plate scale of 0.234arcsec/pixel resulting in a FOV of $4 \times 4$arcmin using the wide-field imaging mode of NOTCam. To resemble the FOV of ALFOSC, we obtained a mosaic of four partly overlapping dithered images per galaxy. Accordingly, the combined FOV of the four quadrants is $\approx 6 \times 6$arcmin.

Data reduction {#dataReduction}
==============

Monitoring data
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All frames obtained for this study were bias-, sky- and flatfield-corrected using standard data reduction routines. As in PaperI, the whole sample of stars was corrected for interstellar reddening adopting the values from the NASA Extragalactic Database (: $A_{V}$=$0\fm574$, $A_{i}$=$0\fm336$, $A_{K_{s}}$=$0\fm064$; : $A_{V}$=$0\fm604$, $A_{i}$=$0\fm354$, $A_{K_{s}}$=$0\fm067$). Images taken in the $i$-band with ALFOSC also suffer from fringing. To compensate for this effect, it would have been necessary to obtain flatfield images before and after each integration of the science target to create a fringe map. Without these additional calibration images, a correction for this effect was not possible. The maximum amplitude of variations caused by fringing is, however, well below the minimum amplitude expected for LPVs. The detection of variable stars was carried out using the image subtraction tool ISIS2.1[^2] of Alard ([@alard]). One carefully chosen $i$-band image was taken as reference frame to 