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Black Hole Growth and Galaxy Evolution

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.

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Black Hole Growth and Galaxy Evolution

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  1. Black Hole Growthand 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 mostaccretion is obscured • GOODS, COSMOS, MUSYC, ECDFS, AGES, Lockman Hole, HDF-N/S, NDWFS, XBootes, XMM/LSS, … • HardX-rayspenetrate obscuration • Energy re-radiated ininfrared • High resolutionopticalseparates host galaxy, constrains redshifts

  10. GOODS

  11. Chandra HST XMM Spitzer

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

  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 • NH, 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

  20. EXIST NuSTAR Virani et al. 2009

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

  22. 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)

  23. Infrared-excess sources 4 3 2 1 0 1 Log F24/FR 2 4 6 8 R  K (Vega) Fiore et al. 2008, Treister et al. 2009b

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

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

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

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

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

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

  30. The Interplay of Black Holes & Star Formation

  31. 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

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

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

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

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

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

  37. red 1 Gyr blue young old Schawinski et al. 2009

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

  39. 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)

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

  41. Host Galaxy Morphologies Disks Spheroids

  42. 3.0 2.5 2.0 1.5 1.0 u-r color 9.0 10.0 11.0 12.0 Log Stellar Mass (Mo)

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

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