Hi-GAL: the Herschel infrared GALactic Plane Survey

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1 Hi-GAL: the Herschel infrared GALactic Plane Survey S. Molinari - IFSI/INAF, Rome Star Formation on the Global Scale: Resolving the Galactic Engine of the Milky Way Measure the star formation rate and history Galaxy-wide Obtain the complete inventory of cold dust in the Galactic Plane Establishing the existence and nature of star formation thresholds as a function of ISM properties across a full range of galactocentric radii metallicity and environmental conditions Determining the relative importance of global vs local mechanisms that give rise to star formation. Provide templates, recipes and prescriptions for Xgal science 20

2 From COBE to Herschel IRAS: FWHM = 5 MSX 8-20mm composite FWHM = 20 DIRBE: FWHM = 42 Resolution matters!

3 Census of Massive Star Forming regions in the Galaxy Characterize them Important to get submm at high-resolution: SCUBA2, APEX Detect them 2MASS - UKIDSS ISO - MSX PACS SPIRE Obtain Mass and Luminosity functions at various scales Spitzer APEX JCMT ATNF - FCRAO VLA DRAO AKARI

4 Broad Evolutionary classification of Star Forming Regions Saraceno et al. (1996), Molinari et al. (in prep.) IRAS : a massive protostellar candidate SED (Molinari appearance et al. 1998) Need Mid-IR data: MSX, MIPSGAL L bol /M env ratio. L bol is a key parameter here --> need CO data to get the distance: IGPS Obtain templates from nearest High-Mass Star Forming Regions for use elsewhere in the Galaxy HCO + (1-0) Strong synergy with the SPIRE GT program OB Star Formation (A. Zavagno in this meeting) IRAS : a massive Hot Core (Cesaroni et al. 1999)

5 Color à DRAO HI 21cm? Contours à FCRAO CO(1-0) Physical Properties in the ISM Morphology (2-d power spectra) and physical properties of dust in 1 ISM, at the sub-parsec scale typical of Star Forming Regions: Temperature, column density, dust opacity, gas/dust ratio 6 Standard diffuse ISM components 15K < T < 22K Peculiar components HISA What are they? Is it where HI-->H2 is taking place? IRAS and CO evidence is controversial (not enough resolution and λ-coverage) Background à MSX 8µ m? Color overlay à SCUBA 850µ m Continuum Importance in Galactic ISM budget (currently only detected in HI@21cm only under favourable fore/background conditions) IR Dark Clouds Initial conditions for Massive Star Formation (they are cold and dense!)? IRAS and CO are not favoured (not enough resolution and λ-coverage, depletion) Importance in Galactic ISM budget (currently only detected in l <30o where favorable 8µm contrast conditions exist) Galactic Inversion to measure the 3-D distribution of dust physical properties in the molecular, atomic and ionized phases of the diffuse ISM december 2006 ASTROCAM Herschel Meeting

6 Hi-Gal mm photometric imaging using the PACS and SPIRE cameras (5 bands) Fast Scanning in Parallel Mode with proper redundancy Sensitivity 120 < l <180 - b <1

7 By-Products (fulfilling KP reqs!) Goldmine for Herschel follow-up (and IRAM and JCMT and APEX and CARMA and SMA and ) Accurate foreground estimate for the interpretation of cosmological backgrounds ALMA input catalogue Dust in SNRs Dust Life-cycle..High density, high irradiation, turbulent conditions, statistical significance Debris dust disks around MS stars Unbiased statistics on frequency and mass as a function of star age Detection of detached dust shells around first ascent giant stars Missing mass in AGB envelopes, limited to distant objects with unresolved envelope, detectable via long-wavelength excess. Detection of multiple shells around AGB stars, post-agb objects and planetary nebulae, as well as around various classes of interacting binaries Detection of ejecta shells and swept-up ISM bubbles around massive stars Complete census of WR and LBV stars Extinction maps Study of individual interesting Star Forming Regions (known or to be discovered) Nearby december Low-Mass 2006 SFRs ASTROCAM on the Galactic Herschel Plane Meeting

8 The Team IFSI-Rome S. Molinari P. Saraceno A.M. DiGiorgio S. Pezzuto M. Benedettini L. Spinoglio Oss. Arcetri L. Testi R. Cesaroni M. Walmsley F. Palla M. Felli Univ. Roma P. DeBernardis S. Masi F. Piacentini Univ. Lecce F. Strafella IPAC/Caltech A. Noriega-Crespo G. Helou K. Ganga B. Ali B. Schulz S. Lord S. Carey W. Reach JPL H. Yorke P. Goldsmith Berkeley M. Cohen NRAO D. Shepherd CfA H. Smith CITA P. Martin Univ. Calgary R. Taylor Univ. Laval G. Joncas Herzberg Inst. J. DiFrancesco MPIfR-Bonn P. Schilke F. Schuller MPE-Munich H. Feuchtgruber T. Muller KU Leuven J. Blommaert CESR-Toulouse J.P. Bernard M. Giard I. Ristorcelli C. Joblin IAS-Paris A. Abergel F. Boulanger M-A. Miville-Deschenes P. Cox LAM-Marseille A. Zavagno J.P. Baluteau D. Russeil CEA-Saclay P. Andrè F. Motte V. Minier Obs. Bordeaux S. Bontemps Univ. Cardiff M. Griffin D. Ward-Thompson RAL B. Swinyard T. Lim Open Univ. G. White UCL M. Barlow Univ. Hertsf. A. Chrysostomou M. Thompson P. Lucas Univ. Leeds M. Hoare Univ. Liverpool T. Moore APEX GPS SCUBA2 GPS IGPS (HI+CO) PLANCK Spitzer/MIPSGAL