A_G vs. A_V (panel a) and E(BP − RP) vs. E(B − V) (panel b) for 22 894stars from the Kepler Input Catalog with parallax uncertainty less than 20%. The dashed line shows the identity relation. As discussed in the main text, this comparison is inconclusive since A_G and E(BP − RP) are subject to large uncertainties but they cannot scatter into negative values (thus causing seeming biases). Furthermore, the Gaia passbands are very broad and thus strongly depend on the intrinsic source SED. Dashed lines indicate one-to-one relations.