A Relationship between Nuclear Black Hole Mass and Galaxy Velocity Dispersion

Gebhardt, Karl; Bender, Ralf; Bower, Gary; Dressler, Alan; Faber, S. M.; Filippenko, A. V.; Green, Richard; Grillmair, Carl J.; Ho, Luis C.; Kormendy, John; Lauer, Tod R.; Magorrian, John; Pinkney, Jason; Richstone, Douglas; Tremaine, Scott

doi:10.1086/312840

Cited by 3,524 publications

(2,989 citation statements)

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“…The same is true of 47 Tuc where McLaughlin et al (2006) report 700 ± 700 M ⊙ . In both of these cases, the value reported, while not significant, is consistent with that mass expected from an extrapolation of the correlation between black hole mass and host dispersion as reported in Gebhardt et al (2000) and Tremaine et al (2002).…”

Section: Massive Black Holes In Globular Clusterssupporting

confidence: 87%

Joint Discussion 6 Neutron stars and black holes in star clusters

et al. 2006

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This article was co-authored by all invited speakers at Joint Discussion 6 onNeutron Stars and Black Holes in Star Clusters, which took place during the IAU General Assembly in Prague, Czech Republic, on August 17 and 18, 2006. Each section presents a short summary of recent developments in a key area of research, incorporating the main ideas expressed during the corresponding panel discussion at the meeting.

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Section: Massive Black Holes In Globular Clusterssupporting

confidence: 87%

Joint Discussion 6 Neutron stars and black holes in star clusters

et al. 2006

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“…The discovery of the M − σ correlation (Ferrarese & Merritt 2000;Gebhardt et al 2000a) has motivated a great deal of observational effort toward measurement of stellar velocity dispersions in active galaxies. Since the M − σ relation is apparently very tight, with < 0.3 dex scatter , it has been used as a means to estimate black hole masses in AGNs directly from their stellar velocity dispersions.…”

Section: Can the Stellar Velocity Dispersions Of Quasar Host Galaxiesmentioning

confidence: 99%

Black hole masses in active galaxies

Barth

2004

Proc. IAU

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“…Nonetheless, there still remain possible systematic uncertainties, for example, due to the intrinsic assumption that the disk truncates at the innermost stable circular orbit. Simulations have been performed specifically aimed at addressing the robustness of this assumption [30], which find that emission within this radius is negligible, especially for rapidly rotating black holes, as is the case here.The ability to measure cosmological black hole spin brings with it the potential to directly study the co-evolution of the black hole and its host galaxy [1]. The ultimate goal is to measure the spin in a sample of quasars as a function of redshift and to make use of the spin distribution as a window on the history of the co-evolution of black hole and galaxies [4].…”

mentioning

confidence: 99%

“…The ability to measure cosmological black hole spin brings with it the potential to directly study the co-evolution of the black hole and its host galaxy [1]. The ultimate goal is to measure the spin in a sample of quasars as a function of redshift and to make use of the spin distribution as a window on the history of the co-evolution of black hole and galaxies [4].…”

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Reflection from the strong gravity regime in a lensed quasar at redshift z = 0.658

Reis

Reynolds

Miller

et al. 2014

Nature

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The co-evolution of a supermassive black hole with its host galaxy[1] through cosmic time is encoded in its spin[2, 3, 4]. At z > 2, supermassive black holes are thought to grow mostly by merger-driven accretion leading to high spin. However, it is unknown whether below z ∼ 1 these black holes continue to grow via coherent accretion or in a chaotic manner [5], though clear differences are predicted [3,4] in their spin evolution. An established method[6] to measure the spin of black holes is via the study of relativistic reflection features [7] from the inner accretion disk. Owing to their greater distances, there has hitherto been no significant detection of relativistic reflection features in a moderateredshift quasar. Here, we use archival data together with a new, deep observation of a gravitationally-lensed quasar at z = 0.658 to rigorously detect and study reflection in this moderate-redshift quasar. The level of relativistic distortion present in this reflection spectrum enables us to constrain the emission to originate within 3 gravitational radii from the black hole, implying a spin parameter a = 0.87 +0.08 −0.15 at the 3σ level of confidence and a > 0.66 at the 5σ level. The high spin found here is indicative of growth via coherent accretion for this black hole, and suggests that black hole growth between 0.5 z 1 occurs principally by coherent rather than chaotic accretion episodes. 1When optically-thick material, e.g. an accretion disc, is irradiated by hard X-rays, some of the flux is reprocessed into an additional 'reflected' emission component, which contains both continuum emission and atomic features. The most prominent signature of reflection from the inner accretion disc is typically the relativistic iron Kα line (6.4-6.97 keV; rest frame) [8] and the Compton reflection hump [7] often peaking at 20 − 30 keV (rest-frame). However, the deep gravitational potential and strong Doppler shifts associated with regions around black holes will also cause the forest of soft X-ray emission lines in the ∼ 0.7 − 2.0 keV range to be blended into a smooth emission feature, providing a natural explanation for the "soft-excess" observed in the X-ray spectra of nearby active galactic nuclei (AGNs) [9,10]. Indeed, both the iron line and the soft excess can be used to provide insight into the nature of the central black hole and to measure its spin [10]. Prior studies have revealed the presence of a soft-excess in 90% of quasars at[11, 12] z 1.7, and broad Fe-lines are also seen in 25% of these objects [11,13], suggesting that reflection is also prevalent in these distant AGNs. However, due to the inadequate S/N resulting from their greater distances, the X-ray spectra of these quasars were necessarily modeled using simple phenomenological parameterizations [12,14].Gravitational lensing offers a rare opportunity to study the innermost relativistic region in distant quasars [15,16], by acting as a natural telescope and magnifying the light from these sources. Quasars located between 0.5 z 1 are considerably ...

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A Relationship between Nuclear Black Hole Mass and Galaxy Velocity Dispersion

Cited by 3,524 publications

References 46 publications

Joint Discussion 6 Neutron stars and black holes in star clusters

Joint Discussion 6 Neutron stars and black holes in star clusters

Black hole masses in active galaxies

Reflection from the strong gravity regime in a lensed quasar at redshift z = 0.658

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