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The S IRTF W ide-Area I nfra- R ed E xtragalactic Survey

The S IRTF W ide-Area I nfra- R ed E xtragalactic Survey. Carol J. Lonsdale IPAC, Caltech. SIRTF & SWIRE. 85 cm cryogenic telescope Launch mid-April 2003 , heliocentric orbit 3-5 year lifetime; 75% open time: 1 st call Nov 8, 2002 3 instruments: 3-160 μ m imaging & spectroscopy

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The S IRTF W ide-Area I nfra- R ed E xtragalactic Survey

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  1. The SIRTF Wide-Area Infra-Red Extragalactic Survey Carol J. Lonsdale IPAC, Caltech Santiago, Chile

  2. SIRTF & SWIRE • 85 cm cryogenic telescope • Launch mid-April 2003, heliocentric orbit • 3-5 year lifetime; 75% open time: 1st call Nov8, 2002 • 3 instruments: 3-160μm imaging & spectroscopy • Legacy Program • 6 large programs; 3 of them extragalactic • To be completed in first year • Non-proprietary: immediate community follow-up • SWIRE: largest Legacy program: 851 hours • 63 sq degs, 7 fields • 3-160 μm imaging, to z~3 • SPHEROIDS,DISKS,STARBURSTS,AGN • 100s of 100Mpc-scale cells Carol Lonsdale

  3. IR Galaxy Populations Optical LF • Luminous IR Galaxies are the dominant population L > 1011Lo • ~30% of local energy density is in the IR IR Galaxy Luminosity Function Soifer et al 1989 Carol Lonsdale

  4. IR Galaxy Populations: LIRGs • Interactions/mergers • IR does not coincide with UV-optical • younger stellar population Carol Lonsdale

  5. IR Galaxy Populations: ULIRGs Compact core: 80% of mid-IR <7% in far-UV Arp 220 Av>100 Surace et al (2001) Scoville et al. (2000), Soifer et al. (2000), Goldader et al (2002) Carol Lonsdale

  6. Strong Evolution of the Infrared Galaxy Population • First discovered for IRAS sources • ISO surveys confirm strong evolution • Also seen in the submm • Xu et al. (2001) model fits multi-λ data: • L α (1+z)4 • ρ α (1+z)2 Carol Lonsdale

  7. IR Dominates the Global Backgrounds 50% or more is in IR Franceschini et al 2001 Carol Lonsdale

  8. CIRB Resembles M82 Elbaz et al 2002 Franceschini et al 2001 Carol Lonsdale

  9. IR & X-Ray Backgrounds Salvati & Maiolino Cosmic X-Ray Background models require a population of highly obscured AGN which increases with z (Comastri et al., Gilli et al, Polletta et al 2002) Hasinger Even MIR and hard X-ray highly obscured What fraction of the CIRB is powered by accretion? Carol Lonsdale

  10. Deep ISO 15µm & X-ray XMM image: Hasinger et al. (2001) ISO image: Fadda et al. (2001) • They are Type II QSOs Carol Lonsdale

  11. The Mid & Far-IR Universe • Evolution to z~1 is greater in IR than UVO • IR is <30% locally but dominates at z>1 • ULIRGs <1% locally but major population at z>1 (SCUBA sources) • AGN account for ~20% of the CIRB ISO/IRAS/SCUBA UVO Chary and Elbaz 2001 Carol Lonsdale

  12. Old Stellar Populations • Slow evolution in color, line strengths, velocity dispersion of spheroids since z>~1 • Stronger morphological than color evolution: red mergers (Van Dokkum) • Large spiral disks in place by z~1 (Vogt) Van Dokkum et al. 2000; z=0.83 cluster Zf for spheroids vs. assembly? Carol Lonsdale

  13. IRAC & Old Stellar Populations Sawicki 2002 IRAC will sample low-mass stellar populations in high-z gals and measure baryonic mass to high-z Carol Lonsdale

  14. SpaceInfraRedTelescopeFacilityM. Werner, Project Scientist • 85 cm telescope • Diffraction limited at 6.5µm • Delta launch: April 15th 2003 • Earth-trailing orbit No eclipses or occultations, continuous operations • only seven distinct observing modes (AOTs) • Single instrument campaigns last 3-to-10 days • Science Center at IPAC, Caltech • Community Time >75% Cycle 1 Call November 8 • Legacy data are non-proprietary: • Archive opens early 2004 Carol Lonsdale

  15. SIRTF: MIPS 24, 70 & 160 µm imaging, G. Rieke, PI U Arizona Freeze-frame scanning with secondary mirror Carol Lonsdale

  16. SIRTF: IRAC 3.6, 4.5, 5.8, 8.0 µm imaging G. Fazio, PI, SAO 256 x 256 1.2"pixels 5' x 5' 3.6 & 4.5 µm: In:Sb 5.8 & 8.0 µm: Si:As Carol Lonsdale

  17. SIRTF: IRS IRS: 5.0 – 40 µm spectroscopy, J. Houck PI, Cornell Short Low: 5.3-14um 62-124 resolution Si:As Short-High 10.3-19.5 600 Si:As Long-Low 14-42 62-124 Si:Sb Long-High 19-37 600 Si:Sb 128 x 128, all modules Carol Lonsdale

  18. 3.6 m 7.3 Jy 4.5 m 9.7 Jy 5.8 m 27.5 Jy 8.0 m 32.5 Jy 24 m 0.45 mJy 70 m 2.75 mJy 160 m 17.5 mJy The SWIRE Survey • 63 square degrees • all 7 SIRTF MIPS & IRACimaging bands • 851 hours – largest SIRTF Program 5σ sensitivities • SIRTF is ideally designed for detailed study of the history of star formation • IRAC is optimized for old and reddened stellar populations • MIPS is optimized for star-forming galaxies and AGN Carol Lonsdale

  19. Galaxies in the IR Stars Dust r IRAC MIPS Polletta et al 2002 Carol Lonsdale

  20. SIRTF Legacy Surveys: Extragalactic GOODS: Great Observatories Origins Deep Survey Mark Dickinson (STScI) 300h 300 sq arcmin/50 sq arcmin IRAC/MIPS 24m SINGS: The SIRTF Nearby Galaxies Survey Rob Kennicutt (U. Arizona) 512h 75 nearby galaxies IRAC/MIPS/IRS SWIRE: The SIRTF Wide-area Infrared Extragalactic Survey Carol Lonsdale (IPAC/Caltech)851h 63 sq deg; 2x106 galaxies IRAC/MIPS Carol Lonsdale

  21. Carol Lonsdale PI IPAC, Caltech Harding E (Gene) SmithDeputy PI, ground-based program UCSD Michael Rowan-RobinsonDeputy PI for ScienceImperial College Dave ShupeLiaison Scientist SSC/IPAC Deborah PadgettMIPS SSC/IPAC Jason SuraceData Processing/IRACSSC/IPAC Cong XuModels IPAC Seb OliverLarge Scale StructureSussex University Jim CondonVLA Survey NRAO Tim ConrowSystem IPAC Herve Dole MIPSU. Arizona Fan FangSimulation/ModelsSSC/IPAC Alberto FranceschiniSpheroids, AGNPadua Dave Frayer MIPSSSC/IPAC Nick GautierCirrusJPL Matt GriffinHerschel/SPIRECardiff Perry HackingModelsVanguard Tom Jarrett Nearby GalaxiesIPAC, Caltech Frank MasciMIPS 24um SSC Glenn MorrisonRadioVanguard JoAnn O’LingerDisksSSC Frazer OwenRadio NRAO Ismael Perez-FournonQSOs IAC, Tenerife Marguerite PierreX-ray/XMMCEA, Saclay Rick PuetterPixonsUCSD Steve Serjeant ELAISU. Kent Gordon StaceyMolecular linesCornell Mike WernerIRS JPL Carol Lonsdale

  22. SWIRE: Environment & LSS Resolving Star Formation History & AGNAccretion & Spheroid Evolution in Time and Space in context of Structure Formation z=3 z=2 Kauffmann et al. (1999); 21x21x8 (Mpc/h)3 red blue: increasing SFR z=1 z=0 Carol Lonsdale

  23. The SWIRE Survey 3.6 m / 8 m / 24 m 10’ x 10’ Xu et al. 2001 • 0.5 < z < 3 • 100s of ~100Mpc cells • 1000ssources in each cell • > 106 galaxies • >104 Type 1 AGN 24m / 70m / 160m 1 x 1 degree Rowan-Robinson 2001 Carol Lonsdale

  24. SWIRE Fields 7 large fields: large scale sizes combat cosmic variance Carol Lonsdale

  25. Field Selection Strategy • Low extinction, cirrus noise: extensive survey for fields with I100µm < 0.5MJy/Sr; b > 40º, β > 40º. See: • http://star-www.cpes.susx.ac.uk/~sjo/swire/I100/index2.html • 2.Avoid bright stars, galaxies, radio sources • 3. Favor prior or planned complementary surveys with either: • large investment of time, or • large effort to repeat Carol Lonsdale

  26. Minimize NH & Cirrus B100 Contours at 1 and 2 MJy/sr LONSDALE ELAIS-N1 LOCKMAN ELAIS-N2 CHANDRA-S XMM-LSS ELAIS-S1 Schlegel et al. 1998 DIRBE-calibrated IRAS 100m map Carol Lonsdale

  27. Fields We Didn’t Select Groth Strip SSA68 Carol Lonsdale

  28. Cirrus Holes Too Small HDF-South HDF-North Carol Lonsdale

  29. SWIRE Survey Fields IRAS 100 m images Lockman HoleELAIS-N1 Carol Lonsdale

  30. SWIRE Survey Fields ELAIS N2 ELAIS S1 Carol Lonsdale

  31. SWIRE Survey Fields CDF-S Lonsdale Hole Carol Lonsdale

  32. SWIRE Survey Fields XMM-LSS Xray surveys are typically very small (eg: Lockman Hole survey below). The large XMM-LSS survey is unique LH XMM-LSS M. Pierre, PI SWIRE Carol Lonsdale

  33. Next Generation “Cosmic Windows” SWIRE is defining the best LARGE cirrus holes on sky which will be observed by many other survey instruments: • GALEX deep imaging survey: AB=25.5 mag • UV 1350-3000Å, 50 cm telescope • imaging and grism, 2003 launch (C. Martin) SWIRE-GALEX very powerful in combination Carol Lonsdale

  34. 10 1 0.1 0.01 l (mm) 100 10 1000 Z = 0.1 1012L 0.5 SPIRE 1 Flux density (Jy) 3 5 • Herschel/SPIRE • 250, 350, 500μm imaging • ~ 2007 launch • M. Griffin,Cardiff Carol Lonsdale

  35. Next Generation “Cosmic Windows” VLA proposal 40μJy 20cm J. Condon SWIRE/GALEX/XMM-LSSoptical ground-based Imaging Spectroscopy Deep J & K (partial SWIRE field coverage); K=21 A. Lawrence Carol Lonsdale

  36. SWIRE SIRTF Observations Lockman Field, incomplete map to illustrate strategy (4.0° x 3.75°) MIPS Scan legs GTO Deep Survey (2°x 0.25°) IRAC Maps Carol Lonsdale

  37. SIRTF Observations • Two epochs & both instruments in one campaign • IRAC: • 2 dithers • 4x30 sec per point • MIPS: • 2 x 10 x 4 sec • at 24 & 70μm • 2 x 1 x 4 sec • at 160μm Carol Lonsdale

  38. Six-band simulation 3.6 4.5 5.8 • Model of Xu et al, 2001, 2002 • 24μm LF • 840 SEDs • Starbursts • Spirals • AGN • Ellipticals • 5 x 5 arcmin 8.0 24 70 Carol Lonsdale

  39. Mosiaced IRAC Simulation Las Campanas NIR HDF Survey (Chen et al. 2001). EROs 0.2 sq deg LCIRS limit Carol Lonsdale

  40. SWIRE Starbursts & AGN 1 sq degree SWIRE survey (excluding spheroids) 8μm 7200 sources 24μm 3300 70μm 2700 Warm AGN: 1000 Starbursts & obscured AGN: 4500 Carol Lonsdale

  41. Bias and SFR-Density Field • Would like to know evolution of the mass density field • What we measure is the galaxy density field: δg = bδm • Complex astrophysics governs galaxy light • Did much star formation happened early & fast in bursts ? • Role of feedback ? Somerville et al 2001 (who conclude extinction & collisional starbursts important) Carol Lonsdale

  42. Bias and SFR-Density Field • So measure evolution of bias of different populations: • Starburst vs Passive systems • Young vs older starbursts • Disks vs spheroids • AGN vs starbursts • Etc. • SWIRE is ideal • Measures all populations in same volume cells Oliver et al 1996 optical IRAS Carol Lonsdale

  43. Additional Science • Hundreds of field brown dwarfs, especially T (“methane”) dwarfs • 50-60 circumstellar debris disks (to 100 pc), and HR4796A analogs to 1kpc • Thermal emission at 8 and 24m from main belt asteroids as small as 1km • Serendipitous discoveries; rare objects to 1-in-104 to 1-in-106 Carol Lonsdale

  44. Data Products and Archive Services • Bi-yearly releases: • source lists • fits images • cross-band identifications • coverage maps • documentation • ancillary data and cross-ids • Successive deliveries: • Increased area coverage • Decreasing SNR levels • Cross-matching, increasing numbers of bands • Image mosaics over increasing area SWIRE Data: Non-proprietary 1st release: early 2004 Carol Lonsdale

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