The Milky Way’s nuclear star cluster: Old, metal-rich, and cuspy - Structure and star formation history from deep imaging

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Volume 641 (September 2020)

A&A, 641 (2020) A102

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Table 3.

Best model fits to the cumulative KLF, considering stellar populations of 16 different ages and different metallicities, with and without spectroscopically confirmed young stars.

Age (Gyr)	0.5 Z_⊙	1 Z_⊙	1.5 Z_⊙	2 Z_⊙	1 Z_⊙ ^(c)	1.5 Z_⊙ ^(c)	2 Z_⊙ ^(c)	1.5 Z_⊙ ^(c)^,^(d)	1.5 Z_⊙ ^(c)^,^(e)	1.5 Z_⊙ ^(c)^,^(f)	Mixed ^(c)^,^(g)
	2.28	0.77	0.83	0.88	0.92	0.70	0.73	0.73	0.60	0.74	1.18
⟨A_{K_s}⟩ ^(a)	2.55	2.45	2.49	2.50	2.50	2.52	2.55	2.50	2.52	2.51	2.53
FWHM_smooth ^(b)	3.48	3.18	3.48	3.72	2.84	2.64	2.91	2.41	2.36	2.27	4.09

13	0.445	0.823	0.745	0.680	0.795	0.821	0.748	0.833	0.729	0.805	0.000
11	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000
9	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.652
7	0.000	0.000	0.105	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000
6	0.368	0.000	0.000	0.165	0.010	0.000	0.084	0.000	0.000	0.000	0.116
5	0.101	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000
4	0.000	0.000	0.000	0.023	0.000	0.000	0.000	0.000	0.000	0.086	0.000
3	0.000	0.15	0.124	0.102	0.144	0.131	0.116	0.127	0.187	0.067	0.129
2	0.050	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000	0.000
1	0.000	0.000	0.000	0.000	0.013	0.002	0.002	0.014	0.013	0.002	0.000
0.8	0.000	0.000	0.000	0.000	0.000	0.005	0.003	0.000	0.000	0.000	0.000
0.5	0.009	0.004	0.004	0.006	0.003	0.035	0.039	0.020	0.036	0.035	0.005
0.25	0.008	0.009	0.008	0.009	0.003	0.002	0.001	0.003	0.004	0.001	0.015
0.15	0.003	0.001	0.002	0.003	0.000	0.000	0.000	0.000	0.000	0.000	0.003
0.1	0.000	0.007	0.004	0.006	0.000	0.000	0.002	0.000	0.000	0.000	0.000
0.08	0.015	0.000	0.003	0.003	0.006	0.003	0.002	0.002	0.005	0.002	0.013
0.03	0.001	0.005	0.004	0.004	0.001	0.002	0.002	0.001	0.002	0.002	0.004

Notes. The columns after line 4 list the fraction of the total initially formed stellar mass corresponding to each age.

^(a)

Mean extinction.

^(b)

FWHM of Gaussian smoothing parameter in units of bins.

^(c)

Spectroscopically identified young stars excluded.

^(d)

Assumption of top heavy IMF.

^(e)

Fit limited to magnitudes brighter than K_s = 18.75.

^(f)

Fit limited to magnitudes brighter than K_s = 19.25.

^(g)

Assumption of mean metallicity [Fe/H] = 0.5 solar for stars older than 10 Gyr, [Fe/H] = 1.5 solar for younger stars.

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