Projected rotational velocity derived for the standard stars.
|ID||v sin i(lit.)||v sin i(FEROS)||v sin i(duPont)||Ref.|
|km s-1||km s-1|
|HD 787a||2.1 ± 1.0||1.3||1.5||1, 2, 3, 4|
|2.1 ± 1.0||–||1.6|
|HD 31767||1.1 ± 1.3||2.0||2.3||2|
|HD 180540||4.8 ± 0.3||4.7||4.8||9|
|HD 4128||3.5 ± 0.4||3.6||3.4||5, 6, 7, 8|
|HD 15453||1.0 ± 1.0||0.9||1.3||2|
Notes. The literature v sin i, and the derived values for the FEROS and DuPont runs, are given in Cols. 2 − 4.
For HD 787 only the FEROS spectrum obtained in the run reported in Table 1 was used for the abundance analysis. However, the star was repeatedly observed during the various duPont and La Silla runs. We report here the rotational velocities measured for the different spectra.
References. 1: de La Reza & Da Silva (1995); 2: de Medeiros & Mayor (1999); 3: de Medeiros et al. (1996); 4: Fekel & Balachandran (1993); 5: Fekel (1997); 6: Gray (1982); 7: Pasquini et al. (2000); 8: Smith & Dominy (1979); 9: Gray & Toner (1986). When more than one estimate was available, the value in Col. 2 is their weighted average, with their standard deviation as associated error.
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