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High-redshift QSOs and Galaxies in the GOODS

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

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High-redshift QSOs and Galaxies in the GOODS

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

  2. THE GOODS TEAM • 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. Optically selected QSO candidates • Optical data from ACS • (Giavalisco et al. 2003) • Optical bands: B435 V606 i775 z850 • 398 orbits (lim 28, 27.5, 27, 27), res. 0.05” • QSOs candidates with M145 < -21

  5. Selection of QSO candidates • 22.45< z850 <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<0.35) & (B-V>3.00) • (i-z<0.50) & (V-i>0.80) & (B-V>2.00) • (i-z<1.00) & (V-i>1.90) • 3.5<z<5.2 • 645 CDF-S • 557 HDF-N • AGN & Galaxies

  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) • MB(-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. The QSO sample GOODS-S #6 Spectrum z=4.76 • 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 CIV NV 1h FORS2 z850=25.09

  8. Optical vs X ray fluxes Estimate of visibility (Vignali et al 2003) Type 1 QSOs with M145<-21 up to z ≥ 5.2 Any z>3.5 source must harbour an Lx~> 1043 AGN • GOODS -S #6 • S/N=3

  9. 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 ( z850 –KS ) • 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

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

  15. 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

  16. Downsizing of the AGN population

  17. 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!

  18. Lucia Ballo Black Hole Mass and Eddington Ratio of AGN contributing most of the XRB 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 S.Cristiani

  19. B V z i V B r(‘’) PA(°) b/a Nuc 25.97 24.02 26.11 25.92 - - - Disk 21.18 21.64 22.71 23.84 0.22 33.21 0.53 Bulge 19.85 20.27 21.60 24.06 0.65 32.91 0.53 i z CDFS source 170 (I) redshift = 0.664 iGOODS=20.00 = 1.80 NH = 1.39.1022 cm-2 HR = 0.13 C-thin L2 – 8 keV = 1.26.1042 erg s-1 L0.5 – 2 keV= 8.33.1041 erg s-1 (Tozzi et al. 2006)

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

  21. λ=Lbol/LEdd LEdd = 1.26.1038 MBH (MSUN) Lbol/LX=50 V. RESULTS In Fig. 5 we show the distributions of our estimates of MBH, Lbol &  Lbol/LX=50 V. RESULTS In Fig. 5 we show the distributions of our estimates of MBH, Lbol &  Lbol/LX=50 V. RESULTS In Fig. 5 we show the distributions of our estimates of MBH, Lbol &  Lbol/LX=50 V. RESULTS In Fig. 5 we show the distributions of our estimates of MBH, Lbol &  Lbol/LX=50 V. RESULTS In Fig. 5 we show the distributions of our estimates of MBH, Lbol &  Lbol/LX=50 V. RESULTS In Fig. 5 we show the distributions of our estimates of MBH, Lbol &  Lbol/LX=10 • red circle: reliable MBH & Lbol • yellow triangle: upper limit on MBH (nucleus-dominated) • green squares: upper limit on Lbol (host-dominated) Lbol/LX=10 • red circle: reliable MBH & Lbol • yellow triangle: upper limit on MBH (nucleus-dominated) • green squares: upper limit on Lbol (host-dominated) Lbol/LX=10 • red circle: reliable MBH & Lbol • yellow triangle: upper limit on MBH (nucleus-dominated) • green squares: upper limit on Lbol (host-dominated) Lbol/LX=10 • red circle: reliable MBH & Lbol • yellow triangle: upper limit on MBH (nucleus-dominated) • green squares: upper limit on Lbol (host-dominated) Lbol/LX=10 • red circle: reliable MBH & Lbol • yellow triangle: upper limit on MBH (nucleus-dominated) • green squares: upper limit on Lbol (host-dominated) Lbol/LX=10 • red circle: reliable MBH & Lbol • yellow triangle: upper limit on MBH (nucleus-dominated) • green squares: upper limit on Lbol (host-dominated) Lbol/LX lower than previous claims [11], but in agreement with [12]. Lbol/LX lower than previous claims [11], but in agreement with [12]. FIG. 5a Lbol/LX lower than previous claims [11], but in agreement with [12]. FIG. 5a Lbol/LX lower than previous claims [11], but in agreement with [12]. FIG. 5a Lbol/LX lower than previous claims [11], but in agreement with [12]. FIG. 5a Lbol/LX lower than previous claims [11], but in agreement with [12]. 2.  lower than at higher redshift; a similar trend is also FIG. 5a 2.  lower than at higher redshift; a similar trend is also FIG. 5a 2.  lower than at higher redshift; a similar trend is also 2.  lower than at higher redshift; a similar trend is also 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 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 • 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 • 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 • 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 • 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. 5b FIG. 5b FIG. 5b FIG. 5b Wide range of MBH & 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]. FIG. 5b Wide range of MBH & 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]. FIG. 5b Wide range of MBH & 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]. Wide range of MBH & 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]. Wide range of MBH & 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]. Wide range of MBH & 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]. FIG. 5c FIG. 5c FIG. 5c FIG. 5c FIG. 5c FIG. 5c RESULTS: Black hole masses and accretion rates Eddington ratio Ballo et al. 2006

  22. Consistent with GALRISE model!

  23. 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

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