基于残差分布度量的M矮星细分类研究  

Research on M Dwarf Sub-Classification Based on the Measurement of Residual Distribution

作　　者：康超[1] 潘景昌[1] 衣振萍[1] 韦鹏[2] 姜斌[1] 

机构地区：[1]山东大学(威海)机电与信息工程学院,山东威海264209 [2]中国科学院光学天文重点实验室,国家天文台,北京100012

出　　处：《光谱学与光谱分析》2016年第7期2279-2283,共5页Spectroscopy and Spectral Analysis

基　　金：国家自然科学基金项目(U1431102,11473019)资助

摘　　要：恒星光谱分类是天文数据处理中一项非常重要的工作,主要对海量光谱巡天数据按照其物理性质进行分类。利用残差分布度量的方法对LAMOST巡天中观测到的M矮星光谱进行细分类研究。残差分布度量是一种光谱间的距离度量方法,计算光谱之间的距离时,先将两条光谱进行归一化处理,之后计算对应波长采样点处的残差,最终以残差分布的标准差作为光谱之间的距离。使用LAMOST DR2中释放的M矮星光谱进行细分类实验。实验结果表明,残差分布度量方法能比较准确地对M矮星光谱数据进行细分类。还研究了信噪比、离群点以及残差标准化系数等因素对分类结果的影响。The classification of stellar spectra is an important job in data processing of astronomy ,which is mainly used for searching celestial spectra with known types in massive data survey .This paper focuses on LAMOST M dwarfs fine classification based on measurement of residual distribution .Residual distribution measurement is a measurement method used to measure the distance between two spectra .In the process of calculating the distance between two spectra ,normalized processing should come first .Then the residuals of the sampling points of corresponding wavelength are calculated .Eventually the standard deviation of the residual distribution as the distance between the spectra is calculated .In this paper ,the M star of LAMOST DR2 is used as the experimental data of classification .The experimental results show that the spectra data can be classified more accurately with the measurement method of residual distribution than the use of other traditional classification methods .The effect of spectral classification is affected by signal to noise ratio ,outliers ,residual standardized coefficient and other factors .

关 键 词：残差分布 距离度量 均方根误差 

分 类 号：P145.4[天文地球—天体物理]