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We present an independent confirmation of the zero-point offset of ${\rm \itGaia}$ Data Release 2 (DR2) parallaxes using asteroseismic data of evolvedstars in the ${\rm \it Kepler}$ field. Using well-characterized red giantbranch (RGB) stars from the APOKASC-2 catalogue we identify a ${\rm \it Gaia}$astrometric pseudo-color ($\nu_{\rm eff}$)- and ${\rm \it Gaia}$ $G$-bandmagnitude-dependent zero-point offset of $\varpi_{\rm seis} - \varpi_{Gaia} =52.8 \pm 2.4 {\rm\ (rand.)} \pm 8.6 {\rm\ (syst.)} - (150.7 \pm 22.7)(\nu_{\rmeff} - 1.5) - (4.21 \pm 0.77)(G - 12.2) \mu{\rm as}$, in the sense that ${\rm\it Gaia}$ parallaxes are too small. The offset is found in high andlow-extinction samples, as well as among both shell H-burning red giant starsand core He-burning red clump stars. We show that errors in the asteroseismicradius and temperature scales may be distinguished from errors in the ${\rm \itGaia}$ parallax scale. We estimate systematic effects on the inferred global${\rm \it Gaia}$ parallax offset, $c$, due to radius and temperaturesystematics, as well as choices in bolometric correction and the adopted formfor ${\rm \it Gaia}$ parallax spatial correlations. Because of possiblespatially-correlated parallax errors, as discussed by the ${\rm \it Gaia}$team, our ${\rm \it Gaia}$ parallax offset model is specific to the ${\rm \itKepler}$ field, but broadly compatible with the magnitude- and color-dependentoffset inferred by the ${\rm \it Gaia}$ team and several subsequentinvestigations using independent methods.

Confirmation of the ${\rm \it Gaia}$ DR2 parallax zero-point offset using asteroseismology and spectroscopy in the ${\rm \it Kepler}$ field