  Accurate (<10%) distances of Galactic star clusters allow precise estimation
of the physical parameters of any physically associated Planetary Nebula (PN)
and also that of its central star (CSPN) and its progenitor. The progenitor's
mass can be related to the PN's chemical characteristics and furthermore,
provides additional data for the widely used white dwarf (WD) initial-to-final
mass relation (IFMR) that is crucial for tracing the development of both carbon
and nitrogen in entire galaxies. To date there is only one PN (PHR1315- 6555)
confirmed to be physically associated with a Galactic open cluster (ESO 96
-SC04) that has a turn-off mass $\sim$2 M$_{\odot}$. Our deep HST photometry
was used for the search of the CSPN of this currently unique PN. In this work,
we present our results.
