Spectral Observations, 1965-1968, of the Peculiar Emission Object V1016 Cygni (MHα328-116)

Identifications and intensities are given for approximately 130 emission lines between 3130 and 5030 A measured on fifteen spechograms, with dispersions ranging from 12 to 130 A , taken during the 1965-1968 seasons. The line intensities and ratios do not give a completely consistent detailed picture; however, they do indicate that the temperature of the emitting regions increased from 1965 through 1967, and possibly through early 1969, and that the density decreased. The continuum remains very weak, and no absorption lines are seen. The radial velocity is -60 + 1.5 km , and tbe line widths (from the 12 A plates) are 80-120 km . Upper limits to radio emission from V1016 Cyg by Bell and Seaquist and by Webster are 0 1 f u at 4.6 cm and 0.07 f u at 11.1 cm. The object may be reaching maximum light: photoelectric results by Fernie and Philip show that V, B - V, and U - B remained essentially constaiit throughout 1968. The object V1016 Cyg may well be a planetary nebula in the early stages of its evolution.