1 Introduction

The symbiotic nova RR Telescopii is one of a subclass of symbiotic stars. These are interacting binaries whose spectra indicate the presence of a late type star and a hot companion (Mürset et al. [1991]). RR Tel has been the subject of many extensive spectroscopic investigations (see, for example, Aller et al. [1973]) due to the great wealth of lines emitted since its outburst in 1944. Thackeray ([1977]) has compiled the observations of RR Tel from its outburst until the mid 1970s, and cites most relevant references.

McKenna et al. ([1997]) have presented a detailed calibrated list of 491 lines in the wavelength range 3444 - 9229Å in RR Tel, at a resolution of $\sim$12 kms^-1 (FWHM). However, it was impossible to distinguish many of the important spectral features due to blending at this resolution, and hence we have decided to further examine RR Tel's optical spectrum with a more powerful telescope. In this study, we have obtained new observations using a CCD detector with the University College London Echelle Spectrograph (UCLES) on the 3.9m telescope at the Anglo-Australian Observatory (AAO). These data are of higher spectral resolution ($\sim$6kms^-1) than the previous spectra, and so we are able to measure reliable emission line intensities for weaker features than was previously possible. The result is an improved line list for the optical spectrum of RR Tel with identifications and intensities of hitherto unidentified lines.