Black Holes, Big and Small Impact on Galaxy Formation Luis C. Ho ( - - PowerPoint PPT Presentation

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Black Holes, Big and Small Impact on Galaxy Formation Luis C. Ho ( - - PowerPoint PPT Presentation

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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,

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Black Holes, Big and Small Impact on Galaxy Formation

Luis C. Ho (何子山)

Kavli Institute for Astronomy and Astrophysics (KIAA) Peking University

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CMB

Optical = stars

X-ray Background = AGN !"! #

2 keV soft hard

Infrared= Stars (+AGN?)

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CMB

Optical = stars

X-ray Background = AGN !"! #

2 keV soft hard

Infrared= Stars (+AGN?)

Comastri, Gilli & Hasinger (2007)

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Vanden Berk et al. (2001)

SDSS quasars: composite spectrum

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Vestergaard (2004)

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Barth et al. (2003)

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!☯ M• = 3 x 109 M☉ ☯ Gas chemical enriched

with metals (C, Mg, Si, Fe)

☯ At z = 6.42, age of the

Universe only 800 Myr !

Barth et al. (2003)

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Richards et al. (2006)

quasar space density

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Richards et al. (2006)

quasar space density dormant massive BHs?

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27 Figure 9

Miyoshi et al. (1995) Herrnstein et al. (2005)

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Bower et al. (1998)

speed of gas clouds distance from the center ➛ ➛ ➙

approaching receding

M84

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Barth et al. (2001)

NGC 3245

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The “Nuker” Team

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Magorrian et al. (1998)

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black hole mass bulge velocity dispersion

Gebhardt et al. (2000); Ferrarese & Merritt (2000); Gültekin et al. (2009)

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Standard “Paradigm”

☯ All bulges contain BHs ☯ M• ~ Mbulge 〈M• / Mbulge〉 ~ 0.1%− 0.2% ☯ M• ∝ σ4 ☯ !M•−σ relation tighter than M• − Mbulge relation ☯ !No strong dependence on galaxy mass or type ☯ Mild to strong evolution with redshift ☯ AGN feedback engineers BH-host correlations

1.0

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Courtesy of S. Heinz

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Crotton et al. (2006)

AGN radio heating No radio heating

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Recent Developments

Ho (2008, ARA&A): Nuclear Activity in Nearby Galaxies Kormendy & Ho (2013, ARA&A): Coevolution of Supermassive Black Holes and Galaxies

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NGC 4889: M• = 2 x 1010 M⊙ (McConnell et al. 2011)

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Kuo et al. (2011)

7 New Megamasers!

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Kuo et al. (2011)

7 New Megamasers!

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black hole galaxy bulge velocity dispersion mass

Kormendy & Ho (2013, ARA&A)

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M• – σ Relation

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  • ✓

◆ ✓

  • ◆

M• 109 M = ✓ 0.309+0.037

0.033

◆ ✓ σ 200 km s1 ◆4.38±0.29 ◆ ; intrinsic scatter = 0.28.

M• – σ Relation

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M• – Mbulge Relation

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M• – Mbulge Relation

M• 109 M =

  • 0.49+0.06

−0.05

Mbulge 1011 M 1.16±0.08 ; intrinsic scatter = 0.29 dex.

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M• – Mbulge Relation

  • ld value

M• 109 M =

  • 0.49+0.06

−0.05

Mbulge 1011 M 1.16±0.08 ; intrinsic scatter = 0.29 dex.

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? ? ?

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M33: M• < 1500 M⊙

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M33: M• < 1500 M⊙

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G1: M• = 2 × 104 M⊙

Gebhardt, Ho & Rich (2005)

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Fan et al.

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  • J. Wise & T. Abel

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Are there mini-quasars in these ‟simpler” galaxies?

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Filippenko & Ho (2003); Barth, Ho et al. (2004)

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Fast-moving gas

Filippenko & Ho (2003); Barth, Ho et al. (2004)

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NGC 4395

Sdm

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NGC 4395

Sdm

M• = 104 −105 M☉

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NGC 4395

Sdm

M• = 104 −105 M☉

POX 52

Sph or dE

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NGC 4395

Sdm

M• = 104 −105 M☉

POX 52

Sph or dE

M• = 1.6 x 105 M☉

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Greene & Ho (2004, 2007); Dong, Ho et al. (2012)

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200-300 new sources

Greene & Ho (2004, 2007); Dong, Ho et al. (2012)

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HST/ACS

Greene, Ho & Barth (2008); Jiang et al. (2011a, 2011b)

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Ho (2014a, b)

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Recent Updates

☯ Central BHs detected from 104 – 1010 M⊙ ☯ All bulges contain BHs, but not all BHs live in bulges ☯ M• ~ Mbulge 〈M• / Mbulge〉 ~ 0.5% ☯ M• ∝ σ4.4 ☯ M•− σ and M• − Mbulge 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

1.2

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Kavli Institute for Astronomy and Astrophysics (KIAA)

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Featured Science 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 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 Journal (http://arxiv.org/abs/1212.4853), he and Zhaohuan Zhu (Princeton University) determined the distributions of planets down to Earth size and in orbits closer than Venus.

Wind Braking of AXP/SGRs

Anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are believed to be magnetars: peculiar neutron stars powered by their super strong magnetic

  • field. Unfortunately, none of the predictions of traditional magnetar models

successfully explain their properties. In a recent paper, the group of Prof. Renxin Xu (PKU Department of Astronomy, with joint appointment at the KIAA), in collaboration with Dr. Hao Tong of the Xinjiang Astronomical Observatory, show that a wind braking mechanism in magnetars, where the energy release generates a strong wind, provides a natural understanding of the multiwavelength observational behavior of AXPs and SGRs.

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