  We performed a detailed spectroscopic analysis of the dwarf nova V2051 Oph at
the end of its 1999 superoutburst. We studied and interpreted the simultaneous
behaviour of various emission lines.
  We obtained high-resolution echelle spectroscopic data at ESO's NTT with
EMMI, covering the spectral range of 4000--7500 Angstrom. The analysis was
performed using standard IRAF tools. The indirect imaging technique of Doppler
tomography was applied, in order to map the accretion disc and distinguish
between the different emission sources.
  The spectra are characterised by strong Balmer emission, together with lines
of HeI and the iron triplet FeII 42. All lines are double-peaked, but the
blue-to-red peak strength and central absorption depth vary. The primary's
velocity was found to be 84.9 km/sec. The spectrograms of the emission lines
reveal the prograde rotation of a disc-like emitting region and, for the Balmer
and HeI lines, an enhancement of the red-wing during eclipse indicates a bright
spot origin. The modulation of the double-peak separation shows a highly
asymmetric disc with non-uniform emissivity. This is confirmed by the Doppler
maps, which apart from the disc and bright spot emission also indicate an
additional region of enhanced emission in the 4th quadrant (+Vx, -Vy), which we
associate with the superhump light source. Given the behaviour of the iron
triplet and its distinct differences from the rest of the lines, we attribute
its existence to an extended gas region above the disc. Its origin can be
explained through the fluorescence mechanism.
