  The nature of the progenitors of type Ia supernovae is still a mystery. While
plausible candidates are known for both the single degenerate and double
degenerate models, the observed numbers fall significantly short of what is
required to reproduce the type Ia supernovae rate.
  Some of the most promising single-degenerate type Ia progenitors are
recurrent novae and super-soft sources (SSS). White dwarfs with higher mass
transfer rates can also be type Ia supernova progenitors. For these rapidly
accreting white dwarfs (RAWD), more material than is needed for steady burning
accretes on the white dwarf, and extends the white dwarf's photosphere. Unlike
super-soft sources, such objects will likely not be detectable at soft X-ray
energies, but will be bright at longer wavelengths, such as the far ultraviolet
(UV). Possible examples include LMC N66 and the V Sagittae stars.
  We present a survey using multi-object spectrographs looking for RAWD in the
central core of the SMC, from objects selected to be bright in the far UV and
with blue far UV-V colors. While we find some unusual objects, and recover
known planetary nebula and WR stars, we detect no candidate RAWD. The upper
limits from this non-detection depending on our expectations of what a RAWD
should look like, as well assumptions about the internal extinction of the SMC.
Assuming they resemble LMC N66 or fainter versions of Wolf-Rayet stars we set
an upper limit of 10-14 RAWD in the SMC. However, our survey is unlikely to
detect objects like V Sge, and hence we cannot set meaningful upper limits if
RAWD generally resemble these.
