the effect of stellar rotation on the parameters $T_\text{eff}$ and $\log(g)$, FB98 presented the following corrective formulae for stars with $T_\mathrm{eff} > 11000$ K:

$$\begin{aligned}
\Delta T_\mathrm{eff} &= 0.0167 (v \sin i)^2 + 218, \\ 
\Delta \log g &= 2.10 \times 10^{-6} (v \sin i)^2 + 0.034.\end{aligned}$$

For stars with $8500 \mathrm{K} \leq T_\mathrm{eff} \leq 11000 \mathrm{K}$, the analogous formulae are:

$$\begin{aligned}
\Delta T_\mathrm{eff} &= 0.0187 (v \sin i)^2 + 150, \\ 
\Delta \log g &= 2.92 \times 10^{-6} (v \sin i)^2 + 0.048.\end{aligned}$$

In both cases, $\Delta T_\mathrm{eff}$ and $\Delta \log g$ are *added* to the $T_\mathrm{eff}$ and $\log g$ values derived from $uvby\beta$ photometry.

Notably, the rotational velocity correction is dependent on whether the star belongs to the early, intermediate, or late group. Specifically, FB98 define three regimes: $T_\mathrm{eff}<$8830 K (no correction), 8830 K$<$Teff$<$9700 K (correction for intermediate A0-A3 stars), Teff$>$9700 K (correction for stars earlier than A3).

[@song2001], who performed a similar isochronal age analysis of A-type stars using $uvby\beta$ photometry, extended the FB98 rotation corrections to stars earlier and later than B7 and A4, respectively. In the present work, a more conservative approach is taken and the rotation correction is applied only to stars in the 