Table 1: Program stars and log of observations.
Object Sp.T $V\sin i$ $\log T_{\rm eff}$ $\log g$ i Date
    km s-1     [deg]  
HD 41335 B1.5IIIne 358 4.320 3.89 69 1,2
HD 45725 B2.5IV-Ve 330 4.251 3.90 67 3
HD 48917 B2III-IVe 205 4.308 3.40 45 3
HD 50013 B1.5IVne 243 4.391 4.02 37 1,2
HD 56139 B2IVe 84 4.291 3.62 17 3
HD 58978 B0Vpe 375 4.388 4.15 55 3
HD 63462 B0Ve 435 4.424 3.60 90 1,2
HD 88661 B2IVpne 237 4.333 3.99 39 1,2
HD 91465 B3IIIne 266 4.240 3.52 67 1,2
HD 105435 B2IVne 258 4.349 3.92 42 1,2
HD 110335 B6IVe 208a 4.120b 3.28b 63 3
HD 112091 B5Vne 210 4.309 3.93 36 3
HD 120991 B2IIIe 70 4.347 3.69 13 1,2
HD 124367 B4IVne 295 4.243 3.76 63 1,2
HD 148184 B0.5Vpe 144 4.459 3.91 20 1,2,4
HD 157042 B2IVe 340 4.338 4.06 53 4
HD 158427 B3Vne 290 4.256 3.99 51 4
HD 164284 B2Ve 262 4.426 3.95 53 4
Dates: 1 $\equiv$ 5 Mar. 1996, 2 $\equiv$ 6 Mar. 1996, 3 $\equiv$ 7 Mar. 1996, 4 $\equiv$ 21 Sep. 1996. Julian days are given in the online Table 4. a Yudin (2001); b de Geus et al. (1989). The inclination angle i was derived using stellar atmospheres calculated for rotationally deformed and gravitationally darkened stars (Frémat et al. 2005).

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