this shift amounts to approximately $0\fm 2-0\fm4$ (depending on sample selection and regression method). A mild difference in the zero-point $b$ is expected owing to the difference in metallicity (Wood [@wooda]). However, for the lower metallicity of relative to the LMC, a star should be brighter at a given period, making the discrepancy even larger. A simple but not necessarily final explanation for this difference would be an error in the distance modulus of . When attempting to bring our observations in line with the LMC relations of Ita et al. ([@ita]), a distance modulus of 24$\fm$30 seems to be more appropriate for this galaxy. This value is obtained by subtracting the resulting $K_{s}$-magnitudes derived from the relation of Ita et al. ([@ita]) and from this work at a constant value of $\lg P = 2.31 $. For , the distance modulus from the literature excellently agrees with our data. The zero-point problem for needs further exploration. However, if the reason for the offset PLRs is indeed an error in the distance modulus, this would be the first correction of a distance to a galaxy based on PLRs of LPVs.

For there are indications of another parallel sequence of LPVs 