Black Holes in Deep Surveys Meg Urry Yale University

The formation and evolution of galaxies is closely tied to the growth of black holes  Cosmic accretion (AGN) important for galaxy formation for black hole physics for understanding ionization, backgrounds, etc.

Cosmic Accretion Optically  selected quasars not representative, do not fairly sample cosmic accretion Need less biased surveys

Supermassive black holes obscured Supermassive black holes likely obscured by gas and dust: 1.Local AGN Unification 2.More likely in early Universe (“Grand Unification”) 3.Explains hard X-ray “background”

Supermassive black holes obscured Supermassive black holes likely obscured by gas and dust: 1.Local AGN Unification 2.More likely in early Universe (“Grand Unification”) 3.Explains hard X-ray “background”

Supermassive black holes obscured Supermassive black holes likely obscured by gas and dust: 1.Local AGN Unification 2.More likely in early Universe (“Grand Unification”) 3.Explains hard X-ray “background”

X-Ray “background” spectrum ( superposition of unresolved AGN ) is very hard Courtesy Brusa, Comastri, Gilli, Hasinger

unabsorbed AGN spectrum Increasing N H

Worsley et al Only  50% X-Ray Background resolved at E>6 keV

Deep Surveys for Obscured Accretion Hard X-rays penetrate most obscuration Energy re-radiated in infrared High resolution optical separates host galaxy

Chandra Spitzer HST

GOODSGreat Observatories Origins Deep Survey

GOODS designed to find obscured AGN out to the quasar epoch, z  2-3 Spitzer Legacy, HST Treasury, Chandra Deep Fields Dickinson, Giavalisco, Giacconi, Garmire

MUSYCMUltiwavelength Survey Survey by Yale Yale & Chile Gawiser, van Dokkum, CMU, Lira, Maza

Extended Chandra Deep Field South Do GOODS/MUSYC/ surveys reveal hidden populations of obscured AGN? Virani et al. 2006, Lehmer et al. 2006

HST ACS color image (0.3% of GOODS)

HST+Spitzer color image (0.3% of GOODS)

Understanding AGN Demographics Quantitatively Model X-ray spectrum  constrain N(L,z,N H ) w XRBG spectrum, N(S x ), N(z) Model full SED  constrain N(L,z,N H ) w XRBG spectrum, N(S x ), N(z), plus N(S opt ), N(S IR ), … Also, can assess selection effects in any filter or spectroscopy OR

CreateAGN Create ensemble of AGN, with continuous range of obscuration, correct SEDs for Unification (model), known luminosity distribution, known cosmic evolution Generate expected survey content Generate expected survey content at X-ray, Optical, Infrared, or any wavelengths, as function of flux and redshift Compare to data GOODS, MUSYC, Compare to data GOODS, MUSYC, SEXSI, SWIRE, CLASXS, H2XMM, AMSS, GROTH, Lockman, Champ, …

Assumptions Hard X-ray LF & LDDE evolution for Type 1 AGN Ueda et al Grid of AGN spectra (L X,N H ) with –SDSS quasar spectrum (normalized to X-ray) –dust/gas absorption (optical/UV/soft X-ray) –infrared dust emission Nenkova et al. 2002, Elitzur et al –L* host galaxy N H distribution corresponding to torus geometry (matches obs) –obscured AGN = 3 x unobscured (matches local obs) –No dependence on z (for now) –Simple linear dependence on luminosity (matches obs) Ezequiel Treister Ezequiel Treister, CMU, Jeffrey van Duyne, Brooke Simmons, Eleni Chatzichristou (Yale U.), David Alexander, Franz Bauer, Niel Brandt (Penn State U.), Anton Koekemoer, Leonidas Moustakas (STScI), Jacqueline Bergeron (IAP), Ranga-Ram Chary (SSC), Christopher Conselice (Caltech), Stefano Cristiani (Padova), Norman Grogin (JHU) 2004, ApJ, 616, 123 Also Treister et al. 2005, 2006a, 2006b, 2007

Dust emission models from Nenkova et al. 2002, Elitzur et al Simplest dust distribution that satisfies N H = – cm -2 3:1 ratio (divided at cm -2 ) Random angles  N H distribution

Treister et al. 2004

Results Match optical counts, N(z)Match optical counts, N(z)  50% AGN not in CDFs Match X-ray background Match IR counts –AGN are low % of IR EBL Integral & Swift surveys for Compton-thick AGN –Number of Compton-thick AGN may be lower than assumed –Gives limit on reflection, accretion efficiency Meta-analysis  obs/unobs ratio increases with z

Treister et al GOODS N+S

redshifts of Chandra deep X-ray sources GOODS-N Barger et al. 2002,3, Hasinger et al. 2002, Szokoly et al Treister et al. 2004

redshifts of Chandra deep X-ray sources GOODS-N Barger et al. 2002,3, Hasinger et al. 2002, Szokoly et al Treister et al. 2004

Results Match optical counts, N(z)  50% AGN not in CDFs Match X-ray backgroundMatch X-ray background Match IR counts –AGN are low % of IR EBL Integral & Swift surveys for Compton-thick AGN –Number of Compton-thick AGN may be lower than assumed –Gives limit on reflection, accretion efficiency Meta-analysis  obs/unobs ratio increases with z

Treister et al X-ray background synthesis

Treister et al X-ray background synthesis

Treister et al X-ray background synthesis

Results Match optical counts, N(z)  50% AGN not in CDFs Match X-ray background Match IR countsMatch IR counts –AGN are low % of IR EBL Integral & Swift surveys for Compton-thick AGN –Number of Compton-thick AGN may be lower than assumed –Gives limit on reflection, accretion efficiency Meta-analysis  obs/unobs ratio increases with z

Near & mid-IR Spitzer counts Treister et al. 2005

Total AGN contribution to EBL <10% Treister et al Infrared “Background”

Total 24  m luminosities Galaxies AGN

AGN dominate at bright 24  m fluxes

Results Match optical counts, N(z)  50% AGN not in CDFs Match X-ray background Match IR counts –AGN are low % of IR EBL Integral & Swift surveys for Compton-thick AGNIntegral & Swift surveys for Compton-thick AGN –Number of Compton-thick AGN may be lower than assumed –Gives limit on reflection, accretion efficiency Meta-analysis  obs/unobs ratio increases with z

X-Ray “Background” Spectrum Energy (keV) E F(E) [keV 2 cm  2 s  1 keV  1 str  1 ] Treister & Urry 2005

3 33 11 11 # of Compton Thick AGN Normalization of Reflection Component Integral & SWIRE Treister et al. (2007)

Normalization of Reflection Component Local Black Hole Mass Density (10 5 M o Mpc  3 ) Marconi et al. (2004) Shankar et al. (2004) Treister et al. (2007)

Hard X-ray Counts  3 10  4 10  5 10     9 Treister et al. (2007) F(20-40 keV) [erg cm  2 s  1 ] N(>S) [deg  2 ] Integral

Results Match optical counts, N(z)  50% AGN not in CDFs Match X-ray background Match IR counts –low AGN % of IR EBL Integral & Swift surveys for Compton-thick AGN –Number of Compton-thick AGN may be lower than assumed –Gives limit on reflection, accretion efficiency Meta-analysis  obs/unobs ratio increases with zMeta-analysis  obs/unobs ratio increases with z

7 surveys 2341 AGN 1229 with z BL=unobscured NL=obscured Area as function of X-ray flux & optical mag Treister & Urry 2006b

Black Hole Accretion Obscured AGN dominate at 0<z<2 –Obscuration decreases w luminosity –Obscuration increases w redshift –Explains X-ray “background” & surveys –True z-distr does peak at z>1 (incomplete spectra) Limits on Compton Thick AGN integral, swift, spitzer –High degree of Compton reflection to match observed low #s of CT AGN to avoid overproducing local BH density Total bolometric AGN light < 10% of extragalactic light (mostly stars) Compare to local BH mass  efficiency of accretion,  , where  = L/mc 2 

Carie Cardamone Shanil Virani Jeff van Duyne Brooke Simmons Ezequiel Treister (PhD 2005) Jonghak Woo (PhD 2005) Matt O’Dowd (PhD 2004) Yasunobu Uchiyama Eleni Chatzichristou Graduate students: Postdocs:

Luminosity-dependent density evolution Hasinger et al >10 46 ergs/s ergs/s ergs/s ergs/s ergs/s

Van Duyne et al Objects with hard X-ray spectra: Objects with hard (absorbed) X-ray spectra: (weak) AGN or galaxy in optical luminous thermal infrared emission AGN SEDs in GOODS

Van Duyne et al. 2007

Host galaxy morphologies Direct view of galaxy formation Simmons et al. 2007

Deep Integral Survey of the XMM-LSS region 300 ksec of our 2 Msec IntegralTreister et al. 2007

1 Msec Integral (300 ksec of our 2 Msec) 1 Compton-Thick AGN in  150 deg 2 Deep Integral Survey of the Greater XMM-LSS region

Hard X-ray Counts  3 10  4 10  5 10     9 Treister et al. (2007) F(20-40 keV) [erg cm  2 s  1 ] N(>S) [deg  2 ] Integral

Barger et al. 2005, Treister et al Simple unification Modified unification Dependence on luminosity ?

“EXO” Extreme X-ray-to-Optical AGN B V R BVR Z J K K AB = 21.4 R-K = 7.88 X-ray ECDFS ID: 29 Blue Green Red Composite optical Redder Near-IR Reddest Near-IR very high redshift AGN with z > 6, or very obscured AGN w old/dusty host galaxies at z~2

EXOs in MUSYC ECDFS

dec 0 RA 24 van Dokkum, Gawiser, Urry, Lira… MUSYC: MUSYC: 1 deg 2, UBVRIzJHK+NB, Spitzer, HST, Chandra, XMM, Galex, VLT, Magellan, Gemini, …

Chandra Deep Field South Castander’s Window ( ) SDSS z=6.3 QSO Field Hubble Deep Field South U,B,R=26 (5  )

HDF-South, UBI composite MUSYC

HDF-South, UBI composite MUSYC

HDF-South, UBI composite MUSYC

HDF-South, UBI composite MUSYC U-band; 13 hrs; limit ~26.5