All Tables

Table 1: Highlight on the four common stars between Slettebak et al. (1975, SCBWP), Abt et al. (2002) and Papers I and II (standard deviation is indicated; dash "-'' stands for only one measurement) and comparison with data from the literature. $\ensuremath{v\sin i}$ from the literature are classified in three subgroups according to the way they are derived: by-product of a spectrum synthesis or frequency analysis of the lines profiles. Flags from HIPPARCOS catalog are indicated: variability flag H52 (C: constant, D: duplicity-induced variability, M: possibly micro-variable, P: periodic variable, -: no certain classification) and double annex flag H59 (C: component solution, -: no entry in the Double and Multiple Systems Annex).
Table 2: Subsamples of Main-Sequence stars (classes V, IV-V and IV): the mean radii ${\overline R}/R_\odot$ and the mean masses ${\overline\mathscr{M}}/\ensuremath{\mathscr{M}_\odot}$ are derived from Habets & Heintze (1981), as well as the relative variation of the radius $\Delta R$ and of the mass $\Delta\mathscr{M}$ along the interval of spectral type. For each subsample, the number of stars is given.
Table 3: Moments of the $\ensuremath{v\sin i}$ distributions for each spectral subsample. "total'' corresponds to the whole subsample (including CP and CB stars); "normal'', CP and CB stars are also distinguished. For both "total'' and "normal'' subsamples, the moments are given for different groups of luminosity class: all (IV, IV-V, V), V and IV (class IV-V luminosity stars only are not considered because they represent a very small fraction of the sample). The number of stars (#), the center and the dispersion of the distribution are given. Centers are estimated using the median and the mean, and the dispersion is evaluated with the standard deviation.
Table 4: (extract) List of the 1541 B9- to F2-type stars, with their $\ensuremath{v\sin i}$ value, spectral type, associated subgroup and classification (CP, CB, blank stands for "normal'').
Table 5: Estimated bandwidth for the kernel method and mean integrated squared error: for each subsample, the size n (number of stars) is given, as well as the estimated $\hat{h}$ according to Sheather & Jones (1991), computed in the logarithmic velocity scale, and the variability band width $\epsilon$ (Eq. (C.4)).
Table 6: Characteristics of the bimodal distributions: the fast rotator mode $\sqrt {2a}$ from the Maxwellian distribution parameter a, the proportion p of slow rotators as the excess compared to the Maxwellian fast rotator distribution, the corresponding number $N_{\rm s}$ of slow rotators in the observed sample, and the mean of the slow rotator distribution $\mu _{\rm s}$ .