scholarly journals Origins and demographics of wandering black holes

2021 ◽  
Vol 503 (4) ◽  
pp. 6098-6111
Author(s):  
Angelo Ricarte ◽  
Michael Tremmel ◽  
Priyamvada Natarajan ◽  
Charlotte Zimmer ◽  
Thomas Quinn
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Seed Mass ◽  
Galaxy Cluster ◽  
Supermassive Black Holes ◽  
Black Hole Mass ◽  
Cosmological Simulations ◽  
Mass Budget ◽  
Satellite Galaxies ◽  
Gas Properties

ABSTRACT We characterize the population of wandering black holes, defined as those physically offset from their halo centres, in the romulus cosmological simulations. Unlike most other currently available cosmological simulations, black holes are seeded based on local gas properties and are permitted to evolve dynamically without being fixed at halo centres. Tracking these black holes allows us to make robust predictions about the offset population. We find that the number of wandering black holes scales roughly linearly with the halo mass, such that we expect thousands of wandering black holes in galaxy cluster haloes. Locally, these wanderers account for around 10 per cent of the local black hole mass budget once seed masses are accounted for. Yet for higher redshifts ($z$ ≳ 4), wandering black holes both outweigh and outshine their central supermassive counterparts. Most wandering black holes, we find, remain close to the seed mass and originate from the centres of previously disrupted satellite galaxies. While most do not retain a resolved stellar counterpart, those that do are situated farther out at larger fractions of the virial radius. Wanderers with higher luminosities are preferentially at lower radius, more massive, and either closer to their host’s mid-planes or associated with a stellar overdensity. This analysis shows that our current census of supermassive black holes is incomplete and that a substantial population of off-centre wanderers likely exists.

scholarly journals EVOLUTION OF SUPERMASSIVE BLACK HOLES FROM COSMOLOGICAL SIMULATIONS

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1233-1240 ◽  
Author(s):  
C. FILLOUX ◽  
F. DURIER ◽  
J. A. F. PACHECO ◽  
J. SILK
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Mass Density ◽  
Mass Function ◽  
Supermassive Black Holes ◽  
Dark Halo ◽  
Black Hole Mass ◽  
Cosmological Simulations ◽  
Redshift Range ◽  
Density Peaks

The correlations between the mass of supermassive black holes and the properties of their host galaxies are investigated through cosmological simulations. Black holes grow from seeds of 100 M⊙ are inserted into density peaks presented in the redshift range 12–15. Seeds grow essentially by accreting matter from a nuclear disk and also by coalescences resulting from merger episodes. At z = 0, our simulations reproduce the black hole mass function and the correlations of the black hole mass, both with stellar velocity dispersion and host dark halo mass. Moreover, the evolution of the black hole mass density derived from the present simulations agrees with that derived from the bolometric luminosity of quasars, indicating that the average accretion history of seeds is adequately reproduced. However, our simulations are unable to form black holes with masses above 109 M⊙ at z ~ 6, whose existence is inferred from the bright quasars detected by the Sloan survey in this redshift range.

scholarly journals Effects of the Hubble parameter on the cosmic growth of the first quasars

2020 ◽  
Vol 496 (1) ◽  
pp. 888-893 ◽  
Author(s):  
Rafael C Nunes ◽  
Fabio Pacucci
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hubble Parameter ◽  
Crucial Role ◽  
Seed Mass ◽  
Early Growth ◽  
Supermassive Black Holes ◽  
Initial Mass ◽  
Seed Formation ◽  
Mcmc Approach

ABSTRACT Supermassive black holes (SMBHs) play a crucial role in the evolution of galaxies and are currently detected up to $z$ ∼ 7.5. Theories describing black hole (BH) growth are challenged by how rapidly seeds with initial mass $M_\bullet \lesssim 10^5 \, {\rm M_\odot }$, formed at $z$ ∼ 20–30, grew to $M_\bullet \sim 10^9 \, {\rm M_\odot }$ by $z$ ∼ 7. Here we study the effects of the value of the Hubble parameter, H0, on models describing the early growth of BHs. First, we note that the predicted mass of a quasar at $z$ = 6 changes by $\gt 300{{\ \rm per\ cent}}$ if the underlying Hubble parameter used in the model varies from H0 = 65 to H0 = 74 km s−1Mpc−1, a range encompassing current estimates. Employing an MCMC approach based on priors from $z$ ≳ 6.5 quasars and on H0, we study the interconnection between H0 and the parameters describing BH growth: seed mass Mi and Eddington ratio fEdd. Assuming an Eddington ratio of fEdd = 0.7, in agreement with previous estimates, we find $H_0 = 73.6^{+1.2}_{-3.3}$ km s−1Mpc−1. In a second analysis, allowing all the parameters to vary freely, we find log (Mi/M⊙) > 4.5 (at 95 per cent CL), $H_0 = 74^{+1.5}_{-1.4}$ km s−1Mpc−1 and $f_{\rm Edd}=0.77^{+0.035}_{-0.026}$ at 68 per cent CL. Our results on the typical Eddington ratio are in agreement with previous estimates. Current values of the Hubble parameter strongly favour heavy seed formation scenarios, with $M_i \gtrsim 10^4 \, {\rm M_\odot }$. In our model, with the priors on BH masses of quasars used, light seed formation scenarios are rejected at ∼3σ.

scholarly journals C iv black hole mass measurements with the Australian Dark Energy Survey (OzDES)

2019 ◽  
Vol 487 (3) ◽  
pp. 3650-3663 ◽  
Author(s):  
J K Hoormann ◽  
P Martini ◽  
T M Davis ◽  
A King ◽  
C Lidman ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dark Energy ◽  
Emission Line ◽  
Galaxy Evolution ◽  
Supermassive Black Holes ◽  
Black Hole Mass ◽  
Mass Measurements ◽  
Dark Energy Survey ◽  
Energy Survey

ABSTRACT Black hole mass measurements outside the local Universe are critically important to derive the growth of supermassive black holes over cosmic time, and to study the interplay between black hole growth and galaxy evolution. In this paper, we present two measurements of supermassive black hole masses from reverberation mapping (RM) of the broad C iv emission line. These measurements are based on multiyear photometry and spectroscopy from the Dark Energy Survey Supernova Program (DES-SN) and the Australian Dark Energy Survey (OzDES), which together constitute the OzDES RM Program. The observed reverberation lag between the DES continuum photometry and the OzDES emission line fluxes is measured to be $358^{+126}_{-123}$ and $343^{+58}_{-84}$ d for two quasars at redshifts of 1.905 and 2.593, respectively. The corresponding masses of the two supermassive black holes are 4.4 × 109 and 3.3 × 109 M⊙, which are among the highest redshift and highest mass black holes measured to date with RM studies. We use these new measurements to better determine the C iv radius−luminosity relationship for high-luminosity quasars, which is fundamental to many quasar black hole mass estimates and demographic studies.

scholarly journals Mass Functions of Supermassive Black Holes across Cosmic Time

2012 ◽  
Vol 2012 ◽  
pp. 1-21 ◽  
Author(s):  
Brandon C. Kelly ◽  
Andrea Merloni
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Cosmic Time ◽  
Theoretical Models ◽  
Mass Function ◽  
Supermassive Black Holes ◽  
Future Research ◽  
Black Hole Mass ◽  
Advantages And Disadvantages ◽  
Mass Functions

The black hole mass function of supermassive black holes describes the evolution of the distribution of black hole mass. It is one of the primary empirical tools available for mapping the growth of supermassive black holes and for constraining theoretical models of their evolution. In this paper, we discuss methods for estimating the black hole mass function, including their advantages and disadvantages. We also review the results of using these methods for estimating the mass function of both active and inactive black holes. In addition, we review current theoretical models for the growth of supermassive black holes that predict the black hole mass function. We conclude with a discussion of directions for future research which will lead to improvement in both empirical and theoretical determinations of the mass function of supermassive black holes.

scholarly journals AGN and Host Galaxies in the COSMOS Survey

2010 ◽  
Vol 6 (S277) ◽  
pp. 21-25
Author(s):  
Christopher D. Impey ◽  
Jonathan R. Trump ◽  
Jared M. Gabor ◽  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Supermassive Black Holes ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Intermediate Mass ◽  
Evolution Of Galaxies ◽  
Accretion Rates ◽  
Deep Survey ◽  
Optical Surveys

AbstractThe Cosmological Evolution Survey (COSMOS) is a unique tool for studying low level AGN activity and the co-evolution of galaxies and supermassive black holes. COSMOS involves the largest contiguous region of the sky ever imaged by HST; it includes very complete multiwavelength coverage, and the largest joint samples of galaxy and AGN redshifts in any deep survey. The result is a search for AGN with low black hole mass, low accretion rates, and levels of obscuration that can remove them from optical surveys. A complete census of intermediate mass black holes at redshifts of 1 to 3 is required to tell the story of the co-evolution of galaxies and their embedded, and episodically active, black holes.

scholarly journals Massive black holes: formation and evolution

2006 ◽  
Vol 2 (S238) ◽  
pp. 51-58 ◽  
Author(s):  
Martin J. Rees ◽  
Marta Volonteri
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Physical Properties ◽  
Supermassive Black Holes ◽  
Black Hole Mass ◽  
Massive Black Holes ◽  
Basic Properties ◽  
Formation And Evolution ◽  
Two Parameters

AbstractSupermassive black holes are nowadays believed to reside in most local galaxies. Observations have revealed us vast information on the population of local and distant black holes, but the detailed physical properties of these dark massive objects are still to be proven. Accretion of gas and black hole mergers play a fundamental role in determining the two parameters defining a black hole: mass and spin. We briefly review here the basic properties of the population of supermassive black holes, focusing on the still mysterious formation of the first massive black holes, and their evolution from early times to now.

scholarly journals Supermassive Black Holes in Active Galactic Nuclei. II. Calibration of the Black Hole Mass–Velocity Dispersion Relationship for Active Galactic Nuclei

2004 ◽  
Vol 615 (2) ◽  
pp. 645-651 ◽  
Author(s):  
Christopher A. Onken ◽  
Laura Ferrarese ◽  
David Merritt ◽  
Bradley M. Peterson ◽  
Richard W. Pogge ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Active Galactic Nuclei ◽  
Mass Velocity ◽  
Velocity Dispersion ◽  
Galactic Nuclei ◽  
Supermassive Black Holes ◽  
Black Hole Mass ◽  
Dispersion Relationship

scholarly journals BLACK HOLE MASS ESTIMATES AND RAPID GROWTH OF SUPERMASSIVE BLACK HOLES IN LUMINOUSz∼ 3.5 QUASARS

2015 ◽  
Vol 799 (2) ◽  
pp. 189 ◽  
Author(s):  
Wenwen Zuo ◽  
Xue-Bing Wu ◽  
Xiaohui Fan ◽  
Richard Green ◽  
Ran Wang ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Rapid Growth ◽  
Supermassive Black Holes ◽  
Black Hole Mass

scholarly journals Maximum PBH mass and primordiality

2018 ◽  
Vol 33 (31) ◽  
pp. 1850176
Author(s):  
Paul H. Frampton
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Cosmic Microwave Background ◽  
Observational Data ◽  
Supermassive Black Holes ◽  
Primordial Black Holes ◽  
Black Hole Mass ◽  
Microwave Background

In order to avoid unacceptable [Formula: see text]-distortions inconsistent with observational data on the Cosmic Microwave Background, Primordial Black Holes (PBHs) must be less massive than [Formula: see text], quite closely above the highest black hole mass yet observed. This comparableness leads us to posit that all supermassive black holes originate as PBHs.

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