scholarly journals Cosmological Evolution of the Hard X-Ray AGN Luminosity Function: Formation History of Supermassive Black Holes

2004 ◽  
Vol 155 ◽  
pp. 209-216 ◽  
Author(s):  
Yoshihiro Ueda ◽  
Masayuki Akiyama ◽  
Kouji Ohta ◽  
Takamitsu Miyaji
Keyword(s):  
Black Holes ◽  
Luminosity Function ◽  
Supermassive Black Holes ◽  
Cosmological Evolution ◽  
X Ray ◽  
Formation History ◽  
History Of

scholarly journals Cosmological Evolution of Supermassive Black Holes: Mass Functions and Spins

2012 ◽  
Vol 8 (S290) ◽  
pp. 259-260 ◽  
Author(s):  
Yan-Rong Li ◽  
Jian-Min Wang ◽  
Luis C. Ho
Keyword(s):  
Black Holes ◽  
Mass Function ◽  
Supermassive Black Holes ◽  
Cosmological Evolution ◽  
Radiative Efficiency ◽  
Bolometric Luminosity ◽  
History Of ◽  
Minor Mergers ◽  
Mass Dependent ◽  
Mass Functions

AbstractWe derive the mass function of supermassive black holes (SMBHs) over the redshift range 0 > z ≲ 2, using the latest deep luminosity and mass functions of field galaxies. Applying this mass function, combined with the bolometric luminosity function of active galactic nuclei (AGNs), into the the continuity equation of SMBH number density, we explicitly obtain the mass-dependent cosmological evolution of the radiative efficiency for accretion. We suggest that the accretion history of SMBHs and their spins evolve in two distinct regimes: an early phase of prolonged accretion, plausibly driven by major mergers, during which the black hole spins up, then switching to a period of random, episodic accretion, governed by minor mergers and internal secular processes, during which the hole spins down. The transition epoch depends on mass, mirroring other evidence for “cosmic downsizing” in the AGN population.

scholarly journals A survey of AGN and supermassive black holes in the COSMOS Survey

2006 ◽  
Vol 2 (S238) ◽  
pp. 287-290 ◽  
Author(s):  
Chris D. Impey ◽  
Jon R. Trump ◽  
Pat J. McCarthy ◽  
Martin Elvis ◽  
John P. Huchra ◽  
...  
Keyword(s):  
Black Holes ◽  
Large Scale ◽  
Supermassive Black Holes ◽  
Host Galaxy ◽  
Data Set ◽  
X Ray ◽  
Cosmic Evolution ◽  
Early Results ◽  
Multi Wavelength ◽  
History Of

AbstractThe Cosmic Evolution Survey (COSMOS) is an HST/ACS imaging survey of 2 square degrees centered on RA = 10:00:28.6, Dec = + 02:12:21 (J2000). While the primary goal of the survey is to study evolution of galaxy morphology and large scale structure, an extensive multi-wavelength data set allows for a sensitive survey of AGN. Spectroscopy of optical counterparts to faint X-ray and radio sources is being carried out with the Magallen (Baade) Telescope and the ESO VLT. By achieving ∼80 redshift completeness down to I AB = 3, the eventual yield of AGN will be ∼1100 over the whole field.Early results on supermassive black holes are described. The goals of the survey include a bolometric census of AGN down to moderate luminosities, the cosmic evolution and fueling history of the central engines, and a study of AGN environments on scales ranging from the host galaxy to clusters and superclusters.

scholarly journals Tracing the accretion history of supermassive black holes through X-ray variability: results from the ChandraDeep Field-South

2017 ◽  
Vol 471 (4) ◽  
pp. 4398-4411 ◽  
Author(s):  
M. Paolillo ◽  
I. Papadakis ◽  
W. N. Brandt ◽  
B. Luo ◽  
Y. Q. Xue ◽  
...  
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
X Ray ◽  
History Of

Formation history of supermassive black holes in a viable cosmological window

2006 ◽  
Vol 2 (S238) ◽  
pp. 345-346
Author(s):  
Carlos H. Coimbra-Araújo ◽  
Amâncio C. S. Friaça
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Supermassive Black Holes ◽  
Intermediate Mass ◽  
Disk Model ◽  
Rapid Rotation ◽  
Supermassive Black Hole ◽  
Formation History ◽  
History Of ◽  
Stable Part

AbstractWe show, performing a viable cosmological window, that only the magneto hydrodynamic (MHD) disk model is capable to explain how an intermediate mass black hole (IMBH) (with masses ∼ 103M⊙) grows unto a supermassive black hole (SMBH) (with masses ∼ 107M⊙). We still calculate the supermassive stars sequence of stability. Those stars, with synthetized helium or oxygen cores, collapse to form IMBHs. In our calculation we show that the primordial stars must have rapid rotation if they are in the stable part of the sequence.

scholarly journals The Cosmic History of Black Hole Growth from Deep Multiwavelength Surveys

2012 ◽  
Vol 2012 ◽  
pp. 1-21 ◽  
Author(s):  
Ezequiel Treister ◽  
C. Megan Urry
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Optical Emission ◽  
Supermassive Black Holes ◽  
X Ray ◽  
Open Questions ◽  
Black Hole Growth ◽  
History Of ◽  
Hole Growth ◽  
Cosmic History

Significant progress has been made in the last few years on understanding how supermassive black holes form and grow. In this paper, we begin by reviewing the spectral signatures of active galactic nuclei (AGN) ranging from radio to hard X-ray wavelengths. We then describe the most commonly used methods to find these sources, including optical/UV, radio, infrared, and X-ray emission, and optical emission lines. We then describe the main observational properties of the obscured and unobscured AGN population. Finally, we summarize the cosmic history of black hole accretion, that is, when in the history of the universe supermassive black holes were getting most of their mass. We finish with a summary of open questions and a description of planned and future observatories that are going to help answer them.

scholarly journals Can we infer the past activity of M31⋆ as we do for Sgr A⋆?

2016 ◽  
Vol 11 (S322) ◽  
pp. 253-256
Author(s):  
Maïca Clavel ◽  
Régis Terrier ◽  
Andrea Goldwurm ◽  
Mark R. Morris ◽  
Gabriele Ponti
Keyword(s):  
Black Holes ◽  
Molecular Clouds ◽  
Galactic Center ◽  
Supermassive Black Holes ◽  
X Ray ◽  
The Past ◽  
Upper Limits ◽  
History Of ◽  
Sgr A ◽  
Past Activity

AbstractThe history of supermassive black holes’ activity can be partly constrained by monitoring the diffuse X-ray emission possibly created by the echoes of past events propagating through the molecular clouds of their respective environments. In particular, using this method we have demonstrated that our Galaxy’s supermassive black hole, Sgr A⋆, has experienced multiple periods of higher activity in the last centuries, likely due to several short but very energetic events, and we now investigate the possibility of studying the past activity of other supermassive black holes by applying the same method to M31⋆. We set strong constraints on putative phase transitions of this more distant galactic nucleus but the existence of short events such as the ones observed in the Galactic center cannot be assessed with the upper limits we derived.

scholarly journals The Luminosity Function of X‐Ray–selected Active Galactic Nuclei: Evolution of Supermassive Black Holes at High Redshift

2008 ◽  
Vol 679 (1) ◽  
pp. 118-139 ◽  
Author(s):  
J. D. Silverman ◽  
P. J. Green ◽  
W. A. Barkhouse ◽  
D.‐W. Kim ◽  
M. Kim ◽  
...  
Keyword(s):  
Black Holes ◽  
Active Galactic Nuclei ◽  
Luminosity Function ◽  
High Redshift ◽  
Galactic Nuclei ◽  
Supermassive Black Holes ◽  
X Ray

scholarly journals Cosmological evolution of the AGN kinetic luminosity function

2006 ◽  
Vol 2 (S238) ◽  
pp. 65-70
Author(s):  
Andrea Merloni ◽  
Sebastian Heinz
Keyword(s):  
Galaxy Formation ◽  
Luminosity Function ◽  
Cosmological Evolution ◽  
Energy Output ◽  
Theoretical Assumption ◽  
X Ray ◽  
Spectrum Radio ◽  
Luminosity Functions ◽  
Jet Power ◽  
Joint Evolution

AbstractWe present a first attempt to derive the cosmological evolution of the kinetic luminosity function of AGN based on the joint evolution of the flat spectrum radio and hard X-ray selected AGN luminosity functions. An empirical correlation between jet power and radio core luminosity is found, which is consistent with the theoretical assumption that, below a certain Eddington ratio, SMBH accrete in a radiatively inefficient way, while most of the energy output is in the form of kinetic energy.We show how the redshift evolution of the kinetic power density from such a low-ṁ mode of accretion makes it a good candidate to explain the so-called “radio mode” of AGN feedback as outlined in many galaxy formation schemes.

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