Hertzsprung–Russell diagram for our final set of Kepler RC stars where the G-band absolute magnitude is computed using L21-corrected Gaia parallaxes (black points). The sample is restricted to G ∈ [11, 13] mag, where we found the residual parallax offset to be approximately zero. The pink dashed line shows the fit given by Eq. (6), and the brown shaded region illustrates how the fit could vary given the uncertainties on the slope and the intercept.