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)