Abstract:
A CCD VI imaging time-series over 11-year is employed to explore the light
curves of stars in the field of Palomar 2. We discovered 20 RRab and 1 RRc
variables. A revision of Gaia-DR3 data enabled us to identify 10 more variables
and confirm the RRab nature of 6 of them and one RGB. The cluster membership is discussed, and 18 variables are most likely cluster members. The Fourier
light curve decomposition for the 11 best quality light curves of cluster member
stars leads to independent estimates of the cluster distance 27.2 ± 1.8 kpc and
[Fe/H]ZW = −1.39 ± 0.55. We confirm the cluster as of the Oo I type.
