Henize 177 - a slow nova, symbiotic star, X-ray source?

The rich emission-line spectrum of Henize 177 between 3300 A and 7100 A is described. Changes in line intensities occur between 1965 and 1972, but no short term radial velocity variation can be established. There is a line width, ionization level relation and the object must contain separate regions of varying velocity, ionization and physical conditions. The mode of ionization and excitation, collisional or radiative, and possible models of the system, single or binary, are discussed. Irrespective of whether the suggested identification of H 177 with the X-ray source 2U I is correct, the star contains high velocity gas with enough energy to produce X-rays.