Spectroscopic Study of Late-type Emission-line Stars Using the Data from LAMOST DR6
作者机构：Department of Physics and ElectronicsCHRIST (Deemed to be University) Department of Astronomy and AstrophysicsTata Institute of Fundamental Research The Oxford College of Science
出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究)
年 卷 期：2024年第12期
页 面：140-157页
核心收录：
学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学]
摘 要：Low-mass emission-line stars belong to various evolutionary stages, from pre-main-sequence young stars to evolved stars. In this work, we present a catalog of late-type (F0 to M9) emission-line stars from the LAMOST Data Release 6. Using the scipy package, we created a Python code that finds the emission peak at Hα in all latetype stellar spectra. A data set of 38,152 late-type emission-line stars was obtained after a rigorous examination of the photometric quality flags and the signal-to-noise ratio of the spectra. Adopting well-known photometric and spectroscopic methods, we classified our sample into 438 infrared (IR) excess sources, 4669 post-main-sequence candidates, 9718 Fe/Ge/Ke sources, and 23,264 d Me sources. From a crossmatch with known databases, we found that 29,222 sources, comprising 65 IR excess sources, 7899 Fe/Ge/Ke stars, 17,533 dMe stars, and3725 PtMS candidates, are new detections. We measured the equivalent width of the major emission lines observed in the spectra of our sample of emission-line stars. Furthermore, the trend observed in the line strengths of major emission lines over the entire late-type spectral range is analyzed. We further classified the sample into four groups based on the presence of hydrogen and calcium emission lines. This work presents a large data set of late-type emission-line stars, which can be used to study active phenomena in late-type stars.
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