Axisymmetric Dynamical Models of the Central Regions of Galaxies

By K. Gebhardt, D. Richstone, S. Tremaine, Tod R. Lauer, R. Bender, G. Bower, A. Dressler, S. Faber, A. Filippenko, R. Green and 5 more. 2002

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We present axisymmetric, orbit superposition models for 12 galaxies using data taken with the Hubble Space Telescope (HST) and ground-based observatories. In each galaxy, we detect a central black hole (BH) and measure its mass to accuracies ranging from 10% to 70%. We demonstrate that in most cases the BH detection requires both the HST and ground-based data. Using the ground-based data alone does provide an unbiased measure of the BH mass (provided that they are fitted with fully general models), but at a greatly reduced significance. The most significant correlation with host galaxy properties is the relation between the BH mass and the velocity dispersion of the host galaxy; we find no other equally strong correlation and no second parameter that improves the quality of the mass-dispersion relation. We are also able to measure the stellar orbital properties from these general models. The most massive galaxies are strongly biased to tangential orbits near the BH, consistent with binary BH models, while lower mass galaxies have a range of anisotropies, consistent with an adiabatic growth of the BH.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8eca970af0e6f87cb04e8e8930f3005181d3081d

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Citations in the corpus

Triaxial orbit based galaxy models with an application to the (apparent) decoupled core galaxy NGC 4365 (2007, methodology): “The aim is to measure the mass of the central black holes (van der Marel et al. 1998; Gebhardt et al. 2003; Valluri, Merritt & Emsellem 2004; Valluri et al. 2005; Shapiro et al. 2006; van den Bosch et al. 2006), to deduce the properties of dark haloes (e.g. Rix et al. 1997; Cretton et al. 1999;…”
SECULAR EVOLUTION OF COMPACT BINARIES NEAR MASSIVE BLACK HOLES: GRAVITATIONAL WAVE SOURCES AND OTHER EXOTICA (2012, methodology): “In this study we explore the evolution of binaries in the environments of SMBHs which are thought to reside at the center of most galaxies (e.g. Gebhardt et al. 2000, 2003); throughout this paper we focus on galactic nuclei similar to the Galactic center (GC) of our own galaxy.”
An Intermediate-Mass Black Hole in the Globular Cluster G1: Improved Significance from New Keck and Hubble Space Telescope Observations (2005, methodology): “These are now commonplace and standard (Gebhardt et al. 2000c, 2003; Cappellari et al. 2002; Krajnovic et al. 2005).”
THE BLACK HOLE MASS, STELLAR MASS-TO-LIGHT RATIO, AND DARK HALO IN M87 (2009, methodology): “Humphrey et al. (2008) model NGC 4649, a galaxy similar in mass to M87, using X-ray gas emission and find a black hole that is 2 times larger than the previous stellar dynamical measure of Gebhardt et al. (2003).”
Measuring the Masses of Supermassive Black Holes (2014, methodology): “Several sophisticated computer codes for this have been developed (e.g., Gebhardt et al. 2003; van der Marel et al. 1998; Creeton et al. 1999; Thomas et al. 2004; Valluri, Merritt, & Emsellem 2004).”
Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies (2013, methodology): “The BH mass in NGC 3377 was also measured in Gebhardt et al. (2003).”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, methodology): “This is only slightly larger than calculated by McLure & Dunlop, due to the addition of Cyg A (Tadhunter et al. 2003) and NGC 5845 (Gebhardt et al. 2003), both of which deviate (significantly in the case of Cyg A) from the best fit relation.”
On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies ! (2006, background): “…determination of the mass of the “massive dark objects”, presumably black holes, located at the center of nearby galaxies, via stellar/gas kinematics (Gebhardt et al. 2003), via black hole mass (MBH) and stellar velocity dispersion (Tremaine et al. 2002) or galaxy bulge mass (Richstone et al.…”
The SAURON project – X. The orbital anisotropy of elliptical and lenticular galaxies: revisiting the (V/σ, ɛ) diagram with integral‐field stellar kinematics (2007, methodology): “Similar axisymmetric implementations were developed by other groups (Gebhardt et al. 2003; Valluri et al. 2004; Thomas et al. 2004).”
Selection Bias in Observing the Cosmological Evolution of the M•-σ and M•-L Relationships (2007, methodology): “L relation in detail in Lauer et al. (2007); in brief, we use the Häring & Rix (2004) relation betweenM and galaxy mass, transformed back to luminosity by adopting the mass-to-light ratio M /LV ’ 6 ; 10 0:092(MVþ22) M /L ; based on the M /L estimates given in Gebhardt et al. (2003).”
REVISITING THE SCALING RELATIONS OF BLACK HOLE MASSES AND HOST GALAXY PROPERTIES (2012, background): “Gebhardt et al. (2003) justified classifying the central point source of NGC 7457 as an active galactic nucleus, but their arguments permit the central mass to be shared by an accreting black hole and a nuclear star cluster.”
Ejection of Hypervelocity Stars by the (Binary) Black Hole in the Galactic Center (2003, background): “The Milky Way, as well as most nearby elliptical galaxies and disk galaxies with spheroids, is believed to house a massive black hole (BH) at its center (e.g. Schödel et al. 2002; Genzel et al. 2003; Schödel et al. 2003; Eisenhauer et al. 2003; Ghez et al. 2003a,b,c; Gebhardt et al. 2003).”
DISSECTING THE GRAVITATIONAL LENS B1608+656. II. PRECISION MEASUREMENTS OF THE HUBBLE CONSTANT, SPATIAL CURVATURE, AND THE DARK ENERGY EQUATION OF STATE (2009, result): “These boundaries are consistent with those in Gebhardt et al. (2003).”
Quantifying the coexistence of massive black holes and dense nuclear star clusters (2009, background): “The BH mass for NGC 7457 was derived assuming that the excess central light, above the inward extrapolation of the outer light profile, is AGN flux (Gebhardt et al. 2003).”
Dynamical modelling of luminous and dark matter in 17 Coma early-type galaxies (2007, methodology): “Dynamical studies of samples of elliptical galaxies using this technique are, however, based on kinematical data inside r reff (Gebhardt et al. 2003; Cappellari et al. 2006) and dark matter is not considered.”
THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES (2016, unknown): “6mu = 0.004 NGC2778 M/LV = 8M /L , D=22.9 Mpc from Gebhardt et al. (2003), not corrected for G.E. AV = 0.069, (V −R) = 0.643, (B − V ) = 0.958, (V − r)0 = −0.63(B − V ) + 1.646(V −R) + 0.124−AV NGC2787 M/L3.”
HST STIS Spectroscopy of the Triple Nucleus of M31: Two Nested Disks in Keplerian Rotation around a Supermassive Black Hole (2005, methodology): “We used the regularized maximum entropy method as implemented by Gebhardt et al. (2000a, 2003) and Thomas et al. (2004).”