  The first results of a photometric survey of faint Cataclysmic Variables are
presented. V359 Cen is an SU UMa star with a period of 112 min. Even though
observed at quiescence, the mass transfer rate in this old nova may be
sufficiently high that in such a short period system (with its implied small
mass ratio) the disc may be excited into an elliptical shape with the result
that the observed brightness modulation gives a superhump period rather than an
orbital period. XZ Eri is an eclipsing dwarf nova with an orbital period
(P(orb)) of 88.1 min. HY Lup has only slight variability. V351 Pup, the remnant
of Nova Puppis 1991, has P(orb) = 2.837 h and a light curve that strongly
resembles that of the magnetic Nova Cyg 1975. V630 Sgr is the first nova
remnant that has both positive superhumps (P(sh) = 2.980 h) and eclipses
(P(orb) = 2.831 h). The YY Tel identification is somewhat uncertain. The
correct identification for CQ Vel is provided from discovery of its flickering
activity. The light curve of CE-315, a recently discovered AM CVn star, shows
similarities to that of GP Com, with no apparent orbital modulation.
