2. Castel Gandolfo, Ottobre 2005 Agn and Galaxy Evolution Paolo Tozzi AGN and Galaxy evolution from Deep X-ray surveys: latest results from the CDFS

3. Deep X-ray Surveys: open issues The unresolved fraction of the XRB at high energies, and its relation with obscured cosmic matter accretion The two epochs of cosmic accretion X-ray properties of optically or radio selected sources: star formation at high z Effects of Large Scale Structure on AGN activity

4. 0.3-1 keV 1-3 keV 3-7 keV Rosati et al. 2002 National Geographic, Dec 2002

5. AGN Contribution to the hard XRB Beppo SAX Vecchi et al. 1999 ASCA2 Ishisaki et al. 1999 ASCA1 Ueda et al. 1999 HEAO1 Marshall et al. 1980 CDFS (1Ms): XRB(S> 4.5 × 10 -16 ) = (1.70 ± 0.15) × 10 -11 erg s -1 cm -2 deg -2 90% resolved in 0.5-2 keV 93% resolved in 2-8 keV AGN contribution 83% in 0.5-2 keV 95% in 2-8 keV (Bauer et al. 2004) CDFN (2Ms): XRB(S> 2 × 10 -16 ) = (2.07 ± 0.15) × 10 -11 erg s -1 cm -2 deg -2

6. Worsley et al. 2004; 2005 Missing XRB: N H =4.5 10 23 cm -2 @ z=0.8 ~50% not resolved yet for E> 5 keV (Worsley et al. 2004, 2005) The unresolved fraction increases with the energy band

10. Compton thick candidates

12. N H vs redshifts for the whole sample

13. Detected fraction as a function of N H and z Sampling different luminosities and spectral population at different z z < 0.7 0.7 < z <1.5 z > 1.5

14. Tozzi et al. 2004 N H histogram corrected for completeness The N H distribution tells us about the fraction of the sky seen from the black hole covered by a given column density Tozzi et al. 2005

15. N H distribution vs Optical Type

16. Whole sample (321) Cthick candidates (14) Consistent with evolutionary sequence: pre-QSO phase C-thin absorbed QSO (QSOII @ high z) unobscured QSO activity quiescent spheroidal galaxy Alexander et al. 2005; Stevens et al. 2005 Model: Granato et al. 2005 Part of the missing XRB is from intermediate z strongly absorbed moderate luminosity, possibly C-thick sources, in a secondary, relatively low-z phase of accretion (see “downsizing” or anti- hierarchical behaviour) Whole sample (321) QSOII (44)

17. Ueda et al 2003 Hasinger et al. 2005 Luminosity dependent density evolution: downsizing or anti-hierarchical behaviour

18. Merloni 2005 It is crucial to understand the properties of accretion through a careful analysis of the X-ray emission properties (luminosity, intrinsic absorption and its dependence on luminosity and redshift)

19. Compute the contribution of the absorbed sources to the XRB

20. Worsley et al. 2004 This work After computing the skycoverage according to the spectral shape of each source

21. Submm detection of a Type II QSO Mainieri et al. 2004 As expected in the starburst/BH model (Fabian 1999)

22. Use secure spectral identifications in CDFS and CDFN Norman et al. 2004 29 galaxies with good spectra in the CDFS and emission line ratios consistent with starbursts or normal galaxies give the X-ray priors. A Bayesian approach allows us to identify 74 galaxies in the CDFS and 136 in the CDFN (2 Ms)

23. SFR densities C ompilation from Tresse et al. 2002: Gallego et al. 1995 (H  ) Gronwall 1999 Hopkins et al. 2000 Pascual et al. 2001 Tresse et al. 2002 Sullivan et al. 2000 Lilly et al. 1996 Lines from 60  m Saunders et al. 1990, Takeuchi et al. 2003 Norman et al. 2004 XLF consistent with a PLE ~ (1+z) 2.7 Consistent with an evolution of SFR Q (1+z) 2.7 for 0<z<1. XLF of Star Forming Galaxies is a goal for future X-ray missions (Con-X, XEUS)

24. Daddi et al. 2004 K20 survey

25. IR selected galaxies at z~2 with massive SF Daddi et al. 2004 Stacked image of 23 BzK galaxies; HR< -0.5 @ 2sigma ; L 2-10 ~10 42 erg/sec SFR ~ 170 M A yr -1 (4 higher than LBG). SFRD of 0.04 M A /yr/Mpc 3 We are witnessing the massive spheroid formation epoch (the peak of just the low-z tail?) Soft Hard

26. Extended CDFS PI N. Brandt ~1000 sources (Lehmer et al. 2005) 1Ms + 4 X 240 ks

27. Radio Catalog 236 sources on ~ the same ECDFS area Match Radio Sources with 366+644 sources in the 1Ms+ECDFS(new only) Combined X-ray images of all the remaining radio sources With K. Kellerman, Ed Fomalont, J. Kelly, P. Shaver, & the CDFS Team.

28. X-ray Radio matches: 48 sources (out of 366 in the 1Msec catalog) 83 sources (in the 1Ms+EXT cat) 45 sources have: spectroscopic redshift and optical type (27) photometric redshift (18) soft and hard band luminosity Intrinsic absorption, spectral shape 160 Radio sources without X-ray counterpart But with sub-treshold X-ray emission: 83 within the 1Ms+ECDFS exposure +77 within the ECDFS (only 240 ks)

29. 13 sources with L X <10 42 erg s -1 8 LEX 2 HEX 3 non id L R -L X correlation for sources with X-ray detection for 45 sources with z (luminosity from best fit X-ray model) (soft hard)

30. Distribution of intrinsic N H Distribution of intrinsic absorption for 45 sources with spec or photometric z, compared with the distribution of the whole X-ray sample 17 sources with high L R 28 sources with low L R N H >10 22 cm -2 ~ Type II AGN 10 21 < N H < 10 22 cm -2 ~ Type I AGN N H <10 21 cm -2 ~ Type I AGN – SF Gal

31. Photometry for the 83 sources within the 1Ms field detected only in the radio: 485 +- 80 soft (0.5-2 keV) 260 +- 80 hard (2-7 keV) X-ray photometry for the remaining Radio sources

32. Gilli et al. 2003 Large Scale structures in CDFS AGN and Early Type galaxies (from K20 survey, Cimatti et al. 2002) are tracing the same structures. Weak hints for enhanced X-ray activity in large scale structures. X-ray to K-band number ratio is 0.33 ± 0.07 in the field 0.36±0.10 at z=0.73 0.7±10.22 z=0.67

33. Gilli et al. 2004 Γ = 1.33 ± 0.11 r 0 = 8.6 ± 1.2 h -1 Mpc CDFS r 0 = 4.2 ± 0.4 h -1 Mpc CDFN consistent with that of early type galaxies

34. Gilli et al. 2004

35. Prospects for the current X-ray surveys Extended CDFSCOSMOS XMM 2 deg 2, 25 pointings, 60 ksec each Hasinger et al. 2006 Other wide X-ray surveys: Bootes (9 deg 2 ); ELAIS (1 deg 2 ) Lehmer et al. 2005 0.3 deg 2, 4 pointings, 250 ksec each

36. COSMOS area galaxy formation simulation : gas  red – yellow stars  blue credit : Takeda 4D2U/NOAJ -- Saitoh & Koda

37. Expected clustering significance Credits to R. Gilli

38. CONCLUSIONS Hard XRB resolved at 90 % level at fluxes S ~ 2×10 -16 below 5 keV (but ~50% @5 keV: the energy density of the XRB peaks at 30 keV) A hard, faint population still to be discovered (possibly Compton thick sources detectable in submm with SCUBA/Spitzer) Part of this “missing population can be already in the faintest part of the X- ray sources population Towards an universal distribution of intrinsic absorption Evidence for strongly absorbed, C-thick sources @ z~1, and a substantial QSOII population at z>~2 >~80% of the AGNs agree with simple unification models. X-ray Emission from Normal Galaxies: SFR up to z~1; Star forming massive galaxies at z~2 seen in X-ray Mild effect of the Large Scale structures on nuclear activity, but larger efforts under way

40. X-ray spectral analysis Power law + intrinsic absorption + Gaussian line @ 6.4 /(1+z) keV + scattered component unabsorbed power law (same slope) Galactic absorption

41. Synthesis Models for the Cosmic XRB (Setti & Woltjer 1989, Madau, Ghisellini & Fabian 1994, Comastri et al. 1995, Gilli, Salvati & Hasinger 2001) were built on the following assumptions: The Cosmic X-ray Background is largely due to accretion onto supermassive black holes integrated over cosmic time. The X-ray observations are consistent with a mixture of absorbed and unabsorbed AGN, folded with the corresponding luminosity function and cosmological evolution. Most of the AGN spectra are heavily absorbed, and ~ 80% of the light produced by accretion is absorbed by gas and dust (in the nuclear starburst region that feeds the AGN).

42. Obscured fraction vs L Tozzi et al. 2005 Ueda et al. 2003

43. ROSAT and ASCA resolved most of the Soft XRB. The spectral index of AGNs detected with ROSAT/ ASCA is  = 1.7 -2.0 steeper than the Hard XRB (  = 1.4). ASCA and SAX resolved ~ 30% of the hard XRB. The remaining ~ 70% is due to a population of absorbed sources seen with Chandra and XMM The XRB is the echo of the formation of Massive Black Holes through the history of the Universe

44. Compton Thick sources Norman et al. 2002 QSOII 6 x 10 23 cm -2 if Compton thin Evidence that the NIR light of QSOII is dominated by the host galaxy 20% of EROS among X-ray selected AGN ~ 20-40% of the QSOII pop (Brusa et al. 2004)

45. Very Hard LogN -LogS (5 -10 keV) CDFS 940 ks XMM LH (Hasinger et al. 2001) Steep slope (~ Euclidean) Hardest sources missed by Chandra? The population of absorbed sources is still increasing at low fluxes How to detect these sources??? α = 1.35

46. R-K vs NH BLAGN HEX LEX GAL

47. Szokoly et al. 2004 A mixed optical-X-ray classification BLAGN HEX LEX ABS  43% of X-ray detected AGN are classified as LEX+ABS

48. CDFS Spectral ID Object class z 2 AGN -1 26-5 5-0 AGN -2 41-41 1-1 QSO -1 12-0 5-2 QSO -2 1-0 7-2 Galaxy 28-5 0 Clusters 5-1 0 Star 7 0 Total 138-57 Szokoly et al. 2004 Unsecure = 1 single line (OII, Ly)

49. Contribution from resolved sources below S= 10 -15 erg s -1 cm -2 in the 1 -2 keV band is 6.25 10 -13 erg cm -2 s -1 deg -2 (14% of the ROSAT value). A total of 83% of the ROSAT-XRB value is resolved. After adding a 6% from bright Clusters, we have a strict upper limit of 11% for the diffuse emission from warm gas (the hidden WHIM). Soft X -ray Background

50. X-ray galaxies detected in the infrared, high F hardX /F opt colors consistent with reddened elliptical at z ~ 1-2 possibly heavily obscured AGN and/or LMXB see also Crawford et al. 2001 Early Type Galaxies Active SF Galaxies? Leitherer et al. 1995 Kennicutt 1992 For 9 emission line galaxies in the Lynx field (180 ks with Chandra) (Stern et al. 2001) Buried AGN rather than OB and HMXB in “normal” galaxies at high fluxes (XBONG). SFR X = 2 -20 ×10 -40 L 2-10 M ⊙ yr -1 SFR X = 10 3 ×SFR OII First results from Deep Chandra Surveys: looking at galaxies at bright fluxes (2001)

51. Zheng et al. 2004 Photometric redshifts: check on spectroscopic redshifts Hyperz: NUV U V B V R I Z J H K

52. Comparing CDFS and K20 surveys ( Cimatti et al. 2002): clear large scale structures are detected as two narrow (dz<0.02) spikes at z = 0.67 (19 obj) z = 0.73 (19 obj) + z=1.04 (6 obj) z=1.22 (4 obj) z=1.62 (5 obj) z= 2.57 (4 obj) Gilli et al. 2003

53. Gilli 2003 Tracing the accretion power is not straightforward even in X-ray (see Brandt et al. 2004)

54. 25 ksec 118 ksec 303 ksec 174 ksec 333 ksec 392 ksec 515 ksec 645 ksec 740 ksec 808 ksec 939 ksec 0.5 -7 keV OCTOBER 1999 DECEMBER 2000 F soft = 5.5 × 10 -17 erg s -1 cm -2 F hard = 4.5 × 10 -16 erg s -1 cm -2 October 15, 1999

55. Szokoly et al. 2004 HEX BLAGN ? ?

56. Szokoly et al. 2004 LEX BLAGN ?

57. Zheng et al. 2004 Mainieri et al. 2004 BPZ F435w F606w F775w F850lp J H K (ISAAC)

59. Net detected counts in the 0.5-2 keV and 2-7 keV bands for the 366 sources in the CDFS

60. CDFS+CDFN XLF Norman et al. 2004 CDFS spectroscopic galaxy sample with the 60  m warm LF, and spectral energy distribution used for k-correction (hot gas from superwinds and X-ray binaries emission). Better agreement with IR sample (maybe hint of some AGN contamination).

61. IR Bright Galaxies at z~2 with massive SFR Daddi et al. 2004 Nine K-band luminous galaxies at 1.7 < z < 2.3, with SFR ~ 100-500 M ⊙ /yr (L X <10 42 erg/s, stacked X-ray img gives 100 M ⊙ /yr each, except one with L 2-10 ~3× 10 42 erg/s, SFR~ 500M ⊙ /yr. Stellar masses M > 10 11 M ⊙ for most of them. They contribute a SFR Density of 0.04 M ⊙ /yr/Mpc Therefore we are witnessing the massive spheroid formation epoch (the peak of just the low-z tail?) They already outnumber by more than 1 order of mag the predictions of hierarchical models of galaxy formation (despite the spectral incompleteness) VLT-ISAAC ACS-F435W ACS-F850LP

62. X-ray properties of Radio sources To Do: Photometry of Radio-only sources in the new ECDFS sources Separate pointlike sources from jets. Stacked spectra of X-ray non detections (1Ms and ECDFS).... Science: Search for Radio emission from heavily obscured AGN (among the X-ray detected, not the missed ones as in Donley et al.)- Radio compactness vs N H Decoupling SF Galaxies from AGN? Distribution of AGN vs SF activity as a function of Radio flux for X-ray detected sources. X-ray non detected: SF high-z galaxies or strongly absorbed AGN? Average X-ray spectral properties of non-detections.....

63. Distribution of optical type among the 27 sources with good optical spectroscopy (fluxes and luminosities)

64. Obscured fraction vs redshift Ueda et al. 2003 Tozzi et al. 2005