ALMA HERSCHEL SYNERGIESALMA HERSCHEL SYNERGIESOrigins of galaxies, stars, planetsOrigins of galaxies, stars, planetsRecommendationsRecommendationsto ESA and ESOto ESA and ESO

Paola Andreani, T. Wilson ……Paola Andreani, T. Wilson ……

D. Bockelee-Morvan (Paris)D. Bockelee-Morvan (Paris)J. Cernicharo (Madrid)J. Cernicharo (Madrid)P. Cox (Grenoble)P. Cox (Grenoble)C. De Breuck (ESO)C. De Breuck (ESO)D. Elbaz (Paris)D. Elbaz (Paris)E. van Dishoeck (Leiden)E. van Dishoeck (Leiden)M. Gerin (Paris)M. Gerin (Paris)R. Fosbury (ECF-ESA)R. Fosbury (ECF-ESA)R. Laing (ESO)R. Laing (ESO)E. Lellouch (Paris)E. Lellouch (Paris)G.L.Pilbratt (ESA)G.L.Pilbratt (ESA)P. Schilke (Bonn)P. Schilke (Bonn)C. Waelkens (Leuven)C. Waelkens (Leuven)M. Zwaan (ESO)M. Zwaan (ESO)ContributorsContributors

TALK OUTLINETALK OUTLINE• Synergies?Synergies?• Why FIR and Submm?Why FIR and Submm?• ALMA, HERSCHELALMA, HERSCHEL ‘complementary’ ‘complementary’ • Common Scientific ProjectsCommon Scientific Projects Stars and dust formation Stars and dust formation Star forming regions and MCsStar forming regions and MCs Nearby spirals, LSBGs, DGs, AGNNearby spirals, LSBGs, DGs, AGN CIRB, high-z sources, AGNCIRB, high-z sources, AGN

• Recommendations to ESA/ESORecommendations to ESA/ESO

• Science topics: objects of both Science topics: objects of both instrumentsinstruments

• ESA+ESO act in common to best ESA+ESO act in common to best exploit scientific returnexploit scientific return

• Legacy? Joint-time?Legacy? Joint-time?• Joint analysis of observationsJoint analysis of observations• How operate data flow?How operate data flow?• Common calibrationCommon calibration

SynergiesSynergies

SB spectrumSB spectrum Protostar developmentProtostar development

Why FIR/submm?Why FIR/submm?

K-correctionK-correctionSensitivity with 6 antennas

Blain, 04Blain, 04 Griffin, 05Griffin, 05

z = 2.55z = 2.55 z ~ 0.7-2.5z ~ 0.7-2.5

Cluster A1835Cluster A1835

(Ivison et al., 2000)

Obscured sourcesObscured sources

ALMA Main + Compact ALMA Main + Compact ArrayArray

Main (50 12m) antennas + ACA (4 12m + 12 7m) Main (50 12m) antennas + ACA (4 12m + 12 7m)

FOV 50-85’’ at 3mm (90GHz)FOV 50-85’’ at 3mm (90GHz) 8.3-14’’ at 0.5mm (600GHz)8.3-14’’ at 0.5mm (600GHz)

Resolution: 0.03-4’’ at 3mmResolution: 0.03-4’’ at 3mm 0.005-0.7’’ at 0.5mm0.005-0.7’’ at 0.5mm

Sensitivity (5Sensitivity (5, 1h) @3mm and 0.5’’ resol (1km , 1h) @3mm and 0.5’’ resol (1km baseline)baseline) continuum 0.03mJycontinuum 0.03mJy line 3mJy line 3mJy

(‘’) = 0.2 (‘’) = 0.2 (mm) / B(km)(mm) / B(km)SS = 2k/Aeff T= 2k/Aeff Tsyssys//√√N(N-1) N(N-1) ttintint

Band3: 84-116 Band4: 125-163 Band5: 163-211 Band6: 211-275 Band3: 84-116 Band4: 125-163 Band5: 163-211 Band6: 211-275 Band7: 275-373 Band8: 385-500 Band9: 602-702 Band10: 787-950Band7: 275-373 Band8: 385-500 Band9: 602-702 Band10: 787-950 GHz GHz

Band1:Band1:31.3-4531.3-45Band2:Band2:67-9067-90GHzGHz

ALMA ReceiversALMA Receivers

★ ★ Japanese contribution all telescopes plus ACAJapanese contribution all telescopes plus ACA★ ★ EC funded 8 receivers ALMA-Herschel synergyEC funded 8 receivers ALMA-Herschel synergy

HerschelHerschel

fourth cornerstone fourth cornerstone mission in ESA's mission in ESA's

Horizon 2000 Horizon 2000 programmeprogramme

launch during 2008launch during 20083.5 m passively cooled to 3.5 m passively cooled to

80 K80 K3 cold focal plan 3 cold focal plan

instruments instruments photometry and photometry and spectroscopy in the spectroscopy in the 60 – 670 µm range60 – 670 µm range

liquid helium cryostat liquid helium cryostat operational lifetime of operational lifetime of

at least 3 yearsat least 3 years

Photometry with Photometry with HerschelHerschelPACSPACS SPIRSPIR

EE

centcent 7575µmµm 110110µmµm 170170µmµm 250250µmµm 350350µmµm 500500µmµm

60-9060-90 90-13090-130 130-130-210210

210-210-290290

290-290-400400

410-580410-580

SensitiviSensitivityty

mJy,5mJy,5,1,1hh

33 33 33 1.11.1 1.21.2 1.51.5

FOVFOV(arcmin)(arcmin)

1.8x3.1.8x3.55

1.8x3.51.8x3.5 1.8x3.51.8x3.5 4x84x8 4x84x8 4x84x8

AngulaAngular res.r res.

5”5” 8”8” 12”12” 17”17” 24”24” 35”35”

Spectroscopy with Spectroscopy with HerschelHerschel

HIFIHIFI PACSPACS SPIRESPIRESpectral range

480-1250GHz (240-480-1250GHz (240-625625µm)µm)

1410-1910GHz(157-1410-1910GHz(157-212212µm)µm)

1426-4997GHz1426-4997GHz

(60-210(60-210µm)µm)447-1499GHz447-1499GHz

(200-670(200-670µm)µm)

Sp band

WBS: 4GHz HRS: WBS: 4GHz HRS: 1/0.5GHz1/0.5GHz

------------------ ------------------

Spectral res

WBS(1MHz) 0.2-0.6km/sWBS(1MHz) 0.2-0.6km/s

HRS(100/200kHz) 0.03-HRS(100/200kHz) 0.03-0.06/0.13km/s R=2 100.06/0.13km/s R=2 1066--101077

100-250 km/s100-250 km/s

R=1200-3000R=1200-3000300-15000km/s300-15000km/s

R=20-1000R=20-1000

Flux limit

R=10R=1033 1.1-3.2 mK (0.5- 1.1-3.2 mK (0.5-1.5Jy)1.5Jy)

R=10R=106 6 34-100 mK (15-46 34-100 mK (15-46 Jy)Jy)

R=10R=1033 0.16- 0.16-0.21 (0.11-0.14 0.21 (0.11-0.14 Jy)Jy)

R=10R=1033 2.9-3.2 Jy PS 2.9-3.2 Jy PS

7.2-8.4Jy 7.2-8.4Jy

Line flux limit10-18W/m2

0.9-7 0.9-7 7.8 (607.8 (60µmµm) PS) PS

2.5 (1802.5 (180µm)µm)38 (200-30038 (200-300µmµm) PS) PS

35 (300-40035 (300-400µmµm))

35-70 (400-67035-70 (400-670µmµm))

FOV 47”x47”47”x47” 2.6’x2.6’2.6’x2.6’

HPBW 46-12”46-12” 9.4”9.4” 18”, 25”18”, 25”

Common scientific Common scientific projectsprojects

• Star formationStar formation• Planetary system formationPlanetary system formation• Nearby galaxiesNearby galaxies• Galaxy formationGalaxy formation• AGN-Host joint formation/BH AGN-Host joint formation/BH

formationformation

Standard model of star Standard model of star formationformation1. Formation of pre-stellar clumps in molecular clouds.

2. The pre-stellar clump collapses

3. Protostar (infall and outflow coexists) 4. Formation of a planetary systemFig. from McCaughrean

Star formationStar formationFour stages of star Four stages of star formationformation

Collapse of MCCollapse of MChigh gas density + low Tkin,grain properties changeAccretion phaseAccretion phase

Optically thick disc+Optically thick disc+Star is emerging, outflowStar is emerging, outflow

Star + disc, outflowStar + disc, outflow

NIR HNIR H22

SiOSiO

Chemistry as a clock for Chemistry as a clock for YSOsYSOs

13CO

C18O

C17O

H13CO+

N2H+

NH3

CH3OH

H2CO

HCOOH

CH3CN

SiOSO

CH3OH

CN HCN

C2H3CN

C2H5CN

• HIGAL (HSO OT proposal) map the Galactic Centre in SPIRE (PACS) bands

• ALMA could map 1 �2 at 350GHz in 180 h to– 0.7mJy sensitivity (0.15 M at 20K)

• 1" beam (8500AU) would give T=0.6K at 1 km/s resolution

• Possible lines in 2x4GHz passband: SiO 8-7, H13CO+ 4-3, H13CN 4-3, CO 3-2

CH3CN, CH3OH

HCN 4-3, HCO+ 4-3

H13CN 4-3, CS 7-6, CO 3-2

SCUBA 850 micron: Pierce-Price et al 2000

SCUBA 450 micron

Star Formation at the Galactic Centre

Star formationStar formation• PACS+SPIRE:PACS+SPIRE: grain properties, maps of star

forming regions in continuum, mass spectrum for small masses (IMF) + OI 63 m line maps on the large scale

• HIFI:HIFI: molecules (mainly H2O) + detailed kinematics of star forming regions

• ALMA:ALMA: molecules at higher spatial resolution + outflows

Leonardo Testi, An HSO Survey of Nearby Star Forming Regions,Garching28 January 2003

An HSO Survey of Nearby SFR

IFSI : P. Saraceno

M. Benedettini , A. di Giorgio, S. Molinari, S. Pezzuto , S. Viti

Arcetri : L. Testi, P. Caselli

OVRO 3mm

PACS 100m

Serpens Serpens (Testi, priv)(Testi, priv)

High spatial res at High spatial res at SED max of most SF SED max of most SF regionsregionsseparate the mainseparate the mainsources of luminositysources of luminosity

Evolved stars and dust Evolved stars and dust formationformation

• AGB POST-AGB PNAGB POST-AGB PN• Outflow mass loss + Outflow mass loss +

properties of the dust and properties of the dust and formation siteformation site

• Most of the solid-state Most of the solid-state features in MIR + NIR features in MIR + NIR

• @FIR: Forsterite + Calcite + @FIR: Forsterite + Calcite + crystalline Hcrystalline H22O iceO ice

• @submm: SiO-H@submm: SiO-H22O masers O masers

IRC+10216IRC+10216

HST optical image HST optical image + CO contoursHST optical image HST optical image + CO contours

(CO : Wilson et al. 2000)(CO : Wilson et al. 2000)(HST: Whitmore et al. 1999)(HST: Whitmore et al. 1999)

Dust and molecular emission from Dust and molecular emission from optically obscured regionsoptically obscured regions

The “Antennae”The “Antennae”

The Cosmic Extragalactic The Cosmic Extragalactic BackgroundBackground

Franceschini 2000

IR Optical

10001000mm

∫ ∫ I(I()d)d = 30nW/m = 30nW/m22/sr/sr

100100mm

3030mm

∫ ∫ I(I()d)d = 17nW/m = 17nW/m22/sr/sr

0.30.3mm

Its origin revealed detectingIts origin revealed detectingthose galaxies responsiblethose galaxies responsiblefor the 100-1000for the 100-1000m radiationm radiation

DEEP HERSCHEL SURVEYS:

FIR (75 – 500 m)

CENSUS OF THE

SF UNIVERSE up to z=2-3

agn1agn1

agn2agn2

normalnormal

starbstarb

totaltotal

We will We will detect at 75 detect at 75 mm and and characterize all the star-forming characterize all the star-forming galaxies making up the galaxies making up the peak of the peak of the differential countsdifferential counts

We will We will detect at 75 detect at 75 mm and and characterize all the star-forming characterize all the star-forming galaxies making up the galaxies making up the peak of the peak of the differential countsdifferential counts

SWIRE 70SWIRE 70mmlimit=18 mJylimit=18 mJy

5 mJy5 mJy

Gruppioni, PozziGruppioni, Pozzi

Confusion noiseConfusion noiseestimatesestimates

Negrello et al., 2004Negrello et al., 2004

Blue: spiralsBlue: spiralsCyan: SBCyan: SBViolet: Radio sourcesViolet: Radio sourcesRed: SF spheroidsRed: SF spheroidsGreen: clustered SFGreen: clustered SFspheroidsspheroids

Detection limits Detection limits (poisson+clustering)(poisson+clustering)

Confusion is avoided Confusion is avoided with ALMAwith ALMA

• Current missions in Current missions in blackblack– Spitzer is +\Spitzer is +\

• Green bar is just a Green bar is just a 500m baseline 500m baseline ALMAALMA

• Red bar is 10-m Red bar is 10-m SAFIRSAFIR– Confusion from galaxies Confusion from galaxies

not met for many not met for many minutes or hoursminutes or hours

– At shortest At shortest wavelengths very deep wavelengths very deep observations are observations are possiblepossible

• Factor of 10 in Factor of 10 in resolution over existing resolution over existing facilities is very facilities is very powerfulpowerful

▬▬

Blain, 2004Blain, 2004

ConclusionsConclusions

• Need to observe in the FIR and submm to Need to observe in the FIR and submm to witness star and galaxy formationwitness star and galaxy formation

• Exploit both ALMA and HSO for common Exploit both ALMA and HSO for common scientific projects: HSO as survey driver and scientific projects: HSO as survey driver and ALMA as follow up (z + physical conditions)ALMA as follow up (z + physical conditions)

• ALMA complementary to HSO because of different ALMA complementary to HSO because of different frequency range and higher resolving power: source frequency range and higher resolving power: source sizes and physical conditionssizes and physical conditions

• Call for HSO Open Time Key Projects end Call for HSO Open Time Key Projects end 20062006

RecommendationsRecommendationsfor the futurefor the future

• Time allocation Time allocation • Supporting observationsSupporting observations• Supporting data and modelSupporting data and model• CalibrationCalibration• Data ArchiveData Archive

• Lower angular resolution preparatory Lower angular resolution preparatory surveys (APEX+LABOCA, SCUBA2, surveys (APEX+LABOCA, SCUBA2, LMT, SCELT+ELT?, Spitzer)LMT, SCELT+ELT?, Spitzer)

• Molecular collision rates, radiative Molecular collision rates, radiative transfer algorithms, chemical reaction transfer algorithms, chemical reaction ratesrates

• More automated form of data reductions More automated form of data reductions (huge datacube) automated comparison (huge datacube) automated comparison with models with models

Supporting Observations and DataSupporting Observations and Data

CalibrationCalibration

• Accurate calibration: Accurate calibration: measurement and measurement and modeling programmes, including time variationmodeling programmes, including time variation

• Different limitations of ALMA and Herschel: Different limitations of ALMA and Herschel: PACS and SPIRE are quickly saturated and PACS and SPIRE are quickly saturated and large bandwidthslarge bandwidths

• Less bright, smaller outer planets and Less bright, smaller outer planets and asteroidsasteroids

• HIFI+ALMA: common bandsHIFI+ALMA: common bands small spectral line sources unresolved by small spectral line sources unresolved by

ALMA but bright enough for HIFI (S/N small)ALMA but bright enough for HIFI (S/N small) Complete ALMA imaging of slightly extended Complete ALMA imaging of slightly extended

calibration sources (large investment of time)calibration sources (large investment of time)

Data ArchiveData Archive

• Optimum exploitation of Optimum exploitation of Herschel data and subsequent Herschel data and subsequent ALMA observationsALMA observations

• Allowing open access to data Allowing open access to data setssets

• Clear policy of data rights Clear policy of data rights (short time interval)(short time interval)

RecommendationsRecommendations

ESAESA• Herschel Herschel • Take the lead in Take the lead in

initiating projectsinitiating projects• PACS+SPIRE: PACS+SPIRE:

finding surveysfinding surveys• HIFI: water HIFI: water

vapourvapour

ESOESO• ALMA ALMA • Quick reactions to Quick reactions to

followupfollowup• Redshift machine Redshift machine

+ identification+ identification• Complementary Complementary

lines + high lines + high resolutionresolution

RecommendationsRecommendationsto ESA and ESOto ESA and ESO

• Combined ALMA-Herschel data sets Combined ALMA-Herschel data sets tremendous advancetremendous advance

• Available sources and common projectsAvailable sources and common projects• Calibration (good S/N + angular sizes)Calibration (good S/N + angular sizes)• Data archive: special procedure and Data archive: special procedure and

clear data rights policyclear data rights policy• Automatic analysis and model Automatic analysis and model

comparisonscomparisons

Recommendations to Recommendations to ESAESA

• Plan of Herschel surveys in Plan of Herschel surveys in ALMA elevation rangeALMA elevation range

• 7575m needed! (SED, AGN)m needed! (SED, AGN)• Legacy projects (extragalactic Legacy projects (extragalactic

and galactic surveys, in and galactic surveys, in continuum and spectroscopy)continuum and spectroscopy)

• Wide access to data, pipelines Wide access to data, pipelines for quick look and data for quick look and data reductionreduction

Recommendations to Recommendations to ESOESO

• Quick reaction to followup of Quick reaction to followup of Herschel observations Herschel observations (allocate observing time)(allocate observing time)

• Plans for finding surveys for Plans for finding surveys for extragalactic/galactic extragalactic/galactic regions/sources regions/sources (APEX+LABOCA)(APEX+LABOCA)

• Synergy with ELT+SCELT ? Synergy with ELT+SCELT ? (mapping speed vs confusion, (mapping speed vs confusion, SZ clusters)SZ clusters)