Table 1: Relevant parameters for program Be stars (ordered by right ascension).
Name HD Name Sp. Ref. $V\sin~i$ Ref. $T_{\rm eff}$ Ref.
${\lambda }$ Eri HD 33328 B2 IVe 1 325 1 24 000 2
$\psi$1 Ori HD 35439 B1 Ve 3 305 1 25 400 3
${\omega }$ Ori HD 37490 B2e III 4 172 5 20 020 5
19 Mon HD 52918 B1 IV 6 264 7 24 000 5
HR 3186 HD 67536 B2.5n(e) 8 292 9 20 000 10
${\mu }$ Cen HD 120324 B2 IVe 11 130 12 19 970 13
${\eta }$ Cen HD 127972 B1.5 IVe 14 350 4 21 860 15
2 Vul HD 180968 B1 IV 6 332 16 25 000 10
${\pi }$ Aqr HD 212571 B1 Ve 6 250 17 25 000 17
6 Cep HD 203467 B2.5e 18 150 18 20 000 10
Reference. 1: Abt (2002), 2: Hummel & Vrancken (2000), 3: Lamer & Waters (1987), 4: Slettebak (1982), 5: Neiner et al. (2003), 6: Lesh (1968), 7: Balona (2002), 8: Hanuschik et al. (1996), 9: Uesugi & Fukuda (1970), 10: this paper, 11: Hiltner et al. (1969), 12: Brown & Verschueren (1997), 13: Rivinius et al. (2001), 14: Levenhagen et al. (2003), 15: Stefl et al. (1995), 16: Balona (1995), 17: Miroshnichenko et al. (2002), 18: Slettebak (1994).

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