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

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Table 2.

Details on the multiplicity of the systems derived from the best-fitting datasets.

Name	Type	χ_red²	F₂	ρ₂	F₃	ρ₃	3-σ
							detection
				(mas)		(mas)	distribution
HD 16582	Single	0.34					0.002 – 0.011
HD 51480*		1.72					0.22 – 1.02
HD 66765		0.54					0.016 – 0.098
HD 67621		0.34					0.005 – 0.021
HD 121743		0.31					0.005 – 0.041
HD 189103		0.56					0.004 – 0.023
HD 205637		1.21					0.005 – 0.073
HD 212571		0.37					0.008 – 0.025
MCW 1019		2.59					0.047 – 0.120

γ Peg	Binary	0.11	0.036 $_{- 0.004}^{+ 0.001}$ $^{+0.001}_{-0.004}$	85.6±0.1			0.026 – 0.330
HD 3379		0.25	0.159 $_{- 0.002}^{+ 0.002}$ $^{+0.002}_{-0.002}$	8.49±0.03			0.005 – 0.018
HD 25558		3.15	0.793 $_{- 0.03}^{+ 0.05}$ $^{+0.05}_{-0.03}$	92.56±0.20			0.020 – 0.088
HD 30836		0.99	0.060 $_{- 0.02}^{+ 0.04}$ $^{+0.04}_{-0.02}$	3.39±0.43			0.010 – 0.073
HD 32249		16.22	0.616±0.01	31.49±0.04			0.071 – 0.278
HD 34816		0.77	0.049 $_{- 0.003}^{+ 0.004}$ $^{+0.004}_{-0.003}$	62.7±0.1			0.026 – 0.084
HD 35337		0.37	0.038 $_{- 0.002}^{+ 0.002}$ $^{+0.002}_{-0.002}$	9.84±0.16			0.037 – 0.127
HD 35149		0.92	0.537±0.008	23.34±0.09			0.427 – 1.23
HD 37017		0.26	0.16 $_{- 0.01}^{+ 0.02}$ $^{+0.02}_{-0.01}$	1.00±0.05			0.157 – 0.756
HD 105382		3.79	0.066 $_{- 0.005}^{+ 0.003}$ $^{+0.003}_{-0.005}$	41.9±0.5			0.102 – 0.397
HD 109026		0.15	0.376 $_{- 0.001}^{+ 0.002}$ $^{+0.002}_{-0.001}$	12.94±0.02			0.003 – 0.014
HD 133518		0.45	0.085 $_{- 0.067}^{+ 0.377}$ $^{+0.377}_{-0.067}$	0.61±3.74			0.019 – 0.057
HD 140008		0.22	0.952 $_{- 0.003}^{+ 0.002}$ $^{+0.002}_{-0.003}$	1.130±0.006			0.398 – 0.938
HD 178175		0.32	0.0245 $_{- 0.001}^{+ 0.0006}$ $^{+0.0006}_{-0.001}$	4.76±0.06			0.006 – 0.017
HD 191263		0.48	0.39 $_{- 0.01}^{+ 0.14}$ $^{+0.14}_{-0.01}$	1.67±0.09			0.014 – 0.073
HD 212076		0.46	0.28 $_{- 0.3}^{+ 0.4}$ $^{+0.4}_{-0.3}$	0.42±2.60			0.013 – 0.092
HD 224990		0.62	0.270 $_{- 0.003}^{+ 0.002}$ $^{+0.002}_{-0.003}$	33.4±0.1			0.015 – 0.054
τ Lib		2.11	0.11 $_{- 0.01}^{+ 0.02}$ $^{+0.02}_{-0.01}$	7.62±0.2			0.066 – 0.693

HD 116658	Triple	2.15	0.08 $_{- 0.01}^{+ 0.03}$ $^{+0.03}_{-0.01}$	0.99±0.30	0.21±0.01	1.69±0.20	0.047 – 0.178
HD 132058		0.21	0.0213±0.002	6.5624±0.1	0.012 $_{- 0.002}^{+ 0.002}$ $^{+0.002}_{-0.002}$	73.7±0.2	0.009 – 0.050
HD 147932		0.55	0.1122 $_{- 0.003}^{+ 0.004}$ $^{+0.004}_{-0.003}$	6.70±0.1	0.028±0.003	83.0±0.3	0.015 – 0.051
HD 161701		0.11	0.219±0.002	1.15±0.1	0.052±0.003	2.89±0.06	0.016 – 0.090
HD 193933		0.11	0.624±0.1	6.17±0.02	0.021 $_{- 0.005}^{+ 0.003}$ $^{+0.003}_{-0.005}$	16.5±0.6	0.007 – 0.037

Notes. F represents the flux ratio of the components with relation to the brightest components (whose flux was set to one as a reference point). The subscript number represents whether the companion is a binary (2) or tertiary (3) and so on. The best-fitting datasets are presented, quantified by the reduced chi-square, χ_red². Systems marked with asterisks are discussed in Section 3.4. We include the distribution of 3σ detections in terms of the flux ratio in the last column.

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