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HERSCHEL/SPIRE les programmes extragalactiques

HERSCHEL/SPIRE les programmes extragalactiques. -SAG2: Galaxies proches, échantillon de référence -SAG1: Sondages profonds. V. Buat pour les SAG 1 & 2. SPIRE/HERSCHEL. SAG 2: LOW-Z EXTRAGALACTIC ASTRONOMY THE HERSCHEL GALAXY REFERENCE SAMPLE Alessandro Boselli , Steve Eales,

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HERSCHEL/SPIRE les programmes extragalactiques

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  1. HERSCHEL/SPIRE les programmes extragalactiques -SAG2: Galaxies proches, échantillon de référence -SAG1: Sondages profonds V. Buat pour les SAG 1 & 2

  2. SPIRE/HERSCHEL SAG 2: LOW-Z EXTRAGALACTIC ASTRONOMY THE HERSCHEL GALAXY REFERENCE SAMPLE Alessandro Boselli, Steve Eales, Veronique Buat, Jonathan Davies, Kate Isaak, Walter K Gear, Matt Griffin, Marc Sauvage, Laurent Vigroux, Suzanne Madden, Koryo Okumura, David Elbaz, Pierre Chanial,George Bendo, Dave Clements, Mattia Vaccari, Frederic Galliano, Jammie Bock, Seb Oliver, Matt Page, Ismael Perez Fournon, Eli Dwek, Bernhard Schulz, Luigi Spinoglio, Jason Stevens, Maarten Baes, Werner Zeilinger, Christine Wilson

  3. SPIRE/HERSCHEL THE HERSCHEL GALAXY REFERENCE SAMPLE Aim of the project: to study the dust content and distribution of “normal” galaxies 1) Dust plays a principal role in the physics of the ISM and in the process of SF in galaxies : HI ->H2; shields the gas from the ISRF (UV radiation); cooling of the gas; produced and injected in the ISM by massive stars 2) Major ingredient in the determination of the extinction - energetic balance (important for measuring SFR) 3) Pollution of the intergalactic medium in clusters 4) Reference sample for high z studies

  4. Why SPIRE?: the pick of the dust emission in “normal” galaxies is ~ 200 µm IRAS, ISO, Spitzer, ASTRO-F < 200 µm Boselli et al 2003

  5. Why SPIRE?: although not important energetically, cold dust is dominant in mass Cold dust difficult to observe with SCUBA in “normal” galaxies Boselli et al 2003

  6. SPIRE/HERSCHEL The Herschel galaxy reference survey • A representative sample of ~300 galaxies in the nearby universe • distance range 15<dist<25 Mpc (to have a volume limited sample) • high galactic latitude (to avoid cirrus contamination) |b|>54 ° • -pointed observations of few tens of minutes per galaxy at 250, 360 & 520 µm

  7. SPIRE/HERSCHEL The Herschel galaxy reference survey: the sample • 2MASS K selected sources (to have a luminosity/mass selection) • 1) K < 9 mag: E + S0 + Spirals • 2) 9 < K< 12 mag: to add late type systems with a large range of • luminosity and morphological type • E+S0: down to 11 mJy -> 104 Msun( dust) • Spirals: down to22 mJy -> to detect dust in the outer disk, from standard gas to dust ratios • 313 selected galaxies, to be observed in 100 h

  8. The whole sample: K< 9 mag: 126 objetcs 9 < K< 12 mag 187 galaxies

  9. The cluster sub-sample (Virgo & Fornax) K< 9 mag 36 galaxies 9 < K< 12 mag 40 galaxies

  10. SPIRE/HERSCHEL The Herschel galaxy reference survey: main objectives • For galaxies of different type and luminosity: • -Dustproperties (mass, temperature, gas to dust ratio,..) • The role of dust in the physics of ISM (relation with SFR) • Spectral Energy Distribution • Effects of the environmenton dust properties of nearby galaxies (clusters vs. field) • Intergalactic dust cycle • Dust properties in ellipticals :merger history (dusty disks) and origin of dust in ellipticals • Local dust-mass function

  11. SPIRE/HERSCHEL The Herschel galaxy reference survey: corollary data • Large surveys available or under way • UV from GALEX (1500-2300 A) • Visible from SDSS (u, g, r, I, z) • NIR from 2MASS (J, H, K) • radio continuum NVSS/FIRST (20 cm) • R~1000 integrated spectroscopy (Balmer decrement, metallicity…) with CARELEC at the OHP • Halpha imaging (SFR) with 2.1m telescope in San Pedro Martir (Mexico • Mid- and Far-IR (<200 mic) from ASTRO-F • HI from HIPASS & ALFALFA • -Westerbok/VLA HI : for ellipticals • -CO survey of all galaxies without CO measurements(JCMT & FCRAO) • -850 microns with SCUBA2 • -Xrays from Chandra/XMM

  12. SPIRE High-z A wedding cake of blank field surveys P.I. Seb Oliver

  13. Resource by Institute 67 Individuals with average effort of 0.25 fte per year

  14. La participation française revue et corrigée…

  15. Resources by Country

  16. Key science • How and when galaxies form • Search for unknown populations of high z IR galaxies • AGN versus SB, AGN fraction • Star formation rates

  17. Summary of the GI proposal • 850 h awarded to the high-z team on SPIRE • Observations of blank fields and clusters with SPIRE & PACS- 650 h for PACS • A single large project: A bolometric exploration of the star formation history of the Universe as a function of the environment --> 1500 hours on Herschel (SPIRE+PACS)

  18. Why Herschel for the high z? • The emission of galaxies and of the cosmic background peaks around 60-200 microns --> SCUBA or SPITZER do not probe the bulk of the emission • The aim of the proposal is to measure the bolometric IR emission of galaxies over a large range of z.

  19. Areas, Depths, Fields

  20. The wedding cake Clusters-lensing GOODs-S- 0.04deg2 4 mJy @ 350µm GOODS-N- 0.04 deg2 8 mJy @ 350 µm GOODS-Groth Strip-Lockman 0.75 deg 2 13 mJy @ 350 µm COSMOS-XMM- 4 deg2 26 mJy @ 350 µm XMM-Lockman-CDFS- 10 deg2 29 mJy @ 350 µm SWIRE- 50 deg2- 74 mJy @ 350 µm

  21. L(bol)-z plane sampled by the surveys

  22. Confusion limits (at 5) • 250 microns: 20 mJy, FWHM= 17 arcsec, 1800 sources/sq.deg • 350 microns: 19 mJy, FWHM= 24 arcsec, 945 sources/sq.deg • 500 microns: 19 mJy, FWHM= 35 arcsec, 420 sources/sq.deg

  23. Observations of clusters • z=0.2 to > 1 • Using gravitational lensing to go below the confusion limit • 50% of the unresolved background might be identified with specific galaxies (against 10% without lensing) • 15 (?) clusters to be observed • Modelling in progress based on the SPIZER analyses of Dole et al. 2006

  24. Science Goals • Key Science Goals • Agreed before hand • Coordinated by individual or small team • Distributed effort through workflows • Specific Papers identified • Secondary Science Goals • Less “managed” • Open process • Schedule tied to data release cycle

  25. Data Products • Primary Data Products • SPIRE Points Source Catalogues (P1) • SPIRE Maps (P2/P3) • PACS Point Source Catalogues (P1) • PACS Maps (P2/3) • Secondary Data Products (best efforts) • SPIRE/PACS band-merge (P2/P3) • X-ID lists (P3) • Key Complementary/Follow-up Data • Various….(P3) • Secondary Complementary/Follow-up Data (Not released)

  26. Time-table (Launch to DR1) Data, Valid. Sci. Perhaps too tight

  27. Merci pour votre attention

  28. Prédictions des modèles(Lagache, Puget & Dole) Redshift distributions 15 mJy @ 350 mu (100 deg2) 100 mJy (400 deg2) Number counts

  29. CIB analysis • Confusion will prevent the detection of individual sources at high z • Stacking technique based on a priori information from PACS and/or SPITZER • Fluctuations analysis

  30. Data processing and releases • Phase 0: checking that the science goals will be achieved, optimization of the tools • Phase 1: quickly after the end of the observations (…). For the best observations, reduction and release to the Herschel community. SPG pipeline used. Optimized tools validated and released to the Herschel community • Phase 2: main stage. All the data are processed with optimized pipelines, band-merging, multi-wavelength catalogs. Specific analyses: extended sources, diffuse emission, P(D). Released to the Herschel community • Phase 3: final archiving, follow-up data combined. First scientific papers.

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