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• Characterizing the population and space density of white dwarfs in our Galaxy
  
• Characterizing the population and space density of white dwarfs binaries in our Galaxy: AM CVn stars, Cataclysmic Variables, detached binaries
• Characterizing the population and space density of subdwarf B-stars in our Galaxy
• With IPHAS: A first digital proper motion survey of the Galactic Plane
• With IPHAS: A 3D Dust mapping of our Galaxy
  

The basis `tool' of the UVEX survey is a colour-colour and colour-magnitude diagram as shown below. From these colour-colour and colour-magnitude diagrams UV-excess sources are automatically selected as described in Verbeek et al. (2010), in prep. The full lines show the middle of the main-sequence locus (right) and the 3-sigma blue edge wrt. to this main location. Objects located to the blue (left) of this 3-sigma line are classified as UV-excess sources. In this field 7 UV-excess sources are clearly identified.

Using a cross-matching with the IPHAS data proper motions are determined, as described in Deacon et al., 2009 (for the IPHAS-POSSI x-match).
The difference between the IPHAS-POSSI x-match and the higher proper motion IPHAS-UVEX x-match is shown in the reduced proper motion diagram below, where the blue symbols are the IPHAS-UVEX x-match and the red points are the IPHAS-POSSI proper motion objects in the same area. This shows the increased depth of the combination of two digital surveys, even if the baseline is shorter than that of the IPHAS-POSSI x-match.