Stellar wind properties of the nearly complete sample of O stars in the low metallicity young star cluster NGC 346 in the SMC galaxy

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Volume 666 (October 2022)

A&A, 666 (2022) A189

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Table 5

Model Parameters derived for O stars within sample with a UV spectrum.

SSN	MPG	v sin i (km s⁻¹)	T_* (kK)	log g (cgs)	log L (L_⊙)	E(B−V) (mag)	ξ_min (km s⁻¹)	(M_⊙ yr⁻¹)	v_∞ (km s⁻¹)	D	β	Comment
9	355	130⁽²⁾	51.7	4.0	6.12	0.13	35	−6.65	2800	200	0.8	MSB
13	324	≥113⁽²⁾	42.0	3.8	5.60	0.11	15⁽¹⁾	−7.4	≥2300	20	1.0	SB1 ⁽²⁾, MSB
14	470	145	37.0	4.4	5.37	0.16	5	−9.5	≥600	20	1.0	MSB
15	368	58⁽²⁾	39.0	4.0	5.45	0.12	15⁽¹⁾	−7.6	≥2100	20	1.0	SB1 ⁽²⁾, MSB
17	396	196	37.0	4.0	5.30	0.11	10	−8.7	≥1000	1	0.8	MSB
18	487	131	37.0	4.4	5.25	0.15	5	−8.45/≤−9.1^(*)	≥1500	5	1.0
22	476	100	38.0	4.0	5.32	0.13	10	−8.2	≥1600	5	0.8
31	417	98⁽²⁾	37.0	4.4	5.09	0.12	10	−8.9	≥1000	10	0.8	MSB
33	467	87	34.0	4.2	4.97	0.14	5	≤−9.5	3210^(†)	10	0.8	SB1 ⁽²⁾, MSB
34	370	158⁽²⁾	33.0	4.2	4.97	0.13	5	≤−9.8	2820^(†)	10	0.8	SB1 ⁽²⁾, MSB
36	495	87⁽²⁾	33.0	4.2	4.86	0.11	5	≤−9.9	2710^(†)	10	0.8	SB1 ⁽²⁾, MSB
43	481	119	32.3	4.4	4.82	0.12	5	≤−10.0	3460^(†)	10	0.8
46	500	316⁽²⁾	37.0	4.4	4.91	0.15	10	≤−9.1	3140^(†)	10	0.8	MSB
57	455	120⁽²⁾	33.0	4.2	4.89	0.14	5	≤−9.9	2850^(†)	10	0.8
59	375	115	32.5	4.2	4.66	0.11	5	≤−9.8	2460^(†)	10	0.8
62	468	113	35.0	4.2	4.74	0.12	5	≤−9.8	2370^(†)	10	0.8
83	429	112	32.0	4.2	4.53	0.12	5	≤−10.0	2210^(†)	10	0.8
105	486	120	32.0	4.2	4.40	0.12	5	≤−10.0	2140^(†)	10	0.8
110	499	100	33.0	4.2	4.58	0.17	5	≤−10.0	2430^(†)	10	0.8

References. (1) Bouret et al. (2003); (2) Dufton et al. (2019).

Notes. SSN 9-SSN 31 are derived from model fits. SSN 33-SSN 110 mass-loss rates are upper limits. ^(†)v_∞ is scaled from v_esc. ^(*)Higher value from G140L low resolution spectrum extraction. Lower value from E140M spectrum, see Sect. 4.3. MUSE Spectral Binary (MSB) are candidate spectroscopic binaries based on observed RV shifts in MUSE observations (Rickard et al., in prep.). SB1, SB2, and SB3 are spectral binaires with one set of photospheric lines observed to be variable, while SB2 and SB3 have sets of lines with 2 and 3 different RV variations respectively.

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