  White dwarfs with a F, G or K type companion represent the last common
ancestor for a plethora of exotic systems throughout the galaxy, though to this
point very few of them have been fully characterised in terms of orbital period
and component masses, despite the fact several thousand have been identified.
Gaia data release 3 has examined many hundreds of thousands of systems, and as
such we can use this, in conjunction with our previous UV excess catalogues, to
perform spectral energy distribution fitting in order to obtain a sample of 206
binaries likely to contain a white dwarf, complete with orbital periods, and
either a direct measurement of the component masses for astrometric systems, or
a lower limit on the component masses for spectroscopic systems. Of this sample
of 206, four have previously been observed with Hubble Space Telescope
spectroscopically in the ultraviolet, which has confirmed the presence of a
white dwarf, and we find excellent agreement between the dynamical and
spectroscopic masses of the white dwarfs in these systems. We find that white
dwarf plus F, G or K binaries can have a wide range of orbital periods, from
less than a day to many hundreds of days. A large number of our systems are
likely post-stable mass transfer systems based on their mass/period
relationships, while others are difficult to explain either via stable mass
transfer or standard common envelope evolution.
