The Black Hole Mass in M87 From Gemini/Nifs Adaptive Optics Observations

Gebhardt, Karl; Adams, Joshua J.; Richstone, D. O.; Lauer, Tod R.; Faber, S. M.; Gültekin, Kayhan; Murphy, J.H.; Tremaine, Scott

doi:10.1088/0004-637x/729/2/119

Cited by 448 publications

(473 citation statements)

References 63 publications

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“…For this source, we found two reliable black hole mass measurements based on stellar and gas dynamics, respectively: log(M BH /M ) = 9.82 ± 0.03 (Gebhardt et al 2011) and log(M BH /M ) = 9.5 ± 0.1 (Walsh et al 2013). For the present analysis we adopt the more recent estimate from Walsh et al (2013).…”

Section: Smbh Masses and Corresponding Time Scalesmentioning

confidence: 76%

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Vovk

Babić

2015

A&A

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Context. The variability time scales of the blazar γ-ray emission contain the imprints of the sizes of their emission zones and are generally expected to be larger than the light-crossing times of these zones. In several cases the time scales were found to be as short ∼10 min, suggesting that the emission zone sizes are comparable with the sizes of the central supermassive black holes. Previously, these measurements also led to the suggestion of a possible connection between the observed minimal variability time scales and the masses of the corresponding black holes. This connection can be used to determine the location of the γ-ray emission site, which currently remains uncertain. Aims. The study aims to investigate the suggested "minimum time scale -black hole mass" relation using the blazars, detected in the TeV band. Methods. To obtain the tightest constraints on the variability time scales this work uses a compilation of observations by the Cherenkov telescopes HESS, MAGIC, and VERITAS. These measurements are compared to the blazar central black hole masses found in the literature.Results. The majority of the studied blazars show the variability time scales which are at least comparable to the period of rotation along the last stable orbit of the central black hole -and in some cases as short as its light-crossing time. For several sources the observed variability time scales are found to be smaller than the black hole light-crossing time. This suggests that the detected γ-ray variability originates, most probably, from the turbulence in the jet, sufficiently far from the central black hole.

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Section: Smbh Masses and Corresponding Time Scalesmentioning

confidence: 76%

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Vovk

Babić

2015

A&A

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“…Based on the stellar or gas dynamics in the core, the mass of the M 87 central BH has been estimated as M BH = 3.2, 3.5, and 6.2 × 10 9 M (by Macchetto et al 1997;Gebhardt et al 2011;Walsh et al 2013, respectively). Here, we adopt the most recent value from the observations, M BH = 6.2 × 10 9 M , in all of our models.…”

Section: Scaling the Model To M 87 Corementioning

confidence: 99%

General relativistic magnetohydrodynamical simulations of the jet in M 87

Mościbrodzka

Falcke

Shiokawa

2016

A&A

294

314

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Context. The connection between black hole, accretion disk, and radio jet can be constrained best by fitting models to observations of nearby low-luminosity galactic nuclei, in particular the well-studied sources Sgr A* and M 87. There has been considerable progress in modeling the central engine of active galactic nuclei by an accreting supermassive black hole coupled to a relativistic plasma jet. However, can a single model be applied to a range of black hole masses and accretion rates? Aims. Here we want to compare the latest three-dimensional numerical model, originally developed for Sgr A* in the center of the Milky Way, to radio observations of the much more powerful and more massive black hole in M 87. Methods. We postprocess three-dimensional GRMHD models of a jet-producing radiatively inefficient accretion flow around a spinning black hole using relativistic radiative transfer and ray-tracing to produce model spectra and images. As a key new ingredient in these models, we allow the proton-electron coupling in these simulations depend on the magnetic properties of the plasma. Results. We find that the radio emission in M 87 is described well by a combination of a two-temperature accretion flow and a hot single-temperature jet. Most of the radio emission in our simulations comes from the jet sheath. The model fits the basic observed characteristics of the M 87 radio core: it is "edge-brightened", starts subluminally, has a flat spectrum, and increases in size with wavelength. The best fit model has a mass-accretion rate ofṀ ∼ 9 × 10 −3 M yr −1 and a total jet power of P j ∼ 10 43 erg s −1 . Emission at λ = 1.3 mm is produced by the counter-jet close to the event horizon. Its characteristic crescent shape surrounding the black hole shadow could be resolved by future millimeter-wave VLBI experiments. Conclusions. The model was successfully derived from one for the supermassive black hole in the center of the Milky Way by appropriately scaling mass and accretion rate. This suggests the possibility that this model could also apply to a wider range of low-luminosity black holes.

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“…Owing to the uncertainty in the bulge effective radius for NGC 1271, we measure the effective stellar velocity dispersion ( e,bul s ) for three different bulge effective radii corresponding to the largest R e estimate from the Galfit decomposition, the smallest estimate of R e , and the average of the two. Additionally, some previous black hole studies have chosen to exclude data within r sphere when determining e,bul s because the stellar kinematics are under the direct influence of the black hole in this region (e.g., Gebhardt et al 2011;McConnell & Ma 2013 , which is the observed stellar velocity dispersion within a 3″. 5 aperture from the major-axis longslit data.…”

Section: Black Hole-host Galaxy Relationsmentioning

confidence: 99%

“…While recent progress has been made in searching for, and revising measurements for, black holes with masses larger than M 10 9  (Shen & Gebhardt 2010;Walsh et al 2010Walsh et al , 2013Gebhardt et al 2011;McConnell et al 2011McConnell et al , 2012van den Bosch et al 2012;Rusli et al 2013), many of these galaxies are giant ellipticals or brightest cluster galaxies (BCGs), which are often large (with R 10 e > kpc; e.g., Dalla Bontà et al 2009), have cored surface brightness profiles, and are dispersionsup-ported, showing little to no rotation. In contrast, the compact, high-dispersion galaxies found through the HET survey are small, are rapidly rotating, and generally exhibit cuspy surface brightness profiles.…”

Section: Introductionmentioning

confidence: 99%

The Black Hole in the Compact, High-Dispersion Galaxy NGC 1271

Walsh

Bosch

Gebhardt

et al. 2015

ApJ

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Located in the Perseus cluster, NGC 1271 is an early-type galaxy with a small effective radius of 2.2 kpc and a large bulge stellar velocity dispersion of 276 km s −1 for its K-band luminosity of L 8.9 10 10  . We present a mass measurement for the black hole in this compact, high-dispersion galaxy using observations from the Near-infrared Integral Field Spectrometer on the Gemini North telescope assisted by laser guide star adaptive optics, large-scale integral field unit observations with PPAK at the Calar Alto Observatory, and Hubble Space Telescope WFC3 imaging observations. We are able to map out the stellar kinematics both on small spatial scales, within the black hole sphere of influence, and on large scales that extend out to four times the galaxy's effective radius. We find that the galaxy is rapidly rotating and exhibits a sharp rise in the velocity dispersion. Through the use of orbit-based stellar dynamical models, we determine that the black hole has a mass of M (3.0 ) 10 1.1 1.0 9 -+  and the H-band stellar mass-to-light ratio is 1.40 0.11 0.13 ¡ -+  (1s uncertainties). NGC 1271 occupies the sparsely populated upper end of the black hole mass distributionbut is very different from the brightest cluster galaxies (BCGs) and giant elliptical galaxies that are expected to host the most massive black holes. Interestingly, the black hole mass is an order of magnitude larger than expectations based on the galaxy's bulge luminositybut is consistent with the mass predicted using the galaxy's bulge stellar velocity dispersion. More compact, high-dispersion galaxies need to be studied using high spatial resolution observations to securely determine black hole masses, as there could be systematic differences in the black hole scaling relations between these types of galaxies and the BCGs/giant ellipticals, thereby implying different pathways for black hole and galaxy growth.

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The Black Hole Mass in M87 From Gemini/Nifs Adaptive Optics Observations

Cited by 448 publications

References 63 publications

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

Minimal variability time scale – central black hole mass relation of theγ-ray loud blazars

General relativistic magnetohydrodynamical simulations of the jet in M 87

The Black Hole in the Compact, High-Dispersion Galaxy NGC 1271

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