2004BaltA..13..156S

A study of the LBV-like star B 416 in M 33 is presented. Spectrum, luminosity and variability indicate that this star is a B[e]-supergiant. We analyze the results of integral field and long slit spectroscopic observations of 1998-2002. The expansion velocity of a ring-like nebula surrounding the star is found to be 20 km/s. Ionization maps and line intensities show that the excitation of gas in the nebula is very similar to that in H II regions. We discuss spectral variability of B416 and compare our results with photometric data by Shemmer et al. (2000). We find its radial velocity variability and argue that the photometric 8.26 day period is actually a half of the orbital period 16.13±0.07 d. The data indicate that the star is a close interactive binary with a mass ratio of ∼0.4. The ring-like nebula could be formed by mass-loss in the equatorial plane. We suggest a possible connection between B[e]-supergiants and interacting binaries in general.