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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
INAF-Trieste ObservatoryINAF-Trieste Observatory
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THE GOODS TEAMTHE GOODS TEAM
D.M.Alexander, L.BalloL.Ballo, F.Bauer, W.N.Brandt, C.Cesarsky, E.T.Chatzichristou, S.CristianiS.Cristiani, M.Dickinson, H.Ferguson, F.FontanotF.Fontanot, R. Fosbury, M.Giavalisco, A.Grazian, J.Haase, A.Koekmoer, H.Kuntschner, R.A.Lucas, J.MaoJ.Mao, P.MonacoP.Monaco, L.Moustakas, M.NoninoM.Nonino, P.Padovani, P.Popesso, A.Renzini, A.Rettura, P.Rosati, D.Stern, P.TozziP.Tozzi, E.Treister, C.M.Urry, E.VanzellaE.Vanzella, J.Vernet
TopicsTopics
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)
Galaxy formation model (Monaco et al.’s poster)
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Optically selected QSO candidatesOptically selected QSO candidates
Optical data from ACS (Giavalisco et al. 2003)
Optical bands: B435 V606 i
775z
850
398 orbits (lim 28, 27.5, 27, 27), res. 0.05”
QSOs candidates with M145 < -21
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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
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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
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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
NVCIV
1h FORS2 z850=25.09
GOODS-S #6 Spectrum z=4.76
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Optical vs X ray fluxesOptical 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
28/03/06
Morphological selection of X-ray z>4 faint AGNs
New selection Criteria
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
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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
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redshift = 0.664redshift = 0.664 iiGOODSGOODS=20.00=20.00
= 1.80= 1.80 NNHH = 1.39 = 1.39..10102222 cm cm-2-2
HR = 0.13HR = 0.13 C-thinC-thin
LL2 – 8 keV2 – 8 keV = 1.26 = 1.26..10104242 erg s erg s-1-1
LL0.5 – 2 keV0.5 – 2 keV= 8.33= 8.33..101041 41 erg serg s-1-1
(Tozzi et al. 2006) (Tozzi et al. 2006)
zz ii VV BB
r(‘’)r(‘’) PA(°)PA(°) b/ab/a
NucNuc 25.9725.97 24.0224.02 26.1126.11 25.9225.92-- -- --
DiskDisk 21.1821.18 21.6421.64 22.7122.71 23.8423.84 0.22 0.22 33.2133.21 0.530.53
BulgeBulge 19.8519.85 20.2720.27 21.6021.60 24.0624.06 0.65 0.65 32.9132.91 0.530.53
zzii
VVBB
CDFS source CDFS source 170170(I)(I)
Elliptical Spiral QSO
U35,38U35,38 BB VV KKii zz JJ
CDFS source CDFS source 170170(II)(II)
bulge & BH mass
+X accretion rate
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RESULTS: Black hole masses and accretion ratesRESULTS: Black hole masses and accretion rates
Ballo et al. 2006Ballo et al. 2006 λλ=L=Lbolbol/L/LEddEdd
LLEddEdd = 1.26 = 1.26..10103838 M MBHBH (M (MSUNSUN))
Ed
din
gton
rat
io
Consistent with GALRISE model!
Conclusions
Dearth of distant low-luminosity AGNsDearth of distant low-luminosity AGNs
LF evolves in density from z~3.5 to z~5LF evolves in density from z~3.5 to z~5
No flattening of the LF of bright quasarsNo flattening of the LF of bright quasars
AGNs producing the XRB are powered byAGNs producing the XRB are powered by
relatively large BHs accreting at ~0.01 Eddingtonrelatively large BHs accreting at ~0.01 Eddington