论文标题
M31中的Star J004229.87+410551.8的确认为A
Confirmation of the star J004229.87+410551.8 in M31 as a B[e] supergiant
论文作者
论文摘要
我们研究了仙女座银河系中的发光蓝色可变候选候选J004229.87+410551.8。早些时候，该恒星显示了光谱异常：尽管已经检测到热发射光谱，但它具有强大的CAII H和K吸收线。随后，恒星被假定为热巨人或b [e]超级巨头。为了进行清晰的恒星分类，我们使用Sao Ras的6米望远镜，Apache Point天文台的3.5-m ARC望远镜以及Sternerberg天文学研究所的高高的山观测站进行了光谱和光度分析。恒星的光谱具有FEII，[FEII]，[OI]和Balmer发射线。由于热的脉冲灰尘，其光谱能分布在近红外范围内显示出多余的范围。 STAR的发光度（$ \ log（l/l _ {\ odot}）= 4.6 \ pm 0.2 $）的指示特征和高估计值使我们最终可以将对象分类为B [e] Supergiant。
We study the luminous blue variable candidate J004229.87+410551.8 in the Andromeda Galaxy. Earlier, the star displayed a spectral anomaly: although a hot emission spectrum had been detected, it had strong CaII H and K absorption lines. Subsequently the star was assumed to be a hot hypergiant or a B[e] supergiant. For the purpose of clear star classification, we conducted spectroscopic and photometric analysis of the object and its surroundings with the 6-m telescope of SAO RAS, the 3.5-m ARC telescope of the Apache Point Observatory and the 2.5-m telescope of the Caucasus Mountain Observatory of the Sternberg Astronomical Institute. The spectrum of the star has the FeII, [FeII], [OI], and Balmer emission lines. Its spectral energy distribution shows an excess in the near-infrared range due to hot circumstellar dust. The indicated features and a high estimated value of star's luminosity ($\log (L/L_{\odot}) = 4.6\pm 0.2$) allow us to finally classify the object as a B[e] supergiant.
