  Nova V2491 Cyg is one of just two detected pre-outburst in X-rays. The light
curve of this nova exhibited a rare "re-brightening" which has been attributed
by some as the system being a polar, whilst others claim that a magnetic WD is
unlikely. By virtue of the nature of X-ray and spectroscopic observations the
system has been proposed as a recurrent nova, however the adoption of a 0.1 day
orbital period is generally seen as incompatible with such a system. In this
research note we address the nature of the progenitor system and the source of
the 0.1 day periodicity. Through the combination of Liverpool Telescope
observations with published data and archival 2MASS data we show that V2491
Cyg, at a distance of 10.5 - 14 kpc, is likely to be a recurrent nova of the U
Sco-class; containing a sub-giant secondary and an accretion disk, rather than
accretion directly onto the poles. We show that there is little evidence, at
quiescence, supporting a ~ 0.1 day periodicity, the variation seen at this
stage is likely caused by flickering of a re-established accretion disk. We
propose that the periodicity seen shortly after outburst is more likely related
to the outburst rather than the - then obscured - binary system. Finally we
address the distance to the system, and show that a significantly lower
distance (~ 2 kpc) would result in a severely under-luminous outburst, and as
such favour the larger distance and the recurrent nova scenario.
