ON THE CONSTRUCTION OF A NEW STELLAR CLASSIFICATION TEMPLATE LIBRARY FOR THE LAMOST SPECTRAL ANALYSIS PIPELINE
ON THE CONSTRUCTION OF A NEW STELLAR CLASSIFICATION TEMPLATE LIBRARY FOR THE LAMOST SPECTRAL ANALYSIS PIPELINE
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DOI：
10.1088/0004-6256/147/5/101
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发表时间：
2014-03
期刊：
影响因子：
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通讯作者：
P. Wei;A. Luo;Yin-Bi Li;Liangping Tu;Fengfei Wang;Jian-Na Zhang;Xiaoyan Chen;W. Hou;X. Kong;Yuehua Wu;F. Zuo;Jingchang Pan;Bin Jiang;Jie Liu;Z. Yi;Yongheng Zhao;Jian-Jun Chen;B. Du;Yan-xin Guo;Juanjuan Ren;Yi-Han Song;Meng-Xin Wang;Ke-Fei Wu;Haifeng Yang;G. Jin
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文献类型：
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作者：
P. Wei;A. Luo;Yin-Bi Li;Liangping Tu;Fengfei Wang;Jian-Na Zhang;Xiaoyan Chen;W. Hou;X. Kong;Yuehua Wu;F. Zuo;Jingchang Pan;Bin Jiang;Jie Liu;Z. Yi;Yongheng Zhao;Jian-Jun Chen;B. Du;Yan-xin Guo;Juanjuan Ren;Yi-Han Song;Meng-Xin Wang;Ke-Fei Wu;Haifeng Yang;G. Jin
LAMOST 光谱分析管道称为一维管道，旨在对 LAMOST 调查中观察到的光谱进行分类和测量。通过该管道，通过与模板光谱匹配，将观测到的恒星光谱分为不同的子类。因此，恒星分类的性能很大程度上取决于模板光谱的质量。本文构建了一个新的LAMOST恒星光谱分类模板库，旨在提高现有LAMOST恒星分类的精度和可信度。从 LAMOST 数据发布一中选择约 100 万个光谱来构建新的恒星模板，并根据两个标准将它们收集为 233 组：（1）通过将 LAMOST 光谱与斯隆数字巡天 ugriz 滤波器响应曲线卷积获得的伪 g − r 颜色，以及（2）LAMOST 管道给出的恒星子类。在每组中，模板光谱都是通过三个步骤构建的。 (1)使用局部异常值概率算法排除异常值，然后对每组的剩余光谱应用主成分分析方法。一百万个光谱中约有 5% 被排除为异常值。 (2) 使用每组的第一主成分重建所有剩余光谱。 (3)将加权平均谱作为各组的模板谱。通过前面的 3 个步骤，我们初步获得了 216 个恒星模板光谱。我们目视检查所有模板光谱，有 29 个光谱由于光谱质量低而被放弃。此外，剩余187个模板光谱的MK分类是通过与3个模板库进行比较来手动确定的。同时，放弃了10个子类难以确定的模板谱。最后，通过与当前库相结合，我们获得了包含 183 个 LAMOST 模板光谱、61 个不同 MK 类的新模板库。
The LAMOST spectral analysis pipeline, called the 1D pipeline, aims to classify and measure the spectra observed in the LAMOST survey. Through this pipeline, the observed stellar spectra are classified into different subclasses by matching with template spectra. Consequently, the performance of the stellar classification greatly depends on the quality of the template spectra. In this paper, we construct a new LAMOST stellar spectral classification template library, which is supposed to improve the precision and credibility of the present LAMOST stellar classification. About one million spectra are selected from LAMOST Data Release One to construct the new stellar templates, and they are gathered in 233 groups by two criteria: (1) pseudo g − r colors obtained by convolving the LAMOST spectra with the Sloan Digital Sky Survey ugriz filter response curve, and (2) the stellar subclass given by the LAMOST pipeline. In each group, the template spectra are constructed using three steps. (1) Outliers are excluded using the Local Outlier Probabilities algorithm, and then the principal component analysis method is applied to the remaining spectra of each group. About 5% of the one million spectra are ruled out as outliers. (2) All remaining spectra are reconstructed using the first principal components of each group. (3) The weighted average spectrum is used as the template spectrum in each group. Using the previous 3 steps, we initially obtain 216 stellar template spectra. We visually inspect all template spectra, and 29 spectra are abandoned due to low spectral quality. Furthermore, the MK classification for the remaining 187 template spectra is manually determined by comparing with 3 template libraries. Meanwhile, 10 template spectra whose subclass is difficult to determine are abandoned. Finally, we obtain a new template library containing 183 LAMOST template spectra with 61 different MK classes by combining it with the current library.