The study of planetary nebulae (PNe) is crucial to understand both late stage stellar evolution, and the chemical evolution of our entire Galaxy. The ionized shell exhibits strong, numerous emission lines that are excellent laboratories for plasma physics. PNe are visible to great distances where their strong lines permit determination of the size, expansion velocity and age of the PN, so probing the physics and timescales of stellar mass loss. We can use them to derive luminosity, temperature and mass of their central stars, and the chemical composition of the ejected gas. Their complex shapes provide clues to their formation, evolution, mass-loss processes, and the shaping role that may be played by magnetic fields, binary central stars or even massive planets. PNe are thus powerful astrophysical tools, providing a unique window into the soul of late-stage stellar evolution. We are also in a golden age of PN discovery. Prof Parker has lead programs that have doubled the totals accumulated over the previous 250 years. Following this motivation we have provided, an accessible, reliable, on-line "one-stop" SQL database for essential, up-to date information for all known Galactic PN called HASH (Hong Kong / AAO/ Strasbourg H-alpha PN research platform). The specific project below will make use of and build on this world-leading new resource. This project will aim to help verify if a candidate object is a bona-fide PN by the detection of a blue, hot, ionising CSPN at or near the geometric centre of the nebulosity. This is considered strong, positive evidence. Until HASH, only ~20% of known PNe had an identified CSPN to help relate PNe properties, such as morphology, ionisation state, kinematic age etc, to the underlying properties of the CSPN. These are extremely inhomogeneous, exhibiting a wide variety of observed characteristics. These range from massive population II Wolf-Rayet stars (denoted as [WR] to distinguish them from their population I counterparts), PG1159, stars, various kinds of weak emission line stars (often denoted WELS though they are not considered to be an independent spectral classification -different kinds of white dwarfs (DA, DAO, DO) and early and late O(H) and Of(H) stars.