early or intermediate groups, as determined by the classification scheme discussed in § \[subsec:atmosphericparameters\]. This decision was partly justified by the abundance of late-type stars that fall below the ZAMS in the open cluster tests (§ \[subsec:openclustertests\]), for which the rotation correction would have a small (due to the lower rotational velocities of late-type stars) but exacerbating effect on these stars whose surface gravities are already thought to be overestimated.

We include these corrections and, as illustrated in Figure \[fig:rotation-vectors\], emphasize that in their absence we would err on the side of over-estimating the age of a star, meaning conservatively overestimating rather than underestimating companion masses based on assumed ages. As an example, for a star with $T_\mathrm{eff} \approx$ 13,275 K and log$g$ $\approx$ 4.1, assumed to be rotating edge-on at 300 km s$^{-1}$, neglecting to apply the rotation correction would result in an age of $\sim$ 100 Myr. Applying the rotation correction to this star results in an age of $\sim$ 10 Myr.

Of note, the FB98 corrections were derived for atmospheric parameters determined using the synthetic $uvby\beta$ color grids of [@moon1985]. It is estimated that any differences in derived atmospheric parameters resulting from the use of color grids 