# White Dwarf Luminosity Functions from the Pan{\ndash}STARRS1 3{\pi} Survey

## TL;DR

This paper constructs white dwarf luminosity functions using Pan-STARRS1 data, enhancing understanding of their distribution and properties in the Milky Way through proper motion selection.

## Contribution

It presents a new, larger sample of white dwarfs from Pan-STARRS1, improving the statistical analysis of their luminosity functions and Galactic distribution.

## Key findings

- White dwarf luminosity functions extend to fainter magnitudes.
- Sample size significantly increased compared to previous surveys.
- Results provide insights into the Galaxy's star formation history.

## Abstract

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.)