The Inner Dynamical Mass Across Galaxy Morphology: A Weak Scaling with
  Total Stellar Mass
  We compile a sample of dispersion-supported and rotation-supported galaxies
for which the dynamical mass enclosed at 500 pc can be measured. We find that
this dynamical quantity increases only slowly with stellar mass
(M$_{total}$(<500pc) $\propto$ M$_{stars}$$^{0.16}$) over ~9 decades in
baryonic mass and ~3 in length scale, with a sudden upturn at the highest
masses (M$_{stars}$ > 10$^{10}$M$_{sun}$). This upturn occurs for the earliest
type (S0 and Sa) disk galaxies, and is consistent with the "extra" mass within
500 pc being predominantly stellar. This sudden change may be indicative of
different bulge formation mechanisms between early and late type disks. We also
compare the data to the results of recent galaxy formation simulations. These
broadly track the observed trend, with some tendency to put too much mass in
the inner 500 pc, depending on the details of each simulation.
