  We report a photometric study of the WZ Sagittae-type dwarf nova PQ
Andromedae. The light curve shows strong (0.05 mag full amplitude) signals with
periods of 1263(1) and 634(1) s, and a likely double-humped signal with
P=80.6(2) min. We interpret the first two as nonradial pulsation periods of the
underlying white dwarf, and the last as the orbital period of the underlying
binary. We estimate a distance of 150(50) pc from proper motions and the two
standard candles available: the white dwarf and the dwarf-nova outburst. At
this distance, the K magnitude implies that the secondary is probably fainter
than any star on the main sequence -- indicating a mass below the Kumar limit
at 0.075 M_sol. PQ And may be another "period bouncer", where evolution now
drives the binary out to longer period.
