1. May 19-22, 2014Bologna pg course Infrared and submillimetre surveys, models for counts and background Michael Rowan-Robinson Imperial College London 1.Extragalactic infrared and submillimetre surveys 2. Models for source-counts and background radiation, from submm to ultraviolet

2. May 19-22, 2014Bologna pg course 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

3. May 19-22, 2014Bologna pg course 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. May 19-22, 2014Bologna pg course 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 new IRAS FSC galaxy redshift catalogue: Wang and R-R 2014

5. May 19-22, 2014Bologna pg course 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

6. May 19-22, 2014Bologna pg course 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. 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

7. May 19-22, 2014Bologna pg course ISO counts at 15  m

8. May 19-22, 2014Bologna pg course 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 SCUBA Legacy Surveys (SASSy and CLS) – in progress

9. May 19-22, 2014Bologna pg course SHADES counts at 850  m Coppins et al, 2007

10. May 19-22, 2014Bologna pg course 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/ AKARI all-sky survey in 6 bands at 9-180  m - http://www.akari.org.uk

11. May 19-22, 2014Bologna pg course 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

12. May 19-22, 2014Bologna pg course SPITZER SWIRE survey 49 sq deg in 6 areas, at 3.6, 4.5, 5.8, 8, 24, 70, 160  m

13. May 19-22, 2014Bologna pg course differential counts at 24  m 24  m differential counts (Shupe et al, 2007, Papovich et al 2004)

14. May 19-22, 2014Bologna pg course AKARI Japanese mission, 68 cm cooled telescope, first all-sky far infrared survey since IRAS, 90 and 140  m, sensitivity comparable to IRAS FSS, better spatial resolution, but worse confirmation rate

15. May 19-22, 2014Bologna pg course HERSCHEL 3.6 m passively cooled telecope operating at 50-500  m layered extragalactic surveys were carried out by SPIRE and PACS teams in guaranteed time

16. May 19-22, 2014Bologna pg course HERSCHEL surveys SPIRE-HerMES survey of ~100 sq deg at 250, 350, 500  m H-ATLAS survey of 550 sq deg at 100, 160, 250, 350, 500  m PACS-PEP survey of GOODS-S at 70, 100, 160  m HerMES counts - Oliver et al 2010 H-ATLAS counts – Clements et al 2010 PEP counts – Berta et al 2010 counts and luminosity functions at 70, 100, 160 – Magnelli et al 2013 evolution and luminosity functions to z ~ 4 at 70-500  m – Gruppioni et al 2013

17. Hermes source-counts Oliver et al. A&A 518, L21 counts + P(D) account for large fraction of infrared background May 19-22, 2014Bologna pg course

18. May 19-22, 2014Bologna pg course PACS 100 and 160  m counts Magnelli et al 2013

19. May 19-22, 2014Bologna pg course FIR luminosity density as function of z

20. May 19-22, 2014Bologna pg course star-formation history to z = 6 Thompson et al 2006 Reddy et al 2007

21. May 19-22, 2014Bologna pg course Templates, z distribns, in PEP survey Gruppioni et al 2013 100 160

22. May 19-22, 2014Bologna pg course FIR luminosity function from z = 0-4

23. May 19-22, 2014Bologna pg course a schematic evolutionary scenario

24. May 19-22, 2014Bologna pg course PLANCK PLANCK carried out a shallow all-sky extragalactic point-source survey, which detected several thousand galaxies, a few high-z very luminous submm galaxies

25. May 19-22, 2014Bologna pg course AKARI AKARI carried out an all-sky point-source survey, at 9, 18, 65, 90, 140, 160  m. AKARI-FIS All-sky Bright Source Catalogue, v 1.0, contains 427,071 sources at 65, 90, 140, 160  m (Yamamura et al 2010) AKARI-IRC All-sky Bright Source Catalogue, v 1.0, contains 844,649 sources at 9  m, 194,551 sources at 18  m (Ishihara et al 2010) also carried out deep surveys at the ecliptic poles (eg Goto et al 2010, 2011)

26. May 19-22, 2014Bologna pg course WISE WISE, launched 2009, carried out all-sky survey at 3.4, 4.6, 12 and 22  m, 5  sensitivities 0.08, 0.11, 1 and 6 mJy. (Wright et al 2010) Source Catalog (2013) lists 563 million objects

27. May 19-22, 2014Bologna pg course Models for source counts and background spectrum, from submm to ultraviolet ingredients for counts model at submm to uv wavelengths star-formation history, luminosity functions assumed seds, parameter estimation predicted counts and background intensity

28. May 19-22, 2014Bologna pg course Far infrared and submillimetre source- count models Franceschini et al, 2001, AA 378, 1 Rowan-Robinson et al, 2001, Elbaz et al, 2002, AA 384, 848 Lagache et al, 2004, ApJS 154, 112 Gruppioni et al, 2005, ApJ 318, 9 (review Lagache, Puget, Dole, 2005, ARAA 43, 727) Rowan-Robinson, 2009, Valiante et al, 2009, Le Borgne et al, 2009, Franceschini et al, 2010, Gruppioni et al, 2010, Lacey et al, 2010, Marsden et al 2011, Rahmati & van der Werf, 2011 Niemi et al, 2012, Bethermin et al, 2012,

29. May 19-22, 2014Bologna pg course MODELS FOR COUNTS AND BACKGROUND FROM OPTICAL TO SUBMM (Rowan-Robinson 2001, ApJ, 549, 745, 2009 MN) * parameterized approach to star formation history * fitted to infrared and submm counts and background * 60  m luminosity function derived from PSCz data * ir and submm seds based on mixture of four components (cirrus, M82-starbust, AGN dust torus, Arp220), proportions depending on luminosity

30. May 19-22, 2014Bologna pg course PARAMETERIZED MODEL FOR STAR FORMATION HISTORY * assumed star formation history: sfr =  * (t)/  * (t o ) = exp Q{1 - t/t o }. (t/t o ) P meaning of parameters: t 0 /Q =  sf (cf Bruzual,Charlot 1993) peak sfr when t/t o = P/Q, or t = P  sf (essentially the Bruzual and Charlot models with an additional parameter to tune the epoch of peak star formation rate) * assume 60 µm luminosity function of the form  (L) = C * (L/ L * ) 1-  exp{-0.5[log 10 (1+L/L * )/  ] 2 } (Saunders et al 1990) * assume luminosity evolution with L * (t)/L * (t o ) =  * (t)/  *( t o ) * for each P,Q, parameters L * (t o ) and  are solved for from PSCz data (15000 IRAS galaxies with known z, S(60)≥ 0.6 Jy)

31. May 19-22, 2014Bologna pg course parameterized star-formation history sfr =  * (t)/  * (t o ) = exp Q{1 - t/t o }. (t/t o ) P meaning of parameters: t 0 /Q =  sf peak sfr when t/t o = P/Q, or t = P  sf

32. May 19-22, 2014Bologna pg course assumed seds, fit to counts, predictions assumed spectral energy distribution, to convert luminosity function to other wavelengths, is mixture of cirrus, M82-starburst, AGN dust torus, Arp220-starburst components (radiative transfer models from Efstathiou et al 2000, Rowan-Robinson 1995), with proportion varying with 60 µm luminosity, to match 12-25-60-100-850 colour-colour and colour-luminosity diagrams * fit to observed counts at 60, 850 µm, and background intensity at 140, 350, 750 µm to find best (least chi 2 ) values of P,Q: Ω o  PQ 0.30.73.09.0 best-fitting models then used to predict counts and background spectrum at 0.1 - 1250  m

33. May 19-22, 2014Bologna pg course Infrared templates

34. May 19-22, 2014Bologna pg course colour-colour, colour-luminosity (Rowan- Robinson 2001)

35. May 19-22, 2014Bologna pg course Luminosity function at 850  m

36. May 19-22, 2014Bologna pg course Luminosity function at 60  m

37. May 19-22, 2014Bologna pg course Luminosity function at 12  m

38. May 19-22, 2014Bologna pg course Redshift distributions 850  m 175  m 60  m 0.44  m

39. May 19-22, 2014Bologna pg course Star- formation history (Rowan-Robinson 2003b)

40. far ir and submm source-counts new model for ir counts (developed from RR 2001 models): independent evolution for each component, evolution has to flatten off at z < 0.5, allow max. z cutoff (RR, 2009) M82 cirrus AGN dust tori May 19-22, 2014Bologna pg course

41. counts at 70-1100  m, ir background new SWIRE 70, 160, SHADES 850, COSMOS,AZTEC 1100  m differential counts (Afonso-Luis et al, 2009, Coppins et al 2009, Austermann et al 2008,2009) models RR 2009 May 19-22, 2014

42. Bologna pg course Bethermin et al (2012) counts model Dependence of key parameters on redshift Evolution of adopted templates with redshift

43. May 19-22, 2014Bologna pg course Bethermin et al (2012) counts model

44. May 19-22, 2014Bologna pg course Bethermin et al (2012) counts model

45. May 19-22, 2014Bologna pg course the interpretation of the extragalactic background the integrated extragalactic background spectrum is a weighted integral of the star-formation history I = c  o to  (t) L Z (t) dt weighting is by K-correction L Z /L so submm weighted to higher redshift than far and mid ir submm background can give strong limit on high z sfr

46. May 19-22, 2014Bologna pg course Models for infrared background Rowan-Robinson 2001

47. May 19-22, 2014Bologna pg course Models for infrared background Rowan-Robinson 2009 now have good bg data at 24, 70, 160  m models, modified to fit 24  m counts, now also give better fit to background spectrum

48. May 19-22, 2014Bologna pg course Evolution of galaxies- the infrared view submillimetre galaxies, window to high redshift ? lensing as a route to high redshift star formation history heavy element formation, evolution of gas and dust far ir and submm counts and background when was the first infrared light from galaxies ?

49. May 19-22, 2014Bologna pg course submillimetre galaxies first z > 2 IRAS galaxy (F10214+4723) turned out to be bright at 850  m (R-R et al 1991, 1993) negative K-correction at submm wavelengths makes these a window to high redshift (Franceschini et al 1994) however, observed z-distribution of submm galaxies peaks at z~2-3 (Chapman et al 2005) source-count models seem to need z cutoff at ~4 to explain 850 and 1100  m counts (R-R 2009)

50. May 19-22, 2014Bologna pg course gravitational lensing Blain (1996) emphasized lensing could be a big factor in explaining luminosities of submillimetre galaxies significant fraction of IRAS hyperluminous infrared galaxies are lensed (R-R and Wang 2010 estimate lensed percentage 10-30%) Negrello et al (2010) show 5 lensed galaxies from the Herschel-Atlas survey, predict more than 100 will be found need to see more systematic use of lenses to survey high-z universe. So far not finding large numbers of z > 4 infrared galaxies.

51. Herschel-ATLAS: lensed galaxies N E 80’’ Bologna pg course May 19-22, 2014 Significant fraction (50%?) of bright (>100mJy) 500  m sources are lenses (Negrello et al 2010)

52. z=2.958 lensed Hermes galaxy N E 80’’ Bologna pg course Spectrum using CSO ZSPEC, Scott et al 2011 May 19-22, 2014

53. Bologna pg course Star formation history Madau (1996) used Lilley et al survey and HDF to estimate sfr(z) R-R et al (1997) used ISO data to derive much higher sf rates to z=1 (uv-opt need dust correction) need to correct far ir for heating by evolved stars (Bell 2003, R-R 2003). With this correction, far ir luminosity is a good estimator for obscured star formation rate compilation based on uv, H , far ir (Hopkins 2007)

54. May 19-22, 2014 Variation of average A V with z Observed points are from study of photometric redshifts in HDF. Curves are closed box galaxy models with constant yield, instantaneous recycling, star-formation history consistent with observed history, and in which all heavy elements are assumed to be in dust. (Rowan-Robinson 2003) 0.3 0.2 0.1 0 z=0 1 2 3 4 5 similar result from SWIRE (R-R et al 2008) Bologna pg course

55. May 19-22, 2014Bologna pg course When was the first (rest-frame) infrared light ? Reionization appears to have taken place between z =11 and z = 6. First stars at z~30 ? First galaxies at z~10? First quasars at z~10? (and which came first?) How long did it take to get A V >1 (and hence most starlight being reprocessed in the infrared) in star-forming clouds ? If supernovae make enough dust, need 10 6 years, if need AGB stars, then need 10 9 years. [1 Gyr from z=10 would be z=4] can learn a lot from dwarf galaxies, with metallicity extending down to 1/30 th solar. Halo of our Galaxy has stars with very low metallicity, which could be from z>10 era.