Revisiting the Scaling Relations of Black Hole Masses and Host Galaxy Properties
Abstract
New kinematic data and modeling efforts in the past few years have substantially expanded and revised dynamical measurements of black hole masses (M _{•}) at the centers of nearby galaxies. Here we compile an updated sample of 72 black holes and their host galaxies, and present revised scaling relations between M _{•} and stellar velocity dispersion (σ), Vband luminosity (L), and bulge stellar mass (M _{bulge}), for different galaxy subsamples. Our bestfitting powerlaw relations for the full galaxy sample are log_{10}(M _{•}) = 8.32 + 5.64log_{10}(σ/200 km s^{1}), log_{10}(M _{•}) = 9.23 + 1.11log_{10}(L/10^{11} L _{⊙}), and log_{10}(M _{•}) = 8.46 + 1.05log_{10}(M _{bulge}/10^{11} M _{⊙}). A logquadratic fit to the M _{•}σ relation with an additional term of β_{2} [log_{10}(σ/200 km s^{1})]^{2} gives β_{2} = 1.68 ± 1.82 and does not decrease the intrinsic scatter in M _{•}. Including 92 additional upper limits on M _{•} does not change the slope of the M _{•}σ relation. When the early and latetype galaxies are fit separately, we obtain similar slopes of 5.20 and 5.06 for the M _{•}σ relation but significantly different intercepts—M _{•} in earlytype galaxies are about two times higher than in late types at a given sigma. Within earlytype galaxies, our fits to M _{•}(σ) give M _{•} that is about two times higher in galaxies with central core profiles than those with central powerlaw profiles. Our M _{•}L and M _{•}M _{bulge} relations for earlytype galaxies are similar to those from earlier compilations, and core and powerlaw galaxies yield similar L and M _{bulge}based predictions for M _{•}. When the conventional quadrature method is used to determine the intrinsic scatter in M _{•}, our data set shows weak evidence for increased scatter at M _{bulge} < 10^{11} M _{⊙} or L_{V} < 10^{10.3} L _{⊙}, while the scatter stays constant for 10^{11} < M _{bulge} < 10^{12.3} M _{⊙} and 10^{10.3} < L_{V} < 10^{11.5} L _{⊙}. A Bayesian analysis indicates that a larger sample of M _{•} measurements would be needed to detect any statistically significant trend in the scatter with galaxy properties.
 Publication:

The Astrophysical Journal
 Pub Date:
 February 2013
 DOI:
 10.1088/0004637X/764/2/184
 arXiv:
 arXiv:1211.2816
 Bibcode:
 2013ApJ...764..184M
 Keywords:

 galaxies: nuclei;
 galaxies: statistics;
 Astrophysics  Cosmology and Nongalactic Astrophysics
 EPrint:
 Final version accepted for publication in ApJ. 15 pages, 5 figures, 3 tables. Our list of black hole masses is available at http://blackhole.berkeley.edu