2007PASP..119..388S

We present time-resolved CCD photometry of the recently discovered (V≃15 at maximum light) eruptive variable star in Taurus, which we dub VS 0329+1250. A total of ∼20 hr of data obtained over six nights reveal superhumps in the light curves, confirming the star as a member of the SU UMa class of dwarf novae. The superhumps recur with a mean period of 0.053394(7) days (76.89 minutes), which represents the shortest known superhump period in a classical SU UMa star. A quadratic fit to the timings of superhump maxima reveals that the superhump period was increasing at a rate given by P{dot}_sh≃(2.1±0.8)x10^–5 over the course of our observations. An empirical relation between orbital period and the absolute visual magnitude of dwarf novae at maximum light suggests that VS 0329+1250 lies at a distance of ∼1.2±0.2 kpc.