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We study the luminous blue variable candidate J004229.87+410551.8 in theAndromeda Galaxy. Earlier, the star displayed a spectral anomaly: although ahot emission spectrum had been detected, it had strong CaII H and K absorptionlines. Subsequently the star was assumed to be a hot hypergiant or a B[e]supergiant. For the purpose of clear star classification, we conductedspectroscopic and photometric analysis of the object and its surroundings withthe 6-m telescope of SAO RAS, the 3.5-m ARC telescope of the Apache PointObservatory and the 2.5-m telescope of the Caucasus Mountain Observatory of theSternberg Astronomical Institute. The spectrum of the star has the FeII,[FeII], [OI], and Balmer emission lines. Its spectral energy distribution showsan excess in the near-infrared range due to hot circumstellar dust. Theindicated features and a high estimated value of star's luminosity ($\log(L/L_{\odot}) = 4.6\pm 0.2$) allow us to finally classify the object as a B[e]supergiant.

Confirmation of the star J004229.87+410551.8 in M31 as a B[e] supergiant