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We report unfiltered photometry during superoutbursts of PU UMa in 2009 and2012. The amplitude was 4.5 magnitudes above mean quiescence and lasted atleast 9 to 10 days. Superhumps were present with a peak-to-peak amplitude of upto ~0.3 mag, thereby confirming it to be a member of the SU UMa family of dwarfnovae. The mean superhump period during the later part of the 2012 outburst wasPsh = 0.08076(40) d. Analysis of the eclipse times of minimum, supplementedwith data from other researchers, revealed an orbital period of Porb =0.077880551(17) d. The superhump period excess was epsilon = 0.037(5). Duringthe 2012 outburst, which was the better observed of the two, the FWHM eclipseduration gradually declined from 9.5 to 5 min. The eclipse depth was up to 1.7magnitudes.

The orbital and superhump periods of the deeply eclipsing dwarf nova PU UMa