the shapes of these light curves are very similar, with the pulse fraction ranging from 53% to 62%, despite the fact that the template functions are obtained from vastly different atmosphere models. Note that in renormalizing the temperature profile (to obtain the $T_0$-$T_{\rm eff}$ mapping), we make the approximation that the magnetic field is normal to the stellar surface, and we keep its magnitude always set to the field strength at the magnetic poles. This speeds up the construction of the temperature profile (i.e., the $T_0$-$T_{\rm eff}$ mapping for a given template function) since the integration in Equation (\[eq:calF\]) can be done more efficiently, and need not be repeated for every surface patch. We have found that this approximation introduces rather small error in the resulting $T_0$-$T_{\rm eff}$ relation; this is understandable because $T_{\rm eff}$ is determined by summing over the emitted spectrum in all directions, and the direction of the magnetic field is averaged over, while the radiative transfer is not too sensitive to factor-of-two changes in field strength. Nevertheless, we note that when computing $I_\nu^e({\bf k})$ for the light curve, the “correct” magnetic strength and direction must be adopted in order to accurately account for the magnetic beaming 