by Ch. Alard (see Schuller et al. ([@schuller]). This allows us to distinguish LPVs from other detected variables in our sample and to study their distribution in consecutive diagrams. For approximately 75% of the identified variables we could assign counterparts in PaperI. The reason for the incompleteness was threefold. First, some stars were obviously at light minimum and, thus, too weak at the epoch of the observations of PaperI. Second, we had to exclude all variables where the cross-correlation was ambiguous because of crowding. Third, a few stars visible on the frames studied in PaperI had photometric errors that were too large to be included in the final list there.

  --------- ---------- ---------- ---------- ---------- ---------- ---------- ----------
    LPVs     $\times$   $\times$   $\times$   $\times$   $\times$   $\times$   $\times$
   Period               $\times$                         $\times$   $\times$   $\times$
    $V,i$                          $\times$                         $\times$   $\times$
      ,                                                             $\times$   $\times$
    $K_S$                                     $\times$   $\times$              $\times$
   objects     213        168        163        182        147        122        113
  --------- ---------- ---------- ---------- ---------- ---------- ---------- ----------

  : Summary of detected variables in , grouped according to the information available for different sub-samples.[]{data-label="table:3"}

  --------- ---------- ---------- ---------- ---------- ---------- ---------- ----------
    LPVs     $\times$   $\times$   $\times$   $\times$   $\times$   $\times$   $\times$
   Period               $\times$                         $\times$   $\times$   $\times$
    $V,i$                          $\times$                         $\times$   $\times$
      ,                                                             