The evolution of the nebular spectrum of the slow nova RR Telescopii

Results of spectroscopic observations of the slow nova RR Tel obtained from 1951 to 1973 with a Cassegrain, a Newtonian, and a coude spectrograph are compiled in order to present lists giving the intensity variations of all emission lines, wavelengths and identifications for these lines, and forbidden lines due to ions of argon and heavier elements. Mean radial velocities of RR Tel relative to the sun are derived separately from 13 H lines, 9 He I lines, 13 Ti II lines, 13 Fe II lines, and 12 Fe II forbidden lines. Temporal changes in the Balmer series are examined along with the behavior of numerous forbidden and allowed emission lines. The forbidden-line wavelengths are compared with those predicted on the basis of laboratory data, the complex structure of various very strong lines is analyzed, and a general working hypothesis is proposed that can account for some of the salient features observed. Four main stages are distinguished in the development of novae, and five nebular spectra are delineated. The nature (binary or single) of RR Tel is considered.