Appendix B: Notes on ${\vec v}$sin${\vec i}$ standard stars with discrepant rotational velocity

Standard stars from SCBWP that are listed in Table 7, are now detailed:

• $\eta$ Phe (HD 4150) is among the A0 dwarf stars investigated by Gerbaldi et al. (1999). They suspect $\eta$ Phe to be a binary system on the basis of the fit between the observed and the computed spectrum, as do Grenier et al. on the basis of the CCF of the spectrum;

• $\nu$ Pup (HD 47670) is a late B giant star. It is part of the sample studied by Baade (1989,b) who searches for line profile variability. He detects roughly central quasi-emission bumps in the rotationally broadened Mg II absorption line. This feature could be caused by the change in effective gravity from equator to poles and the associated temperature differences because of fast rotation. Rivinius et al. (1999) tone down this result but conclude nevertheless that there is strong evidence that this star is a not previously recognized bright Be star. $\nu$ Pup was suspected to be a $\beta$ Cephei star (Shaw 1975) and is newly-classified as an irregular variable on the basis of the HIPPARCOS photometric observations;

• Sirius ($\alpha$ CMa, HD 48915) has a $\ensuremath{v\sin i} =10$ in the catalogue of SCBWP. Several authors have given larger values derived from approximatively the same spectral domain. Smith (1976) finds 17 and Kurucz et al. (1977) 16 $\pm$1 . Deeming (1977), using Bessel functions, finds 16.9 . Lemke (1989), analyzing abundance anomalies in A stars, derives the of Sirius as an optimum fit over the spectral range: 16 . Dravins et al. (1990) using Fourier techniques on high resolution and high signal-to-noise ratio spectra give $15.3\,{{\rm km}\,{\rm s}^{-1}}\ \pm 0.3\,{{\rm km}\,{\rm s}^{-1}}$. Hill (1995) studies a dozen A-type stars using spectral synthesis techniques to make an abundance analysis; fitting the spectra (four 65Å wide spectral regions between 4500 and 5000Å) he finds 16.2 as the of Sirius;

• QW Pup (HD 55892) is an early F-type star. It belongs to the $\gamma$ Dor class of pulsating variable stars (Kaye et al. 1999). Balachandran (1990), studying lithium depletion, determines Li abundances and rotational velocities for a sample of nearly 200 F-type stars. Using her own FWHM- calibration, she finds 50 for QW Pup, which gets closer to our determination. HIPPARCOS results show that QW Pup is a possible micro-variable star;

• a Vel (HD 75063) in an early A-type star. It is part of the sample of IRAS data studied by Tovmassian et al. (1997) in the aim of detecting circumstellar dust shells. They do not rule out that a Vel may have such a feature. No relevant data have been found for this star;

• $\alpha$ Vol (HD 78045) is a dusty A star on the basis of IRAS data (Cheng et al. 1992). Holweger et al. (1999) measure a significantly larger than the from SCBWP and even our determination;

• $\theta$ Leo (HD 97633) is a candidate constant velocity A star. Fekel (1998) monitors it and attributes to it a $\ensuremath{v\sin i} =23\,\ensuremath{{\rm km}\,{\rm s}^{-1}}$. Lemke (1989) and Hill (1995) respectively measured it at 21 and 22.1 . These values are significantly higher than 15 found by SCBWP;

• A Cen (HD 100673) is a B-type emission line star;

• $\lambda$ Mus (HD 102249) has been measured by Noci et al. (1984) who derive its using the CCF and a calibration as described in Stauffer et al. (1984). In HIPPARCOS data, $\lambda$ Mus is a binary star for which orbital parameters are given: period $P = 453\,{\rm d} \pm 8$d, inclination $i=134\,\hbox{$^\circ$ }\pm 8$$^\circ$, semi-major axis of photocentre orbit $a_0 =6.31\,{\rm mas} \pm 1.05$mas;

• $\psi$ Cen (HD 125473) is a dusty A-star (Cheng et al. 1992). The rotational velocity derived by Holweger et al. (1999) agrees with our determination, 30% larger than SCBWP;

• $\epsilon$ Aqr (HD 198001) has a $\ensuremath{v\sin i} =85$ according to SCBWP, much smaller than the value in this work. The velocity derived by Hill is consistent with ours, taking into account the uncertainty of the measurements. Dunkin et al. (1997) found 95 by fitting the observed spectrum with a synthetic one;

• $\omega^2$ Aqr (HD 222661) has, to our knowledge, no further determination of the , independent of the SCBWP's calibration.