| Abstract
| - We present measurements of the $\ion{K}{i}$$\lambda 7699$ line from spectra of 19 late-type members of the αPersei cluster obtained with the Intermediate Dispersion Spectrograph at the Isaac Newton Telescope. These stars span a narrow range of $T_\mathrm{eff}$, from 5091 K to 4771 K, and a wide range of $v \sin i$ values (9 $\mathrm{km\,s}^{-1}$-170 $\mathrm{km\,s}^{-1}$). For a given star, we find empirically that larger rotational broadening apparently increases the equivalent width of $\ion{K}{i}$$\lambda 7699$ linearly for $v \sin i$ values from 15 $\mathrm{km\,s}^{-1}$ to 75 $\mathrm{km\,s}^{-1}$. This correlation breaks down for $v \sin i >$ 75 $\mathrm{km\,s}^{-1}$. After correction for this effect, we show that the potassium line equivalent widths do not really correlate with $v \sin i$.
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