Gaia Data Release 1
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Fig. 21


Classical Cepheid PL relations in the Ks-band obtained i) by linear least-squares fitting the stars’ absolute magnitudes inferred from direct transformation of the TGAS parallaxes (upper panel); ii) via non-linear least-squares fit and the ABL method (middle panel); and iii) using a Bayesian approach (bottom panel). The slope of the fit is adopted from Fouqué et al. (2007). The bottom part of each panel shows the residuals from the best fit line.

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