PL relation in the Ks band of the Type II Cepheids obtained i) via linear least-squares fits of the stars’ absolute magnitudes inferred by direct transformation of the TGAS parallaxes (upper panel); ii) via non-linear least-squares fits and the ABL method (middle panel); and iii) using the Bayesian approach (bottom panel). The slope of the fit is adopted from Ripepi et al. (2015). The bottom part of each panel shows the residuals from the best fit line.
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