0.1%水平下的精密度分光光度法
Precision Spectrophotometry at the Level of 0.1%
摘要：
准确的相对分光光度法对于许多科学应用是至关重要的。通量校准中的小波长标度残差会显著影响光谱中弱发射和吸收特征的测量。利用斯隆数字巡天数据，我们证明了精心挑选的红序列星系的平均光谱可以作为光谱标准，以提高相对分光光度精度为0.1%的小波长尺度（从几个到几百个埃）。我们通过比较微小红移间隔的叠加光谱来实现这种精度。红移间隔必须足够小，以使任何系统的恒星星族演化最小化，并且小于分光光度不确定度。这种纯粹的经验技术不需要任何关于真实星系光谱的理论知识。它可以适用于所有大型光谱星系红移调查，采样大量的星系在一个统一的人口。
英文摘要：
Accurate relative spectrophotometry is critical for many science applications. Small wavelength scale residuals in the flux calibration can significantly impact the measurements of weak emission and absorption features in the spectra. Using Sloan Digital Sky Survey data, we demonstrate that the average spectra of carefully selected red-sequence galaxies can be used as a spectroscopic standard to improve the relative spectrophotometry precision to 0.1% on small wavelength scales (from a few to hundreds of Angstroms). We achieve this precision by comparing stacked spectra across tiny redshift intervals. The redshift intervals must be small enough that any systematic stellar population evolution is minimized and less than the spectrophotometric uncertainty. This purely empirical technique does not require any theoretical knowledge of true galaxy spectra. It can be applied to all large spectroscopic galaxy redshift surveys that sample a large number of galaxies in a uniform population.
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