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Table 3

Objects in our FORS 2 sample with available X-ray observations.

Object Spectral LX Adopted References Comments
type distance
[1031 erg s-1] [kpc]

BD 12° 4982 B0 II 1 1.5 1
HD 110432 B2 pe 40 0.37 2, 3 γ Cas-analog
HD 120324 B2 Vnpe 0.06 0.115 4
HD 120991 B2 IIne 30 0.83 4, 5 γ Cas-analog?
HD 164816 O9.5 V + B0 V 3 6 6 X-ray pulsations
HD 165052 O7 Vz + O7.5 Vz 300 1.2 7 colliding wind binary
HD 166033 B1 V 800 1.5 4, 8
HD 315032 B2 Vne 10 1.2 9
HD 345439 B1/B2 V <0.05 1.5 10 σ Ori E-analog

CPD -59° 2624 O9.5 V 1.9 2.3 11
HD 37020 B0.5 V 25 0.45 12
HD 46056 O8 V 32.5 1.4 13
HD 46106 O9.7 III 0.9 1.4 13
HD 46149 O8.5 V((f)) 1.1 1.4 13
HD 46150 O5 V((f)) 22 1.4 13
HD 46202 O9 V((f)) 1.3 1.4 13
HD 46223 O4 V((f)) 24 1.4 13
HD 46328 B0.7 IV 3 0.42 14 X-ray pulsations
HD 60848 O8:V: 0.13 0.5 15
HD 93027 O9.5 IV 1.3 2.3 11
HD 93521 O9 Vp 1.1 1.2 16
HD 101008 B1 II/III 3 2.3 17
HD 117357 O9.5/B0 V 20 7 18
HD 125823 B7 IIIpv 0.005 0.14 19
HD 152246 O9 IV 14 1.6 20 triple

Notes. Distances and the interstellar absorption column density – used to derive LX – are estimated on the basis of UBV photometry, or taken from the literature.

Reference. (1) De Becker et al. (2005); (2) Motch et al. (2015); (3) Torrejón et al. (2012); (4) Oskinova et al. (in prep.); (5) Frémat et al. (2002); (6) Trepl et al. (2012); (7) Pittard & Parkin (2010); (8) Dahm et al. (2012); (9) Damiani et al. (2004); (10) Eikenberry et al. (2014); (11) Nazé et al. (2011); (12) Stelzer et al. (2005); (13) Wang et al. (2008); (14) Oskinova et al. (2014); (15) Rauw et al. (2013); (16) Rauw et al. (2012); (17) Nazé et al. (2013); (18) Beer (1961); (19) Nazé et al. (2014); (20) Nasseri et al. (2014).

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