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ALMA HERSCHEL SYNERGIES Origins of galaxies, stars, planets Recommendations to ESA and ESO

ALMA HERSCHEL SYNERGIES Origins of galaxies, stars, planets Recommendations to ESA and ESO. Paola Andreani, T. Wilson ……. D. Bockelee-Morvan (Paris) J. Cernicharo (Madrid) P. Cox (Grenoble) C. De Breuck (ESO) D. Elbaz (Paris) E. van Dishoeck (Leiden) M. Gerin (Paris)

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ALMA HERSCHEL SYNERGIES Origins of galaxies, stars, planets Recommendations to ESA and ESO

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  1. ALMA HERSCHEL SYNERGIES Origins of galaxies, stars, planets Recommendations to ESA and ESO Paola Andreani, T. Wilson ……

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

  3. TALK OUTLINE • Synergies? • Why FIR and Submm? • ALMA, HERSCHEL‘complementary’ • Common Scientific Projects Stars and dust formation Star forming regions and MCs Nearby spirals, LSBGs, DGs, AGN CIRB, high-z sources, AGN • Recommendations to ESA/ESO

  4. Synergies • Science topics: objects of both instruments • ESA+ESO act in common to best exploit scientific return • Legacy? Joint-time? • Joint analysis of observations • How operate data flow? • Common calibration

  5. Why FIR/submm? SB spectrum Protostar development

  6. K-correction Sensitivity with 6 antennas Griffin, 05 Blain, 04

  7. Obscured sources Cluster A1835 z ~ 0.7-2.5 z = 2.55 (Ivison et al., 2000)

  8. ALMA Main + Compact Array Main (50 12m) antennas + ACA (4 12m + 12 7m) FOV 50-85’’ at 3mm (90GHz) 8.3-14’’ at 0.5mm (600GHz) Resolution: 0.03-4’’ at 3mm 0.005-0.7’’ at 0.5mm Sensitivity (5, 1h) @3mm and 0.5’’ resol (1km baseline) continuum 0.03mJy line 3mJy (‘’) = 0.2 (mm) / B(km) S= 2k/Aeff Tsys/√N(N-1) tint

  9. Band3: 84-116 Band4: 125-163 Band5: 163-211 Band6: 211-275 Band7: 275-373 Band8: 385-500 Band9: 602-702 Band10: 787-950 GHz Band1: 31.3-45 Band2: 67-90 GHz

  10. ALMA Receivers ★ Japanese contribution all telescopes plus ACA ★ EC funded 8 receivers ALMA-Herschel synergy

  11. Herschel fourth cornerstone mission in ESA's Horizon 2000 programme launch during 2008 3.5 m passively cooled to 80 K 3 cold focal plan instruments photometry and spectroscopy in the 60 – 670 µm range liquid helium cryostat operational lifetime of at least 3 years

  12. Photometry with Herschel

  13. Spectroscopy with Herschel

  14. Common scientific projects • Star formation • Planetary system formation • Nearby galaxies • Galaxy formation • AGN-Host joint formation/BH formation

  15. Standard model of star formation 1. Formation of pre-stellar clumps in molecular clouds. 2. The pre-stellar clump collapses 4. Formation of a planetary system 3. Protostar (infall and outflow coexists) Fig. from McCaughrean

  16. Star formation Four stages of star formation • Collapse of MC • high gas density + low Tkin, • grain properties change Accretion phase Optically thick disc+ Star is emerging, outflow Star + disc, outflow SiO NIR H2

  17. Chemistry as a clock for YSOs H13CO+ CH3CN H2CO 13CO CH3OH C2H3CN C18O N2H+ C17O HCOOH NH3 C2H5CN SiO SO CN HCN CH3OH

  18. Star Formation at the Galactic Centre SCUBA 850 micron: Pierce-Price et al 2000 • 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 450 micron

  19. Star formation • 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: molecules (mainly H2O) + detailed kinematics of star forming regions • ALMA: molecules at higher spatial resolution + outflows Serpens (Testi, priv) High spatial res at SED max of most SF regions separate the main sources of luminosity

  20. Evolved stars and dust formation IRC+10216 • AGB POST-AGB PN • Outflow mass loss + properties of the dust and formation site • Most of the solid-state features in MIR + NIR • @FIR: Forsterite + Calcite + crystalline H2O ice • @submm: SiO-H2O masers

  21. Dust and molecular emission from optically obscured regions HST optical image HST optical image + CO contours The “Antennae” (CO : Wilson et al. 2000) (HST: Whitmore et al. 1999)

  22. The Cosmic Extragalactic Background IR Optical 1000m ∫ I()d = 30nW/m2/sr 100m 30m ∫ I()d = 17nW/m2/sr 0.3m Its origin revealed detecting those galaxies responsible for the 100-1000m radiation Franceschini 2000

  23. DEEP HERSCHEL SURVEYS: FIR (75 – 500 m) CENSUS OF THE SF UNIVERSE up to z=2-3

  24. We will detect at 75 m and characterize all the star-forming galaxies making up the peak of the differential counts total starb SWIRE 70m limit=18 mJy normal agn2 agn1  5 mJy Gruppioni, Pozzi

  25. Confusion noise estimates Detection limits (poisson+clustering) Blue: spirals Cyan: SB Violet: Radio sources Red: SF spheroids Green: clustered SF spheroids Negrello et al., 2004

  26. Confusion is avoided with ALMA Blain, 2004 • Current missions in black • Spitzer is +\ • Green bar is just a 500m baseline ALMA • Red bar is 10-m SAFIR • Confusion from galaxies not met for many minutes or hours • At shortest wavelengths very deep observations are possible • Factor of 10 in resolution over existing facilities is very powerful ▬ ▬

  27. Conclusions • Need to observe in the FIR and submm to witness star and galaxy formation • Exploit both ALMA and HSO for common scientific projects: HSO as survey driver and ALMA as follow up (z + physical conditions) • ALMA complementary to HSO because of different frequency range and higher resolving power: source sizes and physical conditions • Call for HSO Open Time Key Projects end 2006

  28. Time allocation Supporting observations Supporting data and model Calibration Data Archive Recommendationsfor the future

  29. Supporting Observations and Data • Lower angular resolution preparatory surveys (APEX+LABOCA, SCUBA2, LMT, SCELT+ELT?, Spitzer) • Molecular collision rates, radiative transfer algorithms, chemical reaction rates • More automated form of data reductions (huge datacube) automated comparison with models

  30. Calibration • Accurate calibration: measurement and modeling programmes, including time variation • Different limitations of ALMA and Herschel: PACS and SPIRE are quickly saturated and large bandwidths • Less bright, smaller outer planets and asteroids • HIFI+ALMA: common bands small spectral line sources unresolved by ALMA but bright enough for HIFI (S/N small) Complete ALMA imaging of slightly extended calibration sources (large investment of time)

  31. Data Archive • Optimum exploitation of Herschel data and subsequent ALMA observations • Allowing open access to data sets • Clear policy of data rights (short time interval)

  32. ESA Herschel Take the lead in initiating projects PACS+SPIRE: finding surveys HIFI: water vapour ESO ALMA Quick reactions to followup Redshift machine + identification Complementary lines + high resolution Recommendations

  33. Recommendationsto ESA and ESO • Combined ALMA-Herschel data sets tremendous advance • Available sources and common projects • Calibration (good S/N + angular sizes) • Data archive: special procedure and clear data rights policy • Automatic analysis and model comparisons

  34. Recommendations to ESA • Plan of Herschel surveys in ALMA elevation range • 75m needed! (SED, AGN) • Legacy projects (extragalactic and galactic surveys, in continuum and spectroscopy) • Wide access to data, pipelines for quick look and data reduction

  35. Recommendations to ESO • Quick reaction to followup of Herschel observations (allocate observing time) • Plans for finding surveys for extragalactic/galactic regions/sources (APEX+LABOCA) • Synergy with ELT+SCELT ? (mapping speed vs confusion, SZ clusters)

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