Research Article
Are Nuclear Star Clusters the Precursors of Massive Black Holes?
Table 2
Sample of galaxies for which new properties were derived in this paper.
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Galaxies for group 1 are from W05, and we here derived upper limits on the black hole mass and Sersic . Galaxies for groups 2 and 3 are from Gultekin et al. [76]. For group 2 objects we derived upper limits on the NC mass via dynamical arguments, while for group 3 objects we used photometry to derive upper limits. For groups 2 and 3 Sersic values are taken from Graham and Driver [33], bulge masses are from Hring and Rix [3], and velocity dispersions are from Hyperleda. The newly derived quantities are marked with an at the top of the respective column. References for black hole masses are. (1) this work, (2) Gebhardt and Thomas [78], Gebhardt et al. [109], (3) Bower et al. [110], (4) Rusli et al. [83], (5) Devereux et al. [84], (6) Ferrarese et al. [82], (7) Gebhardt et al. [111], (8) De Francesco et al. [88], (9) Sarzi et al. [112], (10) Gebhardt et al. [90]; Shapiro et al. [113], and (11) Cretton and van den Bosch [89]. |