stars. The linear regression $(m_{K}$=$a \log{P} +
b)$; black dashed lines in Fig.\[KlgP\]) of this selection resulted in a slope $a$ of $-3.55$ for and $-3.47$ for . For the of each relation we obtained 25$\fm$46 and 25$\fm$22 for and , respectively. In Table\[PLRs\] we contrast PLRs derived by different studies with those found here. This comparison of results for different stellar systems is of interest for studying the aspect of the universality of the PLRs of Sequence C stars, which may then serve as an additional tool to measure distances in extragalactic systems. Owing to the limited number of carbon stars in our samples, we did not analyse and stars separately. However, for comparison reasons we calculated PLRs for our samples with and without LPVs. The small differences of the values demonstrate that the results are robust against slight changes of the sample selection. For additional calculations we only consider the results of the complete 3.0$\sigma$ clipping sample. The slopes $a$ found for and are close to those given for the combined samples in other stellar systems.

In Fig.\[KlgP\] an obvious offset between the shifted LMC-PLRs and those derived for can be seen. The numbers in Table\[PLRs\] suggest that 