Distribution of photometric metallicities of a selection of nearby stars from Ibukiyama & Arimoto (2002). The temperatures were calculated from the B−V color relation of Boyajian et al. (2013). In black (dashed line) we have overplotted the fit to our [Fe/H] data and in red (dot-dashed line) a fit to these data using the same Gaussian kernel regression method. These stars show the same lack of high-metallicity stars at low ﹩{T}_{\mathrm{eff}}﹩ as our sample. This trend is most likely a systematic induced by errors in the models and extends to photometric metallicities that are calibrated against those from spectra.