Black Hole Growth and Galaxy Evolution Meg Urry Yale University

~All galaxies host supermassive black holes

The formation and evolution of galaxies is closely tied to the growth of black holes ~All galaxies have SMBH Contemporaneous growth of SMBH & stars M-  relation

The formation and evolution of galaxies is closely tied to the growth of black holes ~All galaxies have SMBH Contemporaneous growth of SMBH & stars M-  relation

The formation and evolution of galaxies is closely tied to the growth of black holes ~All galaxies have SMBH Contemporaneous growth of SMBH & stars M-  relation

M-  Relation Black Hole Mass Stellar Velocity Dispersion

Effect of Black Hole on Galaxy

Demographics of supermassive black holes What we learned from multiwavelength surveys

Deep surveys show most accretion is obscured GOODS, COSMOS, MUSYC, ECDFS, AGES, Lockman Hole, HDF-N/S, NDWFS, XBootes, XMM/LSS, … Hard X-rays penetrate obscuration Energy re-radiated in infrared High resolution optical separates host galaxy, constrains redshifts

GOODS

Chandra Spitzer HST XMM

+60  +40  +20  0  2020 4040 6060 ECDFS GOODS-SUDF SDSS HDF-S “COSMOS” “MUSYC” GOODS-NHDF not to scale

HST ACS color image (0.3% of GOODS)

HST+Spitzer color image (0.3% of GOODS)

Treister, Urry & Virani 2009

Survey Results Treister et al. … Most BH accretion obscured – Log N-Log S infrared, optical, X-ray,  -ray – Fits AGN redshift distribution – Fits X-ray “background” Obscuration increases with redshift – N H, narrow lines, infrared selection

Compton-thick & Heavily Obscured AGN Ultra-Deep INTEGRAL Survey Swift BAT Survey Infrared excess

Ultra-Deep INTEGRAL Survey Treister, Urry & Virani 2009, Virani et al. 2009

3 Msec UDIS Treister, Urry & Virani 2009, Virani et al. 2009

NuSTAR EXIST Virani et al. 2009

Compton-thick & Heavily Obscured AGN Ultra-Deep INTEGRAL Survey Swift BAT Survey Infrared excess

Heavily obscured & higher redshift AGN Not detected in deep Chandra/XMM surveys (nearby AGN detected w INTEGRAL/Swift) Infrared-bright (high & low redshift) How to distinguish AGN from starbursts? (X-ray stacking)

R  K (Vega) 432101432101 Log F 24 /F R Fiore et al. 2008, Treister et al. 2009b Infrared-excess sources

Daddi et al. 2007, Fiore et al. 2008

24  m “normal”24  m “excess” X-Ray Stacked Spectra Daddi et al. 2007

Redshift  (Mpc  3 ) Treister et al. 2009b

How do quasars form? Sanders et al mergers  ULIRGs ULIRGs  quasars

Redshift Obscured/Unobscured Quasars Obscured to Unobscured Quasar Ratio Treister et al., submitted

Obscured to Unobscured Quasar Ratio Treister et al. submitted X-ray selected Redshift Obscured/Unobscured Quasars Local ULIRGs IR-selected Treister et al., submitted

The Interplay of Black Holes & Star Formation

First scenario Common trigger (e.g., merger)? Star formation starts (delay?) BH accretion delayed (angular momentum) AGN turns on, heats ISM/IGM Star formation turns off Stars age from blue to red

red blue bright faint Galaxy Colors red sequence blue cloud galaxies merging stars aging Schawinski et al. 2009

red blue bright faint Galaxy Colors Schawinski et al. 2009

red blue bright faint Schawinski et al Galaxy Colors

red blue bright faint Galaxy Colors Schawinski et al. 2009

red blue bright faint AGN avoid the blue cloud Schawinski et al Galaxy Colors

Schawinski et al red blue youngold 1 Gyr

The Future of Deep Surveys Wider areas Deep X-ray (NuSTAR) Far-infrared, submm (Herschel, ALMA)

Survey Goals Cosmic history of BH growth (Treister, Glikman, Virani) – Herschel, NuSTAR deep surveys (COSMOS) – WFC3 imaging (to separate host and nucleus) Form of AGN energy injection – Narrow-band imaging of winds (SINFONI, Paulina Lira) – Absorption spectroscopy in rest-frame UV Phasing of AGN turn-on and SF turn-off (Schawinski) – Galaxy colors – Spectral signatures (better) Role of mergers (Schawinski) – Major vs. minor mergers (Galaxy Zoo, Cardamone) – Connection to cosmological simulations (Kyoungsoo Lee)

Galaxy Morphology “Galaxy Zoo”

Host Galaxy Morphologies Disks Spheroids

u-r color Log Stellar Mass (M o )

AGN Duty Cycle Log Stellar Mass (M o ) u-r color

AGN Duty Cycle

Time (Gyr) nowBig Bang Number of obscured AGN

Time (Gyr) nowBig Bang Number of obscured AGN

Time (Gyr) nowBig Bang Number of AGN

Time (Gyr) nowBig Bang Number of AGN tt

Time (Gyr) nowBig Bang

Treister et al. 2009

Treister, Urry & Virani 2009