Investigating episodic mass loss in evolved massive stars - III. Spectroscopy of dusty massive stars in three northern galaxies

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Volume 698 (May 2025)

A&A, 698 (2025) A279

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Table 4

Stellar parameters of the RSG sample.

ID	Spectral Class.	S/N	Flags^(a)	T_eff,TiO (K)	E(B − V) (mag)	log g (dex)	v_rad (km s⁻¹)	log (L/L_⊙) (dex)	R/R_⊙
NGC 6822-52	M4–M6 I:	61	1, 2	3350 ± 50	0.30 ± 0.01	0.98 ± 0.01	−55 ± 6	5.10 ± 0.06	$1050_{- 100}^{+ 110}$ $\[1050_{-100}^{+110}\]$
NGC 6822-55	K5–M0 I	23	−	3960 ± 50	0.20 ± 0.02	0.2 ± 0.2	−79 ± 6	5.21 ± 0.05	850 ± 70
NGC 6822-66	M0–M2 I	54	−	3740 ± 50	0.14 ± 0.01	0.05 ± 0.08	−79 ± 3	5.19 ± 0.05	940 ± 80
NGC 6822-70	M2–M4 I	51	−	3510 ± 50	0.24 ± 0.01	0.06 ± 0.09	−32 ± 4	5.01 ± 0.05	$860_{- 70}^{+ 80}$ $\[860_{-70}^{+80}\]$
NGC 6822-103	M0–M2 I	41	−	3680 ± 50	0.16 ± 0.01	−0.07 ± 0.09	85 ± 1	5.01 ± 0.05	$790_{- 60}^{+ 70}$ $\[790_{-60}^{+70}\]$
NGC 6822-151	K5–M0 I:	69	4	3750 ± 50	0.10 ± 0.01	−0.44 ± 0.04	−169 ± 3	−	−
NGC 6822-175	M2–M4 I:	52	2	3530 ± 50	0.19 ± 0.01	0.8 ± 0.1	−20 ± 4	4.81 ± 0.05	670 ± 60
NGC 6822-248	M2–M4 I	46	−	3420 ± 50	0.39 ± 0.01	0.70 ± 0.13	0 ± 6	4.46 ± 0.04	480 ± 40
NGC 6822-407	M2–M4 I:	7	4	3510 ± 50	0.12 ± 0.05	${0.7}_{- 0.4}^{+ 0.2}$ $\[0.7_{-0.4}^{+0.2}\]$	56 ± 23	−	−
NGC 6822-R10	M0–M2 I	14	−	3610 ± 50	0.43 ± 0.02	0.3 ± 0.3	61 ± 13	−	−
IC10-5545	K0–K5 I	14	−	4250 ± 100	0.74 ± 0.05	$- {0.3}_{- 0.1}^{+ 0.2}$ $\[-0.3_{-0.1}^{+0.2}\]$	−520 ± 15	4.61 ± 0.06	$370_{- 40}^{+ 50}$ $\[370_{-40}^{+50}\]$
IC10-5660A	M4–M6 I:	48	3	3450 ± 50	0.45 ± 0.01	0.4 ± 0.1	−170 ± 5	5.27 ± 0.06	1210 ± 120
IC10-5660B^(b)	M0–M2 I:	25	−	3530 ± 50	0.44 ± 0.02	0.5 ± 0.2	−302 ± 9	5.27 ± 0.06	1160 ± 90
IC10-9165A	M4–M6 I:	53	3	3360 ± 50	0.94 ± 0.01	0.7 ± 0.1	−140 ± 6	5.26 ± 0.03	1260 ± 80
IC10-9165B^(b)	M0–M2 I	16	−	3510 ± 50	1.31 ± 0.04	0.5 ± 0.3	−336 ± 12	5.26 ± 0.03	1150 ± 70
IC10-20296	M2–M4 I:	16	2, 4	3400 ± 50	0.84 ± 0.06	${0.92}_{- 0.14}^{+ 0.06}$ $\[0.92_{-0.14}^{+0.06}\]$	−455 ± 21	4.13 ± 0.07	$330_{- 30}^{+ 40}$ $\[330_{-30}^{+40}\]$
IC10-26089	K0–K5 I	36	−	4250 ± 50	1.04 ± 0.01	$- {0.44}_{- 0.04}^{+ 0.07}$ $\[-0.44_{-0.04}^{+0.07}\]$	−240 ± 5	5.28 ± 0.04	800 ± 60
IC10-26929	M4–M6 I:	47	2,3	$3330_{- 30}^{+ 50}$ $\[3330_{-30}^{+50}\]$	1.05 ± 0.01	${0.97}_{- 0.05}^{+ 0.02}$ $\[0.97_{-0.05}^{+0.02}\]$	−181 ± 8	−	−
IC10-35694^(b)	M0–M2 I	22	−	3530 ± 50	0.67 ± 0.02	0.2 ± 0.2	−317 ± 9	−	−
IC10-52406^(b)	M0–M2 I	18	−	3420 ± 50	1.71 ± 0.04	−0.1 ± 0.2	−435 ± 11	5.07 ± 0.03	$980_{- 60}^{+ 70}$ $\[980_{-60}^{+70}\]$
IC10-63627^(b)	M0–M2 I	25	−	3650 ± 50	0.83 ± 0.02	0.2 ± 0.2	−384 ± 8	5.35 ± 0.03	$1180_{- 70}^{+ 80}$ $\[1180_{-70}^{+80}\]$
IC10-66828^(b)	M0–M2 I:	38	1,2	3670 ± 50	0.10 ± 0.01	${0.96}_{- 0.06}^{+ 0.03}$ $\[0.96_{-0.06}^{+0.03}\]$	−355 ± 6	−	−
IC10-66981^(b)	M0–M2 I:	10	4	3550 ± 50	0.69 ± 0.04	0.4 ± 0.4	−353 ± 25	−	−
IC10-R3^(b)	M0–M2 I:	69	2	3630 ± 50	0.23 ± 0.01	1.00 ± 0.01	−167 ± 3	4.05 ± 0.08	270 ± 30
IC10-R10	M0–M2 I:	11	4	3480 ± 50	0.85 ± 0.05	0.4 ± 0.4	$- 402_{- 28}^{+ 27}$ $\[-402_{-28}^{+27}\]$	−	−
IC10-R16	K5–M0 I:	9	4	3600 ± 50	0.88 ± 0.07	0.1 ± 0.5	−390 ± 40	−	−
IC10-R17	M2–M4 I:	18	4	3420 ± 50	0.36 ± 0.02	$- {0.43}_{- 0.05}^{+ 0.10}$ $\[-0.43_{-0.05}^{+0.10}\]$	−216 ± 15	−	−
IC10-R20	M0–M2 I:	12	2, 4	3620 ± 50	0.82 ± 0.05	0.70 ± 0.3	−480 ± 30	−	−
IC1613-23465^(b)	M0–M2 I:	44	2, 4	3540 ± 50	0.17 ± 0.01	1.00 ± 0.01	−244 ± 5	4.35 ± 0.09	$400_{- 50}^{+ 60}$ $\[400_{-50}^{+60}\]$
IC1613-28306^(b)	GK I	41	−	4380 ± 50	0.09 ± 0.01	0.23 ± 0.09	−278 ± 4	4.06 ± 0.09	$190_{- 20}^{+ 30}$ $\[190_{-20}^{+30}\]$

Notes. Reported uncertainties are 68.3% confidence level errors. The v_rad of the MOS spectra have systematic uncertainties of ~60 km s⁻¹. The ending A/B in the ID indicates different observations of the same source. ^(a)Flags: (1) bad fit to spectrum, star too cool, parameters unreliable. (2) log g near the edge of the grid, lower limit. (3) acceptable fit, reliable parameters, but to be interpreted with caution. (4) bad fit to Ca II triplet, surface gravity unreliable. ^(b)Long-slit spectra. ^(c)The high S/N, high log g, and low luminosity suggest a foreground nature for this star.

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