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 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 AGNs and Their Host Galaxies in the Local Universe: Two Mass-independent Eddington Ratio Distribution Functions Characterize Black Hole Growth

2017 ◽  
Vol 845 (2) ◽  
pp. 134 ◽  
Author(s):  
Anna K. Weigel ◽  
Kevin Schawinski ◽  
Neven Caplar ◽  
O. Ivy Wong ◽  
Ezequiel Treister ◽  
...  
Keyword(s):  
Black Hole ◽  
Distribution Functions ◽  
Host Galaxies ◽  
Local Universe ◽  
Ratio Distribution ◽  
Black Hole Growth ◽  
Hole Growth

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 LLAMA: The MBH–σ⋆ relation of the most luminous local AGNs

2020 ◽  
Vol 634 ◽  
pp. A114 ◽  
Author(s):  
Turgay Caglar ◽  
Leonard Burtscher ◽  
Bernhard Brandl ◽  
Jarle Brinchmann ◽  
Richard I. Davies ◽  
...  
Keyword(s):  
Black Hole ◽  
Near Infrared ◽  
Velocity Dispersion ◽  
Signal To Noise Ratio ◽  
Broad Line ◽  
Host Galaxies ◽  
Spatially Resolved ◽  
Stellar Velocity ◽  
Black Hole Masses

Context. The MBH–σ⋆ relation is considered a result of coevolution between the host galaxies and their supermassive black holes. For elliptical bulge hosting inactive galaxies, this relation is well established, but there is still discussion concerning whether active galaxies follow the same relation. Aims. In this paper, we estimate black hole masses for a sample of 19 local luminous active galactic nuclei (AGNs; LLAMA) to test their location on the MBH–σ⋆ relation. In addition, we test how robustly we can determine the stellar velocity dispersion in the presence of an AGN continuum and AGN emission lines, and as a function of signal-to-noise ratio. Methods. Supermassive black hole masses (MBH) were derived from the broad-line-based relations for Hα, Hβ, and Paβ emission line profiles for Type 1 AGNs. We compared the bulge stellar velocity dispersion (σ⋆) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We applied an extinction correction to the observed broad-line fluxes and we corrected the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. Results. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34 ≤ log MBH ≤ 7.75 M⊙ and the σ⋆CaT estimates range between 73 ≤ σ⋆CaT ≤ 227 km s−1. From the so-constructed MBH − σ⋆ relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample. Conclusions. We find that our sample of local luminous AGNs is consistent with the MBH–σ⋆ relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion.

scholarly journals Multiplicity functions of quasars: predictions from the MassiveBlackII simulation

2020 ◽  
Vol 492 (4) ◽  
pp. 5620-5633
Author(s):  
Aklant K Bhowmick ◽  
Tiziana Di Matteo ◽  
Adam D Myers
Keyword(s):  
Black Hole ◽  
Surface Density ◽  
Line Of Sight ◽  
Velocity Difference ◽  
Massive Black Hole ◽  
Bolometric Luminosity ◽  
Black Hole Growth ◽  
Hole Growth ◽  
Stellar Masses ◽  
Black Hole Masses

ABSTRACT We examine multiple active galactic nucleus (AGN) systems (triples and quadruples, in particular) in the MassiveBlackII simulation over a redshift range of 0.06 ≲ z ≲ 4. We identify AGN systems (with bolometric luminosity $L_{\mathrm{bol}}\gt 10^{42}~\mathrm{erg\, s}^{-1}$) at different scales (defined by the maximum distance between member AGNs) to determine the AGN multiplicity functions. This is defined as the volume/surface density of AGN systems per unit richness R, the number of AGNs in a system. We find that gravitationally bound multiple AGN systems tend to populate scales of ${\lesssim}0.7~\mathrm{cMpc}\, h^{-1}$; this corresponds to angular separations of ≲100 arcsec and a line-of-sight velocity difference ${\lesssim}200~\mathrm{km\, s}^{-1}$. The simulation contains ∼10 and ∼100 triples/quadruples per deg2 up to depths of DESI (g ≲ 24) and LSST (g ≲ 26) imaging, respectively; at least $20{{\ \rm per\ cent}}$ of these should be detectable in spectroscopic surveys. The simulated quasar ($L_{\mathrm{bol}}\gt 10^{44}~\mathrm{erg\, s}^{-1}$) triples and quadruples predominantly exist at 1.5 ≲ z ≲ 3. Their members have black hole masses $10^{6.5}\lesssim M_{\mathrm{ bh}}\lesssim 10^{9}~\mathrm{M}_{\odot }\, h^{-1}$ and live in separate (one central and multiple satellite) galaxies with stellar masses $10^{10}\lesssim M_{*}\lesssim 10^{12}~\mathrm{M}_{\odot }\, h^{-1}$. They live in the most massive haloes (e.g. ${\sim}10^{13}~\mathrm{M}_{\odot }\, h^{-1}$ at z = 2.5; ${\sim}10^{14}~\mathrm{M}_{\odot }\, h^{-1}$ at z = 1) in the simulation. Their detections provide an exciting prospect for understanding massive black hole growth and their merger rates in galaxies in the era of multimessenger astronomy.

scholarly journals Heavily reddened type 1 quasars at z > 2 – I. Evidence for significant obscured black hole growth at the highest quasar luminosities

2015 ◽  
Vol 447 (4) ◽  
pp. 3368-3389 ◽  
Author(s):  
Manda Banerji ◽  
S. Alaghband-Zadeh ◽  
Paul C. Hewett ◽  
Richard G. McMahon
Keyword(s):  
Black Hole ◽  
Black Hole Growth ◽  
Hole Growth

scholarly journals OBSCURED GOODS ACTIVE GALACTIC NUCLEI AND THEIR HOST GALAXIES ATz< 1.25: THE SLOW BLACK HOLE GROWTH PHASE

2011 ◽  
Vol 734 (2) ◽  
pp. 121 ◽  
Author(s):  
B. D. Simmons ◽  
J. Van Duyne ◽  
C. M. Urry ◽  
E. Treister ◽  
A. M. Koekemoer ◽  
...  
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Growth Phase ◽  
Galactic Nuclei ◽  
Host Galaxies ◽  
Black Hole Growth ◽  
Hole Growth

scholarly journals Self-interacting dark matter and the delay of supermassive black hole growth

2020 ◽  
Vol 500 (2) ◽  
pp. 2177-2187 ◽  
Author(s):  
A Cruz ◽  
A Pontzen ◽  
M Volonteri ◽  
T R Quinn ◽  
M Tremmel ◽  
...  
Keyword(s):  
Black Hole ◽  
Dark Matter ◽  
Galaxy Evolution ◽  
Cold Dark Matter ◽  
Host Galaxies ◽  
Supermassive Black Hole ◽  
Black Hole Growth ◽  
History Of ◽  
Hole Growth ◽  
Delayed Growth

ABSTRACT Using cosmological hydrodynamic simulations with physically motivated models of supermassive black hole (SMBH) formation and growth, we compare the assembly of Milky Way-mass (Mvir ≈ 7 × 1011 M⊙ at z = 0) galaxies in cold dark matter (CDM) and self-interacting dark matter (SIDM) models. Our SIDM model adopts a constant cross-section of 1 cm2 g−1. We find that SMBH formation is suppressed in the early Universe due to SIDM interactions. SMBH–SMBH mergers are also suppressed in SIDM as a consequence of the lower number of SMBHs formed. Lack of initial merger-driven SMBH growth in turn delays SMBH growth by billions of years in SIDM compared to CDM. Further, we find that this delayed growth suppresses SMBH accretion in the largest progenitors of the main SIDM galaxies during the first 5 Gyr of their evolution. Nonetheless, by z = 0.8 the CDM and SIDM SMBH masses differ only by around 0.2 dex, so that both remain compatible with the MBH–M* relation. We show that the reduced accretion causes the SIDM SMBHs to less aggressively regulate star formation in their host galaxies than their CDM counterparts, resulting in a factor of 3 or more stars being produced over the lifetime of the SIDM galaxies compared to the CDM galaxies. Our results highlight a new way in which SIDM can affect the growth and merger history of SMBHs and ultimately give rise to very different galaxy evolution compared to the classic CDM model.

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