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Table 5

Companions of the ONC targets.

Star Component Sep./Period SpT Mass Detection method Comp. detect. limits Reference/Comment
[′′]/days [M] AMBER

θ1 Ori C C1 O5.5  ~38  ~4 M 2, 5
2–240 mas
C2 0.040′′  ~5 speckle interferometry 5, this paper
C3 0.002′′  ~1 spectroscopy 11, 12
C4  ~1.4 spectroscopy 10
C5 28 d around C4  ~1.3 spectroscopy 10
θ1 Ori A A1 B0.5  ~20  ~3 M 6
3–280 mas
A2 0.2′′  ~4 AO 2, 3, 4, this paper
A3 65 d  ≈ 1.5 mas A0  ~4 spectroscopy 1, 13, 14, 15, 16
θ1 Ori D D1 B0.5  ~3 M 4
2–240 mas
D2 1.401′′ AO 4
D3 0.0184′′ interferometry 4, this paper
D4 40 d spectroscopy 22, this paper
θ2 Ori A A1a O9.5  ~25  ~3.5 M 6, 7
2–140 mas
A1b 21 d,  ≈ 1 mas  ~9 spectroscopic 8, 17
A2 0.38′′  ~7 AO 7, 18
NU Ori Aa B1  ~2.7 M 6
2–150 mas
Ab 8–19 d  ≈ 0.4−0.8 mas  ~3 spectroscopic 6, 8, 17
B 0.47′′  ~1 AO 9
C  ~0.015′′ interferometry this paper
V* T Ori Aa A3  ~2.2 M 9
2–200 mas
Ab 14.3 d spectroscopy 20, 21
B 0.84′′ spectroscopy 19

Notes. As the observational limits for detectable companions change with the brightness of the primary target and the used baseline configuration, in row 7 the limits for each of the observed sample stars are given. The mass is the minimum required mass of the companion as obtained from the Siess et al. (2000) models for an age of 106 yrs to be able to be clearly detected. Below the range of separations covered by the observations is given.

References. (1) Bossi et al. (1989); (2) Schertl et al. (2003); (3) Petr et al. (1998); (4) (1) Close et al. (2012); (5) Kraus et al. (2009); (6) Stelzer et al. (2005); (7) Preibisch et al. (1999); (8) Morrell & Levato (1991); (9) Köhler et al. (2006); (10) Vitrichenko et al. (2011); (11) Lehmann et al. (2010); (12) Vitrichenko et al. (2012); (13) Vitrichenko & Plachinda (2001); (14) Vitrichenko et al. (1998); (15) Lohsen (1975); (16) Lohsen (1976); (17) Abt et al. (1991); (18) Mason et al. (2009), (19) Wheelwright et al. (2010); (20) Shevchenko & Vitrichenko (1994); (21) Corporon & Lagrange (1999); (22) Vitrichenko (2002).

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