Black Hole Mass Scaling Relations for Early-Type Galaxies: $M_{BH}$-$M_{\ast ,sph}$ and $M_{BH}$-$M_{\ast ,gal}$

Abstract

Analyzing a sample of 84 early-type galaxies with directly-measured super-massive black hole masses---nearly doubling the sample size of such galaxies with multi-component decompositions---a symmetric linear regression on the reduced (merger-free) sample of 76 galaxies reveals $M_{BH}\propto M_{\ast ,sph}^{1.27\pm 0.07}$ with a total scatter of ${\Delta }_{rms}=$ 0.52 dex in the $\log (M_{BH})$ direction. However, and importantly, we discover that the ES/S0-type galaxies with disks are offset from the E-type galaxies by more than a factor of ten in their $M_{BH}/M_{\ast ,sph}$ ratio, with ramifications for formation theories, simulations, and some virial factor measurements used to convert AGN virial masses into $M_{BH}$. Separately, each population follows a steeper relation with slopes of $1.86\pm 0.20$ and $1.90\pm 0.20$, respectively. The offset mass ratio is mainly due to the exclusion of the disk mass, with the two populations offset by only a factor of two in their $M_{BH}/M_{\ast ,gal}$ ratio in the $M_{BH}$-$M_{\ast ,gal}$ diagram where $M_{BH}\propto M_{\ast ,gal}^{1.8\pm 0.2}$ and ${\Delta }_{rms}=0.6\pm 0.1$ dex depending on the sample. For $M_{BH}\gtrsim 10^7{M}_{\odot }$, we detect no significant bend nor offset in either the $M_{BH}$-$M_{\ast ,sph}$ or $M_{BH}$-$M_{\ast ,gal}$ relations due to barred versus non-barred, or core-Sérsic versus Sérsic, early-type galaxies. For reference, the ensemble of late-type galaxies (which invariably are Sérsic galaxies) follow $M_{BH}$-$M_{\ast ,sph}$ and $M_{BH}$-$M_{\ast ,gal}$ relations with slopes equal to $2.16\pm 0.32$ and $3.05\pm 0.70$, respectively. Finally, we provide some useful conversion coefficients, $\upsilon$, accounting for the different stellar mass-to-light ratios used in the literature, and we report the discovery of a local, compact massive spheroid in NGC 5252.

73 pages, 53 figures, and 5 tables, accepted for publication by the Astrophysical Journal (11 March 2019)

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