  Radio emission has been detected from tens of white dwarfs, in particular in
accreting systems. Additionally, radio emission has been predicted as a
possible outcome of a planetary system around a white dwarf. We searched for 3
GHz radio continuum emission in 846,000 candidate white dwarfs previously
identified in Gaia using the Very Large Array Sky Survey (VLASS) Epoch 1 Quick
Look Catalogue. We identified 13 candidate white dwarfs with a counterpart in
VLASS within 2". Five of those were found not to be white dwarfs in follow-up
or archival spectroscopy, whereas seven others were found to be chance
alignments with a background source in higher-resolution optical or radio
images. The remaining source, WDJ204259.71+152108.06, is found to be a white
dwarf and M-dwarf binary with an orbital period of 4.1 days and long-term
stochastic optical variability, as well as luminous radio and X-ray emission.
For this binary, we find no direct evidence of a background contaminant, and a
chance alignment probability of only ~2 per cent. However, other evidence
points to the possibility of an unfortunate chance alignment with a background
radio and X-ray emitting quasar, including an unusually poor Gaia DR3
astrometric solution for this source. With at most one possible radio emitting
white dwarf found, we conclude that strong (> 1-3 mJy) radio emission from
white dwarfs in the 3 GHz band is virtually nonexistent outside of interacting
binaries.
