to 0.52 for and 0.21 for , respectively. These values fall between the corresponding ratios for the whole population and the ratios when limiting the O-rich sample to spectral types M5 and later, as presented in PaperI. Thereby, our sample selected on variability provides a good representation of the AGB population with which the LPV class is typically associated. If we look at the histograms in Fig.\[aHist\], we notice that the amplitude distributions of the O-rich objects is dominated by small-amplitude variables. Indeed, the histograms suggest that the peak at $0\fm35$ is not real, but that we are missing stars with the shortest amplitudes owing to the limited sampling rate of our monitoring. In contrast, C-rich stars exhibit a much flatter distribution in these plots. For the sake of completeness, the distribution of LPVs without narrow-band photometry is given in the last panels of Fig.\[aHist\] for each of the galaxies.

The period distributions of the LPVs in the two galaxies can be seen in the $\Delta i$ vs. log$P$ diagrams in Fig.\[lgPAmpl2\]. Here, we plotted only the first significant period of all detected LPVs. The range of periods covered by the variables is similar in both systems ($\approx$$90$–$600^{\rm d}$) and 