A detailed spectroscopic analysis of the dwarf nova V2051 Oph at the end of its 1999 superoutburst, will be presented.  We study and interpret the simultaneous behavior of various emission lines.  We obtained high resolution echelle spectroscopic data at ESO's NTT with EMMI, covering the spectral range  of  4000--7500A. The analysis was performed using  the IRAF standard 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 characterized 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 78.5km/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 a 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 fourth quadrant (+Vx, -Vy), which we associate with the superhump light source. Given the behavior 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 well be explained through the fluorescence mechanism.