Growing a nuclear star cluster from star formation and cluster mergers: The JWST NIRSpec view of NGC 4654

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Volume 687 (July 2024)

A&A, 687 (2024) A83

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Table 1.

Properties of the three clusters.

	R_proj	v_*	σ	A_V, spec	r_eff	log(age)	[M/H]	log(M_*)
	(pc)	(km s⁻¹)	(km s⁻¹)	(mag)	(pc)	log(yr)	(dex)	log(M_⊙)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)
Cluster 1	–	1068.3 ± 3.6	44.0 ± 4.4	1.20	9.17 ± 1.15	9.92 $_{- 0.26}^{+ 0.14}$ $^{+0.14}_{-0.26}$	0.16 $_{- 0.26}^{+ 0.15}$ $^{+0.15}_{-0.26}$	7.52 $_{- 0.14}^{+ 0.10}$ $^{+0.10}_{-0.14}$
Cluster 2	31.8	1073.0 ± 4.1	18.8 ± 10.9	1.26	3.39 ± 0.63	6.71 $_{- 0.04}^{+ 0.12}$ $^{+0.12}_{-0.04}$	0.31 $_{- 0.20}^{+ 0.06}$ $^{+0.06}_{-0.20}$	5.10 $_{- 0.05}^{+ 0.10}$ $^{+0.10}_{-0.05}$
Cluster 3	21.0	1060.0 ± 7.1	33.4 ± 13.6	1.24	2.52 ± 0.58	6.52 $_{- 0.39}^{+ 0.10}$ $^{+0.10}_{-0.39}$	–	4.59 $_{- 0.06}^{+ 0.06}$ $^{+0.06}_{-0.06}$

Notes. (1): Cluster identifier as in Fig. 1. (2) Projected distance from cluster 1. (3) and (4) Line-of-sight velocity and dispersion from fitting the NIRSpec spectrum. We note that the dispersions for cluster 2 and 3 are not reliable as they are below the NIRSpec resolution. (5) Extinction in the V-band as derived from the Paschen decrement. (6) Effective radius from IMFIT modelling of the F555W image. (7)–(9) Mass-weighted properties of the bestfitting BAGPIPES SED models.

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