1 High-redshift QSOs and High-redshift QSOs and Galaxies Galaxies in the GOODS in the GOODS Pierluigi Monaco & Pierluigi Monaco & Stefano Cristiani Stefano Cristiani DAUT - University of Trieste DAUT - University of Trieste INAF-Trieste Observatory INAF-Trieste Observatory
High-redshift QSOs and Galaxies in the GOODS. Pierluigi Monaco & Stefano Cristiani DAUT - University of Trieste INAF-Trieste Observatory. THE GOODS TEAM - PowerPoint PPT Presentation
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High-redshift QSOs and Galaxies High-redshift QSOs and Galaxies in the GOODSin the GOODS
Pierluigi Monaco & Pierluigi Monaco &
Stefano CristianiStefano Cristiani
DAUT - University of TriesteDAUT - University of Trieste
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 LF of high-z QSOs ((Cristiani et al 04 ApJ 600, L119, Cristiani et al 04 ApJ 600, L119, Fontanot et al., in prep.)Fontanot et al., in prep.)
Accreting BHs at 0.4<z<1.0 Accreting BHs at 0.4<z<1.0 (L. Ballo et al., submitted)(L. Ballo et al., submitted)
FWHM of images in the optical catalogueFWHM 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
Luminosity function at 3.5<z<5.2
Bright QSOs:
SDSS Quasar
Data Release 3 (Schneider et al. 2005)
I m
agni
tude
redshift
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
Templates for QSO colors:SDSS spectra at 2.2<z<2.25 (215)
Controlling colors of high-z QSOs
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)
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Luminosity Function of high-z QSOs
Dearth of faint AGNs at high redshiftConfirms the results of Cristiani et al. (2004)Consistent with PDE matched to the SDSSConsistent with COMBO-17 @ 4.2<z<4.8See also Barger et al. 2003 @ 5<z<6.5Insufficient to ionize the IGM Lensing statistics (Wyithe 2004)
Evidence for strong feedback effects on small DMH at high redshift
17
Downsizing of the AGN population
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!dirty physics!
28/03/06 S.Cristiani 19
Black Hole Mass and Eddington Black Hole Mass and Eddington Ratio of AGN contributing most of Ratio of AGN contributing most of
the XRBthe XRB
Lucia BalloLucia Ballo
S. Cristiani, L. Danese, F. Fontanot, M. Nonino, E. Vanzella, S. Cristiani, L. Danese, F. Fontanot, M. Nonino, E. Vanzella, G. Fasano, E. Pignatelli, A. Fontana, E. Giallongo, A. Grazian, G. Fasano, E. Pignatelli, A. Fontana, E. Giallongo, A. Grazian,
P. Monaco, P. Tozzi and the GOODS teamP. Monaco, P. Tozzi and the GOODS team