White Dwarf Luminosity Functions from the Pan{\ndash}STARRS1 3{\pi}
  Survey
  White dwarfs are among the most common objects in the stellar halo; however,
due to their low luminosity and low number density compared to the stars in the
discs of the Milky Way, they are scarce in the observable volume. Hence, they
are still poorly understood one hundred years after their discovery as
relatively few have been observed. They are crucial to the understanding of
several fundamental properties of the Galaxy {\mdash} the geometry, kinematics
and star formation history, as well as to the study of the end-stage of stellar
evolution for low- and intermediate-mass stars. White dwarfs were traditionally
identified by their ultraviolet (UV) excess, however, if they have cooled for a
long time, they become so faint in that part of the spectrum that they cannot
be seen by the most sensitive modern detectors. Proper motion was then used as
a means to identify white dwarf candidates, due to their relatively large space
motions compared to other objects with the same colour. The use of proper
motion as a selection criterion has proven effective and has yielded large
samples of candidates with the SuperCOSMOS Sky Survey and Sloan Digital Sky
Survey. In this work I will further increase the sample size with the
Panchromatic Synoptic Telescope And Rapid Response System 1
(Pan{\ndash}STARRS1).
  (cont.)
