  We present an analysis of photometric observations of the eclipsing novalike
variable DW UMa made by the CBA consortium between 1999 and 2015. Analysis of
372 new and 260 previously published eclipse timings reveals a 13.6 year period
or quasi-period in the times of minimum light. The seasonal light curves show a
complex spectrum of periodic signals: both positive and negative superhumps,
likely arising from a prograde apsidal precession and a retrograde nodal
precession of the accretion disc. These signals appear most prominently and
famously as sidebands of the orbital frequency but the precession frequencies
themselves, at 0.40 and 0.22 cycles per day, are also seen directly in the
power spectrum. The superhumps are sometimes seen together and sometimes
separately. The depth, width and skew of eclipses are all modulated in phase
with both nodal and apsidal precession of the tilted and eccentric accretion
disc. The superhumps, or more correctly the precessional motions which produce
them, may be essential to understanding the mysterious SW Sextantis syndrome.
Disc wobble and eccentricity can both produce Doppler signatures inconsistent
with the true dynamical motions in the binary, and disc wobble might boost the
mass-transfer rate by enabling the hot white dwarf to directly irradiate the
secondary star.
