【摘要】：恒星光譜分類是天文數(shù)據(jù)處理中一項非常重要的工作,主要對海量光譜巡天數(shù)據(jù)按照其物理性質(zhì)進(jìn)行分類。利用殘差分布度量的方法對LAMOST巡天中觀測到的M矮星光譜進(jìn)行細(xì)分類研究。殘差分布度量是一種光譜間的距離度量方法,計算光譜之間的距離時,先將兩條光譜進(jìn)行歸一化處理,之后計算對應(yīng)波長采樣點處的殘差,最終以殘差分布的標(biāo)準(zhǔn)差作為光譜之間的距離。使用LAMOST DR2中釋放的M矮星光譜進(jìn)行細(xì)分類實驗。實驗結(jié)果表明,殘差分布度量方法能比較準(zhǔn)確地對M矮星光譜數(shù)據(jù)進(jìn)行細(xì)分類。還研究了信噪比、離群點以及殘差標(biāo)準(zhǔn)化系數(shù)等因素對分類結(jié)果的影響。
[Abstract]:Star spectral classification is a very important work in astronomical data processing, which mainly classifies massive spectral patrol data according to their physical properties. The spectra of M dwarfs observed in LAMOST survey are classified by residual distribution measurement. Residual distribution measurement is a distance measurement method between spectra. When calculating the distance between spectra, the two spectra are first normalized, and then the residual errors at the corresponding wavelength sampling points are calculated. Finally, the standard deviation of residual distribution is used as the distance between spectra. The M dwarf spectrum released from LAMOST DR2 was used for fine classification experiment. The experimental results show that the residual distribution measurement method can subdivide the spectral data of M dwarfs more accurately. The effects of signal-to-noise ratio (SNR), outlier and residual standardization coefficient on the classification results are also studied.
【作者單位】： 山東大學(xué)(威海)機電與信息工程學(xué)院;中國科學(xué)院光學(xué)天文重點實驗室國家天文臺;
【基金】：國家自然科學(xué)基金項目(U1431102,11473019)資助
【分類號】：P145.4
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本文編號：2484887