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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