  We analyse simultaneous UBVR quiescent light curves of the cataclysmic
variable V2051 Oph using the Physical Parameter Eclipse Mapping method in order
to map the gas temperature and surface density of the disc for the first time.
The disc appears optically thick in the central regions and gradually becomes
optically thin towards the disc edge or shows a more and more dominating
temperature inversion in the disc chromosphere. The gas temperatures in the
disc range from about 13500 K near the white dwarf to about 6000 K at the disc
edge. The intermediate part of the disc has temperatures of 9000 K to 6500 K.
  The quiescent disc (chromosphere) shows a prominent bright region with
temperatures of 10500 K around the impact region of the stream from the
secondary with an extension towards smaller azimuths. The disc has a size of
0.53 +- 0.03 R_L1 and a mass accretion rate of between dM/dt = 10^15 g/s to
10^17g/s. The light curves must include an uneclipsed component, a hot
chromosphere and/or a disc wind.
  The PPEM method allows us to determine a new distance of 146+-20pc,
compatible with previous rough estimates. For the white dwarf we then
reconstruct a temperature of 19600 K, if the lower hemisphere of the white
dwarf is occulted by the disc.
  We find that although V2051 Oph is very similar to the SU UMa type dwarf
novae HT Cas, OY Car and Z Cha, there must be a substantial difference in order
to explain its unique light curve. For further details and results see paper.
