Axisymmetric Dynamical Models of the Central Regions of Galaxies

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

doi:10.1086/345081

Cited by 420 publications

(637 citation statements)

References 58 publications

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“…§3) were consistent for these objects. In addition, we took the bulge masses for NGC1023 from Bower et al (2001), for NGC3245 from Barth et al (2001), for NGC4342 from Cretton and van den Bosch (1999) and for NGC3384, for NGC4697, for NGC5845 and for NGC7457 from Gebhardt et al (2003). The Milky Way is a special case, since the black hole mass is by far the most secure but the uncertainty in the bulge mass (mostly conceptual) is yet quite high.…”

Section: The Samplementioning

confidence: 99%

On the Black Hole Mass-Bulge Mass Relation

Haering¹,

Rix²

2004

ApJ

1,602

174

1,931

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We have re-examined the relation between the mass of the central black holes in nearby galaxies, M bh , and the stellar mass of the surrounding spheroid or bulge, M bulge . For a total of 30 galaxies bulge masses were derived through Jeans equation modeling or adopted from dynamical models in the literature. In stellar mass-to-light ratios the spheroids and bulges span a range of a factor of eight. The bulge masses were related to well-determined black hole masses taken from the literature. With these improved values for M bh , compared to Magorrian et al. (1998), and our redetermination of M bulge , we find the M bh − M bulge relation becomes very tight. We find M bh ∼ M 1.12±0.06 bulge with an observed scatter of 0.30 dex, a fraction of which can be attributed to measurement errors. The scatter in this relation is therefore comparable to the scatter in the relations of M bh with σ and the stellar concentration. These results confirm and refine the work of Marconi and Hunt (2003). For M bulge ∼ 5 × 10 10 M ⊙ the median black hole mass is 0.14% ± 0.04% of the bulge mass.

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Section: The Samplementioning

confidence: 99%

On the Black Hole Mass-Bulge Mass Relation

Haering¹,

Rix²

2004

ApJ

1,602

174

1,931

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“…Both Gebhardt et al (2003) and Schulze & Gebhardt (2011) have estimated the SMBH mass in NGC4697, using HST long-slit observations to model the stellar kinematics. They found a black hole mass of ≈1.6×10 8 M .…”

Section: Targetmentioning

confidence: 99%

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

Davis

Bureau

Onishi

et al. 2017

Monthly Notices of the Royal Astronomical Society

106

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As part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project, we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotating early-type galaxy NGC4697. This estimate is based on Atacama Large Millimeter/submillimeter Array (ALMA) cycle-3 observations of the 12 CO(2-1) emission line with a linear resolution of 29 pc (0. 53). We find that NGC4697 hosts a small relaxed central molecular gas disc with a mass of 1.6×10 7 M , co-spatial with the obscuring dust disc visible in optical Hubble Space Telescope (HST) imaging. We also resolve thermal 1 mm continuum emission from the dust in this disc. NGC4697 is found to have a very low molecular gas velocity dispersion, σ gas =1.65 +0.68 −0.65 km s −1 . This seems to be partially because the giant molecular cloud mass function is not fully sampled, but other mechanisms such as chemical differentiation in a hard radiation field or morphological quenching also seem to be required. We detect a Keplerian increase of the rotation of the molecular gas in the very centre of NGC4697, and use forward modelling of the ALMA data cube in a Bayesian framework with the KIN-EMATIC MOLECULAR SIMULATION (KINMS) code to estimate a SMBH mass of (1.3 +0.18 −0.17 ) ×10 8 M and an i-band mass-to-light ratio of 2.14 +0.04 −0.05 M /L (at the 99% confidence level). Our estimate of the SMBH mass is entirely consistent with previous measurements from stellar kinematics. This increases confidence in the growing number of SMBH mass estimates being obtained in the ALMA era.

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“…Many individual galaxies have been investigated by detailed dynamical modeling of the kinematics of gas, stars, and planetary nebulae (e.g., Tenjes et al 1993;Statler 1994;Statler & Fry 1994;Mathieu & Dejonghe 1999;Gerhard et al 2001;Gebhardt et al 2003;Cappellari et al 2007; Thomas et al 2007;de Lorenzi et al 2009). van den Bosch & van de Ven (2009) investigated how well the intrinsic shape of elliptical galaxies can be recovered by fitting realistic triaxial dynamical models to simulated photometric and kinematic observations.…”

Section: Intrinsic Shape Of Elliptical Galaxiesmentioning

confidence: 99%

Structural properties of disk galaxies

Méndez-Abreu

Simonneau

Aguerri

et al. 2010

A&A

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Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A < 0.9). This fraction is 33%, 55%, and 43% if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C < (A + B)/2). Only 18% of the observed bulges have a probability >50% and none has a probability >90% of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with Sérsic index n > 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T > 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n > 2 and B/T > 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n > 2 and with B/T > 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n > 2 and B/T > 0.3.

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Axisymmetric Dynamical Models of the Central Regions of Galaxies

Cited by 420 publications

References 58 publications

On the Black Hole Mass-Bulge Mass Relation

On the Black Hole Mass-Bulge Mass Relation

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

Structural properties of disk galaxies

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