  We present here the first results of UVES observations of RR Tel. The
exceptional performances of the instrument have allowed the detection of new
spectral features and have led to an improvement in the identifications of
several emission lines. A direct comparison with the IUE observations in the
range 3045-3300 A has revealed the appearance of many weak and shallow lines,
most of them lacking a convincing identification. The Balmer lines are visible
up to H38 and are accompanied by the He II lines of the Pickering series. Also,
all of the He II emissions of the Pfund series, from 5858 A to 6408 A have been
detected. We made definite identifications of additional TiO bands at 4955 A
(alpha R_2 1-0), 5167 A (alpha R_2 0-0), 5445 A (alpha R_2 0-1), 5598 A (beta
R_1 0-0), 5847 A (gamma 'R_1 1-0), and 6148 A (gamma ' {^S} R_21 0-0). The
Halpha line has very wide wings, extending to at least 5000 km/s, which are
similar to those reported for the planetary nebula IC 4997 and attributed to
Raman scattering by Ly beta photons. A selective pumping mechanism via the HeII
237 A emission is proposed to explain the intensity of the high-lying lines of
O IV mult. 1 and 2.
