1. Black Hole Growth and Galaxy Evolution Meg Urry Yale University

2. ~All galaxies host supermassive black holes

3. 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

4. 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

5. 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

6. M-  Relation Black Hole Mass Stellar Velocity Dispersion

7. Effect of Black Hole on Galaxy

8. Demographics of supermassive black holes What we learned from multiwavelength surveys

9. 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

10. GOODS

11. Chandra Spitzer HST XMM

12. +60  +40  +20  0  2020 4040 6060 ECDFS GOODS-SUDF SDSS1030 1256 HDF-S “COSMOS” “MUSYC” GOODS-NHDF not to scale

13. HST ACS color image (0.3% of GOODS)

14. HST+Spitzer color image (0.3% of GOODS)

15. Treister, Urry & Virani 2009

16. 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

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

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

19. 3 Msec UDIS Treister, Urry & Virani 2009, Virani et al. 2009

21. NuSTAR EXIST Virani et al. 2009

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

23. 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)

24. 2 4 6 8 R  K (Vega) 432101432101 Log F 24 /F R Fiore et al. 2008, Treister et al. 2009b Infrared-excess sources

25. Daddi et al. 2007, Fiore et al. 2008

26. 24  m “normal”24  m “excess” X-Ray Stacked Spectra Daddi et al. 2007

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

28. How do quasars form? Sanders et al. 1988 mergers  ULIRGs ULIRGs  quasars

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

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

34. The Interplay of Black Holes & Star Formation

35. 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

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

37. red blue bright faint Galaxy Colors Schawinski et al. 2009

39. red blue bright faint Schawinski et al. 2009 Galaxy Colors

40. red blue bright faint Galaxy Colors Schawinski et al. 2009

41. red blue bright faint AGN avoid the blue cloud Schawinski et al. 2009 Galaxy Colors

42. Schawinski et al. 2009 red blue youngold 1 Gyr

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

44. 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)

46. Galaxy Morphology “Galaxy Zoo” www.galaxyzoo.org

47. Host Galaxy Morphologies Disks Spheroids

48. u-r color Log Stellar Mass (M o ) 9.0 10.0 11.0 12.0 3.0 2.5 2.0 1.5 1.0

49. AGN Duty Cycle Log Stellar Mass (M o ) 9.0 10.0 11.0 12.0 u-r color 3.0 2.5 2.0 1.5 1.0

51. AGN Duty Cycle

52. 0 5 10 15 Time (Gyr) nowBig Bang Number of obscured AGN

53. 0 5 10 15 Time (Gyr) nowBig Bang Number of obscured AGN

54. 0 5 10 15 Time (Gyr) nowBig Bang Number of AGN

55. 0 5 10 15 Time (Gyr) nowBig Bang Number of AGN tt

56. 0 5 10 15 Time (Gyr) nowBig Bang

57. Treister et al. 2009

59. Treister, Urry & Virani 2009