New constraints on the structure of the nuclear stellar cluster of the Milky Way from star counts and MIR imaging

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Table 2.

Best-fit model parameters for Sérsic fits to the stellar number density maps.

ID	Mag. range	N_e, nsd^(b)	N_e, nsc^(c)	q^(d)	n^(e)	R_e^(f)
	(K_s, extc)	(stars/bin²) ^(a)	(stars/bin²) ^(a)			(pc)
1	12.5−14	2.45 ± 0.10	3.94 ± 0.68	0.85 ± 0.05	2.59 ± 0.27	5.66 ± 0.32
2	9−12	0.55 ± 0.09	1.16 ± 0.26	0.60 ± 0.04	2.28 ± 0.47	4.57 ± 0.78
3	9−14	3.22 ± 0.19	6.55 ± 1.08	0.78 ± 0.02	2.02 ± 0.46	5.38 ± 0.21

Notes. The MWNSC is aligned with respect to GP.

^(a)

The bin size in the density maps is 5″ × 5″.

^(b)

Stellar number density for the NSD at its effective radius (see value in Table 1).

^(c)

Stellar number density for the NSC at the effective radius R_e.

^(d)

The flattening q is equal to the minor axis divided by the major axis.

^(e)

n is the Sérsic index.

^(f)

R_e is the effective radius for the NSC.

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