1. Aug 8th, 2007MAGPOP Summer School Extragalactic infrared and submillimetre surveys Michael Rowan-Robinson Imperial College London Dole et al 2006 most of the starlight ever generated in the universe is emitted at infrared wavelengths, ~ 50% is absorbed by dust and reemitted at far infrared and submillimetre wavelengths

2. Aug 8th, 2007MAGPOP Summer School 1 micron - 1 mm - a few terrestial windows the infrared and submillimetre bands

3. Aug 8th, 2007MAGPOP Summer School Pre-IRAS, IRAS Pre-IRAS: 1969: Caltech 2 Micron Survey (Neugebauer and Leighton) – circumstellar dust shells, BN object 1976: The AFGL Survey at 4.2, 11, 19.8 and 27.4  m (Price and Walker) – cds, HII regions IRAS: 1984: IRAS all sky survey at 12, 20, 60, 100  m - 30,000 infrared galaxies (measured redshifts of 12000 with S(60)>0.6 Jy - PSCz) - ir cirrus - ULIRGS, HLIRGS - AGN dust tori - ir dipole, large scale structure

4. Aug 8th, 2007MAGPOP Summer School IRAS Horsehead Nebula

5. Aug 8th, 2007MAGPOP Summer School IRAS all-sky survey

6. Aug 8th, 2007MAGPOP Summer School Infrared galaxy populations with IRAS we were able to identify the main infrared galaxy populations - quiescent galaxies (ir cirrus) - starburst galaxies (prototype M82) - extreme starbursts (prototype A220) - AGN dust tori but the IRAS survey was not deep enough (z ~ 0.3) to study the cosmological evolution of these populations, though 60  m source-counts showed that evolution is present, at a comparable rate to that seen in radio-galaxies and quasars an important insight was that as infrared luminosity increased, the proportion of interactions and mergers increased

7. Aug 8th, 2007MAGPOP Summer School ISO ISO, launched 1996, reached z~1, + spectroscopy

8. Aug 8th, 2007MAGPOP Summer School ISO surveys CAM Deep Surveys Fadda et al, 2001, AA, astro-ph/011412 Franceschini et al, 2002, AA, astro-ph/0108292 Elbaz et al, 2002, AA 384, 848 ELAIS Survey at 6.7, 15, 90, 175  m Oliver et al, 2000, MN 316, 749 Serjeant et al, 2000, MN 316, 768 Efstathiou et al, 2000, MN 319, 1169 Serjeant et al, 2001, MN 322, 262 Lari et al, 2001, MN 325, 1173 Gruppioni et al, 2002, MN 341, L1 Rowan-Robinson et al, 2004, MN 351, 1290 ISO HDF-N and HDF-S surveys Oliver et al, 2002, MN 332, 546 Mann et al, 2002, MN 332, 549 FIRBACK 175  m survey Dole et al, 2001, AA 372, 264

9. Aug 8th, 2007MAGPOP Summer School ISO surveys * main result was very strong increase in star-formation rate in galaxies between z = 0 and 1 (factor ~10) (Rowan-Robinson et al 1997, Flores et al 1999), confirming the result from optical surveys (Lilley et al 1996, Madau et al 1996) and that the rate estimated from optical data without correction for extinction is severely underestimated. problems of screen model for extinction correction issue of consistency between estimates of star-formation rate from uv, H , radio, far infrared sfr = 2.2 x 10 -10 L 60 = 2.5x10 -8 L H  = 4.5x10 -10 L 2800A

10. Aug 8th, 2007MAGPOP Summer School Dust extinction in local galaxies ~ 0.3 in local galaxies (Rowan-Robinson, 2003, MN 344, 13)

11. Aug 8th, 2007MAGPOP Summer School comparison of star-formation rate estimates Daddi et al 2007

12. Aug 8th, 2007MAGPOP Summer School HDFN at 850  m Hughes et al 1998 impact of JCMT SHADES blank field surveys at 850  m showed that we were able to survey the whole universe to z = 5 with ultraluminous ir galaxies

13. Aug 8th, 2007MAGPOP Summer School Submillimetre surveys Hubble Deep Field North Hughes et al 1998 Hawaii surveys Barger et al 1998, 1999, Cowie et al 2002, Wang et al 2004 CUDSS survey Eales et al 1999, Webb et al 2003, Clements et al 2004, Ashby et al 2006 UK 8 mJy survey (200 sq arcmin) Scott et al 2001, Fox et al 2001, Ivison et al 2002, Almaini et al 2003 SHADES (0.5 sq deg) Mortier et al 2005, Coppin et al 2006, Ivison et al 2007, Aretxaga et al 2007

14. Aug 8th, 2007MAGPOP Summer School submillimetre associations and galaxy redshift distribution Chapman et al, 2005, ApJ 622, 772 poor spatial resolution of JCMT means that reliable optical or infrared associations can only be made if have millimetre interferometry or radio associations why don’t we see submm galaxies at z > 4 ? is this a selection effect ?

15. Aug 8th, 2007MAGPOP Summer School Near-ir Surveys 2MASS all-sky survey at J, H, K (to 15.8, 15.1, 14.3 mag.) – http://www.ipac.caltech.edu/2mass/ UKIDDS survey of 7500 sq deg in JHK (K=18.3) -http://www.ukidss.org/ FIR Surveys SPITZER surveys (GTO - various, FLS - 4 sq deg, SWIRE - 49 sq deg, GOODS - 0.1 sq deg, AEGIS - 1 sq deg, COSMOS - 1 sq deg) at 3.6, 4.5, 5.6, 8, 24, 70, 160  m - http://ssc.spitzer.caltech.edu/ ASTRO-F all-sky survey in 6 bands at 9-180  m - http://www.akari.org.uk

16. Aug 8th, 2007MAGPOP Summer School 2MASS 2MASS provides a better picture of galaxy distribution at z<0.03

17. Aug 8th, 2007MAGPOP Summer School Layered SPITZER Surveys Wide–shallow FLS GTO-shallow SWIRE –greatest volume 4 8.5 49 sq deg –rare luminous objects –large-scale structure Confusion-limited GTO-deep GOODS-IRAC –maximum information 2.5 sq deg 300 sq arcmin on faintest resolved sources Ultra-deep GTO-ultra GOODS-24  m –confusion distribution 150 300 sq arcmin

18. Aug 8th, 2007MAGPOP Summer School M51 Sombrero combined 3.6, 8 and 24  m images (SINGS consortium)

19. Aug 8th, 2007MAGPOP Summer School M82 N2207/IC2163 Stefan’s Quintet

20. Aug 8th, 2007MAGPOP Summer School SIRTF SWIRE survey 49 sq deg in 6 areas, at 3.6, 4.5, 5.8, 8, 24, 70, 160  m

21. Aug 8th, 2007MAGPOP Summer School ELAIS N1: 9 sq. deg SWIRE 3.6  m survey in ELAIS-N1

22. Aug 8th, 2007MAGPOP Summer School Photometric redshifts method based on fixed galaxy and AGN templates, two passes through data to help identify QSOs and AGN dust tori, and selected priors Rowan-Robinson et al 2007

23. Aug 8th, 2007MAGPOP Summer School Photometric redshifts SWIRE-VVDS sample (with VVDS team, PI LeFevre) VIRMOS-VLT Deep Survey spectra >1000 sources ~3% rms in (1+z) <1% outliers ~ IRAC 3.6 and 4.5  m big help in reducing outliers z = 1234 red: gals, blue QSOs

24. Aug 8th, 2007MAGPOP Summer School Photometric redshifts All SWIRE Catalogue VVDS: 9 optical bands N1,N2: 5 optical bands Lockman: 3-4 optical bnds CDFS: 3 optical bands XMM-LSS: 5 optical bands z = 1 2 3 4 SWIRE Photometric Redshift Catalogue contains over 1 million redshifts, 10% have z >2, 4% have z > 3, 20% detected at 24  m, 1% at 70 or 160  m red: galaxies, blue QSOs

25. Aug 8th, 2007MAGPOP Summer School rms, % outliers, as function of number of bands

26. Aug 8th, 2007MAGPOP Summer School Redshift distributions >=3 bands from U-8  m left: Suburu XDS, R<27.5 below: ELAIS-N1, r<23.5: for optically blank sources use 3.6-8  m for phot-z

27. Aug 8th, 2007MAGPOP Summer School Lir/Lopt for galaxies with an ir excess, we fit ir templates (cirrus, M82, A220, AGN dust torus) and estimate L ir (reasonably accurate if have 70  m detection) for cirrus galaxies, L ir /L opt is a measure of optical depth of ism for star-forming galaxies, L ir /L opt is the specific star formation rate

28. Aug 8th, 2007MAGPOP Summer School Lir/Lopt for starbursts

29. Aug 8th, 2007MAGPOP Summer School star-forming ellipticals * Lir/Lopt (specific star formation rate) versus Lopt (~ M) for galaxies with elliptical galaxy template fits * includes objects like Arp 220, whose star formation is heavily obscured Black: cirrus Red: M82 starburst Green: A220 starburst

30. Aug 8th, 2007MAGPOP Summer School ultraluminous cirrus gals(L), star-forming ellipticals(R)

31. Aug 8th, 2007MAGPOP Summer School AKARI Japanese mission, 68 cm cooled telescope, first all-sky far infrared survey since IRAS, 90 and 140  m, sensitivity probably comparable to IRAS FSS, but much better spatial resolution, so in principle may be able to construct deeper all-sky sample than PSCz

32. Aug 8th, 2007MAGPOP Summer School HERSCHEL 3.6 m passively cooled telecope operating at 50-500  m layered survey will be carried out by SPIRE and PACS teams in guaranteed time, widest area 70 sq deg in 9 areas

33. Aug 8th, 2007MAGPOP Summer School PLANCK PLANCK will carry out a shallow all-sky extragalactic point-source survey, which will detect many high-z very luminous submm galaxies