mittaz, J., Sasseen, T., Vestrand, T., 2001, XMM-Newton Observation of the Coma Galaxy Cluster:Temperature structure in the central region, A&A, 365,L67, 2001.

Bavdaz, M., Peacock, A., Owens, A., Future SpaceApplications of Compound Semiconductor X-rayDetectors, NIM-A, 458, 123, 2001.

Bocchino, F., Bykov, A.M., The plerion nebula in IC443:the XMM-Newton view, A&A, 367, 248, 2001.

Bocchino, F., Lumb, D., Marty, P., Becker, W., Pigot, C.,Warwick, R.S., The X-ray nebula of the filled centersupernova remnant 3C58 and its interaction with theenvironment, A&A, 369, 1078, 2001.

Bocchino, F., Parmar, A.N., Orlandini, M., Santangelo,A., Mereghetti, S., Angelini, L., X-ray emission in thedirection of the SNR G318.2+0.1, A&A, 367, 629,2001.

Bonamente, M., Lieu, R., Nevalainen, J., Kaastra, J.,ROSAT and BeppoSAX evidence of soft X-ray excessemission in the Shapley supercluster: A3571, A3558,A3560 and A3562, ApJ, 552, L7, 2001.

Bontemps, S., Andre, P., Kaas, A. A., Nordh, L.,Olofsson, G., Huldtgren, M., Abergel, A., Blommaert,J., Boulanger, F., Burgdorf, M., Cesarsky, C.J.,Cesarsky, D., Copet, E., Falgarone, E., Lagache, G.,Montmerle, T., Perault, M., Persi, P., Prusti, T., Puget,J.L., Sibille, F., ISOCAM observations of Ophiuchi:Initial luminosity and mass functions of the pre-mailsequence embedded cluster, A&A, 372, 173, 2001.

Brammertz, G., Poelaert, A., Golubov, A., Verhoeve, P.,Peacock, A., Rogalla, H., A generalized proximityeffect model in superconducting bi- and trilayer films,J. App. Phys., 90/1, 355, 2001.

Brammertz, G., Verhoeve, P., Peacock, A., Martin, D.,Rando, N., Hartog, R. den, Goldie, D.J., Developmentof Practical Soft X-ray Spectrometers, IEEE Trans.Applied Superconductivity, 11, 828, 2001.

Brandt, W.N., Guainazzi, M., Kaspi, S., Fan, X.,Schneider, D.P., Strauss, M.A., Clavel, J., Gunn, J.E.,

An XMM-Newton detection of the z=5.80 X-ray weakquasar SDSSp J104433.04-012502, AJ, 121, 591,2001.

Briel, U., Henry, J., Lumb, D., Arnaud, M., Neumann, D.,Aghanim, N., Gastaud, R., Mittaz, J., Sasseen, T.,Vestrand, T., Mosaic of the Coma Cluster of Galaxieswith XMM-Newton, A&A, 365, L60, 2001.

Campana, S., Parmar, A.N., Stella, L, 2001, A Beppo-SAX view of transient black hole candidates inquiescence, A&A, 372, 241, 2001.

Cernicharo, J., Heras, A.M., Pardo, J.R., Tielens,A.G.G.M., Guelin, M., Dartois, E., Neri, R., Waters,L.B.F.M., Methylpolyynes and Small Hydrocarbonsin CRL 618, ApJ, 546, L127, 2001.

Cernicharo, J., Heras, A.M., Tielens, A.G.G.M., Pardo,J.R., Herpin, F., Guelin, M., Waters, L.B.F.M., Infra-red Space Observatory’s Discovery of C4H2, C6H2,and Benzene in CRL618, ApJ, 546, L123, 2001.

Comastri, A., Stirpe, G.M., Vignali, C., Brandt, W.N.,Leighly, K.M., Fiore, F., Guainazzi, M., Matt, G.,Nicastro, F., Puchnarewicz, E.M., Siemiginowska, A.,BeppoSAX observations of Narrow-line Seyfert 1galaxies: II. ionized iron features in Arakelian 564,A&A, 365, 400, 2001.

Dadina, M., Bassani, L., Cappi, M., Palumbo, G.G.C.,Piro, L., Guainazzi, M., Di Cocco, G., Trifoglio, M.,Malaguti, G., On the origin of the FeK-alpha line inthe Seyfert 2 galaxy NGC7172, A&A, 370, 70, 2001.

Dahlem, M., Ehle, M., Ryder, S.D., The mysterious HIdeficiency of NGC 3175, A&A, 371, 45, 2001.

Dahlem, M., Ehle, M., Ryder, S.D., A search forintergalactic HI gas in the NGC 1808 group ofgalaxies, A&A, 373, 485, 2001.

Dahlem, M., Lazendic, J.S., Haynes, R.F., Ehle, M.,Lisenfeld, U., Warm dust as a tracer of galaxies withgaseous halos, A&A, 374, 42, 2001.

Deharveng, J.-M., Buat, V., Le Brun, V., Milliard, B.,Kunth, D., Shull, J. M., Gry, C., Constraints on theLyman continuum radiation from galaxies: Firstresults with FUSE on Mrk 54, A&A, 375, 805, 2001.

Dennerl, K., Haberl, F., Aschenbach, B., Briel, U.,Balasini, M., Brauninger, H., Burkert, W., Hartmann,R., Hartner, G., Hasinger, G., Kemmer, J., Kendziorra,E., Kirsch, M., Krause, N., Kuster, M., Lumb, D.,Massa, P., Meidinger, N., Pfefferman, E., Pietsch, W.,Reppin, C., Soltau, H., Staubert, R., Strüder, L.,Trümper, J., Turner, M., Villa, G., Zavlin, W., The firstbroad-band X-ray images and spectra of the 30-Doradus region in the LMC, A&A, 365, L202, 2001.

Favata, F., Micela, G., Reale, F., Coronal structuregeometries on pre-main sequence stars, A&A, 375,485, 2001.

Frontera, F., Palazzi, E., Zdziarski, A.A., Haardt, F.,Perola, G.C., Chiappetti, L., Cusumano, G., DalFiume, D., Del Sordo, S., Guainazzi, M., Matt, G.,Orlandini, M., Parmar, A.N., Piro, L., Santangelo, A.,Treves, A., Trifoglio, M., Broad band spectrum ofCygnus X-1 in two spectral states with BeppoSAX,ApJ, 546, 1027, 2001.

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Frontera, F., Zdziarski, A.A., Amati, L., Mikolajewska,J., Belloni, T., Del Sordo, S., Haardt, F., Kuulkers, E.,Masetti, N., Orlandini, M., Palazzi, E., Parmar, A.N.,Remillard, R., Santangelo, A., Stella, L., Ameasurement of the broad-band spectrum of XTEJ1118+480 with BeppoSAX and its astrophysicalimplications, ApJ, 561, 1006, 2001.

Giardino, G., Banday, A.J., Fosalba, P., Gorski, K.M.,Jonas, J.L., O’Mullane, W., Tauber, J., The angularpower spectrum of radio emission at 2.3 GHz, A&A,371, 708, 2001.

Gondoin, P., Barr, P., Lumb, D., Oosterbroek, T., Parmar,A., Simultaneous XMM-Newton and BeppoSAXobservation of the Seyfert I galaxy IC 4329 A, A&A,378, 806, 2001.

Gondoin, P., Lumb, D., Siddiqui, H, Guainazzi, M.,Schartel, N., XMM-Newton observation of theSeyfert I galaxy Fairall 9, A&A, 373, 805, 2001.

Gonzalez-Riestra, R., Cassatella, A., Wamsteker, W., TheINES System IV: The IUE Absolute Flux Scale, A&A,373, 730, 2001.

Gry, C., Jenkins, E.B., Local clouds: ionization,temperatures, electron densities and interfaces, fromGHRS and IMAPS spectra of E Canis Majoris, A&A,367, 617, 2001.

Guainazzi, M., Fiore, F., Matt, G., Perola, G.C., On thenature of X-ray absorption in Seyfert 2 galaxies,MNRAS, 326, 199, 2001.

Guainazzi, M., Marshall, W., Parmar, A.N., The recenthistory of the X-ray absorber in NGC3516, MNRAS,323, 75, 2001.

Habing, H.J., Dominik, C., Jourdain de Muizon, M.,Laureijs, R.J., Kessler, M. F., Leech, K., Metcalfe, L.,Salama, A., Siebenmorgen, R., Trams, N., Bouchet, P.,Incidence and survival of remnant disks around main-sequence stars, A&A, 365, 545, 2001.

Harnden, F.R. Jr., Adams, N.R., Damiani, F., Drake, J.J.,Evans, N.R., Favata, F., Flaccomio, E., Freeman, P.,Jeffries, R.D., Kashyap, V., Micela, G., Patten, B.M.,Pizzolato, N., Schachter, J.F., Sciortino, S., Stauffer,J., Wolk, S.J., Zombeck, M.V., Chandra observationsof the open cluster NGC 2516, ApJ, 547, L141, 2001.

Hasinger, G., Altieri, B., Arnaud, M., Barcons, X.,Bergeron, J., Brunner, H., Dadina, M., Dennerl, K.,Ferrando, P., Finoguenov, A., Griffiths, R.,Hashimoto, Y., Jansen, F., Lumb, D., Mason, K.,Mateos, S., MacMahon, R., Miyaji, T., Paerels, F,Page, M, Ptak, A., Sasseen, T., Schartel, N., Szokoly,G., Trümper, J., Turner, M., Warwick, R., Watson, M.,XMM Newton Observation of the Lockman Hole. IX-ray Data, A&A, 365, L45, 2001.

Hornschemeier, A.E., Brandt, W.N., Garmire, G.P.,Schneider, D.P., Barger, A.J., Broos, P.S., Cowie, L.L.,Townsley, L.K., Bautz, M.W., Burrows, D.N.,Chartas, G., Feigelson, E.D., Griffiths, R.E., Lumb,D., Nousek, J.A., Ramsey, L.W., Sargent, W.L.W., TheChandra Deep Survey of the Hubble Deep Field-North Area. II. Results from the Caltech Faint FieldGalaxy Redshift Survey Area, ApJ, 554, 742, 2001.

Israel, G.L, Oosterbroek, T., Stella, L., Campana, S.,Mereghetti, S., Parmar, A.N., The pulse phase-dependent spectrum of the anomalous X-ray pulsar1RXS j170849-400910, ApJ, 560, L69, 2001.

Iwasawa, K., Matt, G., Fabian, A.C., Bianchi, S., Brandt,W.N., Guainazzi, M., Murayama, T., Taniguchi, Y.,Nuclear obscuration in the high-ionization Seyfert 2galaxy Tol 0109-383, MNRAS, 326, 119, 2001.

Jansen, F., Lumb, D., Altieri, B., Clavel, J., Ehle, M.,Erd, C., Gabriel, C., Guainazzi, M., Gondoin, P.,Much, R., Munoz, R., Santos, M., Schartel, N., Texier,D., Vacanti, G., XMM Newton Observatory, I TheSpacecraft and Operations, A&A, 365, L1, 2001.

Jansen, R.A., Franx, M., Fabricant, D.G., [OII] as tracerof current star formation, ApJ, 551, 825, 2001.

Jansen, R.A., Jakobsen, P., The late-time expansion ofthe ejecta of SN 1987A, A&A, 370, 1056, 2001.

Jansen, R.A., Kannappan, S.J., The Nearby Field GalaxySurvey; a spectrophotometric and photometric studyof nearby galaxies, Ap&SS, 276/2-4, 1151, 2001.

Klaas, U., Haas, M., Müller, S.A.H., Chini, R., Schulz,B., Coulson, I., Hippelein, H., Wilke, K., Albrecht,M., Lemke, D., Infrared to millimetre photometry ofultra-luminous IR galaxies: new evidence favouring a3-stage dust model, A&A, 379, 823, 2001.

Kuiper, L. Hermsen, W., Cusumano, G., Diehl, R.,Schönfelder, V., Strong A., Bennett, K., McConnell,M.L., The Crab pulsar in the 0.75-30 MeV range asseen by COMPTEL, A&A, 378, 918, 2001.

Leech, K.J., Metcalfe, L., Altieri, B., ISO Observationsof the dusty quasar BR1202-0725, MNRAS, 328,1125, 2001.

Loon, J. Th. van, Zijlstra, A.A., Kaper, L., Gilmore, G.F.,Loup, C., Blommaert, J.A.D.L., The peculiar clusterHs 327 in the Large Magellanic Cloud: can OH/IRstars and carbon stars be twins?, A&A, 368, 239, 2001.

Lumb, D., Gondoin, P., Guainazzi M., An XMM-Newtonview of the serendipitous sources in the PKS0312-770field, A&A, 376, 387, 2001.

Lyke, J.E., Gehrz, R.D., Woodward, C.E., Barlow, M.J.,Pequignot, D., Salama, A., Schwarz, G. J., Shore,S.N., Starrfield, S., Evans, A., Gonzales-Riesta, R.,Greenhouse, M.A., Hjellming, R.M., Jones, T.J.,Krautter, J., Morisset, C., Ogelman, H.B., Orio, M.,Wagner, R.M., Walton, N.A., Williams, R.E., ISOSWS Observations of V1425 Aquilae (Nova Aquilae1995), AJ, 122, 3305, 2001.

Matt, G., Guainazzi, M., Perola, G.C., Fiore, F., Nicastro,F., Cappi, M., Piro, L., The complex iron line ofNGC5506, A&A, 377, L31, 2001.

Miroshnichenko, A.S., Bjorkman, K.S., Chentsov, E.L.,Klochkova, V.G., Gray, R.O., Garcia-Lario, P., PereaCalderon, J.V., The pre-main-sequence star IP Persei,A&A, 377, 854, 2001.

Møller, P., Warren, S.J, Fall, S.M., Fynbo, J.U., Jakobsen,P., Are High-Redshift Damped Ly-alpha GalaxiesLyman Break Galaxies?, ApJ, 574, 51, 2001.

Moneti, A., Stolovy, S., Blommaert, J.A.D.L., Figer,D.F., Najarro, F., Mid-infrared imaging and spectro-

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scopy of the enigmatic cocoon stars in the QuintupletCluster, A&A, 366, 106, 2001.

Morley, J., Briggs, K., Pye, J., Favata, F., Micela, G.,Sciortino, S., A ROSAT medium sensitivity Galacticplane survey 180 < λ < 280, MNRAS, 326, 1161, 2001.

Natta, A., Prusti, T., Neri, R., Wooden, D., Grinin, V.,Mannings, V., A Reconsideration of Disk Properties inHerbig Ae Stars, A&A, 371, 186, 2001.

Neumann, D., Arnaud, M., Gastaud, R., Aghanim, N.,Lumb, D., Briel, U., Vestrand, T., Stewart, G., Molendi,S., Mittaz, J., The NGC4839 group falling onto theComa Cluster observed by XMM-Newton, A&A, 365,L74, 2001.

Nevalainen, J., Kaastra, J., Parmar, A.N., Markevitch,M., Oosterbroek, T., Colafrancesco, S., Mazzotta, P.,Temperature and total mass profiles of the A3571cluster of galaxies, A&A, 369, 459, 2001.

Nevalainen, J., Lumb, D., dos Santos, S., Siddiqui, H.,Stewart, G., Parmar, A.N., Discovery of an absorbedcluster of galaxies XMMJ183225.4+103645 close tothe Galactic plane with XMM-Newton, A&A, 374, 66.

Oosterbroek, T., Barret, D., Guainazzi, M., Ford, E.C.,Simultaneous BeppoSAX and RXTE observations ofthe X-ray burst sources GX 3+1 and Ser X-1, A&A,366, 138, 2001.

Oosterbroek, T., Parmar, A.N., Orlandini, M., Segreto,A., Santangelo, A., Del Sordo S., A BeppoSAXobservation of Her X-1 during the first main-on afteran anomalous low-state: evidence for rapid spin-down, A&A, 375, 922, 2001.

Oosterbroek, T., Parmar, A.N., Sidoli, L., in ‘t Zand,J.J.M., Heise, J., BeppoSAX observation of the eclips-ing dipping X-ray binary X1658-298, A&A, 376, 532,2001.

Orio, M., Parmar, A.N., Amati, A., Frontera, F., Griener,J., Mineo, T., Ogelman, H., Starrfield, S., Trussoni, E.,BeppoSAX observations of Nova V382 Velorum I.The hard X-ray flux two weeks after the outburst,MNRAS, 326, L13, 2001.

Orio, M., Parmar, A.N., Griener, J., Ogelman, H., Starr-field, S., Trussoni, E., 2001, The X-ray emission fromnova V382 Velorum – II. The super-soft componentobserved with BeppoSAX, MNRAS, 333, 110, 2001.

Orr, A., Barr, P., Guainazzi, M., Parmar, A.N., Young, A.,BeppoSAX spectroscopy of MR 2251-178: a test forionized reflection in radio quiet QSOs, A&A, 376,413, 2001.

Owens, A., Bavdaz, M., Gostilo, V., Gryaznov, D.,Loupilov, A., Peacock, A., Sipila, H., The X-rayresponse of InP, NIM-A, 487, 435, 2001.

Owens, A., Bavdaz, M., Lisjutin, I., Peacock, A.,Zatolova, S., On the development of compound semi-conductor thallium bromide detectors for astro-physics, NIM-A, 458, 413, 2001.

Owens, A., Bavdaz, M., Peacock, A., Poelaert, A.,Andersson, H., Nenonen, S., Troger, L., Bertoccio, G.,Hard X-ray spectroscopy using small format GaAsarrays, NIM-A, 466, 168, 2001.

Owens, A., Bavdaz, M., Peacock, A., Poelaert, A.,

Andersson, H., Nenonen, S., Sipila, H., Troger, L.,Bertuccio, G., High Resolution X-ray SpectroscopyUsing GaAs arrays, J. App. Phys., 90, 5376, 2001.

Oyabu, S., Kawara, K., Tsuzuki, Y., Sofue, Y., Sato, Y.,Okuda, H., Taniguchi, Y., Shibai, H., Gabriel, C.,Hasegawa, T., Nishihara, E., ISO continuumobservations of quasars at z=1-4, A&A, 365, 409, 2001.

Parmar, A.N., Oosterbroek, T., Sidoli, L., Stella, L.,Verbunt, F., Frontera, F., BeppoSAX study of theX-ray binary XB 1832-330 located in the globularcluster NGC 6652, A&A, 380, 490, 2001.

Parmar, A.N., Sidoli, L., Oosterbroek, T., Charles, P.A.,Dubus, G., Guainazzi, M., Hakala, P., Pietsch, W.,Trinchieri, G., BeppoSAX spectroscopy of the luminousX-ray sources in M33, A&A, 368, 420, 2001.

Parthasarathy, M., Garcia-Lario, P., Gauba, G., deMartino, D., Nakada, Y., Fujii, T., Pottasch, S.R., SanFernandez de Cordoba, L., IUE and ISO observationsof the bipolar proto-planetary nebula Hen 401 (IRAS10178-5958), A&A, 376, 941, 2001.

Perryman, M.A.C., Extra-Solar Planets, EurophysicsNews, 32/1, 9, 2001.

Perryman, M.A.C., Cropper, M., Ramsay, G., Favata, F.,Peacock, A., Rando, N., Reynolds, A., High-SpeedEnergy-Resolved STJ Photometry of the EclipsingBinary UZ For, MNRAS, 324, 899, 2001.

Perryman, M.A.C., de Boer, K.S., Gilmore, G. Høg, E.,Lattanzi, M.G., Lindegren, L., Luri, X., Mignard, F.,Pace, O., de Zeeuw, P.T., GAIA: Composition,Formation and Evolution of the Galaxy, A&A, 369,339, 2001.

Pierini, D., Lequeux, J., Boselli, A., Leech, K.J., Volk,H.J., Gas cooling within the diffuse ISM of late-typegalaxies, A&A, 373, 827, 2001.

Ramsay, G., Cropper, M., Cordova, F., Mason, K., Much,R., Pandel, D., Shirey, R., First XMM-Newtonobservations of strongly magnetic cataclysmicvariables I: spectral studies of DP Leo and WW Hor,MNRAS, 326, L27, 2001.

Santos-Lleo, M., Clavel, J., Schulz, B., Altieri, B., Barr,P., Berlind, P., Bertram, R., Crenshaw, D.M., Edelson,R.A., Giveon, U., Horne, K., Huchra, J.P., Kaspi, S.,Kriss, G.A., Krolik, J.H., Malkan, M.A., Malkw,Yu.F., Netzer, H., O’Brien, P.T., Peterson, B.M.,Pogge, R.W., Pronik, V.I., Qian, B.-C., Reichert, G.A.,Rodriguez-Pascual, P.M., Sergeev, S.G., Tao, J.,Tokarz, S., Wagner, R.M., Wamsteker, W., Wilkes,B.J., Monitoring of the optical and 2.5-11.7 micronspectrum and mid-IR imaging of the Seyfert 1 galaxyMrk~279 with ISO, A&A, 369, 57, 2001.

Schild, H., Eyres, S.P.S., Salama, A., Evans, A., ISOobservations of symbiotic stars, A&A, 378, 146, 2001.

Sciortino, S., Micela, G., Damiani, F., Flaccomio, E.,Briggs, K., Denby, M., Pye, J., Grosso, N., Read, A.M., Gondoin, P., Jeffries, R. D., XMM-Newton surveyof the low-metallicity open cluster NGC 2516, A&A,365, L259, 2001.

Setia Gunawan, D.Y.A., van der Hucht, K.A., Williams,P.M., Henrichs, H.F., Kaper, L., Stickland, D.J.,

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132 publications

Wamsteker, W., Multi-frequency variations of theWolf-Rayet HD 193793 (WC7pd+O4-5)., A&A, 376,460, 2001.

Shelton, R, Kruk, J., Murphy, E., Andersson, B., Blair,W., Dixon, W., Edelstein, J., Fullerton, A., Gry, C.,Howk, J., Jenkins, E., Linsky, J., Moos, H., Oegerle,W., Oey, M., Roth, K., Sahnow, D., Sankrit, R.,Savage, B., Sembach, K., Shull, J., Siegmund, O.,Vidal-Madjar, A., Welsh, B., York, D., Observations ofOVI Emission from the Diffuse Interstellar Medium,ApJ, 560, 730, 2001.

Shirey, R., Soria, R., Borozdin, K., Obsorne, J.P.,Guainazzi, M., Hayter, C., La Palombara, N., Mason,K., Molendi, S., Paerels, F., Pietsch, W., Priedhorsky,W., Read, A.M., Tiengo, A., Watson, M.G., West,R.G., The central region of M31 observed with XMM-Newton, A&A, 365, L195, 2001.

Sidoli, L., Belloni, T., Mereghetti, S., A catalogue of softX-ray sources in the galactic center region, A&A, 368,835, 2001.

Sidoli, L., Mereghetti, S., Treves, A., Parmar, A.N., Tur-olla, R., Favata, F., X-ray emission from the giantmolecular clouds in the galactic center region and thediscovery of new X-ray sources, A&A, 372, 651, 2001.

Sidoli, L., Oosterbroek, T., Parmar, A.N., Lumb, D., Erd,C., Discovery of narrow X-ray absorption lines fromthe low-mass X-ray binary MXB 1659-298 withXMM-Newton, A&A, 379, 540, 2001.

Sidoli, L., Parmar, A., Oosterbroek, T., Stella, L.,Verbunt, F., Masetti, N., Dal Fiume, D., BeppoSAXstudy of the broad band properties of luminousglobular cluster X-ray sources, A&A, 368, 451, 2001.

Siebenmorgen, R., Krugel, E., Laureijs, R. J., TheInfrared Continuum Radiation of NGC1808* A PAHand Polarisation Study, A&A, 377, 735, 2001.

Slee, O.B., Roy, A.L., Murgia, M., Andernach, H., Ehle,M., Four Extreme Relic Radio Sources in Clusters ofGalaxies, AJ, 122, 1172, 2001.

Strüder, L., Briel, U., Dennerl, K., Hartmann, R.,Kendziorra, E., Meidinger, N., Pfeffermann, E.,Reppin, C., Aschenbach, B., Brauninger, H., Burkert,W., Elender, M., Freyberg, M., Haberl, F., Hartner, G.,Heuschmann, F., Kastelic, E., Kemmer, S., Ketten-ring, G., Kink, W., Krause, N., Muller, S., Oppitz, A.,Pietsch, W., Popp, M., Predehl, P., Read, A., Stephan,K., Stotter, D., Trümper, J., Holl, P., Kemmer, J.,Soltau, H., Stötter, R., Weber, U., v Zanthier, C., Lutz,G., Richter, R., Solc, P., Bttcher, H., Kuster, M.,Staubert, R., Abbey, A., Holland, A., Turner, M.,Balasini, M., Bignami, G., La Palombara, N., Villa,G., Buttler, W., Lainé, R., Lumb, D., Dhez, P., TheEPIC Camera on XMM-Newton: The pn-CCDCamera, A&A, 365, L18, 2001.

Tamura, T., Kaastra, J., Peterson, J., Paerels, F., Mittaz, J.,Trudolyubov, S., Stewart, G., Fabian, A., Mushotzky,R., Lumb, D., Ikebe, Y., X-ray Spectroscopy of thecluster of galaxies Abell 1795, A&A, 365, L87, 2001.

Torrejon, J. M., Orr, A., BeppoSAX survey of Be/X-raybinary candidates, A&A, 377, 148, 2001.

Turner, M., Abbey, A., Arnaud, M., Balasini, M., Belsole,E., Bennie, P., Bernard, J., Bignami, G., Boer, M., Briel,U., Butler, I., Cara, C., Collura, A., Conte, M., Cros, A.,Denby, M., Dhez, P., Di Cocco, G., Dowson, J.,Ferrando, P., Ghizzardi, S., Gianotti, F., Goodall, C.,Gretton, L., Griffiths, R., Hainaut, O., Hochedez, J.,Holland, A., Jourdain, E., Kendziorra, E., Lagostina, A.,Lainé, R., La Palombara, N., Lotholary, M., Lumb, D.,Marty, P., Molendi, S., Pigot, C., Poindron, E., Pounds,K., Reeves, J., Reppin, C., Rothenflug, R., Salvetat, P.,Sauvageot, J-L., Schmitt, D., Sembay, S., Short, A.,Spragg, J., Stephen, J., Strüder, L., Tiengo, A.,Trifoglio, M., Trümper, J., Vercellone, S., Vigroux, L.,Villa, G., Ward, M., Whitehead, S., Zonca, E., TheEPIC Camera on XMM-Newton: The MOS Cameras,A&A, 365, L27, 2001.

Vernet, J., Fosbury, R.A.E., Villar-Martin, M., Cohen,M.H., Cimatti, A., di Serego Alighieri, S., Goodrich,R.W., Radio galaxies at z ~ 2.5: results from Keckspectropolarimetry, A&A, 366, 7, 2001.

Vilhu, O., Nikula, P., Poutanen, J., Nevalainen, J.,Thermal Comptonization in GRS 1915+105, ApJ,553, L51, 2001.

Vio, R., Andreani, P., Wamsteker, W., Digital Simulationof Non-Gaussian Random Fields with PredefinedCorrelation Structure, PASP, 113, 1009, 2001.

Walker, R.C., Benson, J.M., Unwin, S.C., Lystrup, M.B.,Hunter, T.R., Pilbratt, G.L., Hardee, P.E., TheStructure and Motion of the 3C120 Radio Jet onScales of 0.6 to 300 Parsecs, ApJ, 556, 756, 2001.

Warren, S.J., Møller, P., Fall, S.M., Jakobsen, P.,NICMOS imaging search for high-redshift dampedLy-alpha galaxies, MNRAS, 326, 759, 2001.

Warwick, R., Bernard, J.-P., Bocchino, F., Decourchelle,A., Ferrando, P., Griffiths, R., Haberl, F., LaPalombara, N., Lumb, D., Mereghetti, S., Read, A.,Schaudel, D., Schurch, N., Tiengo, A., Willingale, R.,The extended X-ray Halo of the Crab-like SNRG21.5-09, A&A, 365, L248, 2001.



Aigrain, S., Gilmore, G., Favata, F., A Bayesianalgorithm for the detection of planetary transits,W.R.F. Drent (eds.), in Techniques for the detection ofplanets and life beyond the solar system, 4th AnnualROE Workshop, 8, 2001.

Arndt, M., Connors, A., Lockwood, J., McConnell, M.,Suleiman, R., Ryan, J., Young, C, Rank, G., Schön-felder, V., Debrunner, H., Bennett, K., Williams, O.,Winkler, C., X- and Gamma-Ray Observations of the15 November 1991 Solar Flare, Ritz, S., Gehrels, N.,Shrader, C. (eds.), in Proc. Gamma 2001 Symposium,AIP Conference Proceedings, 587, 618, 2001.

sp1247s4.qxd 3/5/03 3:59 PM Page 132

publications 133

Arviset, C., Hernandez, J., Prusti, T., The ISO DataArchive and Links to other Archives, R. Brunner, S.Djorgovski, A. Szalay (eds.), in Proc. VirtualObservatories of the Future, ASP Conference Series,225, 165, 2001.

Beijersbergen, M., Bavdaz, M., Peacock, A., Tomaselli,E., Fairbend, R., Boutot, J-P., Flyckt, S., Brunton, A.,Price, G., Fraser, G., Herrmann, C., Krumrey, M.,Ziegler, E., Freund, A., High-resolution micro-poreX-ray optics produced with micro-channel platetechnology, Proc. SPIE, 4145, 188, 2001.

Blommaert, J.A.D.L., ISOGAL Collaboration, Mass-losing AGB stars in galactic bulge ISOGAL fields,Galactic Structure, Stars and the ISM, ASPConference Series, 231, 541, 2001.

Bocchino, F., Lumb, D., Marty, P., Becker, W., Pigot, C.,Warwick, R.S., The X-ray nebula of the filled centersupernova remnant 3C58 and its interaction with theenvironment, R. Giacconi, S. Serio, L. Stella (eds.), inProc. X-ray Astronomy 2000, ASP Conference Series,234, 203, 2001.

Collmar, W., Schönfelder, V., Zhang, S., Bloemen, H.,Hermsen, W., McConnell, M., Bennett, K., Williams,O., COMPTEL Observations of the Virgo Blazars 3C273 and 3C 279, Ritz, S., Gehrels, N., Shrader, C.(eds.), in Proc. Gamma 2001 Symposium, AIPConference Proceedings, 587, 271, 2001.

Coustenis, A., Bezard, B., Encrenaz, Th., Gautier, D.,Lellouch, E., Salama, A., Lacy, J., Orton, G., The D/Hratio on Titan from ISO and IRSHELL data, AAS, DPS33, 38.01, 2001.

Coustenis, A., Salama, A., Schulz, B., Lellouch, E.,Encrenaz, Th., Ott, S., Kessler, M.F., Feuchtgruber,H., de Graauw, Th., Past and Future SpaceObservations of Titan in the Infrared and SubmmRanges: ISO, CASSINI and FIRST, G. Pilbratt, J.Chernicharo, A. Heras, T. Prusti, R. Harris (eds.), inProc. The Promise of the Herschel Space Observatory,ESA SP-460, 393, 2001.

Ehle, M., Pietsch, W., Haberl, F., Further Details on theDeep XMM-Newton Survey of M33, H. Inoue, H.Kunieda (eds.), in New Century of X-ray Astronomy,ASP Conference Series, 251, 300, 2001.

Favata, F., Evidence for compact structuring in thecorona of active stars, R. Giacconi, L. Stella, S. Serio(eds.), in X-ray Astronomy 2000, ASP ConferenceSeries, 234, 111, 2001.

Favata, F., The Eddington mission, W.R.F. Drent (eds.) inTechniques for the detection of planets and life beyondthe solar system, 4th Annual ROE Workshop, 7, 2001.

Favata, F., Pace, O., Eddington, ESA Bulletin, 105, 46,2001.

Frontera, F., Amati, L., Dal Fiume, D., Masetti, N.,Orlandini, M., Palazzi, E., Belloni, T., Del Sordo, S.,Parmar, A.N., Observations of new black holecandidates with BeppoSAX, A. Gimenez, V. Reglero,C. Winkler (eds.), in Proc. 4th INTEGRAL Workshop,ESA SP-459, 187, 2001.

Frontera, F., Masetti, N., Orlandini, M., Amati, L.,

Palazzi, E., Dal Fiume, D., Del Sordo, S., Cusumano,G., Parmar, A., Pareschi, G., Lapidus, I., Stella, L.,Discovery of hard X-ray emission from Type II burstsof the Rapid Burster, AIP Conference Proceedings,599, 614, 2001.

Garcia-Hernandez, D.A., Manchado, A., Garcia-Lario,P., Dominguez-Tagle, C., Conway, G., Molecularhydrogen around post-AGB stars, Ap&SS, 265, 383,2001.

Garcia-Lario, P., Manchado, A., Ulla, A., Manteiga, M.,2001, ISO Spectroscopy of the Proto-PlanetaryNebula IRAS 17423-1755 (HEN 3-1475), inHighlights of Spanish Astrophysics II, DordrechtLumer Ac. Publishers, 375, 2001.

Garcia-Lario, P., Perea Calderon, J.V., An Atlas of ISOSWS Spectra: The Transition Phase from AGB Starsto Planetary Nebulae, Ap&SS, 265, 329, 2001.

Giardino, G., Banday, A.J., Bennett, K., Fosalba, P.,Gorski, K.M., O’Mullane, W., Tauber, J., Analysis ofCMB foregrounds using a database for Planck,Banday, A., Zaroubi, S., Bartelmann, M. (eds.), inProc. The MPA/ESO/MPE Joint Astronomy Confer-ence ‘Mining the Sky’, ESO Astrophysics Symposia,458, 2001.

Gimenez, A., Favata, F., Eddington: A European SpaceMission that will measure the age of the stars, T. vonHippel, Ch. Simpson and N. Manset (eds.) inAstrophysical Ages and Times Scales, ASP ConferenceSeries, 245, 304, 2001.

Gondoin, P., Chromospheric and Coronal Emission onG-K Field Giants, R.J. Garcia Lopez, R. Rebolo, M.R.Zapatero Osorio (eds.), in Proc. The 11th CambridgeWorkshop on Cool Stars, Stellar Systems and the Sun,ASP Conference Series, 223, 949, 2001.

Gondoin, P., Lumb, D., Siddiqui, H., Guainazzi, M.,Schartel, N., X-ray Spectroscopy of Fairall 9, J. Kna-pen, J. Beckman, I. Shlosman, T. Mahoney (eds.) in TheCentral Kiloparsec of Starbursts and AGN: The LaPalma Connection, ASP Conf. Series, 249, 438, 2001.

Gonzalez-Riestra, R., Solano, E., Garcia, J., Martinez, J.,Montesinos, B., Rodriguez, F., Sanz, L., Talavera, A.,de la Fuente, A., Ponz, J.D., Skillen, I., Wamsteker,W., INES: The Next Generation Astronomical DataDistribution System, F.A. Primini, F.R. Harnden, H.E.Payne (eds.), in Tenth Annual Conference onAstronomical Data Analysis, ASP Conference Series,156, 2001.

Guainazzi, M., Oosterbroek, T., A catalogue of AGNobserved by the PDS experiment on boardBeppoSAX, J.H.Knapen, J.E. Beckman, I. Shlosman,T.J. Mahoney (eds.), in The central kpc of Starburstsand AGN, ASP Conference Series, 249, 442, 2001.

Guainazzi, M., Parmar, A.N., Oosterbroek, T., Compton-ization in X-ray Bright Neutron Star globular clustersystems, AIP Conference Proceedings, 599, 638,2001.

Hanlon, L., Kinsella, D., Murphy, N., McBreen, B.,Bennett, K., Williams, O., Winkler, C., Preece, R.,Broadband Spectral Deconvolution of GRBs, Costa,

sp1247s4.qxd 3/5/03 3:59 PM Page 133

134 publications

E., Frontera, F., Hjorth, J. (eds.), in Proc. Gamma-RayBursts in the Afterglow Era, Springer, 63, 2001.

Humphrey, P.J., Church, M.J., Balucinska-Church, M.,Parmar, A.N., Spectral Evolution during Dipping in X1624-490 for the BeppoSAX Observation, AIPConference Proceedings, 599, 674, 2001.

Israel, G., Campana, S., Covino, S., Dal Fiume, D.,Oosterbroek, T., Mereghetti, S., Orlandini, M.,Panzera, M., Parmar, A., Tagliaferri, G., Ricci, D.,Stella, L., A systematic search for new X-ray pulsatorsin public Rosat HRI and BeppoSAX SMC fields, AIPConference Proceedings, 599, 674, 2001.

Iyudin, A.F., Diehl, R., Schönfelder, V., Strong, A.,Bennett, K., Winkler, C., Bloemen, H., Hermsen, W.,Ryan, J., Study of Nova-Produced Na22 withCOMPTEL, A. Gimenez, V. Reglero, C. Winkler(eds.), in Proc. 4th INTEGRAL Workshop, ESA SP-459, 41, 2001.

Iyudin, A., Schönfelder, V., Strong, A., Bennett, K.,Diehl, R., Hermsen, W., Lichti, G., Ryan, J., Study ofthe Galactic Distribution of Nova-Produced 22Nawith COMPTEL, Ritz, S., Gehrels, N., Shrader, C.(eds.), in Proc. Gamma 2001 Symposium, AIPConference Proceedings, 587, 508, 2001.

Jansen, F., Parmar, A.N., Status of the XMM-Newtonmission, Proc. New Century of X-ray AstronomyMeeting, APS Conference Series, 251, 10, 2001.

Jimenez-Esteban, F., Engels, D., Garcia-Lario, P., NearInfrared Observations of the Arecibo Sample ofOH/IR Stars, Ap&SS, 265, 49, 2001.

Manchado, A., Suarez, O., Garcia-Lario, P., Manteiga,M., Pottasch, S.R., Optical Survey of Post-AGBCandidates, Ap&SS, 265, 21, 2001.

Martin, D., Owens, A., Erd, C., Andersson, S., Peacock,A., Andersson, H., Lms, V., Nenonen, S., Haack, N.,High resolution X-ray spectroscopy using a largeformat GaAs array, Proc. SPIE, 4507, 152, 2001.

McConnell, M., Bennett, K., Bloemen, H., Collmar, W.,Hermsen, W., Kuiper, L., Paciesas, W., Phlips, B.,Poutanen, J., Ryan, J., Schönfelder, V., Steinle, H.,Strong, A., Zdziarski, A., Gamma-Ray SpectralVariability of Cygnus X-1, Ritz, S., Gehrels, N.,Shrader, C. (eds.), in Proc. Gamma 2001 Symposium,AIP Conference Proceedings, 587, 96, 2001.

Micela, G., Sciortino, S., Favata, F., X-ray surveys andyoung stellar population: constraints on stellarbirthrate in the solar neighborhood, R. Jayawardhana& Th. Greene (eds.), in Young Stars near Earth:progress and prospects, ASP Conference Series, 244,177, 2001.

O’Mullane, W., Banday, A., Gorski, K., Kunszt, P.,Zsalay, A, Splitting the sky – HTM & HEALPix.,Banday, A., Zaroubi, S., Bartelmann, M. (eds.), inProc. The MPA/ESO/MPE Joint AstronomyConference ‘Mining the Sky’, ESO AstrophysicsSymposia, 638, 2001.

Orio, M., Parmar, A.N., Amati, L., Benjamin, R., DellaValle, M., Frontera, F., Greiner, J., Mineo, T.,Ogelman, H., Starrfield, S., Trussoni, E., A

BeppoSAX observation of nova velorum 1999: a verybright classical nova, AIP Conference Proceedings,599, 466, 2001.

Orr, A., Mrk 335: a NLSy1 with an unusual warmabsorber?, Ritz, S., Gehrels, N., Shrader, C. (eds.), inProc. Gamma 2001 Symposium, AIP ConferenceProceedings, 587, 400, 2001.

Orr, A., Barr, P., Parmar, A., Guainazzi, M., Young, A.,BeppoSAX Observations of the Radio-Quiet QSOMR2251-178, A. Gimenez, V. Reglero, C. Winkler(eds.), in Proc. 4th INTEGRAL Workshop, ESA SP-459, 329, 2001.

Orr, A., Guainazzi, M., Parmar, A., Young, A.,BeppoSAX observations of the radio-quiet QSO MR2251-178, Ritz, S., Gehrels, N., Shrader, C. (eds.), inProc. "Gamma 2001 Symposium, AIP ConferenceProceedings, 587, 380, 2001.

Orr, A., Torricelli, G., Pietrini, P., The X-ray spectra ofAGN accretion disk coronae: first results, N. White,G. Malaguti, G. Palumbo (eds.), in Proc. X-rayAstronomy 1999, AIP Conference Proceedings, 599,818, 2001.

Ott, S., Gastaud, R., Ali, B., Delaney, M., Miville-Deschenes, M.A., Okumura, K., Sauvage, M., Guest,S., CIA V5.0 – the Legacy Package for ISOCAMInteractive Analysis, F. Harnden, F. Primini, H. Payne(eds.), in Proc. Astronomical Data Analysis Softwareand Systems X, ASP Conference Series, 238, 170,2001.

Ott, S., Starck, J.-L., Schartel, N., Siebenmorgen, R., Vo,T., Aussel, H., Bertin, E., Source Detection for theISOCAM Parallel Survey, Proc. SPIE, 4477, 289,2001.

Owens, A., Andersson, H., Bavdaz, M., Brammertz, G.,Erd, C., Gagliardi, T., Gostilo, V., Haack, N., Lisjutin,I., Nenonen, S., Peacock, A., Sipila, H., Taylor, I.,Zataloka, S., Development of compound semi-conductor arrays for X- and Gamma ray spectroscopy,Proc. SPIE, 4507, 42, 2001.

Owens, A., Bavdaz, M., Beijersbergen, M., Brunton,A.N., Fraser, G.W., Martin, D., Nieminen, P., Peacock,A., Pia, M.G., HERMES: an imaging X-ray fluor-escence spectrometer for the BepiColombo mission toMercury, Proc. SPIE, 4506, 136, 2001.

Parmar, A.N., Gas Detectors, Encyclopedia of Astronomyand Astrophysics, 947, 2001.

Parmar, A.N., High-energy astronomy from the Internat-ional Space Station, The Observatory, 121, 295, 2001.

Parmar, A.N., High-energy astronomy from theInternational Space Station, Earth Moon and Planets,87, 149, 2001.

Parmar, A.N., Oosterbroek, T., Dal Fiume, D., Orlandini,M., Santangelo, A., Del Sordo, S., Segreto, A.,BeppoSAX Observations of the Her X-1 Short- andAnomalous Low-States, AIP Conference Proceedings,599, 838, 2001.

Parmar, A.N., Peacock, T., Bavdaz, M., 2001, XEUS –The X-ray Evolving Universe Spectroscopy Mission,R. Giacconi, S. Serio, L. Stella (eds.), in Proc. X-ray

sp1247s4.qxd 3/5/03 3:59 PM Page 134

publications 135

Astronomy 2000, ASP Conference Series, 234, 581,2001.

Parmar, A.N., Peacock, T., Bavdaz, M., Hasinger, G.,Arnaud, M., Barcons, X., Barret, D., Blanchard, A.,Bhringer, H., Cappi, M., Comastri, A., Courvoisier, T.,Fabian, A.C., Griffiths, R., Malaguti, P., Mason, K.O.,Ohashi, T., Paerels, F., Piro, L., Schmitt, J., van derKlis, M., Ward, M., XEUS – The X-ray EvolvingUniverse Spectroscopy Mission, AIP ConferenceProceedings, 599, 842, 2001.

Perryman, M.A.C., GAIA: An Introduction to theProject, Bienayme, O. and Turon, C. (eds.), in GAIASummer School, Les Houches, EDP Sciences, 3, 2001.

Pilbratt, G.L., The FIRST ESA Cornerstone Mission,Harwit, M., Hauser, M.G. (eds.), in The ExtragalacticInfrared Background and its CosmologicalImplications, Proc. of IAU Symp, 204, 481, 2001.

Pilbratt, G.L., The Herschel Mission, ScientificObjectives, and this Meeting, G. Pilbratt, J.Chernicharo, A. Heras, T. Prusti, R. Harris (eds.), inProc. The Promise of the Herschel Space Observatory,ESA SP-460, 13, 2001.

Plüschke, S., Diehl, R., Schönfelder, V., Strong, A.,Bloemen, H., Hermsen, W., Bennett, K., Winkler, C.,McConnell, M., Ryan, J., Knödlseder, J., Oberlack, U.,Weidenspointer, G., The COMPTEL 1.809 MeVSurvey, A. Gimenez, V. Reglero, C. Winkler (eds.), inProc. 4th INTEGRAL Workshop, ESA SP-459, 55, 2001.

Plüschke, S., Georgii, R., Diehl, R., Collmar, W., Lichti,G.G., Schönfelder, V., Bloemen, H., Hermsen, W.,Bennett, K., McConnell, M., Ryan, J., 2001, Co56gamma-rays from SN1998bu: COMPTEL upper limits,A. Gimenez, V. Reglero, C. Winkler (eds.), in Proc. 4thINTEGRAL Workshop, ESA SP-459, 87, 2001.

Prusti, T., Young Stellar Clusters: from ISO to Herschel,G. Pilbratt, J. Chernicharo, A. Heras, T. Prusti, R.Harris (eds.), in Proc. The Promise of the HerschelSpace Observatory, ESA SP-460, 239, 2001.

Reiera, A., Garcia-Lario, P., Manchado, A., Dynamics ofthe Collimated Outflows of the Proto-PlanetaryNebula Hen 3-1475, Ap&SS, 265, 209, 2001.

Romaniello, M., Panagia, N., Scuderi, S., Gilmozzi, R.,Tolstoy, E., Favata, F., Kirshner, R., T Tauri Stars inthe Large Magellanic Clouds: a combined HST andVLT effort, J. Alves & M. McCaughrean (eds.), inProc. The Origins of Stars and Planets: the VLT View,ESO, Garching, 275, 2001.

Sciortino, S., Damiani, F., Flaccomio, E., Favata, F.,Micela, G., Results from an XMM-EPIC observationof upper Sco-Cen, R. Jayawardhana & Th. Greene(eds.), in Young Stars near Earth: progress andprospects, ASP Conference Series, 244, 171, 2001.

Sidoli, L., The BeppoSAX View of the Galactic CenterRegion, F. Giovannelli and G. Mannocchi (eds.), inProc. Vulcano2000 workshop, Societa Italiana diFisica, 193, 2001.

Sivarani, T., Parthasarathy, M., Garcia-Lario, P.,Manchado, A., Spectroscopy of HD 168625 (IRAS18184-1623), Ap&SS, 265, 309, 2001.

Sivarani, T., Parthasarathy, M., Garcia-Lario, P.,Manchado, A., Spectroscopy of IRAS 10215-5916,Ap&SS, 265, 305, 2001.

Sivarani, T., Parthasarathy, M., Garcia-Lario, P.,Manchado, A., Spectroscopy of Post-AGB F-Supergiant HD 331319 (IRAS 19475+3119), Ap&SS,265, 301, 2001.

Sivarani, T., Parthasarathy, M., Garcia-Lario, P.,Manchado, A., Pottasch, S.R., High ResolutionSpectroscopy of Post-AGB Supergiant HD 101584(IRAS 11385-5517), Ap&SS, 265, 295, 2001.

Solano, E., Gonzalez-Riestra, R., Talavera, A., Rodri-guez, F., de la Fuente, A., Skillen, I., Ponz, J.D.,Wamsteker, W., INES Version 3.0: Functionalities andContents, F.A. Primini, F.R. Harndenm, H.E. Payne(eds.), in Tenth Annual Conference on AstronomicalData Analysis, ASP Conf. Series, 238, 152, 2001.

Strong, A., Collmar, W., Bennett, K., Bloemen, H., Diehl,R., Hermsen, W., Iyudin, A., Mayer-Hasselwander, H.,Ryan, J., Schönfelder, V., COMPTEL Observations ofa Source in the Direction of the Galactic Centre, Ritz,S., Gehrels, N., Shrader, C. (eds.), in Proc. Gamma2001 Symposium, AIP Conference Proceedings, 587,21, 2001.

Suarez, O., Manteiga, M., Rodriguez, A., Dafonte, J.C.,Arcay, B., Ulla, A., Garcia-Lario, P., Manchado, A.,Automatic Classification of Optical SourcesCandidates to be in the Post-AGB Stage, in Proc. 4thScientific Meeting of the Spanish AstronomicalSociety, Highlights of Spanish Astrophysics II,Santiago de Compostela, Spain, 229, 2001.

Tauber, J.A., The Planck Mission, Harwit, M., Hauser,M.G. (eds.), in The Extragalactic InfraredBackground and its Cosmological Implications, Proc.of IAU Symp, 204, 493, 2001.

Turner, M.J.L., Bleeker, J.A.M., Truemper, J., Hasinger,G., Inoue, H., Kunieda, H., Palumbo, G.G.C., Peacock,A., Parmar, A.N., Bavdaz, M., XEUS: a WorldObservatory for X-ray Spectroscopy of the EvolvingUniverse, Proc. New Century of X-ray AstronomyMeeting, ASP Conference Series, 251, 230, 2001.

Vilhu, O., Nikula, P, Poutanen, J., Nevalainen, J.,Thermal Comptonization in GRS 1915+105, ApSSS,276, 185, 2001.

Wamsteker, W., Multi-Wavelengths Observations ofAGN: Fifteen years along, Cheng Fu-Zhen (eds.), inProc. 14th Guo Shoujing Summer School, Annals ofShanghai Observatory, 22, 133, 2001.

Williams, O.R., Bennett, K., Collmar, W., Iyudin, A.,Schonfelder, V., Steinle, H., Bloemen, H., Hermsen,W., Ryan, J., McConnell, M., Stacy, G., COMPTELObservations of PKS 0208-512 from 1991 to 1998, A.Gimenez, V. Reglero, C. Winkler (eds.), in Proc. 4thINTEGRAL Workshop, ESA SP-459, 357, 2001.

Winkler, C., The INTEGRAL Core Observing Programme,A. Gimenez, V. Reglero, C. Winkler (eds.), in Proc. 4thINTEGRAL Workshop, ESA SP-459, 471, 2001.

Young, C., Arndt, M., Bennett, K., Connors, A.,Debrunner, H., Diehl, R., McConnell, M., Miller, R.,

sp1247s4.qxd 3/5/03 3:59 PM Page 135

136 publications

Rank, G., Ryan, J., Schönfelder, V., Winkler, C.,COMPTEL Gamma-Ray Observations of the C4 SolarFlare on 20 January 2000, Ritz, S., Gehrels, N.,Shrader, C. (eds.), in Proc. Gamma 2001 Symposium,AIP Conference Proceedings, 587, 613, 2001.

Young, C., Bennett, K., Connors, A., Diehl, R.,McConnell, M., Rank, G., Ryan, J., Suleiman, R.,Schönfelder, V., Winkler, C., Energetic Proton Spectrain the 11 June 1991 Solar Flare, Ritz, S., Gehrels, N.,Shrader, C. (eds.), in Proc. Gamma 2001 Symposium,AIP Conference Proceedings, 587, 623, 2001.

Zhang, S., Collmar, W., Iyudin, A., Schönfelder, V.,Bloemen, H., Hermsen, W., Ryan, J., Bennett, K.,Williams, O.R., COMPTEL Observations of theFlaring Gamma-ray Blazar PKS 1622-297, A.Gimenez, V. Reglero, C. Winkler (eds.), in Proc. 4thINTEGRAL Workshop, ESA SP-459, 361, 2001.

Zhang, S., Collmar, W., Schönfelder, V., Bloemen, H.,Hermsen, W., McConnell, M., Bennett, K., Williams,O., COMPTEL Observations of the Blazars 3C 454.3and CTA 102, Ritz, S., Gehrels, N., Shrader, C. (eds.),in Proc. Gamma 2001 Symposium, AIP ConferenceProceedings, 587, 343, 2001.



Aigrain, S., Favata, F., Bayesian detection of planetarytransits: A modified version of the Gregory-Loredomethod for bayesian periodic signal detection, A&A,395, 625, 2002.

Barbera, M., Bocchino, F., Damiani, F., Micela, G.,Sciortino, S., Favata, F., Harnden, F.R., ROSATPSPC/HRI observations of the open cluster NGC2422, A&A, 387, 463, 2002.

Beck, R., Shoutenkov, V., Ehle, M., Harnett, J.I., Haynes,R.F., Shukurov, A., Sokoloff, D.D., Thierbach, M.,2002, Magnetic fields in barred galaxies I. The atlas,A&A, 391, 83, 2002.

Bendo, G.J., Joseph, R.D., Wells, M., Gallais, P., Haas, M.,Heras, A.M., Klaas, U., Laureijs, R.J., Leech, K.,Lemke, D., Metcalfe, L., Rowan-Robinson, M., Schulz,B., Telesco, C., An Infrared Space Observatory Atlas ofBright Spiral Galaxies, AJ, 123, 3067, 2002.

Bendo, G.J., Joseph, R.D., Wells, M., Gallais, P., Haas,M., Heras, A.M., Klaas, U., Laureijs, R.J., Leech, K.,Lemke, D., Metcalfe, L., Rowan-Robinson, M.,Schulz, B., Telesco, C., Star formation in the InfraredSpace Observatory Atlas of bright spiral galaxies, AJ,124, 1380, 2002.

Boirin, L., Parmar, A.N., Oosterbroek, T., Lumb, D.,Orlandini, M., Schartel, N., Strongly absorbedquiescent X-ray emission from the X-ray transientXTE J0421+56 (CI Cam) observed with XMM-Newton, A&A, 394, 205, 2002.

Bridge, C., Cropper, M., Ramsay, G., Perryman, M., deBruijne, J., Favata, F., Peacock, A., Rando, N.,Reynolds, A., STJ Observations of the Eclipse PolarHU Aqr, MNRAS, 336, 1129, 2002.

Bruijne, J. de, Reynolds, A.P., Perryman, M.A.C.,Peacock, A., Favata, F., Rando, N., Martin, D.,Verhoeve, P., Christlieb, N., Direct determination ofquasar redshifts, A&A, 381, L57, 2002.

Campana, S., Stella, L., Israel, G., Moretti, A., Parmar,A., Orlandini, M., The quiescent X-ray emission fromthree transient X-ray pulsars, ApJ, 580, 389, 2002.

Ceccarelli, C., Baluteau, J.P., Walmsley, M., Swinyard,B.M., Caux, C., Sidher, S.D., Cox, P., Gry, C., Kessler,M., Prusti, T., ISO Ammonia Line Absorption Revealsa Layer of Hot Gas Veiling Sgr B2, A&A, 383, 603,2002.

Erd, C., Owens, A., Brammertz, G., Bavdaz, M.,Peacock, A., Lamsa, V., Nenonen, S., Andersson, H.,Haack, N., Hard X-Ray Test and Evaluation of aPrototype 32x32 Pixel Gallium-Arsenide Array,NIM-A, 487, 78, 2002.

Favata, F., Fridlund, C.M.V., Micela, G., Sciortino, S.,Kaas, A.A., Discovery of X-ray emission from theprotostellar jet L1551 IRS5 (HH 154), A&A, 386, 204,2002.

Fordham, J.L.A., Vranesevic, N., Carraminana, A.,Miche, R., Much, R., Wehinger, P., Wyckoff, S.,Phase-Resolved Spectroscopic Imaging of the CrabPulsar, ApJ, 581, 485, 2002.

Fosalba, P., Lazarian, A., Prunet, S., Tauber, J.A.,Statistical Properties of Galactic StarlightPolarization, ApJ, 564, 762, 2002.

Fridlund, C.V.M., The Search for Exo-planets and SpaceInterferometry, Planet. Space Sci., 50, 101, 2002.

Fridlund, C.V.M., Bergman, P., White, G.J., Pilbratt, G.L.,Tauber, J.A., The molecular disk surrounding theprotostellar binary L1551 IRS5, A&A, 382, 573, 2002.

Fujita, Y., Sarazin, C.L., Kempner, J.C., Andernach, H.,Ehle, M., Roy, A.L., Rudnick, L., Slee, O.B., ChandraObservations of the Disruption of the Cool Core inAbell 133, ApJ, 575, 764, 2002.

Garcia-Hernandez, D.A., Manchado, A., Garcia-Lario,P., Dominguez-Tagle, C., Conway, G.M., Prada, F.,Near-IR spectroscopy of planetary nebulae precursors,A&A, 387, 955, 2002.

Georgii, R., Plüschke, S., Diehl, R., Lichti, G.G.,Schönfelder, V., Bloemen, H., Hermsen, W., Ryan, J.,Bennett, K., COMPTEL upper limits for the 56Cogamma-ray emission from SN1998bu, A&A, 394, 517,2002.

Giardino, G., Banday, A.J., Gorski, K.M., Bennett, K.,Jonas, J.L., Tauber, J., Towards a model of full-skyGalactic synchrotron intensity and linear polarisation:a re-analysis of the Parkes data, A&A, 387, 82, 2002.

Gondoin, P., Erd, C., Lumb, D., Structure and evolutionof FK Comae corona, A&A, 383, 919, 2002.

Gondoin, P., Orr, A., Lumb, D, Santos-Lleo, M., XMM-Newton observations of the Seyfert 1 galaxy Mrk 335,A&A, 388, 74, 2002.

sp1247s4.qxd 3/5/03 3:59 PM Page 136

publications 137

Gry, C., Boulanger, F., Nehm, C., Pineau des Forts G.,Habart, E., Falgarone, E., H2 formation and excitationin the diffuse interstellar medium, A&A, 391, 675, 2002.

Guainazzi, M., The formerly X-ray reflection-dominatedSeyfert 2 galaxy NGC6300, MNRAS, 329, L13, 2002.

Guainazzi, M., Matt, G., Fiore, F., Perola, G.C., ThePhoenix galaxy: UGC4203 re-birth from its ashes,A&A, 388, 787, 2002.

Hartog, R. den, Kozorezov, A., Wigmore, J.K., Martin,D., Verhoeve, P., Peacock, A., Poelaert, A.,Brammertz, G., Quasiparticle diffusion and the energyresolution of superconducting tunneling junctions asphoton detectors. II. Experiment, Physical Review B,66 094511, 1, 2002.

Hasinger, G., Schartel, N., Komossa, S., Discovery of anionised Fe-K edge in the z3.91 Broad Absorption LineQSO APM 08279+5255, ApJ, 573, L77, 2002.

Haubold, H.J., Wamsteker, W., Report on the TenthUN/ESA Workshop on Basic Space Science:Exploring the Universe-Sky, Space Exploration, andSpace Technologies, Ap&SS, 282, 341, 2002.

Heras, A.M., Shipman, R.F., Price, S.D., de Graauw, T.,Walker, H.J., Jourdain de Muizon, M., Kessler, M.F.,Prusti, T., Decin, L., Vandenbussche, B., Waters,L.B.F.M., Infrared spectral classification of normalstars, A&A, 394, 539, 2002.

Hoogzaad, S.N., Molster, F.J., Dominik, C., Waters,L.B.F.M., Barlow, M.J., de Koter, A., Thecircumstellar dust shell of the post-AGB starHD161796, A&A, 389, 547, 2002.

in ‘t Zand, J.J.M, Miller, J.M., Oosterbroek, T., Parmar,A.N., Broad-band X-ray measurements of the blackhole candidate XTE J1908+094, A&A, 394, 553, 2002.

Israel, G.L, Covino, S., Stella, L., Campana, S., Marconi,G., Mereghetti, S., Mignani, R., Negueruela, I.,Oosterbroek, T., Parmar, A.N., Angelini, L., Thedetection of variability from the candidate IRcounterpart to the anomalous X-ray pulsar 1E1048.1-5937, ApJ, 580, L143, 2002.

Juvela, M., Mattila, K., Lehtinen, K., Lemke, D.,Laureijs, R., Prusti, T., Far-infrared and molecular lineobservations of Lynds L183-studies of cold gas anddust, A&A, 382, 583, 2002.

Kozorezov, A., Wigmore, J.K., den Hartog, R., Martin,D., Verhoeve, P., Peacock, A., Quasiparticle diffusionand the energy resolution of superconductingtunneling junctions as photon detectors. I. Theory,Physical Review B, 66 094510, 1, 2002.

Laureijs, R.J., Jourdain de Muizon, M., Leech, K.,Siebenmorgen, R., Dominik, C., Habing, H.J., Trams,N., Kessler, M., A 25 micron search for Vega-likedisks around main-sequence stars with ISO, A&A,387, 285, 2002.

Leech, K.J., Saxton, R., Barr, P., Santos Lleo, M.,Jimenez Bailon, E., Diaz, R., Ghosh, K., Soundarara-japervmal, S., Optical to Far-IR observations of 3C446, PASA, 19, 152, 2002.

Lefloch, B., Cernicharo, J., Rodriguez, L.F., Miville-Deschenes, M.A., Cesarsky, D., Heras, A., The

Photoionization of a Star-Forming Core in the TrifidNebula, ApJ, 581, 335, 2002.

Lehner, N., Gry, C., Sembach, K.R., Hbrard, G., Chayer,P., Moos, H.W., Howk, J.C., Dsert, J.-M., DeuteriumAbundance toward WD 0621-376: Results from theFUSE Mission, ApJS, 140, 81, 2002.

Lewis, G.F., Carilli, C., Papadopoulos, P., Ivison, R.J.,Resolved nuclear CO(1-0) emission in APM08279+5255: gravitational lensing by a naked cusp?,MNRAS, 330, L15, 2002.

Lumb, D., Warwick, R., Page, M., DeLuca, A., X-raybackground measurements with XMM-Newton, A&A,389, 93, 2002.

Maceroni, C., Testa, V., Plez, B., Garcia-Lario, P.,D’Antona, F., Lithium during the AGB evolution inyoung open clusters of the Large Magellanic Cloud,A&A, 395, 179, 2002.

Masetti, N., Dal Fiume, D., Cuumano, G., Amati, L.,Bartolini, C., Del Sordo, S., Frontera, F., Guarnieri,A., Orlandini, M., Palazzi, E., Parmar, A.N., Piccioni,A., Santangelo, A., X-ray and optical monitoring ofthe peculiar X-ray source 4U 1700+24/V934 Her,A&A, 382, 104, 2002.

McConnell, M.L., Zdziarski, A. A., Bennett, K.,Bloemen, H., Collmar, W., Hermsen, W., Kuiper, L.,Paciesas, W., Phlips, B.F., Poutanen, J., Ryan, J.M.,Schonfelder, V., Steinle, H., Strong, A.W., The SoftGamma-Ray Spectral Variability of Cygnus X-1, ApJ,572, 984, 2002.

Mereghetti, S., Tiengo, A., Israel, G.L., The X-raySource at the Center of Cassiopeia A SupernovaRemnant, ApJ, 569, 275, 2002.

Miller, J.M., Fabian, A.C., Wijnands, R., Reynolds, C.S.,Ehle, M., Freyberg, M.J., van der Klis, M., Lewin,W.H.G., Sanchez-Fernandez, C., Castro-Tirado, A.J.,Evidence for spin and energy extraction in a galacticblack hole candidate: The XMM-Newton/EPIC-pnspectrum of XTEJ1650-500, ApJ, 570, L69, 2002.

Miroshnichenko, A.S., Bjorkman, K.S., Chentsov, E.L.,Klochkova, G., Manset, N., Garcia-Lario, P., PereaCalderon, J.V., Rudy, R.J., Lynch, D.K., Wilson, J.C.,Gandet, T.L., V669 Cep: A new binary system with aB(e) star, A&A, 388, 563, 2002.

Miroshnichenko, A.S., Bjorkman, K.S., Chentsov, E.L.,Klochkova, V.G., Ezhkova, O.V., Gray, R.O., Garcia-Lario, P., Perea Calderon, J.V., Rudy, R.J., Lynch,D.K., Mazuk, S., Venturini,C.C., Puetter, R., Theluminous B(e) binary AS 381, A&A, 383, 171, 2002.

Molendi, S., De Grandi, S., Guainazzi, M., A BeppoSAXview of the Centaurus Cluster, A&A, 392, 13, 2002.

Moos, H.W., Sembach, K.R., Vidal-Madjar, A., York, D.G., Friedman, S.D., Hbrard, G., Kruk, J.W., Lehner,N., Lemoine, M., Sonneborn, G., Wood, B.E., Ake,T.B., Andr, M., Blair, W.P., Chayer, P., Gry, C.,Dupree, A.K., Ferlet, R., Feldman, P.D., Green, J.C.,Howk, J.C., Hutchings, J.B., Jenkins, E.B., Linsky,J.L., Murphy, E.M., Oegerle, W.R., Oliveira, C., Roth,K., Sahnow, D.J., Savage, B.D., Shull, J.M., Tripp,T.M., Weiler, E.J., Welsh, B.Y., Wilkinson, E.,

sp1247s4.qxd 3/5/03 3:59 PM Page 137

138 publications

Woodgate, B.E., Abundances of Deuterium, Nitrogen,and Oxygen in the Local Interstellar Medium:Overview of First Results from the FUSE Mission,ApJS, 140, 3, 2002.

O’Halloran, B., Metcalfe, L., McBreen, B., Laureijs, R.,Leech, K., Delaney, M., Watson, D., Hanlon, L.,Infrared Space Observatory Observations of HicksonCompact Group 31 with the Central Wolf-RayetGalaxy NGC 1741, ApJ, 575, 747, 2002.

Owens, A., Andersson, H., Bavdaz, M., van den Berg, L.,Peacock, A., Puig, A., The hard X-ray response of alarge area HgI2 detector, NIM-A, 487, 90, 2002.

Owens, A., Bavdaz, M., Andersson, H., Gagliardi, T.,Krumrey, M., Nenonen, S., Peacock, A., Taylor, I.,Troeger, L., The X-ray response of CdZnTe, NIM-A,484, 242, 2002.

Owens, A., Bavdaz, M., Brammertz, G., Krumrey, M.,Martin, D., Peacock, A., Troeger, L., The Hard X-rayresponse of HgI2, NIM-A, 479, 535, 2002.

Owens, A., Bavdaz, M., Peacock, A., Andersson, H.,Nenonen, S., Krumrey, M., Puig, A., High resolutionX-ray spectroscopy using a GaAs pixel detector,NIM-A, 479, 531, 2002.

Owens, A., Fraser, G., McCarthy, K., On the experi-mental determination of the Fano factor in Si at softX-ray wavelengths, NIM-A, 491, 437, 2002.

Owens, A., Peacock, A., Bavdaz, M., Brammertz, G.,Dubecky, F., Gostilo, V., Gryaznov, D., Haack, N.,Krumrey, M., Loupilov, A., The X-ray response ofInP: Part B, synchrotron radiation measurements,NIM-A, 491, 444, 2002.

Papadopoulos, P.P., Ivison, R.J., Low-Excitation Gas inHR 10: Possible Implications for Estimates of Metal-rich H2 Mass at High Redshifts, ApJ, 564, L9, 2002.

Papadopoulos, P.P., Thi, W.-F., Viti, S., Molecular Gas inSpiral Galaxies: A New Warm Phase at LargeGalactocentric Distances?, ApJ, 579, 270, 2002.

Parmar, A.N., Oosterbroek, T., Boirin, L., Lumb, D.,Discovery of narrow X-ray absorption features fromthe dipping low-mass X-ray binary X 1624-490 withXMM-Newton, A&A, 386, 910, 2002.

Perola, G.C., Matt, G., Cappi, M., Fiore, F., Guainazzi, M.,Maraschi, L., Petrucci, P.O., Piro, L., Compton reflec-tion and iron fluorescence in BeppoSAX observationsof Seyfert 1 type galaxies, A&A, 389, 802, 2002.

Reeves, J.N., Watson, D., Osborne, J.P., Pounds, K.A.,O’Brien, P.T.O., Short, A.D.T., Turner, M.J.L.,Watson, M.G., Mason, K.O., Ehle, M., Schartel, N.,The signature of supernova ejecta in the X-rayafterglow of the gamma-ray burst 011211, Nature,416, 512, 2002.

Roueff, E., Felenbok, P., Black, J. H., Gry, C., InterstellarC3 toward HD 210121, A&A, 384, 629, 2002.

Schulz, B., Huth, S., Laureijs, R.J., Acosta-Pulido, J.A.,Braun, M., Castaneda, H.O., Cornwall, L., Gabriel, C.,Hammersley, P., Heinrichsen, I., Klaas, U., Lemke,D., Mueller, T., Osip, D., Roman-Fernandez, P.,Telesco, C., ISOPHOT – Photometric Calibration ofPoint Sources, A&A, 381, 1110, 2002.

Sidoli, L., Parmar, A.N., Oosterbroek, T., Lumb, D.,Discovery of narrow X-ray absorption features fromthe bright low-mass X-ray binary GX 13+1 withXMM-Newton, A&A, 385, 940, 2002.

Vandenbussche, B., Beintema, D., de Graauw, T., Decin,L., Feuchtgruber, H., Heras, A.M., Kester, D., Lahuis,F., Lenorzer, A., Lorente, R., Morris, P., Salama, A.,Waelkens, C., Waters, L., Wieprecht, E., The ISO-SWS post-helium atlas of near-infrared stellar spectra,A&A, 390, 1033, 2002.

Verhoeve, P., den Hartog, R., Kozorezov, A., Martin, D.,van Dordrecht, A., Wigmore, J., Peacock, A., Timedependence of tunnel statistics and the energyresolution of superconducting tunnel junctions,J. App. Phys., 92, 6072, 2002.

Vio, R., Andreani, P., Tenorio, L., Wamsteker, W.,Numerical Simulation of Non-Gaussian RandomFields with Prescribed Marginal Distributions andCross-Correlation Structure II: Multivariate RandomFields, PASP, 114, 1281, 2002.

Vio, R., Tenorio, L., Wamsteker, W., On Optimal Detec-tion of Point Sources in CMB Maps, A&A, 391, 789,2002.

Vio, R., Wamsteker, W., Joint Time-Frequency Analysis:A tool for Exploratory Analysis and Filtering of TimeSeries, A&A, 388, 1124, 2002.

Watson, D., Reeves, J.N., Osborne, J., O’Brien, P.T.,Pounds, K.A., Tedds, J.A., Santos-Lleo, M., Ehle, M.,The X-ray afterglows of gamma-ray bursts GRB001025A and GRB 010220 observed with XMM-Newton, A&A, 393, L1, 2002.

Watson, D., Reeves, J.N., Osborne, J.P., Tedds, J.A.,O’Brien, P.T., Tomas, L., Ehle, M., The X-ray after-glow of GRB 020322, A&A, 395, L41, 2002.

Wijnands, R., Guainazzi, M., van der Klis, M., Mendez,M., XMM-Newton observations of the neutron starX-ray transient KS1731-260 in quiescence, ApJ, 573,L45, 2002.

Zane, S., Haberl, F., Cropper, M., Zlavin, V., Lumb, D.,Sembay, S., Motch, C., Timing analysis of isolatedneutron star RXJ0720-3125, MNRAS, 334, 345, 2002.

Zhang, S., Collmar, W., Bennett, K., Bloemen, J.B.G.M.,Hermsen, W., McConnell, M., Reimer, O., Schon-felder, V., Wagner, S.J., Williams, O.R., COMPTELobservations of the gamma-ray blazar PKS 1622-297,A&A, 386, 843, 2002.



Andernach, H., Slee, O., Roy, A., Ehle, M., ExtremeRelic Radio Sources in Four Southern Clusters, A.Pramesh Rao, G. Swarup, Gopal Krisna (eds.), inProc. IAU Symposium 199: The Universe at LowRadio Frequencies, ASP, 153, 2002.

sp1247s4.qxd 3/5/03 3:59 PM Page 138

publications 139

Bavdaz, M., Peacock, A., Beijersbergen, M., Parmar, A.,Development of X-ray optics at ESA, Proc. SPIE,4496, 94, 2002.

Bavdaz, M., Peacock, A., Parmar, A., Beijersbergen, M.,The XEUS mission and Instruments, Proc. SPIE,4497, 31, 2002.

Brammertz, G., Peacock, A., Verhoeve, P., Kozorezov, A.,den Hartog, R., Rando, N., Venn, R., Strong Quasi-particle Trapping in a 6x6 Array of Vanadium-Aluminum Superconducting Tunnel Junctions, F.S.Porter, D. McCammon, M. Galeazzi, C. Stahle (eds.) inProc. 9th International Workshop on Low TemperatureDetection, AIP Conference Proceedings, 605, 59, 2002.

Bruijne, J. de, Reynolds, A., Perryman, M.A.C., Favata,F., Peacock, A., Analysis of astronomical data fromoptical superconducting tunnel junctions, Ninkov, Zand Forrest, W. (eds.), in Focal plane detector arraydevelopments, SPIE, 41(6), 1158, 2002.

Ehle, M., Beck, R., Shoutenkov, V., Harnett, J.I., Haynes,R.F., Shukurov, A., Sokoloff, D.D., Thierbach, M.,The magnetic fields of barred spiral galaxies, JessicaChapman (ATNF) (eds.), in Australia TelecopeNational Facility Annual Report 2001, Pirie PrintersPty Ltd., Canberra, 26, 2002.

Ehle, M., Harnett, J.I., Beck, R., Haynes, R.F., Gray, A.,Magnetic fields in barred spiral galaxies: NGC 2442& NGC 7552, E. Athanassoula, A. Bosma (eds.), inDisks of Galaxies: Kinematics, Dynamics andPerturbations ASP Conference Series, 275, 361, 2002.

Favata, F., Large stellar flares: a review of recent novelresults, F. Favata & J.J. Drake (eds.), in Stellarcoronae in the Chandra and XMM-Newton era, ASPConference Series, 277, 115, 2002.

Favata, F., Future space missions relevant for theunderstanding of the evolving Sun and its influence onplanetary environments, B. Montesinos, A. Gimenez(eds.), in The evolving Sun and its influence onplanetary environments, ASP Conference Series, 269,353, 2002.

Favata, F., The Eddington baseline mission, F. Favata,I.W. Roxburgh, D. Galadi (eds.), in The 1st EddingtonWorkshop, ESA SP-485, 3, 2002.

Favata, F., Aigrain, S., Activity science with data fromthe upcoming generation of space-based high-accuracy photometric data, Astron. Nachrichten, 323,283, 2002.

Favata, F., Fridlund, C.V.M., Micela, G., Sciortino, S.,Kaas, A.A., Discovery of X-ray emission from theproto-stellar jet L1551 IRS5 (HH 154), F. Favata & J.Drake (eds.), in Stellar Coronae in the Chandra andXMM Era, ASP Conference Series, 277, 467, 2002.

Fosalba, P., Lazarian, A., Prunet, S., Tauber, J.A, DustPolarization from Starlight Data, S. Cecchini, S.Cortiglioni, R. Sault, C. Sbarra (eds.), in AstrophysicalPolarized Backgrounds, AIP Conference Proceedings,609, 44, 2002.

Fraser, G.W., Brunton, A.N., Bannister, N.P., Pearson,J.F., Ward, M.J., Stevenson, T., Watson, D.J.,Warwick, B., Whitehead, S., O’Brien, P.T.O., White,

N., Jahoda, K., Black, K., Hunter, S.D., Deines-Jones,P., Priedhorsky, W., Brumby, S.P., Borodzon, K.N.,Vestrand, T., Fabian, A.C., Nugent, K., Peele, A., Irv-ing, T.H., Price, S., Eckersley, S., Renouf, I., Smith, M.,Parmar, A., McHardy, I.M., Uttley, P., Lawrence, A.,Lobster-ISS: An Imaging X-ray All-Sky Monitor forthe International Space Station, Proc. SPIE, 4497, 115,2002.

Fridlund, M., The Darwin mission and exo-planets, F.Favata, I. Roxburgh, D. Galadi (eds.), in The FirstEddington Workshop, ESA SP-485, 235, 2002.

Gondoin, P., Barr, P., Lumb, D., Oosterbroek, T., Orr, A.,Parmar, A., A Simultaneous XMM-Newton andBeppoSAX observation of the Seyfert Galaxy IC4329A, Workshop on X-ray Spectroscopy of AGN withChandra and XMM-Newton, MPE Report, 279, 283,2002.

Guainazzi, M., Stanghellini, C., Grandi, P., TheCompton-thick AGN in the GPS radio sourceOQ+208, Boller, Hasinger & Parmar (eds.), in XEUSWorkshop Proceedings, MPE Report, 281, 261, 2002.

Hartog, R. den, Kozorezov, A.G., Wigmore, J.K.,Verhoeve, P., Martin, D., Peacock, A., QuasiparticleDiffusion and Energy Resolution in SuperconductingTunneling Junctions, F.S. Porter, D. McCammon, M.Galeazzi, C. Stahle (eds.) in Proc. 9th InternationalWorkshop on Low Temperature Detection, AIP Conf.Proc., 605, 35, 2002.

Hartog, R. den, Kozorezov, A., Martin, D., Brammertz,G., Verhoeve, P., Peacock, A., Scholze, F., Goldie,D.J., Large-Format Distributed Read-Out ImagingDevices for X-ray Imaging Spectroscopy, F.S. Porter,D. McCammon, M. Galeazzi, C. Stahle (eds.) in Proc.9th International Workshop on Low TemperatureDetection, AIP Conf. Proc., 605, 11, 2002.

Hartog, R. den, Kozorezov, A., Martin, D., Brammertz,G., Verhoeve, P., Peacock, A., Scholze, F., Goldie,D.J., Large-Format Distributed Read-Out ImagingDevices for X-ray Imaging Spectroscopy, Proc. SPIE,4497, 50, 2002.

Kozorezov, A., Wigmore, J., Peacock, A., den Hartog, R.,Brammertz, G., Martin, D., Verhoeve, P., Rando, N.,Self-Heating Phenomena in SuperconductingTunnelling Junctions, F.S. Porter, D. McCammon, M.Galeazzi, C. Stahle (eds.) in Proc. 9th InternationalWorkshop on Low Temperature Detection, AIP Conf.Proc., 605, 51, 2002.

Manchado, A., Dominguez-Tagle, C., Garcia-Hernandez,A., Prada, F., Garcia-Lario, P., Conway, G., The onsetof photoionization in post-AGB stars, in Serie deconferencias, Rev. Mexicana de Astronomia yAstrofisica, Mexico, 12, 157, 2002.

Marty, P., Schulz, J., Netopil, J., Nowotny, W., Bayer, C.,Carr, M., Ferrigno, C., Fritz, A., Jean, C., Koprolin,W., Rasmussen, J., Tanvuia, L., Valtchanov, I., Much,R., Parmar, A.N., in XS: project for a futurespaceborne hard X-ray survey, Proc. SPIE, 4497, 1,2002.

Padovani, P., Blazar Surveys, P. Giommi, E. Massaro, G.

sp1247s4.qxd 3/5/03 3:59 PM Page 139

140 publications

Palumbo (eds.), in Blazar Astrophysics withBeppoSAX and other Observatories, Agenzia SpazialeItaliana, Frascati, 101, 2002.

Parmar, A., Gianfiglio, G., Schiemann, J., High-EnergyAstronomy with the International Space Station, ESABulletin, 110, 49, 2002.

Perryman, M.A.C., GAIA and Eddington, Favata, F. et al.(eds.), in First Eddington Workshop, ESA SP-485,229, 2002.

Perryman, M.A.C., GAIA: An Astrometric andPhotometric Survey of our Galaxy, Vansevicius, V.and Hoeg, E. (eds.), in GAIA Photometry Workshop,Ap&SS, 280, 1, 2002.

Prusti, T., Natta, A., Mid Infrared Variability of HerbigAe/Be Stars, J. Alves & M. McCaughrean (eds.), inProc. The Origins of Stars and Planets: the VLT View,ESO, Garching, 351, 2002.

Riera, A., Garcia-Lario, P., Manchado, A., Bobrowsky,M., Estalella, R., New Observations of the High-Velocity Outflows of the Proto-Planetary Nebula HEN3-1475, Serie de conferencias, Rev. Mexicana deAstronomia y Astrofisica, 13, 127, 2002.

Sandri, M., Villa, F., Bersanelli, M., Butler, R.,Mandolesi, N., Tauber, J., Advanced simulationtechniques for straylight prediction of highperformance mm-wave reflecting telescope, L.Fanchi, K. van 't Klooster (eds.), in Proc. ESAAntenna Workshop on Satellite Antenna Technology,ESA WPP-202, 641, 2002.

Thompson, M., White, G., Miao, J., Fridlund, M., Huldt-gren, M., Induced Star Formation Near HII Regions:the Fate of Three Clouds in IC 1848, P. Crowther(eds.) in Hot Star Workshop II: The Earliest Stages ofMassive Star Birth, ASP Conf. Proc., 267, 431, 2002.

Verhoeve, P., Superconducting Tunnel JunctionDetectors for Ground-based Optical astronomy andSpace-based UV and X-ray Astrophysics, F.S. Porter,D. McCammon, M. Galeazzi, C. Stahle (eds.) in Proc.9th International Workshop on Low TemperatureDetection, AIP Conf. Proc., 605, 559, 2002.

Villa, F., Sandri, M., Bersanelli, M., Butler, R.,Mandolesi, N., Marti-Canales, J., Tauber, J.,Planck/LFI: an advanced multi-beam highperformance mm-wave optics for space applications,L. Fanchi, K. van 't Klooster (eds.), in Proc. ESAAntenna Workshop on Satellite Antenna Technology,ESA WPP-202, 277, 2002.

White, G., Nelson, R., Huldtgren White, M., Fridlund,M., Liseau, R., Miao, J., Thompson, M., An Overviewof Induced Star Formation near the Surfaces ofMolecular Clouds, J. Alves & M. McCaughrean(eds.), in Proc. The Origins of Stars and Planets: theVLT View, ESO, Garching, 232, 2002.

Winkler, C., Barr, P., Hansson, L., Much, R., Orr, A.,Parmar, A., The Integral Science, ESA Bulletin, 111,73, 2002.

Wright, C.M., Aitken, D.K., Smith, C.H., Roche, P.F.,Laureijs, R.J., The Mineralogy and Magnetism of Starand Planet Formation as Revealed by Mid-Infrared

Spectropolarimetry, J. Alves & M. McCaughrean(eds.), in Proc. The Origins of Stars and Planets: theVLT View, ESO, Garching, 85, 2002.

sp1247s4.qxd 3/5/03 3:59 PM Page 140

publications 141

Space Telescope Operations DivisionRefereed Journals, 2001

Albrecht, R., Maitzen, H.-M., Schnell, A., Early AsteroidResearch in Vienna, in: Asteroids, Meteorites, Impactsand their Consequences, Jessberger, E.K., Albrecht,R., Miller, H., Schieber, M. (editors), Planet. andSpace Sci., 49 (8), 777, 2001.

Andreuzzi, G., De Marchi, G., Ferraro, F., Paresce, F.,Pulone, L., Buonanno, R., VLT observations of thepeculiar globular cluster NGC6712. II. Luminosityand mass functions, A&A, 372, 851, 2001.

Arribas, S., Colina, L., Clements, D. Two-dimensionalKinematical and Ionization Structure of the Warm Gasin the Nuclear Regions of Arp 220, ApJ, 560, 160,2001.

Arnouts, S., Vandame, B., Benoist, C., Groenewegen,M.A.T., da Costa, L., Schirmer, M., Mignani, R.P.,Slijkhuis, R., Hatziminaoglou, E., Hook, R., Madej-sky, R., Rite, C., & Wicenec, A., ESO imaging survey.Deep public survey: Multi-color optical data for theChandra Deep Field South, A&A, 379, 740, 2001.

Bacon, R., Copin, Y., Monnet, G., et al. (incl. Kunt-schner, H.), The SAURON project: I. The panoramicintegral-field unit, MNRAS, 326, 23, 2001.

Blum, R.D., Schaerer, D., Pasquali, A., Heydari-Malayeri, M., Conti, P.S., Schmutz, W., 2 MicronNarrowband Adaptive Optics Imaging in the ArchesCluster, AJ, 122, 1875, 2001.

Boker, T., Bacinski, J., Bergeron, L.E., Calzetti, D.,Jones, M., Gilmore, D., Holfeltz, S., Monroe, B.,Nota, Sosey, M., Schneider, G., O’Neil, E., Hubbard,P., Ferro, A., Barg, I., Stobie, E. Properties of PACE-IHgCdTe Detectors in Space: the NICMOS Warm-upMonitoring Program, PASP, 113, 859, 2001.

Boker, T., Laine, S., van der Marel, R.P., Sarzi, M., Rix,H.-W., Ho, L.C., Shields, J.C. An HST Census ofNuclear Star Clusters in Late-Type Spiral Galaxies: I.Observations and Image Analysis, AJ, 123, 1389.

Boker, T., van der Marel, R.P., Mazzuca, L., Rix, H.-W.,Rudnick, G., Ho, L.C., Shields, J.C. A Young StellarCluster in the Nucleus of NGC 4449, AJ, 121, 1473,2001.

Celotti, A., Ghisellini, G., Chiaberge, M. Large-scale jetsin active galactic nuclei: multiwavelength mapping,MNRAS, 321, L1, 2001.

Chiaberge, M., Capetti, A., Celotti, A. The BL Lac heartof Centaurus A, MNRAS, 324, L33, 2001.

Colina, L., Alberdi, A., Torrelles, J.M., Panagia, N.,Wilson, A.S., Discovery of a Bright Radio Supernovain the Circumnuclear Starburst of the LuminousInfrared Seyfert 1 Galaxy NGC 7469, ApJ, 553, L19,2001.

Colina, L., Arribas, S., Borne, K.D. `ULIRGs: Tidal-induced Star Formation and Implications for SCUBASources, ApSSS, 277, 413, 2001.

Costamante, L., Ghisellini, G., Giommi, P. et al. Extremesynchrotron BL Lac objects. Stretching the blazarsequence, A&A, 371, 512, 2001.

del Burgo, C., Peletier, R.F., Vazdekis, A., Arribas, S.,Mediavilla, E. A detailed two-dimensional stellarpopulation study of M32, MNRAS, 321, 227, 2001.

de Mello, D.F., Pasquali, A., A close look into anintermediate redshift galaxy using STIS, A&A, 378,L10, 2001.

GarcÍa-Lorenzo, B., Arribas, S., Mediavilla, E. IntegralField Spectroscopy of Active Galaxies, ApSSS, 277,459, 2001.

García-Lorenzo, B., Arribas, S., Mediavilla, E. Stellarand ionized gas kinematics of the interacting Seyfert1.9 galaxy NGC 2992, A&A, 378, 787, 2001.

Gerald, M.S., Bernstein, J., Hinkson, R., Fosbury, R.A.E.Formal method for objective assessment of primatecolor. Am. J. Primatol., 53(2), 79-85; A&A, 378, 787,2001.

Goldhaber, G., Panagia, N., et al., Timescale StretchParameterization of Type Ia Supernova B-band LightCurves, ApJ, 558, 359, 2001.

Goudfrooij, P., Mack, J., Kissler-Patig, M., Meylan, G.,Minniti, D., Kinematics, Ages and Metallicities ofStar Clusters in NGC~1316: a 3-Gyr-old mergerremnant. MNRAS, 322, 643-657, 2001.

Halliday, C., Davies, R.L., Kuntschner, H., et al., Line-of-sight velocity distributions of low luminosityelliptical galaxies, MNRAS, 326, 473, 2001.

Heydari-Malayeri, M., Charmandaris, V., Deharveng, L.,Rosa, M.R., Schaerer, D., Zinnecker, H., HSTobservations of the LMC compact H II region N 11A,A&A, 372, 527, 2001.

Heydari-Malayeri, M., Charmandaris, V., Deharveng, L.,Rosa, M.R., Schaerer, D., Zinnecker, H., HST study ofthe LMC compact star-forming region N 83B, A&A372, 495, 2001.

Holden, B.P., Stanford, S.A., Rosati, P., Squires, G., Tozzi,P., Fosbury, R.A.E., Papovich, C., Eisenhardt, P.,Elston, R., Spinrad, H., RX J0848+4456: Disentanglinga moderate redshift cluster, AJ, 122, 629, 2001.

Jessberger, E.K., Albrecht, R., Miller, H., Schieber, M.(eds), Special Issue: Asteroids, Meteorites, Impactsand their Consequences, Planet. and Space Sci., 49(8), 2001.

Kerber, F., Sakurai’s Object (V4334 Sgr) The evolutionof a final helium flash star, Ap&SS 275, 91.

Krabbe, A., Boker, T., Maiolino, R. N-Band Imaging ofSeyfert Nuclei and the Mid-Infrared X-ray correlation,ApJ, 557, 626, 2001.

Kuntschner, H., Lucey, J.R., Smith, R.J., Hudson, M.J.,Davies, R.L., On the dependence of spectroscopicindices of early-type galaxies on age, metallicity andvelocity dispersion, MNRAS, 323, 615, 2001.

Lamers, H.J.G.L.M., Nota, A., Panagia, N., Smith, L.J.,Langer, N., Chemical Composition and Origin ofNebulae around Luminous Blue Variables, ApJ, 551,764, 2001.

H. Landt, P. Padovani, E.S. Perlman, P. Giommi, H.Bignall, A. Tzioumis, The Deep X-ray Radio BlazarSurvey (DXRBS). II. New Identifications, MNRAS,323, 757, 2001.

sp1247s4.qxd 3/5/03 3:59 PM Page 141

142 publications

Lentz, E.J., Baron, E., Branch, D., Hauschildt, P.H.,Fransson, C., Lundqvist, P., Garnavich, P., Bastian, N.,Filippenko, A.V., Kirshner, R.P., Challis, P., Jha, S.,Chevalier, R., Leibundgut, B., McCray, R., Michael,E., Panagia, N., Phillips, M., Pun, J., Schmidt, B.,Sonneborn, G., Suntzeff, N., Wang, L.F., R.V.,Wheeler, J.C., Analysis of the Type IIn Supernova1998S, Effects of Circumstellar Interaction onObserved Spectra, ApJ, 547, 406, 2001.

Markova, N., Scuderi, S., de Groot, M., Markov, H.,Panagia, N., Simultaneous Halpha and PhotometricObservations of P Cygni, A&A, 366, 935, 2001.

Maíz-Apellániz, J. Structural properties of massiveyoung clusters, ApJ, 563, 151, 2001.

Maíz-Apellániz, J., The Spatial Distribution of O-B5Stars in the Solar Neighborhood as Measured byHipparcos, AJ, 121, 2737, 2001.

Maíz-Apellániz, J., The origin of the Local Bubble,ApJL, 560, 83, 2001.

Meylan, G., Sarajedini, A., Jablonka, P., Djorgovski,S.G., Bridges, T., Rich, R.M., Mayall~II ≈ G1 in M31:Giant Globular Cluster or Core of a Dwarf EllipticalGalaxy?, AJ, 122, 830-841, 2001.

Padovani, P.L. Costamante, P., Giommi, G., Ghisellini,A., Comastri, A., Wolter, L., Maraschi, G., Tagliaferri,C.M. Urry, BeppoSAX Observations of 1 Jy BLLacertae Objects. I, MNRAS, 328, 931, 2001.

Paltrinieri, B., Ferraro, F., Paresce, F., De Marchi, G.VLT observations of the peculiar globular clusterNGC6712. III. The evolved stellar population, AJ,121, 3114, 2001.

Pentericci, L, McCarthy, P.J., Roettgering, H, Miley,G.K., van Breugel, W.J.M., Fosbury, R.A.E.,NICMOS observations of high redshift radio galaxies:witnessing the formation of bright elliptical galaxies?,ApJS, 135, 63, 2001.

Pirzkal, N., Collodel, L., Erben, T., Fosbury, R.A.E.,Freudling, W., Haemmerle, H., Jain, B., Micol, A.,Miralles, J.-M., Schneider, P., Seitz, S., White,S.D.M., Cosmic shear from STIS Pure Parallels: IData, A&A, 375, 351, 2001.

Rajagopal, J., Boker, T., Allen, R.J. The Confusion Limiton Astrometry with the Space Interferometry Mission,PASP, 113, 1232, 2001.

Saha, A., Sandage, A., Tammann, G.A., Dolphin, A.E.,Christensen, J., Panagia, N., Macchetto, F.D., CepheidCalibration of the Peak Brightness of SNe Ia - XI, SN1998aq in NGC 3982, ApJ, 562, 314, 2001.

Saha, A., Sandage, A., Thim, F., Tammann, G.A., Lab-hardt, L., Christensen, J., Macchetto, F.D., Panagia,N., Cepheid Calibration of the Peak Brightness of SNeIa - X, SN 1991T in NGC 4527, ApJ, 551, 973, 2001.

Sahu, K.C., Casertano, S., Livio, M., Gilliland, R.L.,Panagia, N., Potter, M., Gravitational Microlensing byLow Mass Objects in the Globular Cluster M22,Nature, 411, 1022, 2001.

Smail, I., Kuntschner, H., Kodama, T., Smith, G.P.,Packham, C., Fruchter, A. S., Hook, R.N., Aphotometric study of the ages and metallicities of

early-type galaxies in A 2218, MNRAS, 323, 839,2001.

Stiavelli, M., Scarlata, C., Panagia, N., Treu, T., Bertin,G., Bertola, F., Lyman-alpha Emitters with Red Colorsat z~2.4, ApJ, 561, L37, 2001.

Tagliaferri, G., Ghisellini, G., Giommi, P. et al., The 0.1-200 keV spectrum of the blazar PKS 2005-489 duringan active state, A&A, 368, 38, 2001.

Vazdekis, A., Kuntschner, H., Davies, R. L., et al., On theorigin of the colour magnitude relation in Virgo, ApJL,551, L127, 2001.

Vernet, J., Fosbury, R.A.E., Villar-Martin, M., Cohen,M.H., Cimatti, A., di Serego Alighieri, S., Goodrich,R.W., Radio Galaxies at z~2.5: results from Keckspectropolarimetry, A&A, 366, 7, 2001.

Weaver, H.A., Sekanina, Z., Toth, I., Delahodde, C.E.,Hainaut, O.R., Lamy, P.L., Bauer, J.M., A’Hearn,M.F., Arpigny, C., Combi, M.R., Davies, J.K.,Feldman, P.D., Festou, M.C., Hook, R., Jorda, L.,Keesey, M.S.W., Lisse, C.M., Marsden, B.G., Meech,K.J., Tozzi, G.P., West, R., HST and VLTInvestigations of the Fragments of Comet C/1999 S4(LINEAR), Science, 292, 1329, 2001.

Weiler, K.W., Panagia, N., Montes, M.J., SN1998bw/GRB 980425 and Radio Supernovae, ApJ,562, 670, 2001.

Space Telescope Operations DivisionProceedings and other Publications, 2001

Aldering, G.R. Amanullah, P. Antilogus, P. Astier, C.Balland, G. Blanc, M.S. Burns, A. Conley, S.E.Deustua, R. Ellis, S. Fabbro, G. Folatelli, A.S.Fruchter, G. Garavini, R. Gibbons, G. Goldhaber,A. Goobar, D.E. Groom, D. Hardin, I. Hook, D.A.Howell, M. Irwin, A. G. Kim, R.A. Knop, J.M. Levy,C. Lidman, R. McMahon, J. Mendez, M. Mouchet, S.Nobili, P.E. Nugent, R. Pain, Panagia, N., E. Pecontal,C.R. Pennypacker, S. Perlmutter, J. Raux, N.Regnault, P. Ruiz-Lapuente, N.A. Walton, L. Wang,W.M. Wood-Vasey, Supernovae, I.A.U. Circ. 7740,2001.

Alexov, A., Bristow, P., Kerber, F., Rosa, M.R., STPOA– The New Pipeline Package for the HST Post-Operational Archive, ADASS 10, F.R. Harnden, F.A.Primini and H.E. Payne, eds, ASP Conf. Series 238,178, 2001.

Andreuzzi, G., Paresce, F., De Marchi, G., Ferraro, F.,Pulone, L., Buonanno, R., Deep luminosity functionof NGC 6712, Mem. S.A. It., 72, 693, 2001.

Arribas, S., Jakobsen, P., Fosbury, R., Freudling, W.Effects of Facet, Pixel, and Slit Dimensions on thePerformance of a MEMS Type Spectrograph forNGST, AAS Meeting 199, #08.07, 2001.

Beckwith, S., Riess, A., Boffi, F., Casertano, S., Doxsey,R., Ferguson, H., Fruchter, A., Giavalisco, M.,Gilliland, R., Griffin, I., Koekemoer, A., Livio, M.,Margon, B., Meylan, G., Panagia, N., Platais, V.,

sp1247s4.qxd 3/5/03 3:59 PM Page 142

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Sahu, K., Soderblom, D., Supernova 1998ff inAnonymous Galaxy, I.A.U. Circ. 7740, 2001.

Benítez, N., Maíz-Apellániz, J., Cañelles, M. Evidencefor nearby supernova explosions, AAS Meeting 199,#67.05, 2001.

Boffi, F.R., Panagia, N., Radio Emission of Supernovaein Binary Systems, in Young Supernova Remnants ed.S.S. Holt, U. Hwang, AIPCP 565, 73-76, Am. Inst.Phys., Melville, NY, USA, 2001.

Bristow, P.D., Phillipps, S., Modeling FaintMorphological Number Counts, in Proc.ESO/ECF/STScI Workshop Deep Fields, Eds. S.Cristiani, A. Renzini & R.E. Williams, SpringerVerlag, pp.150, 2001.

Bristow, P.D., Hook, R., Faint Galaxy Detection inDrizzled Data, ST-ECF Newsletter, 30, 11, 2001.

Bristow, P.D., Alexov, A., Kerber, F., Rosa, M.R.,Tracking FOS on-board GIMP in commanding, AEDPtelemetry and header contents (12/01), ST-ECFTechnical. Report, POA/FOS-2001-02, 2001.

Bristow, P.D., Alexov, A., Kerber, F., Rosa, M.R., POAAnalysis of FOS Flat Fields (12/01), ST-ECFTechnical. Report, POA/FOS-2001-03, 2001.

Burns, M.S., et al., Panagia, N., et al., NICMOSPhotometry of High Redshift Supernovae, BAAS, 33,1333, 2001.

Capetti, A., Chiaberge, M., Celotti, A. The HST view ofnearby radio-galaxies, Memorie della Societa Astro-nomica Italiana, 72, 101, 2001.

Chiaberge, M., Celotti, A., Capetti, A., Ghisellini, G. HSTobservations of FR I radiogalaxies, what do they tell usabout the BL Lac - FR I unification scheme?, Memoriedella Societa Astronomica Italiana, 72, 107, 2001.

Chiaberge, M., Celotti, A., Capetti, A., Ghisellini, G. TheHST View of the Nuclei of Radio Galaxies,Implications for the Radioloud AGN UnificationModels, ASP Conf.Ser. 227, Blazar Demographicsand Physics, 50, 2001.

Chiaberge, M., Macchetto, F.D., Sparks, W., Capetti, A.,Allen, M.G., Martel, A.R. The nuclei of 3CR radiogalaxies in the UV, AAS Meeting, 199, 2001.

Colina, L., Alberdi, A., Gonzalez-Delgado, R., Torrelles,J.M., Leitherer, C., Panagia, N., Wilson, A.S., Circum-nuclear Star Formation in Active Galaxies in TheCentral kpc of Starbursts and AGNs, eds. J.H.Knapen, J.E. Beckman, I. Shlosman, T.J. Mahoney,ASP Conf. Ser. 249, 119-125., 2001.

Colina, L., Alberdi, A., Torrelles, J.M., Panagia, N.,Wilson, A.S., Probable Radio Supernova in NGC7469, I.A.U. Circ. 7587, 2001.

Costamante, L., Ghisellini, G., Giommi, P. et al., NewExtreme Synchrotron BL Lac Objects, in X-rayAstronomy, Stellar Endpoints, AGN, and the DiffuseX-ray Background, AIP Conf. Proc. 599, 586, 2001.

Costamante, L., Ghisellini, G., Celotti, A. et al. Lookingfor high energy peaked blazars, Memorie della SocietaAstronomica Italiana, 72, 153, 2001.

Costamante, L., Ghisellini, G., A. Wolter, G. Tagliaferri,G. Fossati, P. Padovani, P. Giommi, BL Lacs at the

Blue End of the Blazar Sequence, in Blazar Demo-graphics and Physics, P. Padovani, C. M. Urry (eds.),ASP Conf. Series, 227, 135, 2001.

Cristiani, S. Arnouts, S., Fosbury, R.A.E., Parasitic Lightin NGST instruments: the accuracy of photometricredshifts and the effect of filter leaks in the visible andnear IR camera, ISR NGST 2001-01, 2001.

De Marchi, G., Li Causi, G., Paresce, F., Exposure timecalculators and the estimated SNR, BAAS, 199,157.02, 2001.

De Marchi, G., Paresce, F., The mass function of Galacticclusters and its evolution with time, AGM Abs. Ser.18, 05-51, 2001.

Dennefeld, M., Pasquali, A., Desert, J.M., McGroarty, F.,Marchi, S., Nirski, J., Supernova 2001da in NGC7780, IAU Circ. 7664, 2001.

Dolensky, M., Micol, A., Pierfederici, F., Pirenne, B.,New tools and methods to browse HST images andspectra, Proc. SPIE, 4477, 241, 2001.

Ellis, R.S., et al., Panagia, N., et al., Verifying the Use ofType Ia Supernovae as Probes of the CosmicExpansion, BAAS, 33, 1347, 2001.

Fosbury, R.A.E., Bergeron, J., Cesarsky, C., Cristiani, S.,Hook, R., Renzini, A. Rosati, P., The Great Observa-tories Origins Deep Survey (GOODS), in Messenger105, 40-41, 2001.

Fossati, G., Capalbi, M., Celotti, A., Chiaberge, M.,Zhang, Y.H., X-ray emission of Mkn 421 and jetmicrophysics, Memorie della Societa AstronomicaItaliana, 72, 127, 2001.

Fossati, G., Celotti, A., Chiaberge, M., Chiappetti, L.,Zhang, Y.H., BeppoSAX Observations of MKN 421,Clues on the Particle Acceleration?, AIP Conf. Proc.599, X-ray Astronomy, Stellar Endpoints, AGN, andthe Diffuse X-ray Background, 562, 2001.

Freudling, W., Arribas, S., Cristiani, S., Fosbury, R.,Jakobsen, P., Pirzkal, N., Confusion limits on Spectrataken with the Next generation Space Telescope Near-Infrared Multi-Object Spectrograph, AAS 199,#08.06, 2001.

Garnavich, P.M., SINS collaboration, Panagia, N., Echosof SN 1998bu, BAAS, 33, 1353, 2001.

Giommi, P., A. Pellizzoni, M. Perri, P. Padovani, TheCosmological Evolution of BL Lacertae Objects, inBlazar Demographics and Physics, P. Padovani, C.M.Urry (eds.), ASP Conf. Series, 227, 227, 2001.

Heydari-Malayeri, M., Charmandaris, V., Deharveng, L.,Rosa, M.R., Schaerer, D., Zinnecker, H., The youngestmassive stars in the Magellanic Clouds, in Proc. 17thIAP Astrophysics Colloquium, Eds. R. Ferlet, M.Lemoine, J.-M. Desert, B. Raban, Frontier Group,195, 2001.

Hook, R.N., Arnouts, S., Benoist, C., da Costa, L.,Mignani, R., Rite, C., Schirmer, M., Slijkhuis, R.,Vandame, B., Wicenec, A., The ESO Imaging SurveyProject: Status and Pipeline Software, in AstronomicalData Analysis Software and Systems X, ASP Conf.Proc., 238. Ed. F.R. Harnden, Jr., F.A. Primini, H.E.Payne, ASP, 283, 2001.

sp1247s4.qxd 3/5/03 3:59 PM Page 143

144 publications

Hook, R., SCISOFT – a collection of astronomical soft-ware for ESO users, ESO Messenger, 104, 20, 2001.

Jakobsen, P., Arribas, S., Burgarella, D., Caraveo, P.,Cornelisse, J., Davies, R., Ferrara, A., Fosbury, R.,Hjorth, J., Le Fevre, O., et al., The NGST Near-Infrared Spectrometer, The Science Case and MainDrivers, AAS Meeting 199, #08.05, 2001.

Kerber, F., Asplund, M., The star too tough to die, Sky &Telescope, 102 (5), 48, 2001.

Kerber, F., Rauch, T., Survey of Large Planetary Nebulaein Decay in Teton 4: Galactic Stucture, Stars and theInterstellar medium, ASP Conf. Ser. 231, Eds. C.E.Woodward. M.D. Bicay, J.M. Shull, 543, 2001.

Knop, R.A., et al., Panagia, N., et al., ΩM and Ωλ from 11HST-Observed Supernovae at z=0.36-0.86, BAAS, 33,1332, 2001.

Kuntschner, H., The Stellar Populations of Early-TypeGalaxies in the Fornax Cluster, Ap&SS, 276, 885,2001.

Landt, H., P. Padovani, E. Perlman, P. Giommi, TheEmission Line Properties of DXRBS Blazars, inBlazar Demographics and Physics', P. Padovani, C.M.Urry (eds.), ASP Conf. Series, 227, 73, 2001.

Maíz-Apellániz, J., Walborn, N.R., Massive youngclusters in nearby galaxies, in Galaxies and theirConstituents at the Highest Angular Resolutions,Proc. IAU Symposium #205, ed. R.T. Schilizzi, SanFrancisco, ASP, 222, 2001.

Maíz-Apellániz, J., An HST archival study of massiveyoung clusters, in Highlights of Spanish astrophysicsII, Proc. 4th Scientific Meeting of the Spanish Astron.Soc., ed. J. Zamorano, J. Gorgas, J. Gallego,Dordrecht, Kluwer Acad. Pubs, p.113, 2001.

Maíz-Apellániz, J., The Scorpius-Centaurus OB associa-tion and the origin of the Local Bubble, AAS Meeting199, #11.03, 2001.

Maíz-Apellániz, J., MacKenty, J.W., Norman, C.A.,Walborn, N.R. The spectacular warm ISM of NGC4214, in Tetons 4: Galactic Structure, Stars and theInterstellar Medium, ASP Conf. Ser., 231, ed. C.E.Woodward, M.D. Bicay, J.M. Shull, San Francisco,ASP, p.362, 2001.

Mediavilla, E., Arribas, S., Motta, V., Munoz, J.,Kochaneck, C., Falco, E. Extended C[III] & lambda,1909 Emission in Q0957+561 Galaxies, the ThirdDimension, ASP Conf. Ser. (Ed. M. Rosado, L.Binette, L. Arias), 2001.

Meylan G., Internal Dynamics of Globular Clusters,Observations, invited review in Stellar Dynamics,from Classic to Modern, Proc. St. PetersburgInternational Conf., eds. L.P. Ossipkov, I.I. Nikiforov,St. Petersburg, SPUP, pp.1-10, 2001.

Meylan, G., Magain P., Deconvolving Spectra, Near-IRSpectroscopy of the Lens and Source in HE 1104-1805, in International Astrophysics Conference onGravitational Lensing, Recent Progress and FutureGoals, eds. T.G. Brainerd, C.S. Kochanek, SanFrancisco, ASP, ASP Conf. Ser., 237, pp.85-96, 2001.

Meylan G., Tidal Tails around Galactic Globular

Clusters, Observations and Simulations, invitedreview in Dynamics of Star Clusters and the MilkyWay, Proc. Heidelberg International Spring Conf.STAR2000, eds. S. Deiters, B. Fuchs, R. Spurzem, R.Wielen, San Francisco, ASP Conf. Ser. 228, pp.53-60,2001.

Meylan G., Mass Determinations of Star Clusters,invited review in IAU Symp. 207 on ExtragalacticStar Clusters, eds. D. Geisler, E. Grebel, D. Minniti,San Francisco, ASP, pp.555-565, 2001.

Micol, A., Amico, P., An Enhanced Data Flow Scheme toBoost Observatory Mine-ability and ArchiveInteroperability, ASP Conf. Ser. 238, pp.148, 2001.

Nobili, S., et al., Panagia, N., et al., Supernova Type IaEvolution and Grey Dust Ground and Space BasedFollow up of a Type Ia Supernova at z=0.54, BAAS,33, 1333, 2001.

Nugent, P., et al., Panagia, N., et al., Interpretation ofHigh-z SN Spectra, BAAS, 33, 1370, 2001.

Padovani, P. Deep Blazar Surveys, in BlazarDemographics and Physics, P. Padovani, C.M. Urry(eds.), ASP Conf. Ser., 227, 163, 2001.

Padovani, P., C.M. Urry, Issues in Blazar Research, inBlazar Demographics and Physics, P. Padovani, C.M.Urry (eds.), ASP Conf. Ser., 227, 3, 2001.

Padovani, P. Giommi, Mining the Blazar Sky, in Miningthe Sky, A.J. Banday, S. Zaroubi, M. Bartelmann(eds.), Springer-Verlag, 494, 2001.

Pain, R., et al., Panagia, N., et al., The Distant Type IaSupernovae Rate, BAAS, 33, 1346, 2001.

Panagia, N. & Bono, G., Pre-Supernova Evolution ofMassive Stars, invited review at STScI 1999 MaySymp. The Largest Explosions since the Big BangSupernovae and Gamma Ray Bursts, eds. M. Livio, N.Panagia, K. Sahu, Cambridge Univ. Press, p.184-197,2001.

Panagia, N. The Next Generation Space Telescope,invited talk at the 2000 Vulcano Workshop FrontierObjects in Astrophysics and Particle Physics, eds. F.Giovannelli, G. Mannocchi, Italian Physical Society,p.587, 2001.

Panagia, N., Lamers, H., Bik, A., de Wit, W., Scuderi, S.,Capetti, A., Romaniello, M., Spaans, M., Kirshner,R.P., Star Formation and Stellar Populations in theCentral Regions of M51 in The Central kpc ofStarbursts and AGNs, eds. J.H. Knapen, J.E.Beckman, I. Shlosman, T.J. Mahoney, ASP Conf. Ser.,249, ASP, San Francisco, p.543-549, 2001.

Panagia, N., Romaniello, M., Scuderi, S., the SINSCollaboration, HST Study of the Stellar Populationwithin 30 pc of SN 1987A, invited review at 1997ESO/CTIO/LCO Workshop SN 1987A Ten Years After,eds. M. Phillips, N. Suntzeff, ASP Conf. Ser., in press.

Panagia, N., Stiavelli, M., Ferguson, H.C., Stockman,H.S., Primordial Stars The Next Generation, BAAS,33, 1347.

Panagia, N.,Weiler, K.W., Montes, M.J., Van Dyk, S.D.,Sramek, R.A., Lacey, C.K., Radio Properties ofSupernovae and GRB Sources, invited talk, 2000

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Vulcano Workshop Frontier Objects in Astrophysicsand Particle Physics, eds. F. Giovannelli, G.Mannocchi, Italian Physical Society, p.207, 2001.

Pasquali, A., Pirzkal, N., Walsh, J.R., Hook, R.N.,Freudling, W., Albrecht, R., Fosbury, R.A.E., TheEffective Spectral Resolution of the WFC and HRCGrism, ST-ECF Instrument Science Report 2001-002,2001.

Peletier, R.F., Bacon, R., Bureau, M., et al., TheSAURON Survey of Early-Type Galaxies in theNearby Universe, The Newsletter of the Isaac NewtonGroup of Telescopes (ING Newsl.), issue 5, p.5, 2001.

Perlman, E., P. Padovani, H. Landt, J. Stocke, L.Costamante, T. Rector, P. Giommi, J.F. Schachter,Surveys and the Blazar Parameter Space, in BlazarDemographics and Physics, P. Padovani, C.M. Urry(eds.), ASP Conf. Series, 227, 200, 2001.

Pierfederici, F., Benvenuti, P., Micol, A., Pirenne, B.,Wicenec, A., ASTROVIRTEL: Accessing Astronom-ical Archives as Virtual Telescopes", ASP Conf. Ser.238, pp.141, 2001.

Pirzkal, N., Pasquali, A., Hook, R.N., Walsh, J.R.,Fosbury, R.A.E., Freudling, W., Albrecht, R., TheHDF as Seen by the Advanced Camera for Surveys, inDeep Fields, Eds. S. Cristiani, A. Renzini, R.E.Williams (Springer), p.164, 2001.

Pirzkal, N., Pasquali, A., Hook, R.N., Walsh, J.R.,Fosbury, R.A.E., Freudling, W., Albrecht, R., SLIM: AProgram to Simulate the ACS Spectroscopic Modes,ASP Conf. Proc., 238, 447, 2001.

Pirzkal, N., Hook, R.N., Data fusion and photometricrestoration, in Proc. SPIE, 4477, Astronomical DataAnalysis, Eds. J.-L. Starck, F.D. Murtagh, 277, 2001.

Pirzkal, N., Kerber, F., Clayton, G.C., de Marco, O.,Rosa, M.R., Estimating the distance to V4334 Sgrusing the extinction method, AAS 199, #136.04, 2001.

Pirzkal, N,. Pasquali, A., Walsh, J.R., Hook, R.N.,Freudling, W., Albrecht, R., Fosbury, R.A.E., ACSGrism Simulations Using SLIM 1.0, ST-ECFInstrument Science Report 2001-003, 2001.

Robberto, M., Beckwith, S.V.W., Makidon, R.B.,Panagia, N., HST/WFPC2 image of the Orion Nebulain the U and B bands, BAAS, 33, 852, 2001.

Romaniello, M., Panagia, N., Scuderi, S., Gilmozzi, R.,Tolstoy, E., Favata, F., Kirshner, R.P., T Tauri Stars inthe Large Magellanic Cloud, a combined HST andVLT effort, Proc. ESO Workshop The Origin of Starsand Planets The VLT View, eds. J. Alves and M.McCaughrean, ESO, p.275, 2001.

Rosa, M.R., Alexov, A., Bristow, P., Kerber, F., FOSBlue-side Spectroscopic Data recalibrated by the postoperational archive project, ST-ECF Newsletter, 29, 9,2001.

Rosa, M.R., Bristow, P.D., Alexov, A., Kerber, F., GIMPand YBASE Induced Zero-Point Shifts in FOS Data,POA/FOS-2001-01, 2001.

Rosa, M.R., Bristow, P.D., Alexov, A., Kerber, F.,Physical Model FOS Dispersion Relations,POA/FOS-2001-04, 2001.

Scarlata, C., Stiavelli, M., Panagia, N., Treu, T., Bertin,G., Bertola, F., Lyman alpha emitters with red colorsat z~2.4, BAAS, 33, 1316, 2001.

Schahmaneche, K., et al., Panagia, N., et al., Resultsfrom Recent High-redshift Type Ia SupernovaeSearches, BAAS, 33, 1333, 2001.

Sirianni, M., Nota, A., De Marchi, G., Leitherer, C.,Clampin, M. The low end of the initial mass functionin the young LMC cluster NGC 2164, BAAS, 198,42.08, 2001.

Stiavelli, M., Panagia, N., Scarlata, C., Treu, T.,Properties of high-z galaxies with NGST, BAAS, 33,1315, 2001.

Stiavelli, M., Scarlata, C., Lilly, S., Panagia, N., Treu, T.,Bertin, G., Bertola, F., Star-formation at z = 2.4 froma sample of Lyman-alpha emitters, BAAS, 33, 815,2001.

Tagliaferri, G., Ghisellini, G., Ravasio, M. et al., TwoBeppoSAX observations of BL Lac, Memorie dellaSocieta Astronomica Italiana, 72, 135, 2001.

Tagliaferri, G., Ghisellini, G., Giommi, P. et al., FlaringBlazars with BeppoSAX, AIP Conf. Proc. 599, X-rayAstronomy, Stellar Endpoints, AGN, and the DiffuseX-ray Background, 971, 2001.

Trussoni, E., Capetti, A., Celotti, A., Chiaberge, M.,X-ray observations of 3C 66B and 3C 346, Memoriedella Societa Astronomica Italiana, 72, 111, 2001.

Trussoni, E., Capetti, A., Celotti, A., Chiaberge, M.Spectral Energy Distribution of Low Power FR IRadio Galaxies, ASP Conf. Ser., 227, BlazarDemographics and Physics, 131, 2001.

Trussoni, E., Feretti, L., Capetti, A., Celotti, A.,Chiaberge, M., X-ray Properties of FR I RadioGalaxies, AIP Conf. Proc. 599, X-ray Astronomy,Stellar Endpoints, AGN, and the Diffuse X-rayBackground, 987, 2001.

Weiler, K.W., Panagia, N., Sramek, R.A., Van Dyk, S.D.,Montes, M.J., Lacey, C.K., Radio Supernovae andGRB980425, invited review STScI 1999 May Symp.The Largest Explosions since the Big Bang Supernovaeand Gamma Ray Bursts, eds. M. Livio, N. Panagia, K.Sahu, Cambridge Univ. Press, p.198-217, 2001.

Zhang, Y.H., Celotti, A., Treves, A. et al., EnergyDependent X-ray Variability of the TeV Blazars PKS2155-304 and MKN 421, AIP Conf. Proc. 599, X-rayAstronomy, Stellar Endpoints, AGN, and the DiffuseX-ray Background, 1019, 2001.

Space Telescope Operations DivisionRefereed Journals, 2002

Albrow, M., De Marchi, G., Sahu, K., The spatiallyresolved mass function of the globular cluster M22,ApJ, 579, 660, 2002.

Allen, M.G. Sparks, W.B., Koekemoer, A. et al.,Ultraviolet Hubble Space Telescope Snapshot Surveyof 3CR Radio Source Counterparts at Low Redshift,ApJS, 139, 411, 2002.

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146 publications

Andreani, P., Fosbury, R.A.E., van Bemmel, I., Freud-ling, W., Far-infrared/millimetre emission in 3Csources. Dust in radio galaxies and quasars, A&A,381, 389, 2002.

Arribas, S., Colina, L., INTEGRAL Field Spectroscopyof IRAS 15206+3342: Gas Inflows and Starbursts inan Advanced Merger, ApJ, 573, 576, 2002.

Benítez, N., Maíz-Apellániz, J., Cañelles, M. Evidencefor nearby supernova explosions, PhRvL, 88, 1101,2002.

Bik, A., Lamers, H., Bastian, N., Panagia, N., Romani-ello, M., Clusters in the Inner Spiral Arms of M51, theCluster IMF and the Formation History", A&A, 397,473, 2003.

Blakeslee, J.P., Metzger, M.R., Kuntschner, H., Cote, P.,Lensing in the Hercules Supercluster, AJ, 121, 1,2002.

Burud, I., Courbin, F., Magain, P., Lidman, C.,Hutsemekers, D., Kneib, J.-P., Hjorth, J., Brewer, J.,Pompei, E., Germany, L., Jaunsen, A.O., Letawe, G.,Meylan, G., On Optical Time-Delay for the LensedBAL Quasar HE~2149-2745, A&A, 383, 71-81, 2002.

Capetti, A., Celotti, A., Chiaberge, M., de Ruiter, H.R.,Fanti, R., Morganti, R., Parma, P. The HST survey ofthe B2 sample of radio-galaxies: Optical nuclei andthe FR I/BL Lac unified scheme, A&A, 383, 104,2002.

Chiaberge, M., Macchetto, F.D., Sparks, W.B., Capetti,A., Allen, M.G., Martel, A.R. The Nuclei of RadioGalaxies in the Ultraviolet: The Signature of DifferentEmission Processes, ApJ, 571, 247, 2002.

Chiaberge, M., Capetti, A., Celotti, A. Understanding thenature of FR II optical nuclei: A new diagnostic planefor radio galaxies, A&A, 394, 791, 2002.

Chiaberge, M., Gilli, R., Macchetto, F.D., Sparks, W.B.,Capetti, A. What do HST and Chandra tell us aboutthe jet and the nuclear region of the radio galaxy3C~270?, ApJ, 582 (2), 645, 2003.

Cote, P., Djorgovski, S.G., Meylan, G., Castro, S.,McCarthy, J.K., Palomar~13: An Unusual StellarSystem in the Galactic Halo, ApJ, 574, 783-804.

Courbin, F., Meylan, G., Kneib, J.-P., Lidman, C.,Cosmic Alignment Towards the Radio Einstein RingPKS 1830-211, ApJ, 575, 95-102, 2002.

Davies, R.L., Kuntschner, H., Emsellem, E., et al.,Galaxy mapping with the SAURON integral-fieldspectrograph: The star formation history of NGC4365, ApJL, 548, L33, 2002.

Delgado, R.M.G., Arribas, S., Pérez, E., Heckman, T., Isa Minor Merger Driving the Nuclear Activity in theSeyfert 2 Galaxy NGC 2110?, ApJ, 579, 188, 2002.

D’Elia, V., P. Padovani, H. Landt, The Disc-Jet Relationin Strong-lined Blazars, MNRAS, in press, 2002.

Ferrari, F., Pastoriza, M.A., Macchetto., F.D., Bonatto,C., Panagia, N., Sparks, W.B., Survey of the ISM inEarly-Type Galaxies – IV – The Hot Dust Component,A&A, 389, 355, 2002.

Fruchter, A.S., Hook, R.N., Drizzle: A Method for the

Linear Reconstruction of Undersampled Images,PASP, 114, 144, 2002.

Gnedin, O.Y., Zhao, H.S., Pringle, J.E., Fall, S.M., Livio,M., Meylan, G. The Unique History of the GlobularCluster Omega Cent, ApJ, 568, L23-L26, 2002.

Haemmerle, H., Miralles, J.-M., Schneider, P., Erben, T.,Fosbury, R.A.E., Freudling, W., Pirzkal, N., Jain, B.,White, S.D.M., Cosmic shear from STIS PureParallels: II Analysis, A&A, 385, 743, 2002.

Heydari-Malayeri, M., Charmandaris, V., Deharveng, L.,Meynadier, F., Rosa, M.R., Schaerer, D., Zinnecker,H., Resolving the compact H II regions in N160A withHST, A&A, 381, 941, 2002.

Heydari-Malayeri, M., Rosa, M.R., Schaerer, D., Martins,F., Charmandaris, V., STIS spectroscopy of newbornmassive stars in SMC N81, A&A, 381, 951, 2002.

Homeier, N., Gallagher, J., Pasquali, A., The Star ClusterSystem of the NGC 7673 Starburst, A&A, 391, 857,2002.

Kerber, F., Guglielmetti, F., Mignani, R., Roth, M.,Proper motion of the central star of the PlanetaryNebula Sh 2-68, A&A, 381, L9, 2002.

Kerber, F., Pirzkal, N., De Marco, O., Asplund, M.,Clayton, G.C., Rosa, M.R., Freshly ionized matteraround the final Helium shell flash object V4334 Sgr(Sakurai’s object), ApJL, 581, L39, 2002.

King, N.L., Nota, A., Pasquali, A., Nota, A., Panagia, N.,Gull, T.R., Pasquali, A., Clampin, M., Bergeron, L.E.,An HST Polarization Study of Dust in the Eta CarHomunculus, ApJ, 581, 285, 2002.

King, L.J., Clowe, D.I., Lidman, C., Schneider, P., Erben,T., Kneib, J.-P., Meylan, G., The First Detection ofWeak Gravitational Shear in Infrared Observations:Abell 1689, A&A, 385, L5-L9, 2002.

Kuntschner, H., Ziegler, B.L., Sharples, R.M., Worthey,G., Fricke, K.J., VLT spectroscopy of NGC3115globular clusters, A&A, 395, 761, 2002.

Kuntschner, H., Smith, R.J., Colless, et al., Early-type gal-axies in low-density environments, MNRAS, 337, 172,2002.

Lamers, H., Panagia, N., Scuderi, S., Romaniello, M.,Spaans, M., de Wit, W.J., Kirshner, R.P., OngoingMassive Star Formation in the Bulge of M51, ApJ,566, 818, 2002.

Landt, H., P. Padovani, P. Giommi, The BL LacClassification, MNRAS, 336, 945, 2002.

Li Causi, G., De Marchi, G., Paresce, F. On the accuracyof the signal-to-noise estimates obtained with theexposure time calculator of the Wide Field PlanetaryCamera 2 on board the Hubble Space Telescope,PASP, 114, 770, 2002.

Maíz-Apellániz, J., Cieza, L., MacKenty, J.W. Tip of thered giant branch distances to NGC 4214, UGC 685,and UGC 5456, AJ, 123, 1307, 2002.

Miralles, J.-M., Erben, T., Haemmerle, H., Schneider, P.,Fosbury, R.A.E., Freudling, W., Pirzkal, N., Jain, B.,White, S.D.M., A conspicuous tangential alignment ofgalaxies in a STIS Parallel Shear Survey field: A newdark-lens candidate?, A&A, 388, 68, 2002.

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Moore, S.A.W., Lucey, J.R., Kuntschner, H., & Colless,M., Stellar populations in early-type Coma clustergalaxies – I. The data, MNRAS, 336, 382, 2002.

Motta, V., Mediavilla, E., Muñoz, J. A., Falco, E.,Kochanek, C.S., Arribas, S., García-Lorenzo, B.,Oscoz, A., Serra-Ricart, M. Detection of the 2175 ÅExtinction Feature at z = 0.83 2002, ApJ, 574, 719,2002.

Neeser, M., Sackett, P., De Marchi, G., Paresce, F.,Detection of a thick disc in the edge-on low surfacebrightness galaxy ESO 342-G017. I. VLT photometryin the V and R bands, A&A, 383, 472, 2002.

Padovani, P., L. Costamante, G. Ghisellini, P. Giommi,E. Perlman, BeppoSAX Observations of SynchrotronX-ray Emission from Radio Quasars, ApJ, 581, 895,2002.

Pain, R., et al., Panagia, N., et al., The Distant Type IaSupernova Rate, ApJ, 577, 120, 2002.

Palen, S., Balick, B., Hajian, A.R., Terzian, Y, Bond,H.E., Panagia, N., Hubble Space Telescope ExpansionParallaxes of the Planetary Nebulae NGC 6578, NGC6884, NGC 6891, and IC 2448, AJ, 123, 2666, 2002.

Pasquali, A., Comeron, F., IRAS 18576+0341: A newaddition to the class of Galactic Luminous BlueVariables, A&A, 382, 1005, 2002.

Petrosian, A., Allen, R.J., Leitherer, C., MacKenty, J.W.,McLean, B.J., Panagia, N., Study of the SecondByurakan Survey Galaxies – II – Comparison of UV-Excess and Emission Line Techniques, AJ, 125, 86,2003.

Petrosian, A., McLean, B.J., Allen, R.J., Leitherer, C.,MacKenty, J.W., Panagia, N., Study of the SecondByurakan Survey Galaxies – I – Mergers, InteractingSystems and Close Pairs, AJ, 123, 2280.

Pun, C.S.J., Kirshner, R.P., Garnavich, P., Challis, P.,Baron, E., Branch, D., Chevalier, R.A., Filippenko,A., Fransson, C., Leibundgut, B., Lundqvist, P.,McCray, R., Panagia, N., Phillips, M.M., Schmidt, B.,Sonneborn, G., Suntzeff, N.B., Wang, L., Wheeler,J.C., Modelling the Hubble Space TelescopeUltraviolet and Optical Spectrum of Spot 1 on theCircumstellar Ring of SN 1987A, ApJ, 572, 906,2002.

Robberto, M., Beckwith, S.V.W., Panagia, N., TheInfrared Emission of Circumstellar Envelopes, DarkSilhouttes and Photoionized Disks in HII Regions,ApJ, 578, 897, 2002.

Romaniello, M., Panagia, N., Scuderi, S., Kirshner, R.P.,Accurate Stellar Population Studies from MultibandPhotometric Observations, AJ, 123, 915, 2002.

Savaglio, S., Panagia, N., Padovani, P., The Lyman-alphaforest of a Lyman Break Galaxy at z=2.724: VLTSpectra of MS1512--cB58, ApJ, 567, 702, 2002.

Sirianni, M., Nota, A., De Marchi, G., Leitherer, C.,Clampin, M. The low end of the initial mass functionin young clusters. II. Evidence of primordial masssegregation in NGC330 in the Small MagellanicCloud, ApJ, 579, 275, 2002.

Sollerman, J., Holland, S., Challis, P., Fransson, C.,

Garnavich, P., Kirshner, R.P., Kozma, C., Leibundgut,B., Lundqvist, P., Patat, F., Filippenko, A.V., Panagia,N., Wheeler, J.C., Supernova 1998bw, The finalphases, A&A, 386, 944, 2002.

Villar-Martin, M., Vernet, J., di Serego Alighieri, S.,Fosbury, R., Pentericci, L., Cohen, M., Goodrich, R.,Humphrey, A., Giant low surface brightness haloes indistant radio galaxies: USS0828+193, MNRAS, 336,436, 2002.

Walborn, N.R., Maíz-Apellániz, J., Barbá, R.H., Furtherinsights into the structure of 30 Doradus from theHubble Space Telescope Instruments, AJ, 124, 1601 ,2002.

Wang, L., Wheeler, H.P., Khokhlov, A., Baade, D.,Branch, D., Challis, P., Filippenko, A.V., Fransson, C.,Garnavich, P., Kirshner, R.P., Lundqvist, P., McCray,R., Panagia, N., Pun, C.S.J., Phillips, M.M., Sonne-born, G., Suntzeff, N., The Axially Symmetric Ejectaof Supernova 1987A, ApJ, 579, 671, 2002.

Weiler, K.W., Panagia, N., Montes, M.J., Sramek, R.A.,Radio Emission from Supernovae and Gamma RayBursters, ARAA, 40, 387-438, 2002.

Williams, C.L., Panagia, N., Lacey, C.K., Van Dyk, S.D.,Weiler, K.W., Sramek, R.A., SN 1988Z as a Probe ofMassive Star Evolution, ApJ, 581, 396, 2002.

de Zeeuw, P.T., Bureau, M., Emsellem, E., et al., TheSAURON project – II. Sample and early results,MNRAS, 329, 513, 2002.

Space Telescope Operations DivisionProceedings and other Publications, 2002

Albrecht, R., Where are We and Why? Exploring theUniverse with the Hubble Space Telescope, in Proc.Internat. Symp. on the Human Dimension in SpaceScience and Technology Applications, Ed. N.Rodrigues, UN Office for Outer Space Affairs,Vienna, Austria, A/AC.105/CRP.5, p.27, 2002.

Albrecht, R., Jakobsen, P., Looking back: The ESA FaintObject Camera, ST-ECF Newsletter, 31, 6, 2002.

Alexov, A., Bristow, P.D., Kerber, F., Rosa, M.R., Re-Processing of HST FOS Data (12/01), ST-ECFTechnical. Report, POA/FOS-2001-08, 2002.

Arribas, S., Jakobsen, P., Fosbury, R., Freudling, W.,Effects of Facet, Pixel, and Slit Dimensions on thePerformance of a MEMS Type Spectrograph forNGST, AAS 199.0807A, 2002.

Bond, H.E., Henden, A., Panagia, N., Sparks, W.B.,Starrfield, S., Wagner, R.M., HST Imaging Polari-metry of the Light Echo Around V838 Monocerotis,BAAS, 201, #40.01, 2002.

Bond, H.E., Panagia, N., Sparks, W.B., Starrfield, S.G.,Wagner, R.M., Henden, A., V838 Monocerotis, IAUCirc. 7943, 2002.

Bond, H.E., Panagia, N., Sparks, W.B., Starrfield, S.G.,Wagner, R.M., V838 Monocerotis, IAU Circ. 7892,2002.

Bono, G., Panagia, N., Pulsational Properties of Yellow

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148 publications

Supergiants, invited paper at Workshop The Changesin Abundances in Asymptotic Giant Branch Stars, eds.V. Caloi, F. D’Antona, Mem. S. A. It., in press, 2002.

Bristow, P.D., Alexov, A., Kerber, F., Rosa, M.R., FinalImprovement of HST POA FOS/BLUE Archived Dataand Pipeline Processing, AAS, 200, 5905, 2002.

Bristow, P.D., From Theoretical to Observational ViaSelection Effects, in New Trends in Theoretical andObservational Cosmology, Eds. K. Sato, T. Shiro-mizu, Universal Academy Press, 265, 2002.

Bristow, P.D., Alexov, A., Kerber, F., Rosa, M.R., POAInvestigation of FOS Dark Corrections (12/01),STECF Technical Report, POA/FOS-2001-07, 2002.

Capetti, A., Celotti, A., Chiaberge, M., de Ruiter, H.R.,Fanti, R., Morganti, R., Parma, P., The HST View ofLow Luminosity Radio-Galaxies, ASP Conf. Ser. 258,Issues in Unification of Active Galactic Nuclei, 159,2002.

Capetti, A., Trussoni, E., Celotti, A., Feretti, L.,Chiaberge, M., Spectral energy distributions of fiveFR I radio galaxies, New Astronomy Review, 46, 335, 2002.

Charmandaris, V., Heydari-Malayeri, M., Deharveng, L.,Rosa, M.R., Schaerer, D., Zinnecker, H., HST imagingand spectroscopy of Compact HII regions in theMagellanic Clouds: Revealing the youngest massivestar clusters, AAS 199, #124.05, 2002.

Chiaberge, M., Capetti, A., Celotti, A., Optical synchro-tron emission from the nuclei of FR I radio galaxies,New Astronomy Review, 46, 339, 2002.

Colina, L., Alberdi, A., Torrelles, J.M., Panagia, N.,Wilson, A.S., Garrington, S.T., Supernova 2000ft inNGC 7469, IAU Circ. 7838, 2002.

Fosbury, R., Albrecht, R., The Space Telescope EuropeanCoordinating Facility, STScI Newsletter, 19 (03), 17,2002.

Freudling, W., Arribas, S., Cristiani, S., Fosbury, R.,Jakobsen, P., Pirzkal, N., Confusion limits on Spectrataken with the Next Generation Space TelescopeNear-Infrared Multi-Object Spectrograph, AAS199.0806F, 2002.

Giavalisco, M., Riess, A., Casertano, S., Dahlen, T.,Dickinson, M., Ferguson, H., Hook, R., Idzi, R.,Koekemoer, A., Mobasher, B., Moustakas, L.A.,Ravindranath, S., Strolger, L., Tonry, J., Challis, P.,Supernovae 2002ez, 2002fv, 2002fw, 2002fx, 2002fy,2002fz, 2002ga, IAU Circ. 7981, 2002.

Grogin, N.A., H.C. Ferguson, M.E. Dickinson, M.Giavalisco, B. Mobasher, P. Padovani, R.E. Williams,R. Chary, R. Gilli, T.M. Heckman, D. Stern, C. Winge,The Chandra Deepest Fields in the Infrared: Makingthe Connection between Normal Galaxies and AGN,BAAS, 199, #148.02, 2002.

Gronwall, C., Pasquali, A., Pirzkal, N., Walsh, J.R.,Tsvetanov, Z.I., Martel, A.R., Hook, R.N., Freudling,W., Albrecht, R., Fosbury, R.A.E., Hartig, G., Bohlin,R.C., Tran, H.D., Benítez, N., Early Observations withthe ACS Grism, AAS 200.6204G, 2002.

Hartig, G., Ford, H., Illingworth, G., Clampin, M.,

Bohlin, R., Cox, C., Krist, J., Sparks, W., De Marchi,G., Martel, A., McCann, W., Meurer, G., Sirianni, M.,Tsvetanov, Z., Bartko, F., Lindler, D., An overview ofthe HST Advanced Camera for Surveys’ on-orbitperformance, BAAS, 200, 19.01, 2002.

Heydari-Malayeri, M., Charmandaris, V., Deharveng, L.,Meynadier, F., Rosa, M.R., Schaerer, D., Zinnecker,H., HST photometry of stars in N160A, in VizieR On-line Data Catalog, J/A+A/381/941, SIMBAD, 2002.

Heydari-Malayeri, M., Charmandaris, V., Deharveng, L.,Meynadier, F., Rosa, M.R., Schaerer, D., Zinnecker,H., Unveiling the properties of low metallicitymassive young star clusters, in Semaine del’Astrophysique Francaise, Eds. F. Combes, D. Barret,Editions de Physique Conf. Ser., 2002.

Hook, R., Optical astronomy goes large, Astronomy Now,16, 29, 2002.

Jakobsen, P., Arribas, S., Burgarella, D., Caraveo, P.,Cornelisse, J., Davies, R., Ferrara, A., Fosbury, R.,Hjorth, J., Le Fevre, O., McCaughrean, M., Regan,M., Schneider, P., Ward, M., Wright, G., vanDishoeck, E., The NGST Near-Infrared Spectrometer:The Science Case and Main Drivers, AAS 199.0805J,2002.

Käufl, H.U., Locurto, G., Kerber, F., Heijligers, B., V838Mon, IAU Circ. 7831, 2002.

Kerber, F., Wills, B., Alexov, A., Bristow, P., Seifarth, A.,Rosa, M. R., Science from the refurbished FOS/BLUEarchive: Interstellar absorption lines in a sample oflow red-shift quasars, AAS, 200, 4018, 2002.

Kerber, F., Pirzkal, N., Rosa, M.R., V4334 Sagittarii,IAU Circ. 7879, 3, 2002.

Kerber, F., Bristow, P.D., Alexov, A., Luridiana, V., Rosa,M.R., No Internal/External Offsets in the FOS/BLUEWavelength Calibration Zero Point (12/01), ST-ECFTechnical. Report, POA/FOS-2001-05, 2002.

Kerber, F., Bristow, P.D., Alexov, A., Rosa, M.R.,Science Verification of the POA Corrected FOSArchive (12/01), ST-ECF Technical. Report,POA/FOS-2001-06, 2002.

Lamers, H., Panagia, N., Romaniello, M., Scuderi, S.,Spaans, M., Massive Stars in the Bulge of M51 a newmode of star formation?, invited paper, HeidelbergWorkshop Modes of Star Formation, eds. X.X.Brandner, E. Grebel, ASP Conf. Ser., ASP, SanFrancisco, in press, 2002.

Maíz-Apellániz, J., Photometry of saturated stars in CCDimages, to appear in 2002 HST Calibration Workshop,STScI, edited by S. Arribas, A. Koekemoer, B.Whitmore, 2002.

Maíz-Apellániz, J., Walborn, N.R., MacKenty, J.W.,Norman, C.A., Pérez, E., Mas-Hesse, J.M., Objective-prism spectroscopy with STIS-HST, in Galaxies: theThird Dimension, ed. M. Rosado, L. Binette, L. Arias,in press, 2002.

McDowell, J., Clements, D.L., Lamb, S., Borne, K.,Arribas, S., Colina, L., Hearn, N., Mundell, C., Baker,A., X-Rays From Arp 220 And Its Surroundings, APSAPRJ11003M, 2002.

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Meurer, G., Ford, H., Martel, A., Sirianni, M., Tran, H.,Bohlin, R., Clampin, M., Cox, C., De Marchi, G.,Hartig, G., Kimble, R., Argabright, V., Performance ofthe Solar Blind Channel of the HST Advanced Camerafor Surveys, BAAS, 200, 62.07, 2002.

Meylan G., Omega Cent: A General Overview, invitedreview in Omega Cent, A Unique Window intoAstrophysics, eds. F. van Leeuwen, J. Hughes, G.Piotto, San Francisco, ASP Conf. Ser., 265, pp.3-18.

Padovani, P., Blazar Surveys, in Blazar Astrophysics withBeppoSAX and other Observatories, P. Giommi, E.Massaro, G. Palumbo eds., ASI, 101.

Padovani, P., P. Giommi, H. Landt, E. Perlman, Unifica-tion of Faint Radio-loud Sources: The DXRBS View,in Issues in Unification of AGNs, R. Maiolino, A.Marconi, N. Nagar (eds.), ASP Conf. Ser., 258, 297,2002.

Panagia, N., Primordial Stellar Populations, invitedreview in Workshop Origins 2002 The Heavy ElementTrail from Galaxies to Habitable Worlds, (JacksonLake Lodge, Grand Teton National Park, Wyoming,May 26-29, 2002), eds. C.E. Woodward, E. Smith,ASP, San Francisco, in press, 2002.

Panagia, N., Space Telescopes of Today and TomorrowHST and NGST, invited talk, 1999 Frascati WorkshopMulti-frequency Behaviour of High Energy CosmicSources,, eds. F. Giovannelli, L. Sabau-Graziati, Mem.S. A. It., 73, 88-98, 2002.

Panagia, N., Supernovae at high z clues to the expansionof the Universe, in 44th Annual Meeting, ItalianAstron. Soc., Monte Porzio Catone, 10-15 April 2000,eds. L.A. Antonelli, G. Bono, G. Giobbi, N. Menci,Mem. S. A. It., 72, 875-878, 2002.

Panagia, N., The Hubble Space Telescope at theBeginning of a New Millennium, invited talk, 2001Frascati Workshop Multifrequency Behaviour of HighEnergy Cosmic Sources, eds. F. Giovannelli, L.Sabau-Graziati, Mem. S. A. It., 73, 823, 2002.

Panagia, N., Ultraviolet Properties of Supernovae,invited review, Supernovae and Gamma-Ray Bursts,ed. K.W. Weiler, Springer-Verlag, in press, 2002.

Panagia, N., Stiavelli, M., Ferguson, H.C., Stockman,H.S., Observational Properties of Primordial StellarPopulations, in Galaxy Evolution Theory andObservations, eds. V. Avila-Reese, C. Firmani, C.Frenk, C. Allen, Rev. Mex. A.A. SC, in press, 2002.

Panagia, N., Stiavelli, M., Ferguson, H.C., Stockman,H.S., Primordial Stellar Populations (abstract),Workshop Galaxy Evolution Theory andObservations, Cozumel April 8-12, 2002, ADS2002geto.confE..50P, 2002.

Pasquali, A., de Mello, D.F., The Galaxy Population atIntermediate Redshifts using STIS Parallel Fields, inThe evolution of galaxies. II – Basic Building Blocks,eds. M. Sauvage, G. Stasinska, D. Schaerer, Kluwer,p.541, 2002.

Pavlovsky, C., Clampin, M., De Marchi, G., Gilliland,R., Bohlin, R., Mack, J., Hartig, G., Sirianni, M. ACSsensitivity, BAAS, 200, 62.01, 2002.

Pirzkal, N., Pasquali, A., Daddi, E., Walsh, J.R., Hook,R.N., Spectral Extraction from ACS & VLT multi-object spectroscopic data, AAS, 200, 6208, 2002.

Proffitt, C.R. et al., STIS Calibration Status, in 2002 HSTCalibration Workshop, STScI, eds. S. Arribas, A.Koekemoer, B. Whitmore, in press, 2002.

Quimby, P., et al., Panagia, N., et al. The SupernovaCosmology Project Collaboration, The Host Galaxiesof Type Ia Supernovae at High Redshift, BAAS, 201,#23.05, 2002.

Rauch, T., Kerber, F., van Wyk, F., 2p2Team, V838 Mon,IAU Cir. 7886, 2002.

Sirianni, M., Clampin, M., Hartig, G., Ford, H.,Illingworth, G., Golimowski, D., Martel, A., McCann,W., De Marchi, G., Mutchler, M., Pavlovsky, C.,Argabright, V., Burmester, B., Koldewyn, W., Schrein,R., Sullivan, P. Performance of the ACS WFC andHRC CCDs, BAAS, 200, 62.05, 2002.

Stockdale, C.J., Perez- Torres, M.A., Marcaide, J.M.,Sramek, R.A., Weiler, K.W., Van Dyk, S.D., Panagia,N., Lundqvist, P., Pooley, D., Immler, S., Lewin, W.,Supernova 2001gd IN NGC 5033, IAU Circ. 7830,2002.

Stockdale, C.J., Sramek, R.A., Weiler, K.W., Van Dyk, S.D., Perez- Torres, M.A., Marcaide, J.M., Ray, A.Chandra, P., Panagia, N., Montes, M.J., RadioObservations of SN 2001gd in NGC 5033, BAAS, ,201, #56.02, 2002.

Stockdale, C.J., Sramek, R.A., Rupen, M., Weiler, K.W.,Van Dyk, S.D., Panagia, N., Pooley, D., Lewin, W.,Meyers, S., Taylor, G., Supernova 2002hh IN NGC6946, IAU Circ. 8018, 2002.

Trussoni, E., Capetti, A., Celotti, A., Chiaberge, M., SEDof Low Power Radio Galaxies: Test for FR I/BL LacUnification, in Issues in Unification of Active GalacticNuclei, ASP Conf. Ser., 258, 177, 2002.

Weiler, K.W., Panagia, N., Montes, M.J., RadioObservations of GRB Afterglows, invited review,Supernovae and Gamma-Ray Bursts, ed. K.W. Weiler,Springer-Verlag, in press.

Weiler, K.W., Panagia, N., Montes, M.J., Sramek, R.A.,Radio Emission from Supernovae and Gamma RayBursters, eds. F. Giovannelli, L. Sabau-Graziati, Mem.S. A. It., in press, 2002.

Weiler, K.W., Van Dyk, S.D., Panagia, N., Montes, M.J.,Sramek, R.A., Lacey, C.K., In the Beginning, RadioEmission from Supernovae, in Neutron Stars inSupernova Remnants, eds. P.O Slane, B.M. Gaensler,ASP Conf. Ser., 271, 375-379, 2002.

Zinnecker H., Andersen M., Brandl B., Brandner W.,Hunter D., Larson R., McCaughrean M., Meylan G.,Moneti A., The Infrared Luminosity Function of the30 Doradus Starburst Cluster: NICMOS/HST H-bandPhotometry, in IAU Symposium 207 on ExtragalacticStar Clusters, eds. D. Geisler, E. Grebel, D. Minniti,San Francisco, ASP, 531-538, 2002.

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150 publications

Chief Scientist (formerly Research Support Division)Refereed Journals, 2001

Adelman, S.J., Snow, T.P., Wood, E.L., Ivans, I.I.,Sneden, C., Ehrenfreund, P., Foing, B.H., An ele-mental abundance analysis of the mercury manganesestar HD 29647 2001, MNRAS, 328, 1144, 2001.

Foing, B., Van Susante, P., Almeida, M., Heather, D.,Duke, M., Dunkin, S., Lunar Explorers Society, LunarExplorers Society: Goals And Activities, Earth, Moonand Planets, 85, 533, 2001.

Foing, B.H., Duke, M., Galimov, E., Mizutani, H.,Pieters, C., Racca, G., Heather, D.J., Frischauf, N.,van Susante, P., Almeida, M., Highlights fromICEUM4, the 4th International Conference on theExploration and Utilisation of the Moon, Earth, Moonand Planets, 85, 133, 2001.

Foing, B.H., Heather, D.J., Almeida, M., SMART-1Science Technology Working Team, The ScienceGoals of ESA’s SMART-1 Mission To The Moon,Earth, Moon and Planets, 85, 523, 2001.

Oliveira, J.M., Unruh, Y.C., Foing, B.H., PreliminaryMUSICOS 96 results on Balmer line variability on theT Tauri star SU aurigae 2001, Adv. Space Res., 26,1747, 2001.

Oliveira, J.M., Foing, B.H., Preliminary investigation ofcircumstellar emission and flares in the fast rotatinggiant FK Comae 2001, Adv. Space Res., 26, 1733,2001.

Racca, G.D., Foing, B.H., Coradini, M., SMART-1: TheFirst Time Of Europe To The Moon; Wandering in theEarth-Moon Space, Earth, Moon and Planets, 85, 379,2001.

Chief ScientistProceedings and other Publications, 2001

Boudin, N., in Proc. 2nd European Workshop on Exo-Astrobiology, ESA SP-518, 37, 2001.

Dunkin S.K., Grande M., Browning R., D-CIXS Team,The D-CIXS X-ray spectrometer on ESA’s SMART-1mission to the Moon, Lunar & Planetary ScienceXXXII, Abstract #1310 (CD-ROM), 2001.

Dunkin, S.K., Heather, D.J., Unveiling the face of theMoon, in Thompson, J.M.T. (ed) Visions of theFuture: Astronomy and Earth Science, CambridgeUniv. Press, 115-130, 2001.

Ehrenfreund, P., O’Tuairisg, S., Foing, B.H., Sonnen-trucker, P., Cami, J., The Diffuse Interstellar Bandsand Organic Molecules in Space, in The BridgeBetween the Big Bang and Biology: Stars, PlanetarySystems, Atmospheres, Volcanoes: Their Link to Life,p.150, 2001.

Foing, B.H., Exo-astrobiology with ESA space sciencemissions, in Proc. Exo-astro-biology. Proceedings ofthe First European Workshop, 21-23 May 2001,ESRIN, Frascati, Italy, Eds. P. Ehrenfreund, O.Angerer, B. Battrick. ESA SP-496, 121-126, 2001.

Foing, B.H., Heather, D., Almeida, M., Racca, G.,Marini, A., The SMART-1 Team, ESA’s SMART-1Mission to the Moon, Lunar & Planetary ScienceXXXII, Abstract #1787 (CD-ROM), 2001.

Foing, B.H., Heather, D.J., Duke, M., Racca, G., Pieters,C., Mizutani, H., Galimov, E., Dunkin, S.K., vanSusante, P., Frischauf, N., Almeida, M., Results andRecommendations from the International Conferenceon the Exploration and Utilisation of the Moon 4(ICEUM4), Lunar & Planetary Science XXXII,Abstract #1712 (CD-ROM), 2001.

Foing, B.H., Duke, M., Galimov, E., Mizutani, H.,ILEWG, Next Steps for International LunarExploration, Lunar & Planetary Science XXXII,Abstract #1827 (CD-ROM), 2001.

Foing, B.H., Heather, D.J., Duke, M., Racca, G., Pieters,C.M., Mizutani, H., Galimov, E., Dunkin, S.K., vanSusante, P., Frischauf, N., Almeida, M., ICEUM4participants, Results and Recommendations from theInternational Conference on the Exploration andUtilisation of the Moon 4 (ICEUM4), Lunar &Planetary Science XXXII, Abstract #1712 (CD-ROM),2001.

Foing, B.H., Heather, D., Almeida, M., Racca, G., Mar-ini, A., SMART-1 Team, ESA’s SMART-1 Mission tothe Moon, Lunar & Planetary Science XXXII,Abstract #1787 (CD-ROM), 2001.

Heather, D.J., Dunkin, S.K., Wilson, L., Volcanism onthe Marius Hills Plateau. Lunar & Planetary ScienceXXXII, Abstract #1542 (CD-ROM), 2001.

Heather, D.J., Foing, B.H., van Susante, P., Almeida, M.,Outreach and Education from ESA’s SMART-1Mission to the Moon, Lunar & Planetary ScienceXXXII, Abstract #1983 (CD-ROM), 2001.

Heather, D.J., All Aboard the Mystery Express, EarthSpace Rev., 10 (4), 21-24, 2001.

Heather, D.J., The Ultimate Rendezvous, Earth SpaceRev., 10 (3), 19-23, 2001.

Heather, D.J., Last of the big spenders, Earth Space Rev.,10 (2), 22-25, 2001.

Heather, D.J., Europe goes to the Moon, Astronomy Now,15 (2), 56-58, 2001.

Heather, D.J., Return to the Forgotten Planet, EarthSpace Rev., 10 (1), 22-24, 2001.

Oliveira, J.M., Foing, B.H., Unruh, Y.C., Spectral LineVariability in the Circumstellar Environment of theClassical T Tauri Star SU Aurigae (CD-ROMDirectory: contribs/oliveira), 2001 ASP Conf. Ser.223: 11th Cambridge Workshop on Cool Stars, StellarSystems and the Sun, 11, p.539, 2001.

Petit, P., Donati, J.-F., Wade, G.A., Landstreet, J.D.,Oliveira, J.M., Shorlin, S.L.S., Sigut, T.A.A.,Cameron, A.C., Differential Rotation of Close BinaryStars: Application to HR 1099, Astrotomography,Indirect Imaging Methods in Observational Astron-omy, p.232, 2001.

Ruiterkamp, R., Ehrenfreund, P., Foing, B.H., Salama, F.,Organics experiment on the International SpaceStation, ESA SP-496, 137, 2001.

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publications 151

Chief ScientistRefereed Journals, 2002

Ehrenfreund, P., Cami, J., Jiménez-Vicente, J., Foing,B.H., Kaper, L., van der Meer, A., Cox, N.,d’Hendecourt, L., Maier, J.P., Salama, F., Sarre, P.J.,Snow, T.P., Sonnentrucker, P., Detection of DiffuseInterstellar Bands in the Magellanic Clouds, A.J., 576,L117, 2002.

Foing, B.H., Heather, D.J., Preface to Lunar Exploration,COSPAR B0.2 Symposium, Adv. Space Res., 30 (8),1867, 2002.

Foing, B.H., Lunar Exploration, Planet. Space Sci., 50,14-15, v-vi, 2002.

Grande, M., Dunkin, S.K., Kellet, B., Perry, C.,Browning, R., Waltham, N., Kent, B., Swinyard, B.,Parker, D., Perry, A., Feraday, J., Howe, C., Huovelin,J., Muhli, P., Hakala, P.J., Vilhu, O., Thomas, N.,Hughes, D., Alleyne, H., Grady, M., Russell, S.S.,Lundin, R., Barabash, S., Baker, D., Clarke, P.E.,Murray, C.D., Christou, A., Guest, J., Casanova, I.,d’Uston, L.C., Maurice, S., Foing, B.H., Heather, D.J.,Kato, M., The D-CIXS X-ray spectrometer, and itscapabilities for lunar science, Adv. Space Res., 30 (8),1901-1908, 2002.

Heather, D.J., Dunkin, S.K., Crustal stratigraphy of theAl-Khwarizmi-King/Tsiolkovsky-Stark region of thelunar farside as seen by Clementine, Planet. SpaceSci., 50, 14-15, 1311-1321.

Heather, D.J., Dunkin, S.K., A Stratigraphic Study OfSouthern Oceanus Procellarum Using ClementineMultispectral Data, Planet. Space Sci., 50, 14-15,1299-1309.

Huovelin, J., Alha, L., Andersson, H., Andersson, T.,Browning, R., Drummond, D., Foing, B., Grande, M.,Hamalainen, K., Laukkanen, J., Lamsa, V., Muinonen,K., Murray, M., Nenonen, S., Salminen, A., Sipila, H.,Taylor, I., Vilhu, O., Waltham, N., Lopez-Jorkama, M.The SMART-1 X-ray solar monitor (XSM):calibrations for D-CIXS and independent coronalscience, Planet. Space Sci. 50, 1345, 2002.

Marini, A.E., Racca, G.R., Foing, B.H., SMART-1Technology Preparation for Future PlanetaryMissions, Adv. Space Res., 30 (8), 1895, 2002.

Neiner, C., Hubert, A.-M., Floquet, M., Jankov, S.,Henrichs, H.F., Foing, B., Oliveira, J., Orlando, S.,Abbott, J., Baldry, I.K., Bedding, T.R., Cami, J., Cao,H., Catala, C., Cheng, K.P., Domiciano de Souza, A.,Janot-Pacheco, E., Hao, J.X., Kaper, L., Kaufer, A.,Leister, N.V., Neff, J.E., O’Toole, S.J., Schäfer, D.,Smartt, S.J., Stahl, O., Telting, J., Tubbesing, S.,Zorec, J., Non-radial pulsation, rotation and outburstin the Be star omega Orionis from the MuSiCoS 1998campaign, A&A, 388, 899, 2002.

Racca, G.D., Marini, A., Stagnaro, L., van Dooren, J., diNapoli, L., Foing, B.H., Lumb, R., Volp, J., Brink-mann, J., Grunagel, R., Estublier, D., Tremolizzo, E.,McKay, M., Camino, O., Schoemaekers, J., Hechler,M., Khan, M., Rathsman, P., Andersson, G., Anflo, K.,

Berge, S., Bodin, P., Edfors, A., Hussain, A., Kugel-berg, J., Larsson, N., Ljung, B., Meijer, L., Mortsell,A., Nordeback, T., Persson, S., Sjoberg, F., SMART-1mission description and development status,Planet.Space Sci. 50, 1323, 2002.

Ruiterkamp, R., Halasinski, T., Salama, F., Foing, B.H.,Allamandola, L.J., Schmidt, W., Ehrenfreund, P.,Spectroscopy of large PAHs. Laboratory studies andcomparison to the Diffuse Interstellar Bands, A&A,390, 1153, 2002.

Chief ScientistProceedings and other Publications, 2002

Almeida, M., Foing, B.H., Vilar, E., Heather, D.,Koschny, D., Marini, A., SMART-1 Science Experi-ments Coordination, ESA SP-514, 55-60, 2002.

Berghmans, D., Foing, B.H., Fleck, B., Automated detec-tion of CMEs in LASCO data in 2002, in Proc. SOHO11 Symposium on From Solar Min to Max: Half aSolar Cycle with SOHO, 11-15 March 2002, Davos,Switzerland, A. Wilson (ed), ESA SP-508, 437-440,2002.

Boudin, N., Large Organics in Space: LaboratoryMeasurements of Gas Phase Spectra and DiffuseInterstellar Bands, in Proc. 2nd European Workshopon Exo-Astrobiology, ESA SP-518, 37, 2002.

Cox, N. et al. (incl. B.H. Foing), Complex CarbonChemistry and the Diffuse Interstellar Bands in theMagellanic Clouds, in Proc. 2nd European Workshopon Exo-Astrobiology, ESA SP-518, 447, 2002.

Foing, B. H. Astrobiology with ESA Science Missions, inASP Conf. Ser. 269 The Evolving Sun and its Influ-ence on Planetary Environments, Ed. B. Montesinos,A. Gimenez, E.F. Guinan, p.361, 2002.

Foing, B.H., Space activities in exo-astrobiology, inbook: Astrobiology: The quest for the conditions oflife, G. Horneck, C. Baumstark-Khan (ed.), Physicsand astronomy online, Springer, 389-398.

Foing, B.H., ILEWG, Preface, in Proc. ESLAB36 onEarth-like planets and Moons, ESA SP-514, 3, 2002.

Foing, B.H. et al., Closing Remarks on ESLAB36, ESASP-514, 345, 2002.

Ruiterkamp, R., Halasinski, T., Salama, F., Foing, B.,Schmidt, W., Ehrenfreund, P., Laboratory CalibrationStudies in Support of an ISS Exposure Experimentand Comparison to the Diffuse Interstellar Bands, inNASA Laboratory Astrophysics Workshop, p.77, 2002.

Ten Kate, I. et al. (incl. B.H. Foing, N. Boudin),Laboratory Studies on Complex Organic Moleculeson Mars: Part 1 – Rationale, ESA SP-514, 293, 2002.

Ten Kate, I. et al. (incl. B.H. Foing), Laboratory Studieson Complex Organic Molecules on Mars: Part 2 –Experimental Set-Up and Related Work, in Proc. 2ndEuropean Workshop on Exo-Astrobiology, ESA SP-518, 81, 2002.

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Stagiaire Research Reports and Theses, 2001

Almeida, M. (U. Lisbon), SMART-1 Science PayloadOperations.

Dages, O. (DESS Obs. Paris-Meudon), SMART-1Mission Risk Tree Analysis.

Lefevre, F. (DESS Obs. Paris-Meudon), Optimisation ofPayload Operations Timelining.

Martinez Sanmartin, S. (U. Vigo), Operational RequestFile Acknowledger Testing Tools.

Oliveira, J. (PhD Thesis, RSSD/U. do Porto), Circum-stellar Environments and Activity in Young andEvolved Stars, PhD defence at U. do Porto, April2001.

Reissaus, P. (TU Munich), Simulation of Meteoroid’sRe-entry Behaviour in Earth’s Atmosphere.

Stagiaire Research Reports and Theses, 2002

Bonal, L. (U. Orsay), Study of Comet Dust Analogues &Interplanetary Dust Particles with Atomic ForceMicroscope.

Diaz, J. (U. Vigo), Meteor Orbit & Trajectory Determin-ation Software.

Hijmering, R. (U. Nijmegen), Astronomical Detectors.Lärfars, K. (U. of Umea/ Kiruna), Test and Character-

isation of a Low Noise Multi-channel CustomisedApplication Specific Integrated Circuit.

Manaud, N. (DESS Obs. Paris-Meudon), Auxiliary Datain SPICE format: Conversion, Validation, Distribution.

O’Sullivan J. (ESTEC YGT report), Optimisation ofDust Impact Time of Flight Mass Spectrometer.

Ott, S. (PhD Thesis, RSSD Vilspa/CEA), Observationsof the Infrared Sky with the ISOCAM Parallel Mode,PhD defence at IAP Paris, February 2002.

Riesen, T.-E. (U. Bern), Planetary Data System StandardTutorial.

Ubeira, M. (U. Vigo), Knowledge Management VideoDatabase Application.

Vazquez Garcia, B. (U. Vigo), Study of an ApplicationProgrammer Interface for ESA’s Planetary Archives.

Vilar, E. (UPC Barcelona), Planning & Optimisation ofScience Payload Operations for SMART-1 & Rosetta.

Ziljstra, A. (U. Delft), Mission to the Moon: Lunar ScoutLander Design.

Chief ScientistEditorials/Books

Foing, B.H. & Battrick, B. (eds), Proc. ESLAB36 Earth-like planets and Moons, ESA SP-514, 356pp, 2002.

Foing, B.H., Heather, D.J. (eds), Lunar Exploration, Adv.Space Res., 30 (8).

Foing, B.H., (Guest Editor), Special Issue on LunarExploration, Planet. Space Sci., 50.

Heather, D.J., Foing, B.H. (eds.), First Convention ofLunar Explorers Abstract and Program, Paris, March,58pp, 2001.

Heather, D.J. (ed), New Views of the Moon, Europe:Future Lunar Exploration, Science Objectives, andIntegration of Datasets, Abstracts, ESTEC RSSD,Noordwijk.

152 publications

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ANNEX 3Seminars and Colloquia

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154 seminars and colloquia

Seminars held at ESTEC

2001

12 JanuaryInterstellar ProbesI. Mann, Solar System Division

9 FebruaryThe Cassini Jupiter Fly-by and the InternationalJupiter WatchH.O. Rucker, Austrian Academy of Sciences

23 February15 years After the Halley Encounter – Are we Enteringthe Golden Age of Cometary Exploration?G. Schwehm, Solar System Division

6 AprilThe X-ray/Infrared Connection: New Observations ofStarburst Galaxies and Active Galactic NucleiM. Ward, Leicester University

27 AprilSpacecraft Mass Modelling in High-Energy Astro-physics and Some Recent Scientific ResultsA.J. Dean, Southampton University

1 JuneMars Express: Science, Payload and MissionOverviewA. Chicarro, Solar System Division

8 JuneComets and Circumstellar Environments of YoungStarsC. Waelkens, University of Leuven

22 JuneThe Darwin MissionM. Fridlund, Astrophysics Division

10 SeptemberA Novel Method for the Analysis of Planetary TransitData: A Bayesian Algorithm for the Analysis of theEddington DataS. Aigrain, Astrophysics Division

21 SeptemberOptical/Infrared Interferometry with the VLTIW. Jaffe, Leiden University

19 OctoberTomography of Stars and Circumstellar EnvironmentsA. Collier Cameron, St. Andrews

17 NovemberLarge Molecules and the Interstellar MediumA. Tielens, Kapteyn Astronomical Institute

30 NovemberThe Interior and Evolution of Terrestrial PlanetsT. Spohn, University of Munster

14 DecemberLeonid Meteor Observations in Australia – What weCan Learn from their Light CurvesD. Koschny, Solar System Division

2002

25 JanuaryObservations of the Sky with the ISOCAM ParallelModeS. Ott, ISO, VILSPA

7 FebruaryChemical Composition of Planetary Surfaces fromRemote Sensing TechniquesS. Maurice, Observatoire Midi-Pyrenees

22 FebruaryHerbig-Haro Objects: A New Class of AstrophysicalX-ray SourcesF. Favata, Astrophysics Missions Division

8 MarchThe Messenger Mission to MercuryJ. Slavin, NASA Goddard Space Flight Center

22 MarchRe-ionizing the Universe: Why? When? How?P. Jakobsen, Astrophysics Missions Division

12 AprilWater in Europa: Evidence from Surface CompositionObtained by GalileoT. McCord, University of Hawaii

17 MayThe Astrophysical Virtual Observatory – More ThanJust a Federation of ArchivesP. Benvenuti, ST-ECF, Garching

31 MaySerendipity in Science: Using Microwave WindScatterometers for Non-wind ApplicationsM. Drinkwater, Earth Sciences Division

14 JuneSearch for Extrasolar Planets: Earth ObjectiveD. Queloz, Observatoire de Geneve

5 JulyThe Stellar IMF and the Disruption of GlobularClustersG. de Marchi, STScI, Baltimore

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6 SeptemberAstromineralogy: the Search for the CrystallineSilicatesF. Molster, Research Support Division

17 SeptemberDiscontinuous Cusp: A Spatial or Temporal FeatureK.-H. Trattner, Lockheed Martin ATC

30 SeptemberThe Public Interest Perspective in PlanetaryExplorationL. Friedman, The Planetary Society

4 OctoberMassive Stars: Observations versus TheoreticalSimulationsD. Vanbeveren, Free University of Brussels

1 NovemberSearch for Aromatic Cations in Interstellar SpaceN. Boudin, Research Support Division

29 NovemberEinstein’s Telescope: Gravitational Lensing as aCosmological ToolM. Barthelman, Max-Planck-Institute, Garching

13 DecemberPrecision Atom Interferometry on Ground and inSpaceW. Ertmer, University of Hannover

Colloquia held at ESTEC

2001

8 FebruaryOur Galaxy – In Three DimensionsM. Perryman, Astrophysics Division

21 MarchThe Taming of Plasmas: Order from ChaosG. Morfill, MPI, Garching

2002

3 JuneA Family Portrait of Earth-like Planets and Moons:Similarities and DifferencesJ. Head, Brown University

7 JuneTo the Moon and BeyondH. Schmitt, Annapolis Center

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ANNEX 4Acronyms

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158 acronyms

AAS American Astronomical SocietyAAT Anglo-Australian TelescopeACE Atomic Composition Explorer (NASA)ACR Anomalous Cosmic RaysACS Advanced Camera for Surveys (HST)ADS Astrophysics Data System (NASA)AFM Atomic Force MicroscopeAGB Asymptotic Giant BranchAGN Active Galactic NucleiAGU American Geophysical UnionAIV Assembly, Integration & VerificationALICE Rosetta Orbiter UV imaging spectrometerALMA Atacama Large Millimetre ArrayAMIE Asteroid Moon micro-Imager Experiment

(SMART-1)AO Announcement of OpportunityAOT Astronomical Observing Template

APPLES ACS Pure Parallel Ly-alpha Emission SurveyAPXS Alpha-Proton-X-ray Spectrometer (Rosetta)AR Archival ResearchASI Italian Space AgencyASIC Application Specific Integrated CircuitASPOC Active Spacecraft Potential Control (Cluster)AU Astronomical Unit

BATSE Burst and Transient Source Experiment(CGRO)

BeppoSAX Satellite per Astronomia in raggi X(Italy/The Netherlands)

BHE banded hiss emissionBiSON Birmingham Solar Oscillations NetworkBLR Broad Line Region

CBRF Cosmic Background Radiation FieldCCD Charge Coupled DeviceCDMS Cluster Data Management SystemCDF-S Chandra Deep Field - SouthCDS Coronal Diagnostics Spectrometer (SOHO)CDS Centre de Données astronomiques de

StrasbourgCdTe cadmium tellurideCELIAS Charge, Element and Isotope Analysis

System (SOHO)CEPHAG Centre d’Etude des Phenomenes Aleatoires

et Geophysiques (France)CERN Centre Européen de Recherches Nucléaires

(France)CESR Centre d'Etude Spatial des Rayonnements

(France)CETP Centre d’Etudes des Environments Terrestres

et Planetaires (France)CFHT Canadian-French-Hawaiian TelescopeCIR Corotating Interaction RegionCIS Cluster Ion SpectrometryCIVA Comet Infrared and Visible Analyser

(Rosetta)CMB Cosmic Microwave BackgroundCMD colour magnitude diagramCME Coronal Mass EjectionCMOS Complementary Metal Oxide Semiconductor

CNES Centre National d’Etudes SpatialesCNR Consiglio Nazionale della Ricercha (Italy)CNRS Centre National de la Recherche Scientifique

(France)CNSA Chinese National Space AdministrationCo-I Co-InvestigatorCOMPTEL Compton Telescope (CGRO)CONSERT Comet Nucleus Sounding Experiment by

Radiowave Transmission (Rosetta)COPUOS Committee for the Peaceful Use of Outer

Space (United Nations)COROT COnvection, ROtation and planetary TransitsCOS Cosmic Origins Spectrograph (HST)COSAC Comet Sampling and Composition

Experiment (Rosetta)COSIMA Cometary Secondary Ion Mass Analyser

(Rosetta)COSPAR Committee on Space ResearchCOSPIN Cosmic Ray & Solar Charged Particles

Investigation (Ulysses)COSTEP Comprehensive Measurements of the Supra-

Thermal and Energetic Particles Populations(SOHO)

CP Charge ParityCPM Chemical Propulsion Module

(BepiColombo)CR Carrington RotationCSA Canadian Space AgencyCSDS Cluster Science Data SystemCsI caesium iodideCSRC Czech Space Research CentreCTIO Cerro Tololo Inter-American ObservatoryCTTS Classical T-Tauri StarCXB Cosmic X-ray Background

D-CIXS Demonstration of a Compact Imaging X-raySpectrometer (SMART-1)

D/SCI Directorate of Scientific Programmes (ESA)DESPA Observatoire de Paris, Département SpatialDIB Diffuse Interstellar BandDISR Descent Imager/Spectral Radiometer

(Huygens)DLR Deutsches Zentrum für Luft- und RaumfahrtDPC Data Processing CentreDPU Data Processing UnitDROID distributed readout architectureDRS disturbance reduction system (SMART-2)DSDS Double Star Data System DSN Deep Space NetworkDSP Digital Signal Processor; Double Star

Programme (China)DSRI Danish Space Research InstituteD/TOS Directorate of Technical and Operational

Support (ESA)DTP Darwin Technology PackageDXRBS Deep X-ray Radio Blazar Survey

EAS European Astronomical SocietyECF European Coordinating FacilityEC European CommissionEDI Electron Drift Instrument (Cluster)ESC Eddington Science Centre

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EFW Electric Field and Wave experiment (Cluster)

EGS European Geophysical SocietyEIT Extreme UV Imaging Telescope (SOHO)EQM Electrical Qualification ModelELF Extremely Low FrequencyEM Electrical Model, Engineering ModelEOF Experiment Operations Facility (SOHO)EP Equivalence PrincipleEPAC energetic particle instrument (Ulysses)EPDP Electric Propulsion Diagnostic Package

(SMART-1)EPIC European Photon Imaging Camera (XMM-

Newton)EPS European Physical SocietyERNE Energetic and Relativistic Nuclei and

Electron experiment (SOHO)ESA European Space AgencyESLAB European Space Laboratory (former name of

SSD/RSSD)ESO European Southern ObservatoryESOC European Space Operations Centre,

Darmstadt (Germany)ESPADONS Echelle SpectroPolarimetric Device for the

Observation of Stars at CFHTESR Emergency Sun Reacquisition (SOHO)ESRIN ESA’s Documentation and Information

Centre (Italy)ESRO European Space Research OrganisationESTEC European Space Research and Technology

Centre, Noordwijk (The Netherlands)

EUSO Extreme Universe Space ObservatoryEUV Extreme Ultra-VioletEW equivalent width

FEEP Field Emission Electric PropulsionFES Fine Error SensorFET field effect transistorFGS Fine Guidance Sensor (HST)FIRST Far Infrared and Submillimetre Space

Telescope (now Herschel)FM Flight ModelFMI Finnish Meteorological InstituteFOC Faint Object Camera (HST)FORS2 FOcal Reducer/low dispersion

Spectrograph 2 (ESO VLT)FOS Faint Object Spectrograph (HST)FOV Field of ViewFP Fabry-PérotFSRQ Flat Spectrum Radio QuasarFTE Flux Transfer EventFTS Fourier Transform SpectrometerFUV far-ultravioletFWHM Full Width at Half Maximum

GaAs gallium arsenideGC Galactic CentreGENIE Ground-based European Nulling

Interferometer ExperimentGIADA Grain Impact Analyser and Dust

Accumulator (Rosetta)

GMT Greenwich Mean TimeGOLF Global Oscillations at Low Frequency

(SOHO)GONG Global Oscillation Network GroupGOODS Great Observatories Origins Deep SurveyGORID Geostationary Orbit Impact DetectorGR General RelativityGRB Gamma Ray BurstGSE Ground Support EquipmentGSFC Goddard Space Flight Center (NASA)GSTP General Support & Technology Programme

(ESA)GTO Geostationary Transfer Orbit

HASI Huygens Atmospheric Structure InstrumentHCS Heliospheric Current SheetHDF Hubble Deep FieldHEASARC High Energy Astrophysics Science Archive

CenterHEB Hot Electron BolometerHEMT High Electron Mobility TransistorHEW Half Energy WidthHFI High Frequency Instrument (Planck)HGA High-Gain AntennaHIFI Heterodyne Instrument for FIRST (Herschel)HPGSPC High Pressure Gas Scintillation Proportional

Counter (BeppoSAX)HPOC Huygens Probe Operations CentreHR Hertzsprung-RussellHRSC High Resolution Stereo Camera (Mars

Express)HSC Herschel Science CentreHST Hubble Space Telescope

IAC Instituto de Astrofisica de CanariasIACG Inter-Agency Consultative Group for Space

ScienceIAEA International Atomic Energy AgencyIAP Institute of Atmospheric Physics (Czech

Republic)IAS Institut d’Astrophysique Spatiale, Orsay

(France)IAS Istituto di Astrofisica Spaziale (Rome)IAU International Astronomical UnionIBIS Integral imagerICC Instrument Control CentreIDC ISO Data CentreIDIS Integrated Data and Information System

(Planck)IDP Interplanetary Dust PArticleIDT Instrument Dedicated Team IFS Integral Field SpectroscopyIFSI Istituto Fisica Spazio Interplanetario (Italy)IFTS Imaging Fourier Transform SpectrometerIGM intergalactic mediumIGPP Institute of Geophysics & Planetary PhysicsILEWG International Lunar Exploration Working

GroupILWS International Living With a Star programmeIMEWG International Mars Exploration Working

GroupIMF Initial Mass Function

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160 acronyms

IMF Interplanetary Magnetic FieldIMPACT In-situ Measurements of Particles And CME

TransientsINES IUE Newly Extracted SpectraINT Isaac Newton TelescopeINTA Instituto Nacional de Técnica Aerospacial

(Spain)IOA Institute of Astronomy (Cambridge, UK)IPAC Infrared Processing Analysis CenterIR InfraredIRAS Infrared Astronomy SatelliteIRF-U Institute for Space Physics-Uppsala

(Sweden)IRSA Infrared Science ArchiveIRSI InfraRed Space InterferometerISAAC Infrared Spectrometer and Array CameraISAS Institute of Space and Astronautical Science

(Japan)ISDC Integral Science Data CentreISGRI Integral Soft Gamma Ray ImagerISL Instrument Sonde de LangmuirISM Interstellar MediumISO Infrared Space Observatory (ESA)ISOC Integral Science Operations CentreISSI International Space Science Institute, Bern

(Switzerland)Istituto TeSRE Istituto Technologie e Studio Radiazioni

Extraterrestri (Italy)ITT Invitation to TenderIUE International Ultraviolet ExplorerIUEFA IUE Final ArchiveIUPAP International Union of Pure and Applied

Physics

JCMT James Clark Maxwell TelescopeJEM-X Integral X-ray monitorJPL Jet Propulsion Laboratory (NASA)JSOC Joint Science Operation Centre (Cluster)JWST James Webb Space Telescope (formerly

NGST)

KATE X/Ka-band Telemetry & TelecommandExperiment (SMART-1)

LAEFF Laboratory for Space Astrophysics andFundamental Physics

LAP Langmuir Probe (Rosetta)LAPP Laboratoire d’Annecy-Le-Vieux de Physique

des Particules (CNRS, France)LASCO Large Angle Spectroscopic Coronagraph

(SOHO)LASP Laboratory for Astronomy and Solar Physics

(NASA)LBV Luminous Blue VariableLECS Low Energy Concentrator Spectrometer

(BeppoSAX)LEGSPC Low Energy Gas Scintillation Proportional

CounterLET Low Energy Telescope (Ulysses)LFCTR Laboratorio di Fisica Cosmica e Techologie

Relative del CNR (Italy)LFI Low Frequency Instrument (Planck)

LIC Local Interstellar CloudLISA Laser Interferometer Space AntennaLIST LISA International Science TeamLMC Large Magellanic CloudLMXRB Low Mass X-ray BinaryLOI Luminosity Oscillation Imager (SOHO)LOWL Ground-based instrument for observing solar

low p-modes, High Altitude Observatory,USA

LPCE Laboratoire de Physique et Chemie, del’Environnement (France)

LPSP Laboratoire de Physique Stellaire etPlanétaire (France)

LPV Long-Period VariableLTE Local Thermal EquilibriumLTP LISA Technology PackageLWS Long Wavelength Spectrometer (ISO)

MCP Microchannel PlateMDC Mars Dust CounterMDI Michelson Doppler Imager (SOHO)MDPU Model Data Processing UnitMECS Medium-Energy Concentrator Spectrometer

(BeppoSAX)MEDOC Multi-Experiment Data Operations CentreMHD MagnetohydrodynamicsMicroscope MICROSatellite à traînée Compensée pour

l’Observaton du Principe d’Equivalence(CNES)

MIDAS Micro-Imaging Dust Analysing System(Rosetta)

MIP Mutual Impedance Probe (Rosetta)MIRO Microwave Instrument for the Rosetta

Orbiter (Rosetta)MLT Magnetic Local TimeMMO Mercury Magnetospheric Orbiter

(BepiColombo)MOC Mission Operations CentreMOLA Mars Observer Laser AltimeterMOS-CCD Metal Oxide Semiconductor Charge Coupled

DeviceMoU Memorandum of UnderstandingMPAE Max-Planck-Institut für AeronomieMPE Max-Planck-Institut für Extraterrestrische

PhysikMPI Max-Planck Institut (Germany)MPIA MPI für AstronomieMPIK Max-Planck-Institut für KernphysikMPO Mercury Planetary Orbiter (BepiColombo)MSE Mercury Surface Element (BepiColombo)MSSL Mullard Space Science Laboratory (UK)MUPUS Multi-Purpose Sensors for Surface and

Subsurface Science (Rosetta)MUSICOS Multi-Site Continuous SpectroscopyMXB Medium X-ray Band

NAC Narrow Angle Camera (OSIRIS)NARVAL New Echelle Spectropolarimeter at Bernard

Lyot Telescope (Pic du Midi, France)NASA National Aeronautics & Space

Administration (USA)NED NASA Extragalactic Database

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NFI Narrow Field Instrument (BeppoSAX)NGST Next Generation Space Telescope (now

James Webb Space Telescope)NHSC NASA Herschel Science CenterNICMOS Near-Infrared Camera and Multi-Object

Spectrometer (HST)NIS normal incidence spectrometerNLR Narrow Line RegionNOT Nordic Optical TelescopeNRAO National Radio Astronomy Observatory

(USA)NRT Near Real TimeNSI NASA Science InternetNSSDC National Space Science Data Center (at

GSFC, USA)NSLS National Synchotron Light Source (USA)NTT New Technology TelescopeNVSS NRAO/VLA Sky Survey

OAT Osservatorio Astronomico di TriesteOHP Observatoire de Haute-ProvenceOM Optical Monitor (XMM-Newton)OMC Optical Monitor Camera (Integral)ONC Orion Nebula ClusterOSIRIS Optical and Spectroscopic Remote Imaging

System (Rosetta)

PACS Photodetector Array Camera andSpectrometer (Herschel)

PAH Polycyclic Aromatic Hydrocarbonpc parsecPCD Photon Counting DetectorPDD Payload Definition DocumentPDFE Particle Detector Front EndPDS Planetary Data SystemPDS Phoswich Detector SystemPI Principal InvestigatorPIA (ISO)PHOT Interactive AnalysisPIPS Passivated Implanted Planar SiliconPLM Payload ModulePMS Pre-Main SequencePN Planetary NebulaPOS Payload Operations Service (Mars Express)PP Permittivity Probe (SESAME on Rosetta)ppm parts per millionPR Public RelationsPS Project ScientistPST Project Scientist TeamPSF Point Spread FunctionPWA Permitivity, Waves and Altimetry (part of

HASI on Huygens)PWG Payload Working Group

QED Quantum ElectrodynamicsQM Qualification ModelQPO Quasi Periodic OscillationsQSO Quasi Stellar ObjectR&D Research and DevelopmentRAL Rutherford Appleton Laboratory (UK)RF Radio FrequencyRGS Reflection Grating Spectrometer (XMM-

Newton)

RHESSI Reuven Ramaty High Energy SolarSpectroscopic Imager (NASA)

RMOC Rosetta Mission Operations CentreROLIS Rosetta Lander Imaging SystemROMAP RoLand Magnetometer & Plasma Monitor

(Rosetta)ROSINA Rosetta Orbiter Spectrometer for Ion and

Neutral Analysis (Rosetta)ROSITA Roentgen Survey with an Imaging Telescope

ArrayRPC Rosetta Plasma ConsortiumRSI Radio Science InvestigationRSOC Rosetta Science Operations CentreRSSD Research and Scientific Support Department

(ESA)

SAO Smithsonian Astrophysical Observatory (US)SAp/Saclay Service d’Astrophysique (Commissariat à

l’Energie Atomique; Saclay, France)SAS Scientific Analysis Software (XMM-

Newton); Science Analysis Subsystem(XMM-Newton)

SAX Satellite per Astronomia in raggi X(Italy/The Netherlands)

SCAM Superconducting CameraSciSIM Science SimulatorSCUBA Submillimetre Common User Bolometer

ArraySEA Sociedad Española de AstronomiaSED Spectral Energy DistributionSEM Scanning Electron MicroscopeSEP solar energetic particleSEPM Solar Electric Propulsion Module

(BepiColombo)SEPP Solar Electric Primary PropulsionSEPT Solar Energetic Particle Telescope (STEREO

mission)SESAME Surface Electric, Seismic and

Acoustic Monitoring Experiment (Rosetta)SEST ESO sub-mm telescopeSETI Search for Extra-Terrestrial IntelligenceSFH Star Formation HistorySFR Star Formation RateSGS Science Ground System (Integral)SIMBA SEST Imaging Bolometer ArraySIMBAD Set of Identifications, Measurements and

Bibliography on Astronomical DataSIR Stream Interacting RegionSIRTF Space Infrared Telescope Facility (NASA)SIS Superconductor-Insulator-SuperconductorSLP Segmented Langmuir ProbeSM Servicing Mission (Hubble)SMART Small Mission for Advanced Research in

Technology (ESA)SMC Small Magellanic CloudSMEX Small Explorer (NASA)SMOG Survey of Molecular Oxygen in the Galaxy

(SMART-1)SN SupernovaSNR Supernova RemnantSOC Science Operations Centre; self-organising

criticality

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162 acronyms

SOHO Solar and Heliospheric ObservatorySOS Silicon-on-SapphireSOT Science Operations TeamSPC Science Programme Committee (ESA)SPEDE Spacecraft Potential, Electron & Dust

Experiment (SMART-1)SPI Integral spectrometerSPIRE Spectral and Photometric Imaging Receiver

(Herschel)SQUID Superconducting Quantum Interference

Device (STEP)SRON Space Research Organisation NetherlandsSRV Semi-Regular VariableSSAC Space Science Advisory Committee (ESA)SSC Survey Science ConsortiumSSD Space Science Department (ESA), now

RSSDSSP Surface Science Package (Huygens and

Rosetta)SSWG Solar System Working GroupST Science Team; Space Technology (NASA)ST-ECF Space Telescope European Coordinating

FacilitySTAFF Spatio-Temporal Analyis of Field

Fluctuations (Cluster)STEP Satellite Test of the Equivalence PrincipleSTEREO Solar-Terrestrial Relations Observatory

(NASA)STIS Space Telescope Imaging SpectrographSTJ Superconducting Tunnel JunctionSTScI Space Telescope Science InstituteSUMER Solar UV Measurements of Emitted

Radiation (SOHO)SWAN Solar Wind Anisotropies (SOHO)SWAS Submillimeter Wave Astronomy Satellite

(NASA)SWS Short Wavelength Spectrometer (ISO)SWT Science Working TeamSVM service moduleSXB Soft X-ray BandSXT Soft X-ray Telescope (Yohkoh)SZ Sunyaev-Zeldovich Effect

TAC Time Allocation CommitteeToO Target of OpportunityTPF Terrestrial Planet Finder (NASA)TRACE Transition Region & Coronal Explorer

(NASA)TRIP Technology Readiness and Implementation

PlanTRM Technology Reference MissionTRP Technology Research Programme (ESA)TSI Total Solar Irradiance

UCB University of California BerkeleyUCLA University of California Los AngelesUH Ultra-heavy (cosmic ray nuclei)ULIRG ultraluminous infrared galaxyURSI Union Radio Scientifique InternationaleUSNO US Naval ObservatoryUV Ultra-VioletUVCS Ultra-Violet Coronal Spectrometer (SOHO)UVES Ultraviolet-Visual Echelle Spectrograph

(ESO VLT)

VILSPA Villafranca Satellite Tracking StationVIMOS VLT Visible Multi-Object Spectrograph

(ESO VLT)VIRGO Variability of Irradiance and Gravity

Oscillations (SOHO)VIRTIS Visible Infra Red Thermal Imaging

Spectrometer (Rosetta)VLA Very Large ArrayVLBI Very Long Baseline InterferometryVLF Very Low FrequencyVLT Very Large TelescopeVLTI Very Large Telescope Interferometer (ESO

VLT)VMC Venus Monitoring CameraVTT Vacuum Tower Telescope

WAC Wide Angle Camera (OSIRIS on Rosetta)WBD Wide Band Data (Cluster)WEC Wave Experiment Consortium (Cluster)WFC Wide-Field Camera (HST)WFPC Wide-Field Planetary Camera (HST)WHISPER Waves of High Frequency and Sounder for

Probing of Density by Relaxation (Cluster)WHT William Herschel TelescopeWTTS Weak-lined T Tauri StarWWW World Wide Web

XEUS X-ray Evolving Universe Spectroscopymission (ESA)

XMM X-ray Multi-Mirror Mission (ESA); nowXMM-Newton

YGT Young Graduate TraineeYSO Young Stellar Object

ZAMS Zero Age Main Sequence

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