Black Hole Mass Scaling Relations for Early-Type Galaxies:
  $M_{BH}$-$M_{*,sph}$ and $M_{BH}$-$M_{*,gal}$
  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 $M_{BH}\propto
M_{*,sph}^{1.27\pm 0.07}$ 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 $M_{BH}/M_{*,sph}$ 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 $1.86\pm0.20$ and $1.90\pm0.20$, 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 $M_{BH}$-$M_{*,gal}$ diagram where $M_{BH}\propto
M_{*,gal}^{1.8\pm 0.2}$ 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 $M_{BH}$-$M_{*,sph}$ or $M_{BH}$-$M_{*,gal}$ relations due
to barred versus non-barred, or core-S\'ersic versus S\'ersic, early-type
galaxies. For reference, the ensemble of late-type galaxies (which invariably
are S\'ersic galaxies) follow $M_{BH}$-$M_{*,sph}$ and $M_{BH}$-$M_{*,gal}$
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.
