Quantitative spectroscopy of late O-type main-sequence stars with a hybrid non-LTE method

Open Access

Table 4

Stellar parameters for the sample stars.

#	Name	T_eff (K)	log(g) (cgs)	y	ξ	υ sin(i)	ζ	E(B − V) (mag)	R_V	B.C. (mag)	M_V (mag)	M_bol (mag)	M/M_⊙	R/R_⊙	log L/L_⊙	log τ_evol (yr)	d_Gaia (a) (pc)	d_spec (pc)

					(km s⁻¹)
2	HD 14633	34000	3.90	0.088	6	125	74	0.09	2.80	−3.05	−4.67	−7.72	23.2	9.0	4.98	6.64	1482	2142
		± 1000	0.10	0.008	2	5	18	0.02	0.10	0.07	0.22	0.21	1.3	1.2	0.08	0.07		253
2a^(b)											−3.74	−6.79	9.8	5.8	4.61	…		…
		±									0.32	0.32	3.0	1.1	0.13	…		…
4	HD 258691	33300	4.02	0.080	8	20	39	0.90	3.35	−3.08	−4.08	−7.16	19.9	7.2	4.76	6.63	1563	1433
		± 500	0.05	0.007	2	6	8	0.04	0.20	0.04	0.10	0.09	0.4	0.5	0.04	0.07		84
5	HD 201345	32000	3.80	0.089	12	91	61	0.18	2.70	−2.97	−4.66	−7.63	21.7	9.7	4.95	6.72	1918	2328
		± 500	0.10	0.007	2	2	10	0.02	0.10	0.04	0.28	0.28	1.8	1.6	0.11	0.02		284
5a^(b)											−4.27	−7.21	14.7	8.0	4.78	…		…
		±									0.32	0.32	4.0	1.5	0.13	…		…
6	HD 57682	33500	3.93	0.082	4	10	33	0.12	3.10	−3.11	−4.40	−7.51	21.7	8.4	4.90	6.65	1115	1228
		± 800	0.05	0.012	2	1	4	0.02	0.10	0.06	0.11	0.09	0.8	0.5	0.04	0.04		74
7	HD 227757	33300	4.04	0.094	8	17	31	0.51	3.10	−3.08	−4.02	−7.10	19.6	7.0	4.73	6.61	2080	2141
		± 400	0.08	0.008	2	4	4	0.02	0.10	0.03	0.20	0.20	0.7	0.8	0.08	0.14		201
8	BD − 134930	32900	4.14	0.093	6	8	23	0.55	3.30	−3.07	−3.63	−6.70	18.0	6.0	4.58	6.49	1664	1786
		± 300	0.05	0.007	2	2	4	0.02	0.10	0.02	0.10	0.10	0.2	0.4	0.04	0.17		104
9	BD + 60499	33800	4.09	0.092	6	19	34	0.83	3.25	−3.13	−3.91	−7.04	19.7	6.6	4.71	6.53	2052	2023
		± 300	0.05	0.007	2	2	2	0.02	0.10	0.02	0.11	0.11	0.3	0.4	0.04	0.11		118
10	BD + 57 247	31200	3.87	0.096	16	16	31	0.63	2.51	−2.91	−4.30	−7.21	19.0	8.4	4.78	6.76	3469	3403
		± 500	0.05	0.010	2	1	5	0.02	0.10	0.04	0.11	0.10	0.5	0.6	0.04	0.03		200
11	HD 207538	31400	3.93	0.089	8	32	42	0.62	2.70	−2.94	−4.12	−7.05	18.4	7.7	4.72	6.75	849	891
		± 500	0.05	0.006	2	3	3	0.02	0.10	0.04	0.10	0.09	0.4	0.5	0.04	0.03		52
13	HD 46202	33900	4.16	0.080	6	11	33	0.55	3.00	−3.14	−3.71	−6.85	19.2	6.0	4.64	6.38	1411	1130
		± 500	0.05	0.008	2	1	4	0.02	0.10	0.04	0.09	0.08	0.4	0.3	0.03	0.23		66
14	HD 38666	33400	4.12	0.096	8	125	42	0.04	3.10	−3.09	−3.78	−6.87	18.9	6.3	4.64	6.49	587	581
		± 300	0.05	0.007	2	8	10	0.02	0.10	0.02	0.11	0.11	0.3	0.4	0.04	0.15		34
16	HD 54879	32200	4.06	0.086	4	0	0	0.36	3.10	−3.02	−3.78	−6.80	17.8	6.5	4.62	6.65	1252	1149
		± 700	0.05	0.008	2	1	1	0.02	0.10	0.05	0.10	0.09	0.6	0.3	0.03	0.10		69
17	HD 214680	34550	4.04	0.083	5	14	32	0.11	3.10	−3.19	−4.17	−7.36	21.6	7.4	4.84	6.55	456	552
		± 300	0.05	0.009	2	1	2	0.02	0.10	0.02	0.12	0.12	0.5	0.5	0.05	0.08		32
18	HD 34078	33200	4.06	0.085	8	9	23	0.56	3.20	−3.08	−3.93	−7.01	19.2	6.8	4.70	6.60	389	418
		± 300	0.05	0.008	2	2	3	0.02	0.10	0.02	0.11	0.11	0.3	0.5	0.04	0.08		24
19	HD 206183	33100	4.06	0.085	4	4	21	0.45	3.10	−3.08	−3.91	−6.99	19.1	6.8	4.69	6.60	921	970
		± 300	0.05	0.006	2	2	4	0.02	0.10	0.02	0.11	0.11	0.3	0.5	0.04	0.08		57
20	HD 36512	32900	4.20	0.087	7	8	26	0.05	3.10	−3.07	−3.45	−6.52	17.5	5.5	4.51	6.29	407	386
		± 600	0.05	0.006	2	4	4	0.02	0.10	0.04	0.09	0.08	0.5	0.3	0.03	0.37		23

Notes. Uncertainties are 1σ values. ^(a)Gaia Collaboration (2016, 2021), distances and uncertainties correspond to inverted EDR3 parallaxes. ^(b) Alternative solution, adopting the Gaia distance instead of the spectroscopic distance. See Sect. 5 for details.

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