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Fig. B.2
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Radial velocity offset for dwarfs (log g > 3.5 according to Zhang et al. (2023)) as a function of the difference in the best-fit log g and Teff we obtain versus those from APOGEE. The contour lines give the underlying source density. The stars in the sample have 10 < G < 16, 2 < BP − RP < 2.5, and E(B−V) < 0.1.
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