I am now to the point where the high resolution magnitude code is implemented and working correctly, meaning that I can create useful CMDs for photometric analysis. The Kepler band is still not available as I have yet to apply/find the zero-point flux to the code, but that has not been a problem yet. Included here is a CMD for V vs. (V-K) as a function of photospheric temperature and fractional spot temperature.

Each color in the gradient represents  the same photospheric temperature range, 7000K to 3200K. The gradient is a range of spot temperatures, fractionally compared to the photo temperature in the legend. The star was modeled with a 30% filling factor. The trends here show that for a cooler spot, the V(mag) is lower and the (V-K) color separation becomes greater. Looking far forward, I will be attempting to find a set of parameters, i.e. spot size and temp, that recreate the data from (Figure 1) from Kevin’s 2016 Pleiades paper, a V(mag) vs. (V-K) diagram for Pleiades members.