1. AGN deep multiwavelength surveys: the case of the Chandra Deep Field South Fabrizio Fiore Simonetta Puccetti, Giorgio Lanzuisi

2. Table of content  Introduction  Big scenario for structure formation: AGN & galaxy co-evolution  SMBH census: search for highly obscured AGN  X-ray surveys  Unobscured and moderately obscured AGN density  Infrared surveys  Compton thick AGN  CDFS 2Msec observation: the X-ray view of IR bright AGN:  Spectra of IR sources directly detected in X-rays  X-ray “stacking” analysis of the sources not directly detected.  Introduction  Big scenario for structure formation: AGN & galaxy co-evolution  SMBH census: search for highly obscured AGN  X-ray surveys  Unobscured and moderately obscured AGN density  Infrared surveys  Compton thick AGN  CDFS 2Msec observation: the X-ray view of IR bright AGN:  Spectra of IR sources directly detected in X-rays  X-ray “stacking” analysis of the sources not directly detected.

3. A brief cosmic history Big bang Recombination Dark ages First stars, SN, GRB,galaxies, AGN Reionization, light from first objects ionize IGM Transparent Universe Today X. Fan, G. Djorgovski

4. Co-evolution of galaxies and SMBH Two seminal results: 1.The discovery of SMBH in the most local bulges; tight correlation between M BH and bulge properties. 2.The BH mass density obtained integrating the AGN L.-F. and the CXB ~ that obtained from local bulges  most BH mass accreted during luminous AGN phases! Most bulges passed a phase of activity: 1)Complete SMBH census, 2) full understanding of AGN feedback are key ingredients to understand galaxy evolution

6. AGN and galaxy co-evolution  Early on  Strong galaxy interactions= violent star-bursts  Heavily obscured QSOs  When galaxies coalesce  accretion peaks  QSO becomes optically visible as AGN winds blow out gas.  Later times  SF & accretion quenched  red spheroid, passive evolution  Early on  Strong galaxy interactions= violent star-bursts  Heavily obscured QSOs  When galaxies coalesce  accretion peaks  QSO becomes optically visible as AGN winds blow out gas.  Later times  SF & accretion quenched  red spheroid, passive evolution To prove this scenario we need to have: 1)Complete SMBH census, 2)Physical models for AGN feedbacks 3)Observational constraints to these models

7. Hierarchical clustering  most massive BH in most massive galaxies, which are in the most massive clusters  Complete BH census needed.  Strong evidences for missing BH  most massive BH in most massive galaxies, which are in the most massive clusters  Complete BH census needed.  Strong evidences for missing BH Marconi 2004-2007 Gilli et al. 2007

8. Evidences for missing SMBH While the CXB energy density provides a statistical estimate of SMBH growth, the lack, so far, of focusing instrument above 10 keV (where the CXB energy density peaks), frustrates our effort to obtain a comprehensive picture of the SMBH evolutionary properties. Gilli et al. 2007 Marconi 2004-2007 Menci, Fiore et al. 2004, 2006, 2008 43-44 44-44.5

9. AGN density 43-44 44-44.5 44.5-45.5 >45.5 42-43 La Franca, Fiore et al. 2005 Menci, Fiore et al. 2008 Paucity of Seyfert like sources @ z>1 is real? Or, is it, at least partly, a selection effect? Are we missing in Chandra and XMM surveys highly obscured (N H  10 24 cm -2 ) AGN? Which are common in the local Universe… Paucity of Seyfert like sources @ z>1 is real? Or, is it, at least partly, a selection effect? Are we missing in Chandra and XMM surveys highly obscured (N H  10 24 cm -2 ) AGN? Which are common in the local Universe…

10. Highly obscured Mildly Compton thick INTEGRAL survey ~ 100 AGN Sazonov et al. 2006

11. Completing the census of SMBH  X-ray surveys:  very efficient in selecting unobscured and moderately obscured AGN  Highly obscured AGN recovered only in ultra-deep exposures  IR surveys:  AGNs highly obscured at optical and X-ray wavelengths shine in the MIR thanks to the reprocessing of the nuclear radiation by dust  X-ray surveys:  very efficient in selecting unobscured and moderately obscured AGN  Highly obscured AGN recovered only in ultra-deep exposures  IR surveys:  AGNs highly obscured at optical and X-ray wavelengths shine in the MIR thanks to the reprocessing of the nuclear radiation by dust Dusty torus Central engine

12. X-ray-MIR surveys  CDFS-Goods MUSIC catalog (Grazian et al. 2006, Brusa, FF et al. 2008) Area 0.04 deg2  ~200 X-ray sources, 2-10 keV down to 2  10 -16 cgs, 0.5-2 keV down to 5  10 -17 cgs 150 spectroscopic redshifts  1100 MIPS sources down to 40  Jy, 3.6  m detection down to 0.08  Jy  Ultradeep Optical/NIR photometry, R~27.5, K~24  ELAIS-S1 SWIRE/XMM/Chandra survey (Puccetti, FF et al. 2006, Feruglio,FF et al. 2007, La Franca, FF et al. 2008). Area 0.5 deg2  500 XMM sources, 205 2-10 keV down to 3  10 -15 cgs, >half with spectroscopic redshifts.  2600 MIPS sources down to 100  Jy, 3.6  m detection down to 6  Jy  Relatively deep Optical/NIR photometry, R~25, K~19  COSMOS XMM/Chandra/Spitzer. Area ~1 deg 2  ~1700 Chandra sources down to 6  10 -16 cgs, >half with spectroscopic redshifts.  900 MIPS sources down to 500  Jy, 3.6  m detection down to 10  Jy, R~26.5  In future we will add:  CDFS-Goods, Chandra 2Msec observation  CDFN-Goods  COSMOS deep MIPS survey  CDFS-Goods MUSIC catalog (Grazian et al. 2006, Brusa, FF et al. 2008) Area 0.04 deg2  ~200 X-ray sources, 2-10 keV down to 2  10 -16 cgs, 0.5-2 keV down to 5  10 -17 cgs 150 spectroscopic redshifts  1100 MIPS sources down to 40  Jy, 3.6  m detection down to 0.08  Jy  Ultradeep Optical/NIR photometry, R~27.5, K~24  ELAIS-S1 SWIRE/XMM/Chandra survey (Puccetti, FF et al. 2006, Feruglio,FF et al. 2007, La Franca, FF et al. 2008). Area 0.5 deg2  500 XMM sources, 205 2-10 keV down to 3  10 -15 cgs, >half with spectroscopic redshifts.  2600 MIPS sources down to 100  Jy, 3.6  m detection down to 6  Jy  Relatively deep Optical/NIR photometry, R~25, K~19  COSMOS XMM/Chandra/Spitzer. Area ~1 deg 2  ~1700 Chandra sources down to 6  10 -16 cgs, >half with spectroscopic redshifts.  900 MIPS sources down to 500  Jy, 3.6  m detection down to 10  Jy, R~26.5  In future we will add:  CDFS-Goods, Chandra 2Msec observation  CDFN-Goods  COSMOS deep MIPS survey

13. 40 arcmin 52 arcmin z = 0.73 struct ure z-COSMOS faint Color: XMM first year Full COSMOS field Chandra deep and wide fields CDFS 2Msec 0.05deg 2 CCOSMOS 200ksec 0.5deg 2 100ksec 0.4deg 2 ~400 sources 1.8 Msec ~1800 sources Elvis et al. 2008 20 arcmin 1 deg

14. AGN directly detected in X-rays Open circles=logNH>23 Open squares = MIR/O>1000 sources (Tozzi et al. 2003)

15. IR surveys  Difficult to isolate AGN from star- forming galaxies (Lacy 2004, Barnby 2005, Stern 2005, Polletta 2006 and many others) Dust heated by AGN Colder dust/PAHs (Glikman et al. 2005) (Lagache et al. 2004)

16. MIR selection of CT AGN ELAIS-S1 obs. AGN ELAIS-S1 24mm galaxies HELLAS2XMM CDFS obs. AGN Fiore et al. 2003 Open symbols = unobscured AGN Filled symbols = optically obscured AGN Unobscured obscured X/0 MIR/O

17. MIR selection of CT AGN CDFS X-ray HELLAS2XMM GOODS 24um galaxies COSMOS X-ray COSMOS 24um galaxies R-K Fiore et al. 2008a Fiore et al. 2008b Open symbols = unobscured AGN Filled symbols = optically obscured AGN * = photo-z

18. GOODS MIR AGNs Fiore et. al. 2008a directly Stack of Chandra images of MIR sources not directly detected in X-rays  F24um/FR>1000 R-K>4.5  logF(1.5-4keV) stacked sources=-17 @z~2 logL obs (2- 8keV) stacked sources ~41.8  log ~44.8 ==> logL(2- 8keV) unabs.~43  Difference implies logN H ~24 F24/FR>1000 R-K>4.5  ~200!! Msun/yr  ~7!! Msun/yr  ~65 Msun/yr F24um/FR 4.5  ~ 18 Msun/yr  ~13 Msun/yr  ~20 Msun/yr F24/FR>1000 R-K>4.5  ~200!! Msun/yr  ~7!! Msun/yr  ~65 Msun/yr F24um/FR 4.5  ~ 18 Msun/yr  ~13 Msun/yr  ~20 Msun/yr

19. Program of the project (1)  Selection of IR sources with X- ray detection which are likely to host a highly obscured AGN  Extraction of the Chandra spectra of these sources from the event files  Characterization of the X-ray spectra: estimate of the absorbing column density  Evaluation of systematic errors:  Background evaluation  Combination of data from different observations  Selection of IR sources with X- ray detection which are likely to host a highly obscured AGN  Extraction of the Chandra spectra of these sources from the event files  Characterization of the X-ray spectra: estimate of the absorbing column density  Evaluation of systematic errors:  Background evaluation  Combination of data from different observations

20. Program of project (2)  Selection of IR sources without a direct X-ray detection which are likely to host a highly obscured AGN  ‘Stacking’ of X-ray images at the position of these sources  Analysis of the ‘stacked’ images  Selection of IR sources without a direct X-ray detection which are likely to host a highly obscured AGN  ‘Stacking’ of X-ray images at the position of these sources  Analysis of the ‘stacked’ images

22. X-ray (and multiwavelength) surveys Fabrizio Fiore

23. Table of content  A historical perspective  Tools for the interpretation of survey data  Number counts  Luminosity functions  Main current X-ray surveys  What next  A historical perspective  Tools for the interpretation of survey data  Number counts  Luminosity functions  Main current X-ray surveys  What next

24. A historical perspective  First survey of cosmological objects: radio galaxies and radio loud AGN  The discovery of the Cosmic X-ray Background  The first imaging of the sources making the CXB  The resolution of the CXB  What next?  First survey of cosmological objects: radio galaxies and radio loud AGN  The discovery of the Cosmic X-ray Background  The first imaging of the sources making the CXB  The resolution of the CXB  What next?

25. Radio sources number counts First results from Cambridge surveys during the 50’: Ryle Number counts steeper than expected from Euclidean universe

26. Number counts Flux limited sample: all sources in a given region of the sky with flux > than some detection limit Flim. Consider a population of objects with the same L Assume Euclidean space

27. Number counts Test of evolution of a source population (e.g. radio sources). Distances of individual sources are not required, just fluxes or magnitudes: the number of objects increases by a factor of 10 0.6 =4 with each magnitude. So, for a constant space density, 80% of the sample will be within 1 mag from the survey detection limit. If the sources have some distribution in L:

28. Problems with the derivation of the number counts Completeness of the samples. Eddington bias: random error on mag measurements can alter the number counts. Since the logN-logFlim are steep, there are more sources at faint fluxes, so random errors tend to increase the differential number counts. If the tipical error is of 0.3 mag near the flux limit, than the correction is  15%. Variability. Internal absorption affects “color” selection. SED, ‘K-correction’, redshift dependence of the flux (magnitude).

29. Galaxy number counts

30. Optically selected AGN number counts z<2.2 B=22.5  100 deg -2 B=19.5  10 deg -2 z>2.2 B=22.5  50 deg -2 B=19.5  1 deg -2 B-R=0.5

31. X-ray AGN number counts OUV sel. AGN=0.3 R=22 ==> 3  10 -15  1000deg -2 R=19 ==> 5  10 -14  25deg -2 The surface density of X-ray selected AGN is 2-10 times higher than OUV selected AGN

32. The cosmic backgrounds energy densities

33. The Cosmic X-ray Background Giacconi (and collaborators) program: 1962 sounding rocket 1970 Uhuru 1978 HEAO1 1978 Einstein 1999 Chandra!

34. The Cosmic X-ray Background  The CXB energy density:  Collimated instruments:  1978 HEAO1  2006 BeppoSAX PDS  2006 Integral  2008 Swift BAT  Focusing instruments:  1980 Einstein 0.3-3.5 keV  1990 Rosat 0.5-2 keV  1996 ASCA 2-10 keV  1998 BeppoSAX 2-10 keV  2000 RXTE 3-20 keV  2002 XMM 0.5-10 keV  2002 Chandra 0.5-10 keV  2012 NuSTAR 6-100 keV  2014 Simbol-X 1-100 keV  2014 NeXT 1-100 keV  2012 eROSITA 0.5-10 keV  2020 IXO 0.5-40 keV  The CXB energy density:  Collimated instruments:  1978 HEAO1  2006 BeppoSAX PDS  2006 Integral  2008 Swift BAT  Focusing instruments:  1980 Einstein 0.3-3.5 keV  1990 Rosat 0.5-2 keV  1996 ASCA 2-10 keV  1998 BeppoSAX 2-10 keV  2000 RXTE 3-20 keV  2002 XMM 0.5-10 keV  2002 Chandra 0.5-10 keV  2012 NuSTAR 6-100 keV  2014 Simbol-X 1-100 keV  2014 NeXT 1-100 keV  2012 eROSITA 0.5-10 keV  2020 IXO 0.5-40 keV

35. The V/V max test Marteen Schmidt (1968) developed a test for evolution not sensitive to the completeness of the sample. Suppose we detect a source of luminosity L and flux F >F lim at a distance r in Euclidean space: If we consider a sample of sources distributed uniformly, we expect that half will be found in the inner half of the volume V max and half in the outer half. So, on average, we expect V/V max =0.5

36. The V/V max test In an expanding Universe the luminosity distance must be used in place of r and r max and the constant density assumption becomes one of constant density per unit comuving volume.

37. Luminosity function In most samples of AGN > 0.5. This means that the luminosity function cannot be computed from a sample of AGN regardless of their z. Rather we need to consider restricted z bins. More often sources are drawn from flux-limited samples, and the volume surveyed is a function of the Luminosity L. Therefore, we need to account for the fact that more luminous objects can be detected at larger distances and are thus over-represented in flux limited samples. This is done by weighting each source by the reciprocal of the volume over which it could have been found:

38. Luminosity function

39. Assume that the intrinsic spectrum of the sources making the CXB has  E =1 I 0 =9.8  10 -8 erg/cm 2 /s/sr  ’=4  I 0 /c

40. Optical (and soft X-ray) surveys gives values 2-3 times lower than those obtained from the CXB (and of the F.&M. and G. et al. estimates)

41. Flux 0.5-10 keV (cgs) Area HELLAS2XMM 1.4 deg 2 Cocchia et al. 2006 Champ 1.5deg2 Silverman et al. 2005 XBOOTES 9 deg 2 Murray et al. 2005, Brand et al. 2005 XMM-COSMOS 2 deg 2 -16 -15 -14 -13 CDFN-CDFS 0.1deg 2 Barger et al. 2003; Szokoly et al. 2004 EGS/AEGIS 0.5deg 2 Nandra et al. 2006 SEXSI 2 deg 2 Eckart et al. 2006 C-COSMOS 0.9 deg 2 E-CDFS 0.3deg 2 Lehmer et al. 2005 ELAIS-S1 0.5 deg 2 Puccetti et al. 2006 Pizza Plot A survey of X-ray surveys

42. Point sources Clusters of galaxies

43. A survey of surveys Main areas with large multiwavelength coverage:  CDFS-GOODS 0.05 deg 2 : HST, Chandra, XMM, Spitzer, ESO, Herschel, ALMA  CDFN-GOODS 0.05 deg 2 : HST, Chandra, VLA, Spitzer, Hawaii, Herschel  AEGIS(GS) 0.5 deg 2 : HST, Chandra, Spitzer, VLA, Hawaii, Herschel  COSMOS 2 deg 2 : HST, Chandra, XMM, Spitzer, VLA, ESO, Hawaii, LBT, Herschel, ALMA  NOAO DWFS 9 deg 2 : Chandra, Spitzer, MMT, Hawaii, LBT  SWIRE 50 deg 2 (Lockman hole, ELAIS, XMMLSS,ECDFS): Spitzer, some Chandra/XMM, some HST, Herschel  eROSITA! 20.000 deg 2 10 -14 cgs 200 deg 2 3  10 -15 cgs Main areas with large multiwavelength coverage:  CDFS-GOODS 0.05 deg 2 : HST, Chandra, XMM, Spitzer, ESO, Herschel, ALMA  CDFN-GOODS 0.05 deg 2 : HST, Chandra, VLA, Spitzer, Hawaii, Herschel  AEGIS(GS) 0.5 deg 2 : HST, Chandra, Spitzer, VLA, Hawaii, Herschel  COSMOS 2 deg 2 : HST, Chandra, XMM, Spitzer, VLA, ESO, Hawaii, LBT, Herschel, ALMA  NOAO DWFS 9 deg 2 : Chandra, Spitzer, MMT, Hawaii, LBT  SWIRE 50 deg 2 (Lockman hole, ELAIS, XMMLSS,ECDFS): Spitzer, some Chandra/XMM, some HST, Herschel  eROSITA! 20.000 deg 2 10 -14 cgs 200 deg 2 3  10 -15 cgs

44. 40 arcmin 52 arcmin z = 0.73 struct ure z-COSMOS faint Color: XMM first year Full COSMOS field Chandra deep and wide fields CDFS 2Msec 0.05deg 2 CCOSMOS 200ksec 0.5deg 2 100ksec 0.4deg 2 ~400 sources 1.8 Msec ~1800 sources Elvis et al. 2008 20 arcmin 1 deg

45. XMM surveys COSMOS 1.4Msec 2deg 2 Lockman Hole 0.7Msec 0.3deg 2

46. Chandra surveys AEGIS: Extended Groth Strip Bootes field

47. Spitzer large area surveys: SWIRE Elais-N1 Elais-N2 XMM-LSS Elais-S1 Lockman Hole

48. eROSITA ~30ks on poles, ~1.7ksec equatorial

49. What next? The X-ray survey discovery space -13 -15 -17 cgs log Sensitivity log Energy range 1 10 100 keV Log Area deg 2 4 2 0 Einstein ROSAT ROSAT eROSITA ASCA/BSAX XMM ChandraIXO ASCA/BSAX XMM Chandra IXO IXO NS NeXT SX BSAX/ASCA XMM Swift