shifted towards shorter periods (sequence C$^{\prime}$). On average, stars on this sequence exhibit smaller amplitudes than objects on sequence C (see lower panel of Fig.\[KlgP\]). A similar PLR was found in the LMC (e.g. Ita et al. [@ita], Fraser et al. [@fraser2]) and is associated with first overtone pulsation. The smaller light amplitude of this group identified in our sample agrees with this interpretation. Note that the trend for the zero point of sequence C is also visible for sequence C$^{\prime}$ but the number of detected LPVs populating sequence C$^{\prime}$ in prohibits another linear regression. For demonstration purpose only, we plotted sequence C$^{\prime}$ of Ita et al. ([@ita]) and shifted it according to the difference in distance obtained for sequence C. This line is drawn as thin dashed line in Fig.\[KlgP\]. A handful of targets in may also be located on this sequence. Variables corresponding to higher overtone pulsation were not accessible to our study owing to the sampling rate limitations.

From studies in various stellar systems it is known that the LSPs, visible in a significant fraction of all LPVs, form another sequence to the right of sequence C in the PLD. This sequence D, taken from Ita et 