scales, where the long secondary period (LSP) is about ten times the shorter period. The origin of these LSPs is still unknown (Nicholls et al. [@nich2]). By comparing a sample of sequenceD stars with similar red giants (not showing LSPs), Wood & Nicholls ([@wooni]) found that such objects have a significant excess in the mid-infrared ($8-24$$\mu$m), which is thought to originate from circumstellar dust. This is not the case for sequenceE stars (Nicholls et al. [@nich]). Within the last decade, several studies were carried out to explore PLRs of LPVs in different stellar systems of the Local Group (see Groenewegen [@groene] for an overview). Rejkuba et al. ([@rejka]) and Rejkuba ([@rejk]) were able to study LPVs even beyond the Local Group, namely in NGC5128 in the Centaurus group. This growing sample of PLRs for LPVs raises the question whether these relations are universal or not and if they are indeed universal, they can, therefore, be used as an additional tool to measure distances. Here we aim to contribute to this discussion by investigating LPVs in the two dwarf galaxies and .

The two target galaxies of our investigation, and , were discovered by J. Herschel in September 1829 and by 