1. SWIRE Octiber 30, 2002Santiago, Chile1 The SIRTF Wide-Area Infra-Red Extragalactic Survey Carol J. Lonsdale IPAC, Caltech

2. October 30, 2002 Santiago, ChileCarol Lonsdale2 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: 3-160μm 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

3. October 30, 2002 Santiago, ChileCarol Lonsdale3 IR Galaxy Populations  Luminous IR Galaxies are the dominant population L > 10 11 L o  ~30% of local energy density is in the IR IR Galaxy Luminosity Function Optical LF Soifer et al 1989

4. October 30, 2002 Santiago, ChileCarol Lonsdale4 IR Galaxy Populations: LIRGs  Interactions/mergers  IR does not coincide with UV-optical –younger stellar population

5. October 30, 2002 Santiago, ChileCarol Lonsdale5 IR Galaxy Populations: ULIRGs Surace et al (2001) Scoville et al. (2000), Soifer et al. (2000), Goldader et al (2002) Compact core: 80% of mid-IR <7% in far-UV Arp 220 A v >100

6. October 30, 2002 Santiago, ChileCarol Lonsdale6 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

7. October 30, 2002 Santiago, ChileCarol Lonsdale7 IR Dominates the Global Backgrounds 50% or more is in IR Franceschini et al 2001

8. October 30, 2002 Santiago, ChileCarol Lonsdale8 CIRB Resembles M82 Elbaz et al 2002 Franceschini et al 2001

9. October 30, 2002 Santiago, ChileCarol Lonsdale9 IR & X-Ray Backgrounds 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) What fraction of the CIRB is powered by accretion? Hasinger Salvati & Maiolino Even MIR and hard X-ray highly obscured

10. October 30, 2002 Santiago, ChileCarol Lonsdale10 Deep ISO 15 µm & X-ray XMM image: Hasinger et al. (2001) ISO image: Fadda et al. (2001)  They are Type II QSOs

11. October 30, 2002 Santiago, ChileCarol Lonsdale11 The Mid & Far-IR Universe  Evolution to z~1 is greater in IR than UVO  IR is 1  ULIRGs 1 (SCUBA sources)  AGN account for ~20% of the CIRB Chary and Elbaz 2001 ISO/IRAS/SCUBA UVO

12. October 30, 2002 Santiago, ChileCarol Lonsdale12 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 Z f for spheroids vs. assembly ?

13. October 30, 2002 Santiago, ChileCarol Lonsdale13 IRAC & Old Stellar Populations Sawicki 2002 IRAC will sample low-mass stellar populations in high-z gals and measure baryonic mass to high-z

14. October 30, 2002 Santiago, ChileCarol Lonsdale14 Space InfraRed Telescope Facility M. Werner, Project Scientist  85 cm telescope  Diffraction limited at 6.5µm  Delta launch: April 15 th 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

15. October 30, 2002 Santiago, ChileCarol Lonsdale15 SIRTF: MIPS 24, 70 & 160 µm imaging, G. Rieke, PI U Arizona Freeze-frame scanning with secondary mirror λ (µm) Array size Detector FOV Pix size 24128x128Si:As5' x 5 ' 7" 70 32x32Ge:Ga5' x 5 '17 " 160 2x20 Ge:Ga (stressed) 0.5x5 '40 "

16. October 30, 2002 Santiago, ChileCarol Lonsdale16 SIRTF: IRAC 256 x 256 1.2" pixels 5' x 5' 3.6 & 4.5 µm: In:Sb 5.8 & 8.0 µm: Si:As 3.6, 4.5, 5.8, 8.0 µm imaging G. Fazio, PI, SAO

17. October 30, 2002 Santiago, ChileCarol Lonsdale17 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

18. October 30, 2002 Santiago, ChileCarol Lonsdale18 The SWIRE Survey  63 square degrees  all 7 SIRTF MIPS & IRAC imaging bands  851 hours – largest SIRTF Program 17.5 mJy 160  m 2.75 mJy 70  m 0.45 mJy 24  m 32.5  Jy8.0  m 27.5  Jy5.8  m 9.7  Jy4.5  m 7.3  Jy3.6  m 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 5σ sensitivities

19. October 30, 2002 Santiago, ChileCarol Lonsdale19 Galaxies in the IR IRACMIPS Polletta et al 2002 r Stars Dust

20. October 30, 2002 Santiago, ChileCarol Lonsdale20 GOODS: Great Observatories Origins Deep Survey Mark Dickinson (STScI) 300 h 300 sq arcmin/50 sq arcmin IRAC/MIPS 24  m SINGS: The SIRTF Nearby Galaxies Survey Rob Kennicutt (U. Arizona) 512 h 75 nearby galaxies IRAC/MIPS/IRS SWIRE: The SIRTF Wide-area Infrared Extragalactic Survey Carol Lonsdale (IPAC/Caltech) 851 h 63 sq deg; 2 x 10 6 galaxies IRAC/MIPS SIRTF Legacy Surveys: Extragalactic

21. October 30, 2002 Santiago, ChileCarol Lonsdale21 Carol LonsdalePIIPAC, Caltech Harding E (Gene) SmithDeputy PI, ground-based programUCSD Michael Rowan-RobinsonDeputy PI for ScienceImperial College Dave ShupeLiaison ScientistSSC/IPAC Deborah PadgettMIPSSSC/IPAC Jason SuraceData Processing/IRACSSC/IPAC Cong XuModelsIPAC Seb OliverLarge Scale StructureSussex University Jim CondonVLA SurveyNRAO Tim ConrowSystemIPAC Herve DoleMIPSU. Arizona Fan Fang Simulation/ModelsSSC/IPAC Alberto FranceschiniSpheroids, AGNPadua Dave FrayerMIPSSSC/IPAC Nick GautierCirrusJPL Matt Griffin Herschel/SPIRECardiff Perry Hacking ModelsVanguard Tom JarrettNearby GalaxiesIPAC, Caltech Frank MasciMIPS 24umSSC Glenn MorrisonRadioVanguard JoAnn O’Linger DisksSSC Frazer Owen RadioNRAO Ismael Perez-Fournon QSOsIAC, Tenerife Marguerite Pierre X-ray/XMMCEA, Saclay Rick Puetter PixonsUCSD Steve SerjeantELAISU. Kent Gordon Stacey Molecular linesCornell Mike WernerIRSJPL

22. October 30, 2002 Santiago, ChileCarol Lonsdale22 SWIRE: Environment & LSS Kauffmann et al. (1999); 21x21x8 (Mpc/h) 3 red  blue: increasing SFR Resolving Star Formation History & AGN Accretion & Spheroid Evolution in Time and Space in context of Structure Formation z=3 z=0 z=1 z=2

23. October 30, 2002 Santiago, ChileCarol Lonsdale23 The SWIRE Survey 24  m / 70  m / 160  m 1 x 1 degree Rowan-Robinson 2001 3.6  m / 8  m / 24  m 10’ x 10’ Xu et al. 2001 0.5 < z < 3 100s of ~100Mpc cells 1000s sources in each cell > 10 6 galaxies >10 4 Type 1 AGN

24. October 30, 2002 Santiago, ChileCarol Lonsdale24 FIELDRA (J2000) DecISSA MJy/sr E(B-V)Size Sq. deg ELAIS-S100 h 38 m 30 s -44º 00'0.420.00814.0 XMM-LSS02 h 21 m 00 s -05º 00'1.30.027 8.8 Chandra-S03 h 32 m 00 s -28º 16'0.460.001 6.9 Lockman10 h 45 m 00 s +58º 00'0.380.00614.0 Lonsdale14 h 41 m 00 s +59º 25'0.470.012 6.5 ELAIS-N116 h 11 m 00 s +55º 00'0.440.007 8.8 ELAIS-N216 h 36 m 48 s +41º 01‘ 45"0.420.007 4.3 SWIRE Fields 7 large fields: large scale sizes combat cosmic variance

25. October 30, 2002 Santiago, ChileCarol Lonsdale25 Field Selection Strategy 1.Low extinction, cirrus noise: extensive survey for fields with I 100µm 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

26. October 30, 2002 Santiago, ChileCarol Lonsdale26 Minimize N H & Cirrus B 100 Contours at 1 and 2 MJy/sr CHANDRA-S ELAIS-S1 XMM-LSS LOCKMAN ELAIS-N1 LONSDALE ELAIS-N2 Schlegel et al. 1998 DIRBE-calibrated IRAS 100  m map

27. October 30, 2002 Santiago, ChileCarol Lonsdale27 Fields We Didn’t Select Groth Strip SSA68

28. October 30, 2002 Santiago, ChileCarol Lonsdale28 Cirrus Holes Too Small HDF-South HDF-North

29. October 30, 2002 Santiago, ChileCarol Lonsdale29 SWIRE Survey Fields Lockman Hole ELAIS-N1 IRAS 100  m images

30. October 30, 2002 Santiago, ChileCarol Lonsdale30 SWIRE Survey Fields ELAIS N2 ELAIS S1

31. October 30, 2002 Santiago, ChileCarol Lonsdale31 CDF-S Lonsdale Hole SWIRE Survey Fields

32. October 30, 2002 Santiago, ChileCarol Lonsdale32 SWIRE Survey Fields XMM-LSS SWIRE XMM-LSS M. Pierre, PI LH Xray surveys are typically very small (eg: Lockman Hole survey below). The large XMM-LSS survey is unique

33. October 30, 2002 Santiago, ChileCarol Lonsdale33 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

34. October 30, 2002 Santiago, ChileCarol Lonsdale34 Flux density (Jy) 10 100 1000 10 12 L  0.5 10 1 0.1 0.01 5 3 1 Z = 0.1 SPIRE (  m) Herschel/SPIRE 250, 350, 500μm imaging ~ 2007 launch M. Griffin,Cardiff

35. October 30, 2002 Santiago, ChileCarol Lonsdale35 Next Generation “Cosmic Windows” VLA proposal 40μJy 20cm J. Condon SWIRE/GALEX/ XMM-LSS optical ground-based Imaging Spectroscopy Deep J & K (partial SWIRE field coverage); K=21 A. Lawrence

36. October 30, 2002 Santiago, ChileCarol Lonsdale36 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

37. October 30, 2002 Santiago, ChileCarol Lonsdale37 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

38. October 30, 2002 Santiago, ChileCarol Lonsdale38 Six-band simulation 3.64.55.8 8.02470 Model of Xu et al, 2001, 2002 24μm LF 840 SEDs Starbursts Spirals AGN Ellipticals 5 x 5 arcmin

39. October 30, 2002 Santiago, ChileCarol Lonsdale39 Mosiaced IRAC Simulation 0.2 sq deg EROs Las Campanas NIR HDF Survey (Chen et al. 2001 ). LCIRS limit

40. October 30, 2002 Santiago, ChileCarol Lonsdale40 SWIRE Starbursts & AGN 1 sq degree SWIRE survey (excluding spheroids) 8μm 7200 sources 24μm 3300 70μm 2700 Warm AGN: 1000 Starbursts & obscured AGN: 4500

41. October 30, 2002 Santiago, ChileCarol Lonsdale41 Bias and SFR-Density Field  Would like to know evolution of the mass density field  What we measure is the galaxy density field: δ g = bδ m  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)

42. October 30, 2002 Santiago, ChileCarol Lonsdale42 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 optical IRAS Oliver et al 1996

43. October 30, 2002 Santiago, ChileCarol Lonsdale43 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-10 4 to 1-in-10 6

44. October 30, 2002 Santiago, ChileCarol Lonsdale44 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 Data Products and Archive Services SWIRE Data: Non-proprietary 1st release: early 2004