  I report updates to the substellar mass-radius diagram for 11 transiting
brown dwarfs (BDs) and low-mass stars published before the third data release
from the Gaia mission (Gaia DR3). I reanalyse these transiting BD systems whose
physical parameters were published between 2008 and 2019 and find that when
using the parallax measurements from Gaia DR3, 7 BDs show significant
differences in their radius estimate or an improvement in the radius
uncertainty. This has important implications for how these BDs are used to test
substellar evolutionary models in the mass-radius diagram. The remaining 4 BDs
show mass-radius estimates that are consistent with their previous pre-Gaia DR3
measurements. The 7 BDs that show significant deviation from the original
mass-radius measurements are AD 3116b, CoRoT-3b, CoRoT-15b, EPIC 201702477b,
Kepler-39b, KOI-205b, and KOI-415b. Of these, AD 3116b is a known member of the
Praesepe cluster at an age of 600 Myr. Additionally, some of the previously
smallest known transiting BDs, KOI-205b and KOI-415b, are not as small as once
thought, leaving the mass-radius region for the very oldest BDs relatively
sparse as a result of this work.
