Are Nuclear Star Clusters the Precursors of Massive Black Holes?

Table 2

Sample of galaxies for which new properties were derived in this paper.

Galaxy	Type	𝜎 (km/s)	Dist (𝑀pc)	𝑀BH (𝑀⊙)	𝑀NC (𝑀⊙)	Sersic 𝑛	𝑀Bulge (𝑀⊙)	Ref
group 1				×
NGC 300	SAd	13±2	2.2	<1×10^2	1×10^6	1.1	—	[105]
NGC 428	SABm	24.4±4	16.1	<3 ×10^4	3×10^6	1.05	—	[105]
NGC 1042	SABcd	32±5	18.2	<2.5×10^4	3×10^6	1.15	—	[105]
NGC 1493	SBcd	25±4	11.4	<2.5×10^5	2×10^6	2.36	—	[105]
NGC 2139	SABcd	17± 3	23.6	<1.5×10^5	8×10^5	1.53	—	[105]
NGC 3423	SAcd	30 ±5	14.6	<1.5×10^5	3×10^6	1.20	—	[105]
NGC 7418	SABcd	34± 5	18.4	<1.5×10^5	6×10^7	—	—	[105]
NGC 7424	SABcd	16±2	10.9	<1.5×10^5	1×10^6	0.91	—	[105]
NGC 7793	SAd	25±4	3.3	<5×10^3	8×10^6	1.27	—	[105]
group 2					×
NGC 4486	E1	375±18	17.0	6.3×10^9	<2×10^8	6.86	6.0×10^11	[68]
NGC 4374	E1	296±14	17.0	1.5×10^9	<6.3×10^7	5.60	3.6×10^11	[41]
NGC 1332	S0	321±14	19.6	1.45×10^9	<1.4×10^7	—	—	[60]
NGC 3031	Sb	143±7	4.1	8×10^7	<7×10^6	3.26	—	[37]
NGC 4261	E2	315±15	33.4	5×10^8	<1.7×10^6	7.30	3.6×10^11	[70]
group 3					×
NGC 4649	E2	385±19	16.5	2.1×10^9	<2×10^6	6.04	4.9×10^11	[103]
NGC 3998	S0	305±15	14.9	2.4×10^8	<8.5×10^5	—	—	[98]
NGC 2787	SB0	189±9	7.9	0.7×10^8	<1.9×10^6	1.97	—	[95]
NGC 3379	E0	206±10	11.7	1.2×10^8	<1.4×10^4	4.29	6.8×10^10	[108]
NGC 4342	S0	225±11	18.0	3.6×10^8	<2.5×10^6	5.11	1.2×10^10	[13]
NGC 4291	E2	242±12	25.0	3.2×10^8	<5×10^6	4.02	1.3×10^11	[103]

Galaxies for group 1 are from W05, and we here derived upper limits on the black hole mass and Sersic 𝑛. 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 𝑀_𝑁𝐶 upper limits. For groups 2 and 3 Sersic 𝑛 values are taken from Graham and Driver [33], bulge masses are from Häring 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].