  The open cluster (OC) NGC 2453 is of particular importance since it has been
considered to host the planetary nebula (PN) NGC 2452, however their distances
and radial velocities are strongly contested. In order to obtain a complete
picture of the fundamental parameters of the OC NGC 2453, 11 potential members
were studied. The results allowed us to resolve the PN NGC 2452 membership
debate. Radial velocities for the 11 stars in NGC 2453 and the PN were measured
and matched with Gaia data release 2 (DR2) to estimate the cluster distance. In
addition, we used deep multi-band UBVRI photometry to get fundamental
parameters of the cluster via isochrone fitting on the most likely cluster
members, reducing inaccuracies due to field stars.The distance of the OC NGC
2453 (4.7 $\pm$ 0.2 kpc) was obtained with an independent method solving the
discrepancy reported in the literature. This result is in good agreement with
an isochrone fitting of 40-50 Myr. On the other hand, the radial velocity of
NGC 2453 ($78 \pm 3$ km s$^{-1}$) disagrees with the velocity of NGC2452 ($62
\pm 2$ km s$^{-1}$). Our results show that the PN is a foreground object in the
line of sight. Due to the discrepancies found in the parameters studied, we
conclude that the PN NGC 2452 is not a member of the OC NGC 2453.
