【摘要】：恒星光譜分類是天文數(shù)據(jù)處理中一項(xiàng)非常重要的工作,主要對(duì)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(duì)LAMOST巡天中觀測(cè)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(jì)算光譜之間的距離時(shí),先將兩條光譜進(jìn)行歸一化處理,之后計(jì)算對(duì)應(yīng)波長(zhǎng)采樣點(diǎn)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(shí)驗(yàn)。實(shí)驗(yàn)結(jié)果表明,殘差分布度量方法能比較準(zhǔn)確地對(duì)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(diǎn)以及殘差標(biāo)準(zhǔn)化系數(shù)等因素對(duì)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(jī)電與信息工程學(xué)院;中國(guó)科學(xué)院光學(xué)天文重點(diǎn)實(shí)驗(yàn)室國(guó)家天文臺(tái);
【基金】：國(guó)家自然科學(xué)基金項(xiàng)目(U1431102,11473019)資助
【分類號(hào)】：P145.4
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本文編號(hào)：2484887