Notes
Previously classified as a VV Cep-type star, consisting of an M3Ia supergiant and a B-type companion, its possible symbiotic nature was suggested by Tomov & Mikołajewski (1988). They proposed that the hot component is notably fainter than a B2-3 main sequence star and observed rapid variability in the U band. Their spectroscopic data indicated a resemblance to the CH Cyg spectrum rather than VV Cep. The symbiotic classification was supported by Luthardt (1990), who identified irregular photometric variability occurring on a timescale of 275 to 450 days, along with a longer period around 5000 days. However, an analysis of IUE spectra by Shaw & Guinan (1989) did not align with the symbiotic classification. The absolute infrared magnitude confirmed the presence of an Iab class star (Munari et al., 2021).