走向理解B[e]现象：VI。HD 85567的性质和光谱变化
Towards Understanding The B[e] Phenomenon: VI. Nature and Spectral Variations of HD 85567
摘要：
本文报道了HD 85567的高分辨率（$R \sim 80,000$）光谱观测结果，HD 85567被归类为FS CMa型天体或前主序星。主要目标是对对象的基本参数以及其性质和演化状态施加更多约束。HD 85567的吸收谱线与中B型矮星的吸收谱线相似，对应于以下基本参数：T $_{\rm eff} = 15000\pm500$ K，$v \sin i = 31\pm3$ km s $^{-1}$，$\log g \sim 4.0$ .星际消光，A $_V$ $= 0.50\pm0.02$ mag，是用一些弥散星际带的强度来测量的。我们还获得了一个$10^{\prime} \times 10^{\prime}$区域周围的对象的$UBV(RI)_{\rm c}$图像。通过对投影近的恒星进行测光，得出了该方向的星际消光定律，并得出该天体的距离为1300 $\pm$ 100 pc，光度为$\log$（L/L $_\odot) = 3.3\pm0.2$。我们在2012年和2015年两个月的时间内获得的HD 85567光谱中没有发现吸收线的显著径向速度变化。我们对这颗恒星的光谱和光度数据的分析使我们得出结论，它不可能是一颗前主序星Herbig Ae/Be。我们认为，拱星气体和尘埃是在对象的演化过程中产生的，最有可能是一个二元系统，其中包含一个未检测到的次要成分，不太可能是合并的产物。
英文摘要：
We report the results of high-resolution ($R \sim 80,000$) spectroscopic observations of the emission-line object HD 85567, which has been classified as a FS CMa type object or a pre-main-sequence star. The main goal is to put more constraints on the object's fundamental parameters as well as on its nature and evolutionary state. Absorption lines in the spectrum of HD 85567 were found similar to those of mid B--type dwarfs and correspond to the following fundamental parameters: T$_{\rm eff} = 15000\pm500$ K, $v \sin i = 31\pm3$ km s$^{-1}$, $\log g \sim 4.0$. The interstellar extinction, A$_V$ $= 0.50\pm0.02$ mag, was measured using the strengths of some diffuse interstellar bands. We also obtained $UBV(RI)_{\rm c}$ images of a $10^{\prime} \times 10^{\prime}$ region around the object. Photometry of projectionally close stars was used to derive an interstellar extinction law in this direction and resulted in a distance of 1300$\pm$100 pc to the object and a luminosity of $\log$ (L/L$_\odot) = 3.3\pm0.2$. We found no significant radial velocity variations of the absorption lines in the spectra of HD 85567 obtained during two month-long periods of time in 2012 and 2015. Our analysis of the spectroscopic and photometric data available for the star led us to a conclusion that it cannot be a pre-main-sequence Herbig Ae/Be star. We argue that the circumstellar gas and dust were produced during the object's evolution as most likely a binary system, which contains an undetected secondary component and is unlikely to be a merger product.
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