Comparison of distance and absolute luminosity in the K_s band between the literature and our best results from non-linear models. (a) Comparison of distances obtained using variant of SBCR Baade-Wesselink methods based on (V − R) (Gieren 1988; Hindsley & Bell 1989; Gieren et al. 1993; V − K) (Storm et al. 2004, 2011; Barnes et al. 2005; Groenewegen 2008, 2013); interferometric Baade-Wesselink method (Mérand et al. 2007; Kervella et al. 2004a); distance obtained from the parallax measured by Gaia DR2 and DR3 (Gaia Collaboration 2022); and distance inferred from RSP models (see Table 3) as vertical strips for each stellar mass assuming uncertainty of ±15 pc. The average of both BW distances based on (V − K) color and their p-factor are indicated. (b) Comparison of K_S-band absolute magnitude derived from different PL relations (Benedict et al. 2007; Fouqué et al. 2007; Gieren et al. 2018; Groenewegen 2018; Breuval et al. 2020, 2021; Trahin et al. 2021) established in the 2MASS filter (see Breuval et al. 2020), and the magnitude as we derived in the 2MASS filter from MESA-RSP non-linear models.