使用非负矩阵分解寻找SDSS BALQSO
Finding SDSS BALQSOs Using Non-Negative Matrix Factorisation
摘要：
现代光谱数据库提供了丰富的信息，与天体物理种群的物理过程和环境。盲源分离（BSS）等技术将光谱分解为许多分量，提供了识别潜在物理排放过程特征的前景。主成分分析（PCA）已经取得了一定的成功，但严重限制了固有的正交性的限制，组件必须满足。非负矩阵分解（NMF）是一种相对较新的BSS技术，它在其分量上引入了非负性约束。在这方面，与使用主成分分析的情况相比，所得到的成分可以更接近地反映物理排放特征。我们讨论了一些应用NMF时必须考虑的问题，并通过其应用程序的类星体光谱在斯隆数字巡天（SDSS）DR6，我们表明，NMF是一种快速的方法产生紧凑和准确的重建的光谱。精确重建光谱的能力有许多天体物理学应用。结合改进的SDSS红移，我们将NMF应用于定义具有强宽吸收线（BAL）系统的类星体的鲁棒连续谱的问题。由此产生的SDSS DR6 BAL类星体目录将是最大的。重要的是，NMF的方法允许定量误差估计的Balnicity指数作为一个关键的天体物理和观测参数，如类星体的红移和光谱的信噪比的函数。
英文摘要：
Modern spectroscopic databases provide a wealth of information about the physical processes and environments associated with astrophysical populations. Techniques such as blind source separation (BSS), in which sets of spectra are decomposed into a number of components, offer the prospect of identifying the signatures of the underlying physical emission processes. Principle Component Analysis (PCA) has been applied with some success but is severely limited by the inherent orthogonality restriction that the components must satisfy. Non-negative matrix factorisation (NMF) is a relatively new BSS technique that incorporates a non-negativity constraint on its components. In this respect, the resulting components may more closely reflect the physical emission signatures than is the case using PCA. We discuss some of the considerations that must be made when applying NMF and, through its application to the quasar spectra in the Sloan Digital Sky Survey (SDSS) DR6, we show that NMF is a fast method for generating compact and accurate reconstructions of the spectra. The ability to reconstruct spectra accurately has numerous astrophysical applications. Combined with improved SDSS redshifts, we apply NMF to the problem of defining robust continua for quasars that exhibit strong broad absorption line (BAL) systems. The resulting catalogue of SDSS DR6 BAL quasars will be the largest available. Importantly, the NMF approach allows quantitative error estimates to be derived for the Balnicity Indices as a function of key astrophysical and observational parameters, such as the quasar redshifts and the signal-to-noise ratio of the spectra.
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