From gas to stars: MUSEings on the internal evolution of IC 1613

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Volume 689 (September 2024)

A&A, 689 (2024) A88

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Table 4.

Results from the Bayesian kinematic analysis performed for each pointing and stellar type applying a dispersion-only model.

Sample		N_P	${\bar{v}}_{Field}$ $\bar{v}_{\mathrm{Field}}$	σ_v
			(km s⁻¹)	(km s⁻¹)
	F1	410	−231.3 ± 0.7	$12 . 1_{- 0.5}^{+ 0.6}$ $12.1^{+0.6}_{-0.5}$
Main	F2	274	−236.2 ± 0.7	9.0 ± 0.6
	F3	62	−234.5 ± 1.3	$8 . 2_{- 1.0}^{+ 1.2}$ $8.2^{+1.2}_{-1.0}$
	Total	746
	F1	331	−230.6 ± 0.7	12.2 ± 0.6
RGS	F2	230	−236.1 ± 0.8	9.3 ± 0.6
	F3	54	−234.4 ± 1.4	$8 . 6_{- 1.1}^{+ 1.2}$ $8.6^{+1.2}_{-1.1}$
	Total	615	–	11.2 ± 0.4
	F1	79	$- 234 . 9_{- 1.6}^{+ 1.6}$ $-234.9^{+1.6}_{-1.6}$	$11 . 8_{- 1.3}^{+ 1.5}$ $11.8^{+1.5}_{-1.3}$
MS	F2	44	−237.3 ± 1.6	$6 . 2_{- 1.6}^{+ 2.0}$ $6.2^{+2.0}_{-1.6}$
	F3	8	$- 236 . 6_{- 2.8}^{+ 4.2}$ $-236.6^{+4.2}_{-2.8}$	$5 . 2_{- 3.2}^{+ 5.2}$ $5.2^{+5.2}_{-3.2}$
	Total	131	–	$10 . 2_{- 1.0}^{+ 1.1}$ $10.2^{+1.1}_{-1.0}$
	F1	84	−230.9 ± 1.3	$11 . 3_{- 0.9}^{+ 1.0}$ $11.3^{+1.0}_{-0.9}$
RGB-MR	F2	44	−237.0 ± 1.4	$8 . 1_{- 1.1}^{+ 1.3}$ $8.1^{+1.3}_{-1.1}$
	F3	10	$- 237 . 5_{- 1.5}^{+ 1.7}$ $-237.5^{+1.7}_{-1.5}$	$3 . 5_{- 1.4}^{+ 1.8}$ $3.5^{+1.8}_{-1.4}$
	Total	138	–	10.3 ± 0.7
	F1	70	$- 229 . 1_{- 1.6}^{+ 1.7}$ $-229.1^{+1.7 }_{-1.6}$	$13 . 0_{- 1.2}^{+ 1.3}$ $13.0^{+1.3}_{-1.2}$
RGB-MP	F2	50	$- 236 . 8_{- 1.4}^{+ 1.5}$ $-236.8^{+1.5 }_{-1.4}$	$9 . 6_{- 1.1}^{+ 1.3}$ $9.6^{+1.3}_{-1.1}$
	F3	17	$- 231 . 8_{- 3.1}^{+ 2.9}$ $-231.8^{+2.9}_{-3.1}$	$11 . 6_{- 2.2}^{+ 2.7}$ $11.6^{+2.7}_{-2.2}$
	Total	137	–	$12 . 0_{- 0.8}^{+ 0.9}$ $12.0^{+0.9}_{-0.8}$

Notes. The results refer to the main sample, as well as to the subsamples of RGS and MS stars defined in Sect. 4.3, and to the MP and MR subsamples of RGB stars with metallicity measurements defined in Sect. 6.1. The values of the kinematic parameters and their associated uncertainties were calculated as reported in Table 3.

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