Journal of the observations and physical properties of the sample stars.
|Target name||Sp. type||d||log(LBOL/L⊙)||R ⋆||T eff||ObsID (Rev)||Obs. mode||PI||Start date||Flare?||Duration|
|HD 34816 (λ Lep)||B0.5 V *||261||4.22||4.7||30400||1.66e-2||0690200601 (2415)||ff+thick||Nazé||2013-02-15@07:41:26||N||26.5|
|HD 35468 (γ Ori)||B2 IV–III *||77||3.87||6.4||21250||1.82e-3||0690680501 (2342)||ff+thick||Waldron||2012-09-22@19:27:17||Y||42.0|
|HD 36512 (υ Ori)||B0 V *||877||5.21||12.1||33400||1.95e-2||0690200201 (2326)||ff+thick||Nazé||2012-08-22@02:46:15||Y||20.2|
|HD 36960||B0.7 V *||495||4.58||7.8||29000||2.24e-2||0690200501 (2433)||ff+thick||Nazé||2013-03-23@08:57:52||Y||28.2|
|HD 38771 (κ Ori)||B0.5 Ia ||198||4.72||12.5||24800||3.39e-2||9940||ACIS-S||Waldron||2008-12-26@23:50:00||234.2|
|HD 44743 (β CMa)||B1 II–III ||151||4.41||8.8||24700||2.00e-4||0503500101 (1509)||ff+thick||Waldron||2008-03-06@15:33:36||Y||10.6|
|HD 52089 (ϵ CMa)||B1.5 II ||124||4.35||9.9||22500||1.00e-4||0069750101 (0234)||ff(MOS)/sw(pn)+thick||Cohen||2001-03-19@12:05:51||Y||31.2|
|HD 63922 (P Pup)||B0.2 III+? [1,5]*||505||4.95||10.4||31200||6.71e-2||0720390601 (2552)||ff+thick||Nazé||2013-11-15@02:11:45||N||46.5|
|HD 79351 (a Car)||B2.5 V+? [6,7]*||137||3.60||5.8||19150||6.04e-2||0690200701 (2393)||ff+thick||Nazé||2013-01-02@00:12:30||N||47.1|
|HD 144217 (β1 Sco)||B0.5IV-V+B1.5V *||124||4.44||6.1||30400||1.37e-1||0690200301 (2425)||ff+thick||Nazé||2013-03-06@16:04:28||N||26.6|
|HD 158926 (λ Sco)||B1.5 IV+ (DA.79|
|or PMS)+B [9,10]*||175||4.73||15.3||22500||2.51e-3||0690200101 (2424)||ff+thick||Nazé||2013-03-04@15:37:29||N||17.8|
Notes. References for spectral types:  Nieva (2013);  Morel et al. (2008);  Lennon et al. (1992);  Fossati et al. (2015);  Nieva & Przybilla (2014);  Slettebak (1982);  Buscombe & Morris (1960);  Holmgren et al. (1997);  Holberg et al. (2013);  Uytterhoeven et al. (2004a). Distances, based on Hipparcos, come from van Leeuwen (2007) and interstellar absorbing columns were taken from Table 2 (the most recent values) of Gudennavar et al. (2012), except for HD 36960 (for which there is no available value in Gudennavar et al. 2012; so the adopted value is taken from Diplas & Savage 1994) and HD 63922, for which only the colour excess is known (E(B−V) = 0.11; Katyal et al. 2013), which was converted into an absorbing column using the relation of Gudennavar et al. (2012). Bolometric luminosities (for the primary star if binary) were calculated using their Simbad V magnitudes, Hipparcos distances, reddenings from Gudennavar et al. (2012, except for HD 63922, see above), and bolometric corrections of Nieva (2013) for non-supergiant stars (identified by *) and the scale of Cox (2002) for HD 38771. Effective temperatures Teff were also taken from the latter two references with the addition of Fossati et al. (2015) for HD 44743 and HD 52089 (these authors also provided LBOL values for those stars, which are quoted in a previous column). Radii were calculated from . For the EPIC cameras, “ff” and “sw” correspond to full frame and small window modes, respectively; the thick filter was always needed to reject optical/UV light in view of the (optical/UV) brightness of the targets. The durations in the last column correspond to exposure times after flare filtering for EPIC-pn or ACIS-S (0th order). The κ Ori data, taken within 10 days, were combined, so that only the total duration is provided.
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