Akiyama Alexander Altieri Arnaud Barcons Barger Bauer Barkhouse Bergeron Borgani Brandt Broos Brunner Cameron Capak Castander Coppi Cowie Dadina Dennerl Eckart Hornschemeier Jannuzi Janson Kewley Kim Kim Koekemoer Fernandez Ferrando Finoguenov Garmire Gawiser Giacconi Gilli Gilmozzi Gonzalez Green Griffiths Grogin Gunn Harrison Hasinger Hashimoto Helfand Herrera Lehmann Lumb Maccarone Mason Mainieri Mason Mateos Maza Mao

McMahon Miyaji Montoya Mossman Mushotzky Nonino Norman Ohta Page Paerels Pineda Pozzetti Ptak Romaniello Rosati Sasseen Schartel Schmidt Schneider Schreier Silverman/MPE Smith Smith Stanke Steffen Stern Szokoly Wang Wilkes Tananbaum Thompson Townsley Tozzi Treister Turner Trumper Ueda Urry Vignali Warwick Watson Wilson Yang Yost Zamorani Zheng Zirm

Evolution of Supermassive Black Holes out to z~5

Trace the growth of Supermassive Black Holes to early cosmic times

(Mass and accretion rate distributions)

AGN luminosity function

Surveys of broad band (0.5-8 keV) X-ray sources

• Low-moderate luminosity (i.e Seyfert-type) AGN out to z~2

• Obscured AGN

ASCA

CLASXS

Chandra Multiwavelength (ChaMP)24 Chandra fields

Lockman Hole/XMM

CDF-S

CDF-N

Compilation of AGN from extragalactic surveys

Depth Surveys

Area

• Measure intrinsic 2-8 keV luminosity (no NH correction)

• Observed soft band (0.5-2.0 keV) for z > 3 selection

• 799 AGN with 34 at z > 3 (ChaMP: ~50%)

Flux distribution

Optical mag distribution

Comoving space density

La Franca et al. 2005, Barger et al. 2005, Hasinger et al. 2005; Silverman et al. 2005; Fiore et al. 2003 ,Ueda et al. 2003

Hard (2-8 keV) X-ray luminosity function

Binned estimate: 1/Va

Model fit: PLE-z dependent faint end slope (Hopkins et al. 2006)

Model fit: Luminosity-dependent density evolution (LDDE) z = 0

Silverman, Green, Barkhouse & the

ChaMP 2007

Submit Dec 1, 2006

Black Hole mass function

Andrea Merloni

Improving the HXLF: Higher statistics at z > 3

Survey 3 < z < 4 4 < z < 6 Total

Log Lx < 44 > 44 < 44 > 44

ChaMP* 2 23 0 7 32

CDF-N 6 3 2 2 13

E-CDF-S 13 8 4 5 30

EGS 15 15 4 8 42

cCOSMOS 18 21 4 11 54

Total 54 70 14 33 171

• New LDDE model + flux vs. area curves

• Number of AGN roughly below and above the break luminosity

* ChaMP 2 deg2 subsample (~ 30 Chandra fields)

Improving the HXLF: Faint end slope at the QSO epoch

Limited samples of Seyfert-type AGN at z ~ 2

Binned estimate: 1/Va

Model fit: PLE-z dependent faint end slope (Hopkins et al. 2006)

Model fit: Luminosity-dependent density evolution (LDDE) z = 0

Does ‘cosmic downsizing’ extend to higher redshifts?

Extended Chandra Deep Field - South

P.I. N. Brandt; Lehmer et al. 2005

Improving the HXLF: Faint end slope at the QSO epoch (z~2)

BLAGN

NELG

ALG

No class

Spectroscopic redshifts

Photo-z

(COMBO-17, Zheng et al.

200?)

Optical spectroscopic followup of E-CDF-S sources with VLT/VIMOS(Silverman, Mainieri, Bergeron, Hasinger & the full E-CDF-S team)

-75 new spectroscopic redshifts

~50% of the 762 X-ray sources have a redshift (photometric+spectroscopic)

Improving the HXLF: Faint end slope at the QSO epoch (z~2)

5 hr exposures with LRblue grism

‘Optically dull’ AGN at high z!

Optical spectroscopic followup of E-CDF-S sources with VLT/VIMOS(Silverman, Mainieri, Bergeron, Hasinger & the full E-CDF-S team)

-75 new spectroscopic redshifts

~50% of the 762 X-ray sources have a redshift (photometric+spectroscopic)

ConclusionsNew hard X-ray luminosity function out to z ~ 5 ChaMP effectively finding the most luminous (log Lx > 44.5) at z > 3

CDF N+S probe the faint end slope

Future improvements (e.g. faint end slope, high z) from the E-CDF-S, Extended Groth Strip and cCOSMOS surveys

Rapid buildup of the most massive (M > 108 Msolar) SMBHs at z > 1

Emergence of low mass (M < 108 Msolar) SMBHs at z < 1

Well defined peak in the number density of AGNs with strong luminosity dependence