Do Nuclear Star Clusters and Supermassive Black Holes Follow the Same Host-Galaxy Correlations?
Figure 3
As for Figure 2, but now plotting NSC mass versus total stellar mass (a) and bulge stellar mass (b) (Data and sources in Table 2). Green circles are galaxies with dynamical mass estimates for their NSCs; black diamonds are the spectroscopically estimated masses of Rossa et al. [11] (bulge mass estimates are not complete for these galaxies). Filled symbols indicate galaxies with direct distance measurements (e.g., from Cepheid stars). Arrows show nominal upper limits for three bulgeless spirals (assuming that ). The diagonal black line is a fit of NSC mass to total stellar mass for the dynamical-mass sample (green circles); for comparison, the diagonal dashed red and blue lines are the fits for ellipticals (red) and disk galaxies (blue) from Figure 2. The situation is now the reverse of that for SMBHs: NSC masses clearly correlate better with total galaxy mass than they do with bulge mass.
