In what precedes, we have seen that the absorption lines do not permit to attribute a unique spectral type to the star. The equivalent widths of H delta gave B5; the He I lines, B7-8 III; Ca II (3933), A0; Si II, B 5 III; Mg II (4481) B 5 Ia and finally CII (4267) gives B 5 III. Furthermore we remark that the emission lines present (Fe II, [FeII], N I) are usually found only in stars earlier than B 5. We recall that Houziaux (1961) classed the star as B 5 IV and Doazan B 5 V, the former from low dispersion spectra and the latter from high dispersion spectra. We adopt finally B 5 III from Jaschek et al. (1992) as the best spectral type for the blue spectral region.
Outside the present spectral range, the star was classified in the near ultraviolet as B9 pec by Heck et al. (1984); Hutsemekers calls it B 8.
We recall that we found a similar inconsistency of the spectral type from the blue region and the ultraviolet in the case of HD 45677, a star which shares many characteristics with the present one.
A luminosity class III is also compatible with the astrometric data. The distance of the
star would be 450 pc. The proper motion (0
014 /year)
gives then 30 km/s, the galactic latitude (-3.1) a heigth of 27 pc
above the galactic plane and even the small interstellar extinction
(<=0.10) would be compatible with the relatively small distance.