Appendix A: Notes on stars with uncertain rotational velocity

A.1 Stars with no selected line

In a few cases, the selected lines are all discarded either from their Fourier profile or from their skewness (Table 3). For these stars, an uncertain value of is derived from the lines that should have been discarded. They are indicated by a colon and flagged as "NO'' in Table 5. These objects are listed below. It is worth noticing that none of them have spectra collected in $\Lambda _3$ spectral range:

• HD 27459 and HD 27819 are early-F and late-A type stars from Hyades open cluster. Due to their rotational broadening and their late spectral type, no lines are retained in $\Lambda _1$. Their uncertain are respectively 78: and 41:  . Varenne & Monier (1999) measure their rotational velocity and find 78 and 47  .
• HD 32537 is a early-F type star, whose derived from discarded line in $\Lambda _1$ is 27:  . The rotational velocity measured by Hui-Bon-Hoa (2000) is 21  .
• HD 53929 is a late-B giant star, its spectra in $\Lambda _1$ exhibit very few lines. The is derived from Fe II 4233 that is usually discarded because blended. For this spectral type, blend of the iron line is less pronounced, and the is 25:  . Dworetsky et al. (1998) find the same value.
• Following stars are high rotators whose only measurable line in $\Lambda _1$ is the blended line Fe II 4233.
  • HD 59059, 260: 
  • HD 77104, 183: 
  • HD 111469, 197: 
  • HD 224404, 190:  .

   
A.2 Stars with high external error

A few stars of the sample exhibit an external error higher than the estimation carried on in Sect. 3.3. It can be the signature of a multiple system. The following stars have variable from spectrum to spectrum and are labeled as "SS'' in Table 5:

• HD 4321 has a mean $\ensuremath{v\sin i} =25\pm 4$  , but for its different spectra, this value is respectively 38, $22\pm 3$ and $25\pm 1$  .
• HD 40446 has a mean $\ensuremath{v\sin i} =27\pm 5$  (respectively 27, 32 and 22  ). The HIPPARCOS solution for this object is flagged "suspected non single''.
• HD 40626 has a mean $\ensuremath{v\sin i} =18\pm 3$  ($16\pm 1$ and $20\pm 1$  ). The found by Ramella et al. (1989) is 10.8  .
• HD 103578 has a mean $\ensuremath{v\sin i} =16\pm 4$  ($14\pm 1$, $19\pm 1$  ). It is a SB2 system, and Hummel et al. (2001) who study its orbital motion, find $11.03\pm 0.14$  and $8.12\pm 0.27$  for the of each component.