1. 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

2. 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

3. 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 N H 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

4. 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

5. 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

6. Black Hole mass functionBlack Hole mass function Andrea Merloni

7. Improving the HXLF: Higher statistics at z > 3 Survey 3 < z < 4 4 < z < 6 Total Log Lx 44 44 ChaMP* 2 23 0 7 32 CDF-N 6 3 2 2 13 E-CDF-S13 8 4 5 30 EGS15 15 4 8 42 cCOSMOS18 21 411 54 Total54 701433 171 New LDDE model + flux vs. area curves Number of AGN roughly below and above the break luminosity * ChaMP 2 deg 2 subsample (~ 30 Chandra fields)

8. 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?

9. Extended Chandra Deep Field - South P.I. N. Brandt; Lehmer et al. 2005

10. 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)

11. 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)

12. Conclusions New 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 > 10 8 M solar ) SMBHs at z > 1 Emergence of low mass (M < 10 8 M solar ) SMBHs at z < 1 Well defined peak in the number density of AGNs with strong luminosity dependence