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We present a critical review of the determination of fundamental parametersof white dwarfs discovered by the Gaia mission. We first reinterpretcolor-magnitude and color-color diagrams using photometric and spectroscopicinformation contained in the Montreal White Dwarf Database (MWDD), combinedwith synthetic magnitudes calculated from a self-consistent set of modelatmospheres with various atmospheric compositions. The same models are thenapplied to measure the fundamental parameters of white dwarfs using theso-called photometric technique, which relies on the exquisite Gaiatrigonometric parallax measurements, and photometric data from Pan-STARRS,SDSS, and Gaia. In particular, we discuss at length the systematic effectsinduced by these various photometric systems. We then study in great detail themass distribution as a function of effective temperature for the white dwarfsspectroscopically identified in the MWDD, as well as for the white dwarfcandidates discovered by Gaia. We pay particular attention to the assumedatmospheric chemical composition of cool, non-DA stars. We also briefly revisitthe validity of the mass-radius relation for white dwarfs, and the recentdiscovery of the signature of crystallization in the Gaia color-magnitudediagram for DA white dwarfs. We finally present evidence that the corecomposition of most of these white dwarfs is, in bulk, a mixture of carbon andoxygen, an expected result from stellar evolution theory, but never empiricallywell established before.

On the Measurement of Fundamental Parameters of White Dwarfs in the Gaia Era