An interferometric study of B star multiplicity | Astronomy & Astrophysics (A&A)

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Table 1.

Information on the B stars of our sample.

Name	RA	Dec	Hmag	Distance	SpT	Mass	Comments
	(h m s)	(° ′″)		(pc)		(M_⊙)
γ Peg	00:13:14.15	+15:11:00.94	3.43	146 $_{- 11}^{+ 10}$ $^{+10}_{-11}$	B2 IV	8.8±0.3^a	β Cep variable
HD 3379	00:36:47.31	+15:13:54.18	6.275	279 $_{- 6}^{+ 6}$ $^{+6}_{-6}$	B2.5 IV	5.4±0.9^b	β Cep variable
HD 16582	02:39:28.96	+00:19:42.63	4.74	194 $_{- 10}^{+ 9}$ $^{+9}_{-10}$	B2 IV	8.4±0.7^c	β Cep variable
HD 25558	04:03:44.60	+05:26:08.23	5.58	222 $_{- 11}^{+ 12}$ $^{+12}_{-11}$	B5 V	4.6±0.5^d
HD 30836	04:51:12.36	+05:36:18.37	4.09	263 $_{- 18}^{+ 20}$ $^{+20}_{-18}$	B2 III	11.0±1.0^e
HD 32249	05:01:26.35	−07:10:26.27	5.30	277 $_{- 9}^{+ 10}$ $^{+10}_{-9}$	B3 IV	7.0±0.4^e	Orion X
HD 34816	05:19:34.52	−13:10:36.44	4.98	299 $_{- 14}^{+ 18}$ $^{+18}_{-14}$	B0.5 V	15.0±3.5^a
HD 35149	05:22:50.00	+03:32:39.98	5.443	575 $_{- 78}^{+ 119}$ $^{+119}_{-78}$	B2 V	12.5±0.6^f
HD 35337	05:23:30.15	−13:55:38.46	5.80	370 $_{- 11}^{+ 15}$ $^{+15}_{-11}$	B2 IV	9.8±0.6^g

HD 37017	05:35:21.87	−04:29:39.04	6.88	356 $_{- 9}^{+ 8}$ $^{+8}_{-9}$	B1.5 V	6.4±0.5^g
HD 51480	06:57:09.38	−10:49:28.06	5.12	1106 $_{- 25}^{+ 31}$ $^{+31}_{-25}$	Besh	6.4±0.5^h	Be star
HD 66765	08:02:55.72	−48:19:29.95	7.01	372 $_{- 9}^{+ 12}$ $^{+12}_{-9}$	B1.5 V	6.6±1.0ⁱ
HD 67621	08:06:41.61	−48:29:50.59	6.86	355 $_{- 6}^{+ 7}$ $^{+7}_{-6}$	B2 IV	5.5±0.5^h	Vel OB 2 - cluster
HD 105382	12:08:05.23	−50:39:40.58	4.95	109 $_{- 2}^{+ 2}$ $^{+2}_{-2}$	B4 III	5.7±0.4^j	Lower Cen Crux/Sco OB 2-4, Be star
HD 109026	12:32:28.01	−72:07:58.76	4.25	117 $_{- 4}^{+ 4}$ $^{+4}_{-4}$	B3 V	5.0±0.5^h	Pulsating variable
HD 116658	13:25:11.58	−11:09:40.75	1.54	^*77 $_{- 3}^{+ 4}$ $^{+4}_{-3}$	B1 V	11.4±1.2^k	β Cep variable
HD 121743	13:58:16.27	−42:06:02.71	4.46	140 $_{- 6}^{+ 7}$ $^{+7}_{-6}$	B2 IV	8.5±0.3^f	II Sco/Upper Cen Lupus, Variable

HD 132058	14:58:31.93	−43:08:02.27	3.25	^*117 $_{- 2}^{+ 3}$ $^{+3}_{-2}$	B2 III	8.8±0.2^f
HD 133518	15:06:55.97	−52:01:47.24	6.666	602 $_{- 30}^{+ 23}$ $^{+23}_{-30}$	B2 VpHe	6.3±0.5^h
HD 140008	15:42:41.02	−34:42:37.46	5.11	128 $_{- 3}^{+ 3}$ $^{+3}_{-3}$	B5 V	4.5±0.5^h	Upper Cen Lupus/ Sco OB 2-3
HD 147932	16:25:35.08	−23:24:18.79	5.92	122 $_{- 1}^{+ 1}$ $^{+1}_{-1}$	B5 V	5.0±0.5^l	Ass Sco OB 2-2/Upper Sco/Ophiuchus, Rotationally variable
HD 161701	17:47:36.78	−14:43:32.97	5.88	167 $_{- 2}^{+ 1}$ $^{+1}_{-2}$	B9III pHgMn	3.96±0.14^m
HD 178175	19:08:16.70	−19:17:25.05	5.39	414 $_{- 22}^{+ 24}$ $^{+24}_{-22}$	B2 Ve	8.8±0.6ⁿ	Be star
HD 189103	19:59:44.18	−35:16:34.70	4.79	208 $_{- 13}^{+ 14}$ $^{+14}_{-13}$	B3 IV	6.6±0.1^f
HD 191263	20:08:38.28	+10:43:33.11	6.656	441 $_{- 13}^{+ 11}$ $^{+11}_{-13}$	B3 V	6.0±0.5^h

HD 193933	20:23:26.26	−14:15:23.17	7.068	440 $_{- 10}^{+ 10}$ $^{+10}_{-10}$	B5 IV	5.6±0.5^h
HD 205637	21:37:04.83	−19:27:57.65	4.91	269 $_{- 13}^{+ 14}$ $^{+14}_{-13}$	B3 V	8.6±0.5^o	Be star
HD 212076	22:21:31.08	+12:12:18.66	4.803	^*498 $_{- 61}^{+ 81}$ $^{+81}_{-61}$	B2 Ve	12.5±0.7ⁿ	Be star
HD 212571	22:25:16.62	+01:22:38.63	5.37	330 $_{- 11}^{+ 14}$ $^{+14}_{-11}$	B1 III-IVe	10.7±0.7^f	Be star
HD 224990	00:02:19.93	−29:43:13.60	5.41	207 $_{- 5}^{+ 6}$ $^{+6}_{-5}$	B5 V	5.5±0.5^f	Cl Blanco 1 (open galactic cluster)
MCW 1019	22:00:07.93	+06:43:02.81	6.212	453 $_{- 21}^{+ 27}$ $^{+27}_{-21}$	B3 III	6.9±0.7^p
τ Lib	15:38:39.37	−29:46:39.90	4.05	112 $_{- 2}^{3}$ $^{3}_{-2}$	B2.5 V	7.25±0.49^e	II Sco/Upper Cen Lupus

Notes. All distances come from Gaia DR3 (Bailer-Jones et al. 2021), except for the distances with an asterisk, which were determined by HIPPARCOS (Perryman et al. 1997). In the penultimate column, we provide masses from the literature (references as footnotes). Any star without information in the final column is a field star without a parent association in the literature (as reported by the SIMBAD Astronomical Database (Wenger et al. 2000) and Cantat-Gaudin & Anders 2020). References:

^(a)

Nieva & Przybilla (2014),

^(b)

Hubrig et al. (2006),

^(c)

Hubrig et al. (2009),

^(d)

Sódor et al. (2014),

^(e)

Hohle et al. (2010),

^(f)

Tetzlaff et al. (2011),

^(g)

Jin et al. (2024),

^(h)

Kervella et al. (2019),

⁽ⁱ⁾

Cidale et al. (2007),

^(j)

Briquet et al. (2004),

^(k)

Tkachenko et al. (2016),

^(l)

Allen et al. (2018),

^(m)

González et al. (2014),

⁽ⁿ⁾

Zorec et al. (2016),

^(o)

Silaj et al. (2014),

^(p)

Irrgang et al. (2016).

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