The Black Hole Mass Distribution in Early-Type Galaxies: Cusps in [ITAL]Hubble Space Telescope[/ITAL] Photometry Interpreted through Adiabatic Black Hole Growth

1999 ◽  
Vol 117 (2) ◽  
pp. 744-763 ◽  
Author(s):  
Roeland P. van der Marel
Keyword(s):  
Black Hole ◽  
Mass Distribution ◽  
Hubble Space Telescope ◽  
Early Type ◽  
Black Hole Mass ◽  
Space Telescope ◽  
Black Hole Growth ◽  
Hole Growth

scholarly journals Black Hole Growth and Host Galaxy Morphology

2009 ◽  
Vol 5 (S267) ◽  
pp. 438-441
Author(s):  
Kevin Schawinski ◽  
C. Megan Urry ◽  
Shanil Virani ◽  
Paolo Coppi ◽  
Steven P. Bamford ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Host Galaxy ◽  
Early Type ◽  
Black Hole Mass ◽  
Local Universe ◽  
Opposite Trend ◽  
The Galaxy ◽  
Black Hole Growth ◽  
Hole Growth

AbstractWe use data from large surveys of the local universe (SDSS+Galaxy Zoo) to show that the galaxy–black hole connection is linked to host morphology at a fundamental level. The fraction of early-type galaxies with actively growing black holes, and therefore the AGN duty cycle, declines significantly with increasing black hole mass. Late-type galaxies exhibit the opposite trend: the fraction of actively growing black holes increases with black hole mass.

scholarly journals The Distribution and Evolution of Black Hole Mass in Broad Line Quasars

2009 ◽  
Vol 5 (S267) ◽  
pp. 263-263
Author(s):  
Brandon C. Kelly ◽  
Marianne Vestergaard ◽  
Xiaohui Fan ◽  
Lars Hernquist ◽  
Philip Hopkins ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Mass Function ◽  
Sloan Digital Sky Survey ◽  
Broad Line ◽  
Black Hole Mass ◽  
Sky Survey ◽  
Black Hole Growth ◽  
Hole Growth ◽  
Eddington Limit

We present the first estimate of the black hole mass function (BHMF) of broad-line quasars (BLQSOs) that self-consistently corrects for incompleteness and the statistical uncertainty in the mass estimates, based on a sample of 9886 quasars at 1 < z < 4.5 drawn from the Sloan Digital Sky Survey. We find evidence for “cosmic downsizing” of black holes in BLQSOs, where the peak in their number density shifts to higher redshift with increasing black hole mass. We estimate the lifetime of the BLQSO phase to be 70 ± 5 Myr for supermassive black holes (SMBHs) at z = 1 with a mass of MBH = 109M⊙, and we constrain the maximum mass of a black hole in a BLQSO to be ~ 1010M⊙. We find that most BLQSOs are not radiating at or near the Eddington limit. Our results are consistent with models for self-regulated black hole growth, where the BLQSO phase occurs at the end of a fueling event when black hole feedback unbinds the accreting gas.

scholarly journals CONSTRAINTS ON BLACK HOLE GROWTH, QUASAR LIFETIMES, AND EDDINGTON RATIO DISTRIBUTIONS FROM THE SDSS BROAD-LINE QUASAR BLACK HOLE MASS FUNCTION

2010 ◽  
Vol 719 (2) ◽  
pp. 1315-1334 ◽  
Author(s):  
Brandon C. Kelly ◽  
Marianne Vestergaard ◽  
Xiaohui Fan ◽  
Philip Hopkins ◽  
Lars Hernquist ◽  
...  
Keyword(s):  
Black Hole ◽  
Mass Function ◽  
Broad Line ◽  
Black Hole Mass ◽  
Black Hole Growth ◽  
Hole Growth

scholarly journals Quasar Sightline and Galaxy Evolution (QSAGE) survey – II. Galaxy overdensities around UV luminous quasars at z = 1–2

2020 ◽  
Vol 497 (3) ◽  
pp. 3083-3096
Author(s):  
J P Stott ◽  
R M Bielby ◽  
F Cullen ◽  
J N Burchett ◽  
N Tejos ◽  
...  
Keyword(s):  
Black Hole ◽  
Galaxy Evolution ◽  
Rest Frame ◽  
Narrow Band ◽  
Hubble Space Telescope ◽  
High Signal ◽  
Signal To Noise ◽  
Redshift Range ◽  
Black Hole Growth ◽  
Hole Growth

ABSTRACT We demonstrate that the UV brightest quasars at z = 1–2 live in overdense environments. This is based on an analysis of deep Hubble Space Telescope WFC3 G141 grism spectroscopy of the galaxies along the lines-of-sight to UV luminous quasars in the redshift range z = 1–2. This constitutes some of the deepest grism spectroscopy performed by WFC3, with four roll angles spread over a year of observations to mitigate the effect of overlapping spectra. Of the 12 quasar fields studied, 8 display evidence for a galaxy overdensity at the redshift of the quasar. One of the overdensities, PG0117 + 213 at z = 1.50, has potentially 36 spectroscopically confirmed members, consisting of 19 with secure redshifts and 17 with single-line redshifts, within a cylinder of radius ∼700 kpc. Its halo mass is estimated to be log (M/M⊙) = 14.7. This demonstrates that spectroscopic and narrow-band observations around distant UV bright quasars may be an excellent route for discovering protoclusters. Our findings agree with previous hints from statistical observations of the quasar population and theoretical works, as feedback regulated black hole growth predicts a correlation between quasar luminosity and halo mass. We also present the high signal-to-noise rest-frame optical spectral and photometric properties of the quasars themselves.

scholarly journals An Estimate of the Local Active Black Hole Mass Function and the Distribution Function of Eddington Ratios

2009 ◽  
Vol 5 (S267) ◽  
pp. 266-266
Author(s):  
Andreas Schulze ◽  
Lutz Wisotzki
Keyword(s):  
Black Hole ◽  
Mass Function ◽  
Distribution Functions ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Underlying Distribution ◽  
Black Hole Growth ◽  
Hole Growth ◽  
Black Hole Masses

The observed relations between the black hole mass and the properties of the spheroidal galaxy component imply a close connection between the growth of supermassive black holes and the evolution of their host galaxies. An effective approach to study black hole growth is to measure black hole masses and Eddington ratios of well-defined type 1 AGN samples and determine the underlying distribution functions.

scholarly journals THE ROLE OF MERGERS IN EARLY-TYPE GALAXY EVOLUTION AND BLACK HOLE GROWTH

2010 ◽  
Vol 714 (1) ◽  
pp. L108-L112 ◽  
Author(s):  
Kevin Schawinski ◽  
Nathan Dowlin ◽  
Daniel Thomas ◽  
C. Megan Urry ◽  
Edward Edmondson
Keyword(s):  
Black Hole ◽  
Galaxy Evolution ◽  
Early Type ◽  
Black Hole Growth ◽  
Hole Growth ◽  
Early Type Galaxy

scholarly journals Mass transport in galaxy discs limits black hole growth to sub-Eddington rates

2019 ◽  
Vol 488 (2) ◽  
pp. 2006-2017
Author(s):  
Daniel S Eastwood ◽  
Sadegh Khochfar ◽  
Arthur Trew
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Extreme Case ◽  
Big Bang ◽  
Limiting Factor ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Orbital Parameters ◽  
Black Hole Growth ◽  
Hole Growth

ABSTRACT Supermassive black holes (SMBHs) observed to have masses of $M_\bullet \sim 10^9 \, \mathrm{M_\odot }$ at z ≳ 6, <1 Gyr after the big bang, are thought to have been seeded by massive black holes that formed before growing concurrently with the formation of their host galaxies. We model analytically the idealized growth of seed black holes, fed through gas inflow from growing proto-galaxy discs. The inflow depends on the disc gravitational stability and thus varies with black hole and disc mass. We find that for a typical host halo, the efficiency of angular momentum transport, as parametrized by the disc viscosity, is the limiting factor in determining the inflow rate and the black hole accretion rate. For our fiducial case, we find an upper black hole mass estimate of $M_\bullet \sim 1.8 \times 10^7 \, \mathrm{M_{\odot }}$ at z = 6. Only in the extreme case of ∼1016 M⊙ haloes at z = 6 produces SMBH masses of ∼109 M⊙. However, the number density of such haloes is many orders of magnitude below the estimated 1 Gpc−3 of SMBHs at z = 6, indicating that viscosity driven accretion is too inefficient to feed the growth of seeds into $M_\bullet \sim 10^9 \, \mathrm{M_\odot }$ SMBHs by z ∼ 6. We demonstrate that major mergers are capable of resolving the apparent discrepancy in black hole mass at z = 6, with some dependence on the exact choice of orbital parameters of the merger.

scholarly journals The Relation between Mid-Infrared Emission and Black Hole Mass in Active Galactic Nuclei: A Direct Way to Probe Black Hole Growth?

2002 ◽  
Vol 571 (1) ◽  
pp. L1-L5 ◽  
Author(s):  
Almudena Alonso-Herrero ◽  
Valentin D. Ivanov ◽  
Ray Jayawardhana ◽  
Takashi Hosokawa
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Infrared Emission ◽  
Black Hole Mass ◽  
Mid Infrared ◽  
Black Hole Growth ◽  
Hole Growth
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