1. 1 High-redshift QSOs and Galaxies in the GOODS Pierluigi Monaco & Stefano Cristiani DAUT - University of Trieste INAF-Trieste Observatory

2. 2 THE GOODS TEAM L.Ballo S.Cristiani F.Fontanot J.MaoP.Monaco M.Nonino P.Tozzi E.Vanzella D.M.Alexander, L.Ballo, F.Bauer, W.N.Brandt, C.Cesarsky, E.T.Chatzichristou, S.Cristiani, M.Dickinson, H.Ferguson, F.Fontanot, R. Fosbury, M.Giavalisco, A.Grazian, J.Haase, A.Koekmoer, H.Kuntschner, R.A.Lucas, J.Mao, P.Monaco, L.Moustakas, M.Nonino, P.Padovani, P.Popesso, A.Renzini, A.Rettura, P.Rosati, D.Stern, P.Tozzi, E.Treister, C.M.Urry, E.Vanzella, J.Vernet

3. Topics FORS2 spectroscopy (Vanzella et al. 05 A&A 434, 53, astro-ph/0601367) Lyman-break galaxies at z~6 (Giavalisco’ talk, Vanzella et al.’s poster) U-band imaging of GOODS-S (Nonino et al.’s poster) LF of high-z QSOs ( Cristiani et al 04 ApJ 600, L119, Fontanot et al., in prep.) Accreting BHs at 0.4<z<1.0 (L. Ballo et al., submitted) Galaxy formation model (Monaco et al.’s poster)

4. 4 Optically selected QSO candidates Optical data from ACS (Giavalisco et al. 2003) Optical bands: B 435 V 606 i 775 z 850 398 orbits (lim 28, 27.5, 27, 27), res. 0.05” QSOs candidates with M 145 < -21

5. 5 Selection of QSO candidates 22.45< z 850 <25.25 Tailored colour criteria tested on QSO spectra (i-z<0.35) & (V-i<1.00) & (1.00<B-V<3.00) (i-z 3.00) (i-z 0.80) & (B-V>2.00) (i-z 1.90) 3.5<z<5.2 645 CDF-S 557 HDF-N AGN & Galaxies

6. 6 Match with Chandra sources 2 Ms CDF-N, 1 Ms CDF-S 0.5-8 KeV log S=-16 (S/N=3,0.5-2 KeV) M B (-23) QSO up to z~6 1000 sources (Alexander et al 03, Giacconi et al. 02) 3 sigma positional error box 10 candidates CDF-S 6 candidates HDF-N

7. 7 The QSO sample 16 Candidates High-z quasars 16 spectroscopic z 13 QSO 2.6<z<5.2 1 QSO @ z=5.186 1 QSO @ z=4.76 + 1 Type II QSO z=0.6 + 1 galaxy z=0.7 + 1 galaxy z=3.7? Ly alpha NV CIV 1h FORS2 z 850 =25.09 GOODS-S #6 Spectrum z=4.76

8. 8 Optical vs X ray fluxes Estimate of visibility (Vignali et al 2003) Type 1 QSOs with M 145 <-21 up to z ≥ 5.2 Any z>3.5 source must harbour an Lx~> 10 43 AGN  GOODS -S #6  S/N=3

9. 28/03/06 Morphological selection of X-ray z>4 faint AGNs  New selection Criteria  FWHM of images in the optical catalogue  Match with infrared catalogues (Capak et al. 2003; GOODS Team, in prep.; SPITZER Catalogue, in prep.)  New color criteria based on ( z 850 –K S )  Results: 2 x-ray selected candidates recovered  No new QSOs in the sample

10. Luminosity function at 3.5<z<5.2 Bright QSOs: SDSS Quasar Data Release 3 (Schneider et al. 2005) I magnitude redshift

11. Computing LFs (La Franca & Cristiani 1997) Assume an analytical form for LF (double power-law) Assume a PLE or PDE evolution Compute the true expected number of QSOs Assign SED and simulate magnitute and colors Apply selection criteria to create mock catalogues Compare # of observed and mock object Use chi square and 2D-KS estimators to quantify the level of agreement

12. Templates for QSO colors: SDSS spectra at 2.2<z<2.25 (215)

13. Controlling colors of high-z QSOs

15. Results: LFs BRIGHT END FAINT END Density evolution faint end is steep (Boyle 2000) bright end does not flatten! - disagreement with Fan et al. (2003)

16. 16 Luminosity Function of high-z QSOs Dearth of faint AGNs at high redshift Confirms the results of Cristiani et al. (2004) Consistent with PDE matched to the SDSS Consistent with COMBO-17 @ 4.2<z<4.8 See also Barger et al. 2003 @ 5<z<6.5 Insufficient to ionize the IGM Lensing statistics (Wyithe 2004) Evidence for strong feedback effects on small DMH at high redshift

17. 17 Downsizing of the AGN population

18. Consistent with CDM-based models (see GALRISE poster by Monaco et al.) Kinetic feedback in star-forming bulges at the origin of downsizing? dirty physics!

19. 28/03/06S.Cristiani19 Black Hole Mass and Eddington Ratio of AGN contributing most of the XRB Lucia Ballo S. Cristiani, L. Danese, F. Fontanot, M. Nonino, E. Vanzella, G. Fasano, E. Pignatelli, A. Fontana, E. Giallongo, A. Grazian, P. Monaco, P. Tozzi and the GOODS team

20. 20 redshift = 0.664i GOODS =20.00  = 1.80N H = 1.39. 10 22 cm -2 HR = 0.13C-thin L 2 – 8 keV = 1.26. 10 42 erg s -1 L 0.5 – 2 keV = 8.33. 10 41 erg s -1 (Tozzi et al. 2006) ziVB r(‘’)PA(°)b/a Nuc25.9724.0226.1125.92 --- Disk21.1821.6422.7123.84 0.2233.210.53 Bulge19.8520.2721.6024.06 0.6532.910.53 z i VB CDFS source 170 (I)

21. Elliptical Spiral QSO U35,38BVK i z J CDFS source 170 (II) bulge & BH mass +X accretion rate

22. 22 RESULTS: Black hole masses and accretion rates Ballo et al. 2006 λ =L bol /L Edd λ =L bol /L Edd L Edd = 1.26. 10 38 M BH (M SUN ) L Edd = 1.26. 10 38 M BH (M SUN ) Wide range of M BH & low  renewal of activity in previously formed objects. Consistent with the antihierachical behaviour already found in AGN evolution and expected on the basis of a bimodal scenario for the cosmic mass accretion history [15], [16]. V. RESULTS In Fig. 5 we show the distributions of our estimates of M BH, L bol &  red circle: reliable M BH & L bol  yellow triangle: upper limit on M BH (nucleus-dominated)  green squares: upper limit on L bol (host-dominated) 1.L bol /L X lower than previous claims [11], but in agreement with [12]. 2. lower than at higher redshift; a similar trend is also  suggested by observations, even if the mean values found by [13] are higher (optically selected quasars - black dots in Fig. 5b)  proposed by [14] to match accretion mass function & local SMBH mass function FIG. 5a L bol /L X =10 L bol /L X =50 FIG. 5b FIG. 5c Wide range of M BH & low  renewal of activity in previously formed objects. Consistent with the antihierachical behaviour already found in AGN evolution and expected on the basis of a bimodal scenario for the cosmic mass accretion history [15], [16]. V. RESULTS In Fig. 5 we show the distributions of our estimates of M BH, L bol &  red circle: reliable M BH & L bol  yellow triangle: upper limit on M BH (nucleus-dominated)  green squares: upper limit on L bol (host-dominated) 1.L bol /L X lower than previous claims [11], but in agreement with [12]. 2. lower than at higher redshift; a similar trend is also  suggested by observations, even if the mean values found by [13] are higher (optically selected quasars - black dots in Fig. 5b)  proposed by [14] to match accretion mass function & local SMBH mass function FIG. 5a L bol /L X =10 L bol /L X =50 FIG. 5b FIG. 5c Wide range of M BH & low  renewal of activity in previously formed objects. Consistent with the antihierachical behaviour already found in AGN evolution and expected on the basis of a bimodal scenario for the cosmic mass accretion history [15], [16]. V. RESULTS In Fig. 5 we show the distributions of our estimates of M BH, L bol &  red circle: reliable M BH & L bol  yellow triangle: upper limit on M BH (nucleus-dominated)  green squares: upper limit on L bol (host-dominated) 1.L bol /L X lower than previous claims [11], but in agreement with [12]. 2. lower than at higher redshift; a similar trend is also  suggested by observations, even if the mean values found by [13] are higher (optically selected quasars - black dots in Fig. 5b)  proposed by [14] to match accretion mass function & local SMBH mass function FIG. 5a L bol /L X =10 L bol /L X =50 FIG. 5b FIG. 5c Wide range of M BH & low  renewal of activity in previously formed objects. Consistent with the antihierachical behaviour already found in AGN evolution and expected on the basis of a bimodal scenario for the cosmic mass accretion history [15], [16]. V. RESULTS In Fig. 5 we show the distributions of our estimates of M BH, L bol &  red circle: reliable M BH & L bol  yellow triangle: upper limit on M BH (nucleus-dominated)  green squares: upper limit on L bol (host-dominated) 1.L bol /L X lower than previous claims [11], but in agreement with [12]. 2. lower than at higher redshift; a similar trend is also  suggested by observations, even if the mean values found by [13] are higher (optically selected quasars - black dots in Fig. 5b)  proposed by [14] to match accretion mass function & local SMBH mass function FIG. 5a L bol /L X =10 L bol /L X =50 FIG. 5b FIG. 5c Wide range of M BH & low  renewal of activity in previously formed objects. Consistent with the antihierachical behaviour already found in AGN evolution and expected on the basis of a bimodal scenario for the cosmic mass accretion history [15], [16]. V. RESULTS In Fig. 5 we show the distributions of our estimates of M BH, L bol &  red circle: reliable M BH & L bol  yellow triangle: upper limit on M BH (nucleus-dominated)  green squares: upper limit on L bol (host-dominated) 1.L bol /L X lower than previous claims [11], but in agreement with [12]. 2. lower than at higher redshift; a similar trend is also  suggested by observations, even if the mean values found by [13] are higher (optically selected quasars - black dots in Fig. 5b)  proposed by [14] to match accretion mass function & local SMBH mass function FIG. 5a L bol /L X =10 L bol /L X =50 FIG. 5b FIG. 5c Wide range of M BH & low  renewal of activity in previously formed objects. Consistent with the antihierachical behaviour already found in AGN evolution and expected on the basis of a bimodal scenario for the cosmic mass accretion history [15], [16]. V. RESULTS In Fig. 5 we show the distributions of our estimates of M BH, L bol &  red circle: reliable M BH & L bol  yellow triangle: upper limit on M BH (nucleus-dominated)  green squares: upper limit on L bol (host-dominated) 1.L bol /L X lower than previous claims [11], but in agreement with [12]. 2. lower than at higher redshift; a similar trend is also  suggested by observations, even if the mean values found by [13] are higher (optically selected quasars - black dots in Fig. 5b)  proposed by [14] to match accretion mass function & local SMBH mass function FIG. 5a L bol /L X =10 L bol /L X =50 FIG. 5b FIG. 5c Eddington ratio

23. Consistent with GALRISE model!

24. Conclusions  Dearth of distant low-luminosity AGNs  LF evolves in density from z~3.5 to z~5  No flattening of the LF of bright quasars  AGNs producing the XRB are powered by relatively large BHs accreting at ~0.01 Eddington