Masses of quasars

Sołtan, A.

doi:10.1093/mnras/200.1.115

Cited by 1,012 publications

(252 citation statements)

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“…The classic argument of Soltan (1982), compares the total mass of black holes today with the total radiative output by known quasars, by integration over redshift and luminosity of the luminosity function of quasars (Yu and Tremaine, 2002;Elvis et al, 2002;Marconi et al, 2004). The total energy density can be converted into the total mass density accreted by black holes during the active phase, by assuming a mass-to-energy conversion efficiency, (Aller and Richstone, 2002;Merloni et al, 2004;Elvis et al, 2002;Marconi et al, 2004):…”

Section: The Early Growth Of Massive Black Holesmentioning

confidence: 99%

Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

794

707

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Evidence shows that massive black holes reside in most local galaxies. Studies have also established a number of relations between the MBH mass and properties of the host galaxy such as bulge mass and velocity dispersion. These results suggest that central MBHs, while much less massive than the host (∼ 0.1%), are linked to the evolution of galactic structure. In hierarchical cosmologies, a single big galaxy today can be traced back to the stage when it was split up in hundreds of smaller components. Did MBH seeds form with the same efficiency in small proto-galaxies, or did their formation had to await the buildup of substantial galaxies with deeper potential wells? I briefly review here some of the physical processes that are conducive to the evolution of the massive black hole population. I will discuss black hole formation processes for 'seed' black holes that are likely to place at early cosmic epochs, and possible observational tests of these scenarios.

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Section: The Early Growth Of Massive Black Holesmentioning

confidence: 99%

Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

794

707

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“…Consequently, the emitted luminosity is suppressed to the point thatṁ can greatly exceed 1 (supercritical accretion), still resulting in a subEddington luminosity. Note that early supercritical accretion is still consistent with the Soltan [86] argument: MBHs can in principle grow this way to 10 7 -10 8 M , complete the last couple of e-folding in mass via radiatively efficient accretion, and still satisfy the quasar luminosity function-mass conversion constraints. However, simulations of radiative inefficient accretion flows [107][108][109][110][111] showed that most of the infalling matter is driven away by wind-like outflows, and the actual accretion rate can exceed the Eddington limit by a factor of ≈10 only.…”

Section: The Highest Redshift Quasarsmentioning

confidence: 52%

“…Soltan [86] first noticed that the optical luminosity function of quasars directly implies a large population of nuclear MBHs lurking in quiescent galaxies today. Infact, to an observed luminosity L corresponds a mass accretion ratė…”

Section: The Making Of the Giants: Massive Black Hole Accretion Historymentioning

confidence: 99%

A Practical Guide to the Massive Black Hole Cosmic History

Sesana

2012

Advances in Astronomy

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I review our current understanding of massive black hole (MBH) formation and evolution along the cosmic history. After a brief introductory overview of the relevance of MBHs in the hierarchical structure formation paradigm, I discuss the main viable channels for seed BH formation at high redshift and for their subsequent mass growth and spin evolution. The emerging hierarchical picture, where MBHs grow through merger triggered accretion episodes, acquiring their mass while shining as quasars, is overall robust, but too simplistic to explain the diversity observed in MBH phenomenology. I briefly discuss which future observations will help to shed light on the MBH cosmic history in the near future, paying particular attention to the upcoming gravitational wave window.

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“…8,9 Moreover, there are indications that periods of significant black hole growth are associated with episodes of enhanced host-galaxy star formation, both from models and observations. [10][11][12] This is intriguing, but spectroscopic confirmation is required to establish the presence of AGN, measure the partitioning of the energy between the AGN and star formation, and study the interaction between the AGN and the host galaxy. The same wideband far-IR spectra that probe the star-formation properties will also find and study buried AGN in the early Universe via:…”

Section: Revealing the Black-hole-galaxy Connectionmentioning

confidence: 99%

Progress toward BLISS, the background-limited infrared-submillimeter spectrograph for SPICA

Bradford

Beyer

Kenyon

et al. 2012

Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave

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We are developing the Background-Limited Infrared-Submillimeter Spectrograph (BLISS) for SPICA to provide a breakthrough capability for far-IR survey spectroscopy. The 3.2-meter, actively-cooled (T<6K) SPICA telescope allows mid-IR to submm observations which are limited only by the natural backgrounds, and BLISS is designed to operate near this fundamental limit. BLISS-SPICA provide a line sensitivity of 10 −20 W m −2 , thereby enabling spectroscopy of dust-obscured galaxies at all epochs back to the first billion years after the Big Bang (redshift 6), and study of all stages of planet formation in circumstellar disks.BLISS covers the 35-430 micron waveband at moderate resolving power (300

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Masses of quasars

Cited by 1,012 publications

References 0 publications

Formation of supermassive black holes

Formation of supermassive black holes

A Practical Guide to the Massive Black Hole Cosmic History

Progress toward BLISS, the background-limited infrared-submillimeter spectrograph for SPICA

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