relativistic and particle astrophysics enrico costa – iasf, 25 november 2007 – 1 presentations...

RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 1

Presentations to the Visiting Committee

RELATIVISTIC and PARTICLE ASTROPHYSICS

Relativistic and particle Astrophysicsthe past and the present

This part of the institute has systematically grown and is now ~ 40% of IASF

Senior scientists, expert technicians, many young reserchers, graduation and PHD thesis, post-doc.

Many projects reasonably staffed but (according to italian standards) too much unbalanced toward temporary positions on external funds.




The first stepsIn the Gratton Era

1968-1969. Two rocketts for all sky X-Ray survey: a Nike-Apache and a Skylark.Payloads all made in the house except detectors (purchased from LND)

LAS

1975 – 1977 A rocket experiment in collaboration with AS&E and MIT → CFA

1-d Baez telescope with an imaging proportional counter:

Role of LAS (now IASF): refurbishment, alignment and calibration of the telescope. IPC. Front End. Electronics.

1975-1976 Preparation of a rocket experiment with CFA (never flown):

Si(Li) detector in the focus of a grazing incidence concentrator.

Role of LAS: Detector, telescope, electronics.

R&D driven by these experiments:

Imaging Proportional Counters, X-ray optics, Electronics




The Balloon Era (1976 – 1990)

Experiments aboard stratospheric Balloons launched from Sicily, USA, Brazil, India, Australia for HardX-Ray Soft -Ray Astronomy

An all domestic line:

Large area high pressure proportional counters coolimated

Imaging high pressure proportional counters with coded masks

In collaboration with other institutes (+Southampton, Saclay, Toulouse, Tubingen)

Large area -ray imager with coded mask

Large area -ray timing experiment

Low background scintillators

Some success, some failure, more than a decent scientific throughput

A great school! How to handle an experiment from the first concept, to the building, to flight operations, to data analysis.A boost to R&D: Proportional Counters, Imaging Detectors, Scintillators, theory and practice of Coded Masks




High Energy Astrophysicsnot only connected to hardware

e.g. 25 years study of symbiotic star AG Draconis




XMM & ground observations of AG Dra during quiescence and outburst

burst min

Energy distribution at V min & V max

AG DRACONIS K 3 III + WD

Pop II symbiotic binary

Recurrent outbursts

Strong UV source

Super Soft XR source (15 eV,2600 L)

Optical and X-ray light curves Path of the WD in the L-T diagram (from IUE)

X-ray Vs. visual/UV anticorrelation

XMM observations before & after the 2005 burst




AG Draconis is a symbiotic binary composed of a red giant stars and a White Dwarf.

The wind of the giant is accreted onto the WD surface. The hydrogen burning heats the WD to 15 eV.

Since 3 decades we are monitoring AG Draconis in optical, ultraviolet and X-ray bands.

AG Draconis is subject to recurrent light maxima, or bursts, during which the optical and ultraviolet flux increases – while the X-rays above 100 eV nearly disappear. (See the EXOSAT, ROSAT and XMM light curves on the top of the panel).

The next panel shows the path of the WD in the L-T diagram as derived from our IUE observations.

The third panel shows variation of the X ray to optical energy distribution. The X-ray variations are best seen in the next panel, where XMM observations taken 44 days apart before and after the beginning of a new burst are shown.

Finally, XMM unveiled the presence of a, probably steady, higher energy tail that we suppose be formed in a shocked region around the system.

Our XMM observations are basic to best quantify the X-ray Vs. optical-ultraviolet ANTICORRELATION, as seen in the last panel.




Another long term research

Multifrequency Studies

an example:




GeV – TeV anticorrelated emission from Cyg X-1

1-10 GeVjet+counter jet

1-10 GeVjet

> 0.2 TeVjet+counter jet

> 0.2 TeVjet

-ray light curves produced by electrons accelerated in the jets of Cyg X-1

Power law spectrum of electrons E-2

Bednarek, W. & Giovannelli, F.: 2007, A&A 464, 437-445

AGILEGLAST

MAGICVERITAS



RELATIVISTIC and PARTICLE ASTROPHYSICSSAXSAX was proposed to CNR (ASI would arrive later) in June 1981

IAS is present from the first proposal

A role in all the Working Groups of the mission and in the Science Management

The role of IAS increases wit time and becomes outstanding after the launch: Mission Scientist, Leadership in GRB research, leadership in LMXRB




The Role of IASF

A role in the Payload Development: • Phoswich Detector System

• Gamma Ray Burst Monitor

• Wide Field Cameras

A role in science management• Experiment Investigator WG

• DataAnalysis WG

• Science WG After the Launch Mission Scientist from IASF




GRB: The BeppoSAX ERAThe major discoveries

• X-ray afterglow• Optical Afterglow• Host Galaxy• Red-shift• Broad Band Variability • Dark Afterglows• Supernova Connection• X-ray Flash• Ep – Eiso relation

The discovery of the X-ray afterglow was the starting point of all the Beppo Sax revolution. It proceeded from the combined use of the wide field/narrow field instruments of SAX following an ad hoc procedure involving many teams (GRBM/PDS, WFC, MECS, Science Operation Center, Operation Control Center, Mission Scientist, Mission Director). 2 out of the 4 coordinators and 3 out of the 8 PIs were from IAS.




Clues of GRB revolution

GRBM

First X-Ray Afterglow

First Optical Afterglo

w

First Red-shift

First Radio

Afterglow




SAX not only GRBs

An instance of relevant result:

The hard X-Ray emission of some Clusters




NT HXR emission was predicted in 1970s in clusters showing diffuse radio emission (see: Perola & Reinhardt 1972, Rephaeli 1979) IC emission relativistic radio electrons CMB photons

Observations:

Balloon experiments Bazzano et al 1984;1990

HEAO-1 Rephaeli, Gruber & Rothschild 1987

Rephaeli & Gruber 1988

OSSE exp. (Compton-GRO) Rephaeli, Ulmer & Gruber 1994

RXTE & ASCA Delzer & Henriksen 1998

Cluster Hard Excess




Coma Cluster & Abell 2256

Excess ~ 4.8FNT

X ~ 1.5 x 10-11 cgs (20-80 keV)

Fusco-Femiano et al 2004 Fusco-Femiano et al. 2005

Coma A2256

FNTX ~ 9 x 10-12 cgs

(20-80 keV)

BeppoSAX BeppoSAX




GRBs in the SWIFT Era




GRB engine re-activation? X-ray versus GeV flares •Roughly 40% of GRBs show X-ray flares at hundreds-thousands of seconds

after the prompt, carrying a significant amount of the total energy.

•Most present models require a central source producing energy on time scales much longer than few seconds. Crucial to the understanding of the central source

• HOW ? We predict that X-ray flares should be associated with high energy flares (expected by IC), and find that their properties are strictly connected and model dependent. Simultaneous X-ray (SWIFT) and GeV observations (AGILE and GLAST) are thus very important to constrain the duration of engine activity.Delayed External Shock

LAT sensitivity

XRT BAT

Late InternalShock




The mysterious origin of X-Ray Flashes

HIGH REDSHIFT SCENARIO: XRFs are GRBs at high redshift (z >5) . Swift XRFs are at low redshift. This clearly rules out the high distance hypothesis.

OFF AXIS SCENARIO: XRFs are GRBs seen at large angles from the direction of the jet. Different jet structures have been proposed which predict a specific value of the GRB-to-XRF X-ray afterglow luminosity ratio.

Swift has permitted for the first time the access to XRF X-ray afterglow luminosity. Only a jet with uniform energy distribution can account for XRF afterglow properties. However, this models does not explain prompt emission properties …

A NEW POPULATION of subenergetic progenitors?

XRFs are a new population of GRBs discovered by BeppoSAX with most of the energy emitted in the X-ray band.

We are investigating their origin using BeppoSAX and Swift data.




Long and short GRBs are likely related to different progenitors:Long and short GRBs are likely related to different progenitors:collapsars vs compact binary coalescencecollapsars vs compact binary coalescence

E.g. of E.g. of 22 mapping (Emapping (E52 52 - n - n

plane) around plane) around the best fit the best fit solution for solution for short GRB short GRB

051221051221

The The circum-burst mediumcircum-burst medium should should reflect this difference: relatively high reflect this difference: relatively high density environments vs a more density environments vs a more tenuous ISM. Using a numerical tenuous ISM. Using a numerical routine based on routine based on 2 mapping, broad-2 mapping, broad-band afterglow data are analyzed in band afterglow data are analyzed in the standard fireball model, to test if the standard fireball model, to test if present data allow to discern the present data allow to discern the expected difference in density expected difference in density between short-long GRBs.between short-long GRBs.

In the gravitational wave (GW) In the gravitational wave (GW) domain, an in-spiral signal is a domain, an in-spiral signal is a telltail signature for distinguishing a telltail signature for distinguishing a short GRB progenitor from a short GRB progenitor from a collapsar. We thus develop a collapsar. We thus develop a parallel study in the GW domain, parallel study in the GW domain, using Virgo & LIGO data collected using Virgo & LIGO data collected between May and September 2007, between May and September 2007, and in view of the future advanced and in view of the future advanced configurations of these detectors.configurations of these detectors. ns-ns m1= m2 =1.4 M

- - - - in-spiral - - - - in-spiral - - -merger

53 Mpc

220 Mpc

1100 Mpc

Advanced VirgoVirgo

Short GRBs: environment and GW signal as clues to the progenitorShort GRBs: environment and GW signal as clues to the progenitor




INTEGRAL




INTEGRALINTEGRALGamma-ray observatory 15 keV – 10 MeVHigh resolution spectroscopy (SPI) and fine imaging (IBIS) within large FOVMedium-size mission (ESA, Russia, NASA), launched in Oct 2002Community involved via AOs Public archive access, User Group, TAC

IBIS/INTEGRAL: THE unique imager for high energy point sources

Fine imaging of high energy sources and monitoring of large parts of the highly variable sky is crucial for astrophysics

IBIS (Imager)IBIS (Imager)

9x99x9°° PCFOV PCFOV30x3030x30° FOV° FOV

12’ angular resolution12’ angular resolution

positions to ~1’positions to ~1’

ISGRI: 15keV – 1MeVISGRI: 15keV – 1MeVPICSIT: 0.2 – 10 MeVPICSIT: 0.2 – 10 MeV

~10% energy ~10% energy resolutionresolution

<<1ms timing<<1ms timing

IASF-Roma responsible for IBIS in-flightPerformances & Instrument responce

Core Programme Assigned Scientific Topics:Weak BHCs ,X-ray Bursts sources, 1E1740.7-2942, and SURVEY




Spectral evolution of Black hole candidates, Capitanio et al., 2006

Observational INTEGRAL data as inputs for modelling, 1E1740.9-2942 from Del Santo et a., 2006

X-ray Burst Sources most of time @ low luminosity hard state with energy “flat” spectra very similar (Fiocchi et al. 2007)

First Non-thermal emission detected in the hard state for 4U1820-30, Tarana et al.,2007




From BeppoSAX/WFCs to INTEGRAL/IBIS

30 sources detected in the bulge in the 3-20 keV band and 2003 ‘s view of sky distribution of X-ray binaries

~ 70 sources in a ±10 degree region around G.C. and 120 in a ±20 degree, 20-100 keV460 souces in total! i.e. 1‰ of the classical (>10 keV) X-ray sources discovered so far




0

20

40

60

80

100

120

CV AGN HMXB LMXB Other ?

Cat 1

Cat 2

Cat 3

0

10

20

30

40

50

LMXB HMXB AGN Others ?

Sources at energy > 100 keV

Survey 2

Survey 1

Bird A.J., Malizia A., Bazzano A. and Survey team 2007

The nature of the Galactic diffuse continuum emission :

E <100 keV, 80% due to point sources

Individual point souces contribute for 70-80% in the 100 keV-300 KeV band

While active galaxies account for only 3% of the X ray background for E>100 keV

Bazzano A. Stephen J. , Fiocchi MT.and Survey team 2006 and 2007

IBIS Survey, specific source classes analysis and follow-up in collaboration with Soton University & IASF Bologna




What we expect in 1993!!

Compact stellar-size objectsHigh energy transientsExtragalactic sourcesStellar and Explosive NucleosynthesisDiffuse continuum &diffuse line emission plus: Unexpected Discoveries !!

UNEXPECTED DISCOVERIS already!

Obscured HMXB:Find slow (100-1000s) NS, <1013 G, no cyclotron lines, no BH.-: Transient and persistent sources with NH in excess of 10 23 cm-2 difficult to

catch

Super-giant fast transients:Accretion via wind, but disk is

needed to explain fast luminosity increase (x 102 – 103).

-: Transient sources, difficult to catch

A long term monitoring programme with large FOV is crucial to enlarge the database

V. Sguera et al., ApJ 646, 453 2006

IGR J174544-2619 2 hr flare




The keV to TeV connection: a new class of cosmic accelerators

X & Gamma-ray observations of TeV sources crucial to discriminate between leptonic versus hadronic scenarios a source natureThe Integral survey with about 500 sources in the 20-100 keV band provide a fantastic tool to this item.

Ubertini et al., 2005

Dean A.J., De Rosa A. et al., 2007

HESS J1813-178 characteristcs pointed to a PWN/SNR nature:

IGR J1813-1751 from IBIS plus ASCA archival data clearly identified it

IBIS measurement of the composite SNR G11.2-0.3 and associated Pulsar, suggested that soft γ-ray emission is NOT coming from SNR but originates within complex structure associated with the Pulsar and its PWN system




The last son




AGILEThe AGILE Payload: a highly compact instrument for high-energy astrophysics: it combines for the first time a gamma-ray imager (30 MeV- 30 GeV) with a hard X-ray imager (18-60 keV) with large FOVs (2.5 sr and 1 sr respectively) and optimal angular resolution.

Compactness from Si microstrip technology.

Complex functions implemented aboard: 1 DSP, 27 FPGA.

High resolution (2 s) timing with PPS

And all this with:only ~100 kg of Payloadonly ~100 W of PL absorbed poweronly 350 kg of satellite…limited budget and resources




An all italian mission: ASI with contributions of INAF&INFNINAF: IASF Roma, IASF Bologna, IASF MilanoINFN: Sez.Trieste, Sez. Roma I, Sez. Roma IIUniversità di Roma “Tor Vergata”, Università “La Sapienza”CIFS - Consorzio Interuniversitario per la Fisica Spaziale (Torino)

ASI Scientific Data Center has an important role in archiving, interface to the community, support to guest activities, S/W documentation.

PI (M.Tavani) and PI Team, Payload Management, Team Data CenterThe X-ray monitor SuperAGILE

The role of IASF Roma

The role of the community

AOO, Open Archive, Distribution by web of X-ray fluxes, networks of multifrequency observers

Selected topics on the Core Program:

GRBs, Diffuse, New Sources, Selcted Targets



RELATIVISTIC and PARTICLE ASTROPHYSICSWho has done what

ANTICOINCIDENCE

INAF-IASF-Mi (F.Perotti)

HARD X-RAY IMAGER (SUPER-AGILE)

INAF-IASF-Rm (E.Costa, M. Feroci)

GAMMA-RAY IMAGER

SILICON TRACKER

INFN-Trieste

(G.Barbiellini, M. Prest)

(MINI) CALORIMETER

INAF-IASF-Bo, Thales-Alenia Space (LABEN)

(G. Di Cocco, C. Labanti)




GRID Effective Area

20-100 MeV

500-> 400 cm²

Gamma Ray Imaging Detecor - GRID

A Silicon TrackerA Silicon Tracker

AndAnd

A Mini-CalorimeterA Mini-Calorimeter

Thanks to Silicon Strip Technique and onboard preselection and on ground selection of events based on logic only (no TOF, no Cherekov) the GRID has a very large f.o.v. = 2.5 sr

Information from MCAL combined with information on scattering of pairs in converters allows for energy reconstruction

10 planes with * 0.07 X0

40 mm resolutionTotal: ~0.9 X0




PSLV-C8 launch, 23 Apr. 2007




AGILE first results (July-November, 2007)• Vela and Crab PSR calibration

• Several Galactic hard X-ray sources• 4 detections of blazars

3C 279 3C 454.3 (repeated gamma-ray flares) HB 1510-089 TXS 0716+714 • Several GRBs detected by Super-A and MCAL (MCAL detects ~ 1/week)• 2 GRBs positioned by SA (X-ray AG by SWIFT) and 1 by SA+IPN




September 28, 2007

The Great Triade

AGILE AND PULSARS

Thanks to PPS we can easily handle high resolution timing.

Agreements are active with radio telescopes to have ephemeris of known and candidate PSR

By folding photons (E>100MeV) detected within the PSF of PS0835-45, in bins of 0.5 ms with the radio period we have the light curve (20 days, July – August 2007)

.




More than 30 sources already detected (+GRBs+SGR)

SuperAGILE is a double 1-d imager based on Silicon Strip Detectors and Tungsten coded mask. ~ 10 kg ~ 10W (Feroci et al.NIM 2007)

SuperAGILE View of the Galactic Plane(3.6 days, l=337, b=8)




BLAZARS

3C 279 ! (9-13 July, 2007)




3C 454.3

+AGILE pointing centroid

~ 36°




HB 1510-089

Galactic Center




GRBs with AGILE




GRB 071104, at ~22º Localized by SA, XRT by SWIFT, OT by Telescopio Nazionale Galileo

SA (20-60keV)

Light curve

Image

Minicalorimeter 350-700 keV

GRIDS-events (<30MeV)suspect activity

>30MeV

No activity




Something Very Recent




3C 454.3

Cygnus region

AGILE gamma-ray sky: 22 Nov. 2007

INTEGRAL

TOO




Commissioning of AGILE was not completed in July.

Some activities are in progress in these weeks included Activation of the GRB onboard

capability.The GRB is triggered as a step in the counting rate of SA and/or

MCAL v/s moving average.

The SuperAGILE image is analysed aboard (included corrections for aspect instability) and compared with pre-burst image. The coordinates of the Burst are determined and transmitted to ground via a text message by ORBCOMM network.

Trigger Deconvolved Image to ORBCOMM

Del Monte et al. 2007 A&A




Waiting for future missions….

relativistic and particle astrophysics enrico costa – iasf, 25 november 2007 – 1 presentations...

Documents

imaging proportional

burst slide

imaging detectors

iasf senior scientists

rocket experiment

iue xray

xray optics

role of las