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Black Holes, Big and Small Impact on Galaxy Formation Luis C. Ho ( ) Kavli Institute for Astronomy and Astrophysics (KIAA) Peking University Wednesday, February 26, 14 Wednesday, February 26, 14 Wednesday, February 26, 14 Wednesday,

  1. Black Holes, Big and Small Impact on Galaxy Formation Luis C. Ho ( 何子山 ) Kavli Institute for Astronomy and Astrophysics (KIAA) Peking University Wednesday, February 26, 14

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  15. CMB Optical = stars !" ! # Infrared= Stars X-ray Background = AGN (+AGN?) soft hard 2 keV Wednesday, February 26, 14

  16. Comastri, Gilli & Hasinger (2007) CMB Optical = stars !" ! # Infrared= Stars X-ray Background = AGN (+AGN?) soft hard 2 keV Wednesday, February 26, 14

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  19. Vanden Berk et al. (2001) SDSS quasars: composite spectrum Wednesday, February 26, 14

  20. Vestergaard (2004) Wednesday, February 26, 14

  21. Barth et al. (2003) Wednesday, February 26, 14

  22. Barth et al. (2003) !☯ M • = 3 x 10 9 M ☉ ☯ Gas chemical enriched with metals (C, Mg, Si, Fe) ☯ At z = 6.42, age of the Universe only 800 Myr ! Wednesday, February 26, 14

  23. Richards et al. (2006) quasar space density Wednesday, February 26, 14

  24. Richards et al. (2006) quasar space density dormant massive BHs? Wednesday, February 26, 14

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  27. 27 Miyoshi et al. (1995) Herrnstein et al. (2005) Figure 9 Wednesday, February 26, 14

  28. ➛ M84 distance from the center ➙ Bower et al. (1998) ➛ speed of gas clouds approaching receding Wednesday, February 26, 14

  29. NGC 3245 Barth et al. (2001) Wednesday, February 26, 14

  30. The “Nuker” Team Wednesday, February 26, 14

  31. Magorrian et al. (1998) Wednesday, February 26, 14

  32. Gebhardt et al. (2000); Ferrarese & Merritt (2000); Gültekin et al. (2009) black hole mass bulge velocity dispersion Wednesday, February 26, 14

  33. Standard “Paradigm” ☯ All bulges contain BHs 1.0 ☯ M • ~ M bulge 〈 M • / M bulge 〉 ~ 0.1% − 0.2% ☯ M • ∝ σ 4 ☯ ! M • −σ relation tighter than M • − M bulge relation ☯ ! No strong dependence on galaxy mass or type ☯ Mild to strong evolution with redshift ☯ AGN feedback engineers BH-host correlations Wednesday, February 26, 14

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  36. Courtesy of S. Heinz Wednesday, February 26, 14

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  41. Crotton et al. (2006) No radio heating AGN radio heating Wednesday, February 26, 14

  42. Recent Developments Ho (2008, ARA&A) : Nuclear Activity in Nearby Galaxies Kormendy & Ho (2013, ARA&A) : Coevolution of Supermassive Black Holes and Galaxies Wednesday, February 26, 14

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  46. NGC 4889: M • = 2 x 10 10 M ⊙ (McConnell et al. 2011) Wednesday, February 26, 14

  47. 7 New Megamasers! Kuo et al. (2011) Wednesday, February 26, 14

  48. 7 New Megamasers! Kuo et al. (2011) Wednesday, February 26, 14

  49. Kormendy & Ho (2013, ARA&A) black hole mass velocity dispersion galaxy bulge Wednesday, February 26, 14

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  51. M • – σ Relation Wednesday, February 26, 14

  52. M • – σ Relation ✓ ◆ ✓ ◆ � � ◆ 4 . 38 ± 0 . 29 ✓ ◆ ✓ M • ◆ σ 0 . 309 +0 . 037 = ; intrinsic scatter = 0 . 28 . 10 9 M � � 0 . 033 200 km s � 1 Wednesday, February 26, 14

  53. M • – M bulge Relation Wednesday, February 26, 14

  54. M • – M bulge Relation � � M bulge � 1 . 16 ± 0 . 08 � M • 0 . 49 +0 . 06 = ; intrinsic scatter = 0 . 29 dex . 10 9 M � 10 11 M � − 0 . 05 Wednesday, February 26, 14

  55. M • – M bulge Relation � � M bulge � 1 . 16 ± 0 . 08 � M • 0 . 49 +0 . 06 = ; intrinsic scatter = 0 . 29 dex . 10 9 M � 10 11 M � − 0 . 05 old value Wednesday, February 26, 14

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  61. M33: M • < 1500 M ⊙ Wednesday, February 26, 14

  62. M33: M • < 1500 M ⊙ Wednesday, February 26, 14

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  67. G1: M • = 2 × 10 4 M ⊙ Gebhardt, Ho & Rich (2005) Wednesday, February 26, 14

  68. Fan et al. Wednesday, February 26, 14

  69. J. Wise & T. Abel Wednesday, February 26, 14

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  74. Are there mini-quasars in these ‟ simpler” galaxies? Wednesday, February 26, 14

  75. Filippenko & Ho (2003); Barth, Ho et al. (2004) Wednesday, February 26, 14

  76. Filippenko & Ho (2003); Barth, Ho et al. (2004) Fast-moving gas Wednesday, February 26, 14

  77. NGC 4395 Sdm Wednesday, February 26, 14

  78. NGC 4395 Sdm M • = 10 4 − 10 5 M ☉ Wednesday, February 26, 14

  79. POX 52 NGC 4395 Sph or dE Sdm M • = 10 4 − 10 5 M ☉ Wednesday, February 26, 14

  80. POX 52 NGC 4395 Sph or dE Sdm M • = 10 4 − 10 5 M ☉ M • = 1.6 x 10 5 M ☉ Wednesday, February 26, 14

  81. Wednesday, February 26, 14

  82. Greene & Ho (2004, 2007); Dong, Ho et al. (2012) Wednesday, February 26, 14

  83. Greene & Ho (2004, 2007); Dong, Ho et al. (2012) 200-300 new sources Wednesday, February 26, 14

  84. HST /ACS Greene, Ho & Barth (2008); Jiang et al. (2011a, 2011b) Wednesday, February 26, 14

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  89. Ho (2014a, b) Wednesday, February 26, 14

  90. Recent Updates ☯ Central BHs detected from 10 4 – 10 10 M ⊙ ☯ All bulges contain BHs, but not all BHs live in bulges 1.2 ☯ M • ~ M bulge 〈 M • / M bulge 〉 ~ 0.5% ☯ M • ∝ σ 4.4 ☯ M • − σ and M • − M bulge relations have similar scatter ☯ Scaling relations only tight for classical bulges and Es ☯ Scaling relations already in place for high- z QSOs ☯ Mild evolution only for most massive BHs ☯ AGN feedback effective only for classical bulges and Es Wednesday, February 26, 14

  91. Kavli Institute for Astronomy and Astrophysics (KIAA) Wednesday, February 26, 14

  92. Wednesday, February 26, 14

  93. ���� English HOME ABOUT KIAA PEOPLE ACTIVITIES NEWS SCIENCE OPPORTUNITIES OUTREACH VISITOR INFO ADMIN Search @ KIAA-PKU Featured Science Search New Patterns in Planet Distributions Subo Dong ( �� 勃 ) joined the faculty of KIAA in Fall 2013 through the 1000 Talents Program for young researchers ( 青年千人 � 划 ). One of his research interests is to Upcoming Events robustly derive the distributions of extrasolar planets in order to find clues on how planet systems form and evolve. In a paper recently published in the Astrophysical How much cosmological Journal (http://arxiv.org/abs/1212.4853), he and Zhaohuan Zhu (Princeton information can be University) determined the distributions of planets down to Earth size and in orbits measured? closer than Venus. Speaker: Yinzhe Ma, University of British Columbia Wind Braking of AXP/SGRs Time: Mon, 2014-01-06 12:00 to 13:00 Anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are believed Location: DoA, Rm 2907 to be magnetars: peculiar neutron stars powered by their super strong magnetic field. Unfortunately, none of the predictions of traditional magnetar models Finding Transiting successfully explain their properties. In a recent paper, the group of Prof. Renxin Xu Exoplanets and (PKU Department of Astronomy, with joint appointment at the KIAA), in Characterizing their collaboration with Dr. Hao Tong of the Xinjiang Astronomical Observatory, show Atmospheres: HATSouth that a wind braking mechanism in magnetars, where the energy release generates a and ACCESS strong wind, provides a natural understanding of the multiwavelength observational Speaker: Andrés Jordán (PUC) behavior of AXPs and SGRs. Time: Thu, 2014-01-09 16:00 to 17:00 kiaa.pku.edu.cn Wednesday, February 26, 14

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