fulfilled. The significance ($sig$) of a period is defined in SIGSPEC as the inverse of the logarithmic scaled false-alarm-probability (FAP) that a discrete Fourier transform amplitude is caused by noise (see Reegen [@piet] for details). A spectral significance of 5 therefore corresponds to an inverse FAP of $10^5$ or, in other words, the risk of the amplitude being just caused by noise is 1:10$^5$. Example light curves showing different types of LPVs from both galaxies together with our best model fit are shown in Fig.\[LC\]. The results of the period search are summarised in Table\[periods147\] and \[periods185\], which are available online only. Beside the periods and corresponding significance of the detected LPVs, the table also lists the mean $i$-magnitudes that were obtained from the light curve. The corresponding photometric errors of the mean brightness in the $i$-band after the calibration are listed in Table\[errors\] for different ranges of magnitude. We only used Fourier-amplitudes from the SIGSPEC-output to fit the light curves (see red line in Fig.\[LC\]). Additionally, we defined a $\sigma$-amplitude that is twice the statistical standard deviation from the mean brightness of the variable. A purely sinusoidal light curve, for example, with a peak-to-peak-amplitude $A=1\fm0$ would result in a 