  As part of a project to better characterize comparatively bright but so far
little studied cataclysmic variables in the southern hemisphere, we have
obtained spectroscopic and photometric data of the nova-like variables LS IV
-08$^{\rm o}$ 3 and HQ Mon, and of the Z Cam type dwarf nova ST Cha. The
spectra of all systems are as expected for their respective types. We derive
improved orbital ephemeris of LS IV -08$^{\rm o}$ 3 and map its accretion disk
in the light of the H$\alpha$ emission using Doppler tomography. We find that
the emission has a two component origin, arising in the outer parts of the
accretion disk and possibly on the illuminated face of the secondary star. The
light curve of LS IV -08$^{\rm o}$ 3 exhibits a low level of flickering and
indications for a modulation on the orbital period. Spectroscopy of HQ Mon
suggests an orbital period of $\approx$5.15 hours which is incompatible with
previous (uncertain) estimates. The light curves show the typical low scale
flickering of UX UMa type nova-like systems, superposed upon variations on
longer time scales. During one night a modulation with a period of $\approx$41
min is observed, visible for at least 4 hours. However, it does not repeat
itself in other nights. A spectroscopic orbital period of $\approx$5.5 hours is
derived for ST Cha. A previously suspected period of 6.8 hours (or
alternatively 9.6 hours), based on historical photographic photometry is
incompatible with the spectroscopic period. Moreover, we show that our new as
well as previous photometry does not contain evidence for the quoted
photometric period.
