Notes
Initially suggested to be a symbiotic binary or a recurrent nova due to its spectrum resembling the quiescent spectra of T CrB or RS Oph (Kopylov et al., 1988), later observations raised doubts. In Kato et al. (2002), it was argued that the object would be too close for a symbiotic binary based on its high proper motion. Additionally, the spectrum presented in Kopylov et al. (1988) was contested, with Kato et al. (2002) suggesting a low luminosity class instead. Henden et al. (2003) reported that the star studied by Kato et al. (2002) is not the one originally classified as V379 Peg; the star of interest is a faint blue object to the east of the red star. The blue star is the one that showed an outburst in 1981 (UV excess object, Lipovetsky & Stepanian, 1981). The star was classified as a confirmed symbiotic star in SIMBAD (Wenger et al., 2000). However, recent observations and data from Gaia EDR3 reported in Merc et al. (2021) confirm the non-symbiotic nature of the object.