Fractional contribution of equivalent widths of the P I line in the CO(v = 7−4) blended line vs. T_eff for a set of MARCS (Gustafsson et al. 2008) stellar models in the grid of 3900 ≤ T_eff ≤ 5000 K, 1.0 ≤ log g ≤ 3.0, and [Fe/H]of −1, −0.5, 0.0, and 0.5 dex, all with solar-scaled phosphorus abundances. Different combinations of [Fe/H] and a change in log g are represented by different colored lines and bands, respectively, with lower log g at each [Fe/H] resulting in lower equivalent widths for the P I line.