Top row shows the slopes and intercepts for the fit to the σ_vz – P_rot relations in logarithmic space for each G_BP − G_RP bin. Bottom row shows the physical parameters associated with the spindown law in Equation (5), derived from the slopes and intercepts. The red solid line shows the classic “Skumanich” spindown, where d = 0.5, and the blue solid line shows the Deeming regression result for partially convective stars with G_BP − G_RP < 2.6. Our fitting result suggests G dwarfs possibly exhibit a faster spindown compared to KM dwarfs, perhaps due to contribution from radius inflation. We also find the traditional power-law form for the color dependency of stellar spindown agrees with observational data within uncertainty.