  The third data release of Gaia introduced a large catalog of astrometric
binaries, out of which about 3,200 are likely main-sequence stars with a
white-dwarf (WD) companion. These binaries are typically found with orbital
separations of ~1 AU, a separation range that was largely unexplored due to
observational challenges. Such systems are likely to have undergone a phase of
stable mass transfer while the WD progenitor was on the asymptotic giant
branch. Here we study the WD mass distribution of a volume-complete sample of
binaries with K/M-dwarf primaries and orbital separations ~1 AU. We find that
the number of massive WDs relative to the total number of WDs in these systems
is smaller by an order of magnitude compared to their occurrence among single
WDs in the field. One possible reason can be an implicit selection of the WD
mass range if these are indeed post-stable-mass-transfer systems. Another
reason can be the lack of merger products in our sample compared to the field,
due to the relatively tight orbital separations of these systems. In addition,
we find that about 14% of these systems have distant tertiary companions within
1 pc.
