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Evolution of Supermassive Black Holes out to z~5

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Evolution of Supermassive Black Holes out to z~5

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  1. Akiyama Alexander Altieri Arnaud Barcons Barger BauerBarkhouseBergeron Borgani Brandt Broos BrunnerCameronCapak Castander Coppi Cowie Dadina Dennerl Eckart HornschemeierJannuziJanson KewleyKim KimKoekemoer Fernandez Ferrando Finoguenov Garmire Gawiser Giacconi Gilli Gilmozzi GonzalezGreenGriffiths Grogin Gunn HarrisonHasingerHashimoto Helfand Herrera Lehmann Lumb Maccarone Mason Mainieri Mason Mateos Maza Mao McMahon Miyaji MontoyaMossmanMushotzky Nonino Norman Ohta PagePaerels Pineda Pozzetti Ptak Romaniello Rosati Sasseen Schartel Schmidt Schneider SchreierSilverman/MPE SmithSmithStanke Steffen Stern Szokoly WangWilkesTananbaumThompson 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. Flux distribution Optical mag distribution Compilation of AGN from extragalactic surveys Depth Surveys ASCA CLASXS Chandra Multiwavelength (ChaMP) 24 Chandra fields Lockman Hole/XMM CDF-S CDF-N 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%)

  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 Silverman, Green, Barkhouse & the ChaMP 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

  6. BlackHolemassfunction Andrea Merloni

  7. 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 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 * ChaMP 2 deg2 subsample (~ 30 Chandra fields)

  8. 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

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

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

  11. 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!

  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 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

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