Akiyama Alexander Altieri Arnaud Barcons Barger Bauer Barkhouse

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 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 Evolution of Supermassive Black Holes out to z~5 Mc. Mahon Miyaji Montoya Mossman Mushotzky Nonino Norman Ohta Page Paerels Pineda Pozzetti Ptak Romaniello Rosati Sasseen Schartel Schmidt Schneider Schreier Silverman/MPE 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

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 ke. V) X-ray sources • Low-moderate luminosity (i. e Seyfert-type) AGN out to z~2 • Obscured AGN

Compilation of AGN from extragalactic surveys Fluxmag distribution Optical distribution Depth Surveys ASCA CLASXS Chandra Multiwavelength (Cha. MP) 24 Chandra fields Lockman Hole/XMM CDF-S Area CDF-N • Measure intrinsic 2 -8 ke. V luminosity (no NH correction) • Observed soft band (0. 5 -2. 0 ke. V) for z > 3 selection • 799 AGN with 34 at z > 3 (Cha. MP: ~50%)

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 ke. V) X-ray luminosity function Silverman, Green, Barkhouse & the Cha. MP 2007 Submit Dec 1, 2006 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

Black Hole mass function Andrea Merloni

Improving the HXLF: Higher statistics at z > 3 • New LDDE model + flux vs. area curves • Number of AGN roughly below and above the break luminosity Survey 3<z<4 Log Lx < 44 4<z<6 > 44 < 44 > 44 Total Cha. MP* 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 c. COSMOS 18 21 4 11 54 Total 54 70 14 33 171 * Cha. MP 2 deg 2 subsample (~ 30 Chandra fields)

Improving the HXLF: Faint end slope at the QSO epoch Limited samples of Seyfert-type AGN at z ~ 2 Does ‘cosmic downsizing’ extend to higher redshifts? 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

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) 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) Spectroscopic redshifts BLAGN NELG ALG No class Photo-z (COMBO-17, Zheng et al. 200? )

Improving the HXLF: Faint end slope at the QSO epoch (z~2) 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) 5 hr exposures with LRblue grism ‘Optically dull’ AGN at high z!

Conclusions New hard X-ray luminosity function out to z ~ 5 Cha. MP effectively finding the most luminous (log Lx > 44. 5) at z > 3 CDF N+S probe the faint end slope Well defined peak in the number density of AGNs with strong luminosity dependence Rapid buildup of the most massive (M > 108 Msolar) SMBHs at z > 1 Emergence of low mass (M < 108 Msolar) SMBHs at z < 1 Future improvements (e. g. faint end slope, high z) from the E-CDF-S, Extended Groth Strip and c. COSMOS surveys