Fit to the bottom 10th percentile of total rotational broadening (﹩v\sin i﹩ and ﹩{v}_{{\rm{mac}}}﹩) for stars with S/N ≥ 100 in the sample. The relations of VF05 and Saar & Osten (1997) are overplotted in dash-dotted and dashed lines, respectively. Blue points are stars with ﹩\mathrm{log}g﹩ ≥ 4, green have ﹩4\gt \mathrm{log}g\geqslant 3﹩, and red have ﹩\mathrm{log}g﹩ < 3. Heavier points with error bars represent bin centers and uncertainties used in fitting the relations. Neither of the previous studies separated dwarfs from subgiants, but our separate relations coincide with those of the previous studies.