Black Hole Mass Scaling Relations for Early-type Galaxies. I. M BH-M ∗, sph and M BH-M ∗,gal

Analyzing a sample of 84 early-type galaxies (ETGs) with directly measured supermassive black hole masses- nearly doubling the sample size of such galaxies with multicomponent decompositions-a symmetric linear regression on the reduced (merger-free) sample of 76 galaxies reveals M-BH proportional to M-*(,sph)1.27 +/- 0.07 with a total scatter of Delta(rms) = 0.52 dex in the log (M-BH) direction. Importantly, however, 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-*,M-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 +/- 0.20 and 1.90 +/- 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(*,gal )ratio in the M-BH-M-*,M-gal diagram where M-BH proportional to M-*(,gal)1.8 +/- 0.2 and Delta(rms) = 0.6 +/- 0.1 dex depending on the sample. For M-BH greater than or similar to 10(7) M-circle dot, we detect no significant bend nor offset in either the M-BH-M-*,M-sph or M-BH-M-*,M-gal relations due to barred versus non-barred, or core-Sersic versus Sersic, ETGs. For reference, the ensemble of late-type galaxies (which invariably are Sersic galaxies) followM(BH)/M-*,M-sph and M-BH-M-*,M-gal relations with slopes equal to 2.16 +/- 0.32 and 3.05 +/- 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.