用SDSS恒星光谱测量红化和重新校准SFD
Measuring Reddening with SDSS Stellar Spectra and Recalibrating SFD
摘要：
我们目前的尘埃红化的测量使用的颜色与光谱的恒星在斯隆数字巡天。我们测量变红作为恒星的测量和预测颜色之间的差异，从SEGUE恒星参数管道（Lee et al. 2008 a）的恒星参数中导出。我们在每颗恒星的u-g，g-r，r-i和i-z颜色上获得了56，34，25和29 mmag的不确定度，尽管不确定度取决于恒星类型和恒星的大小。基于光谱的红化测量证实了我们早期的“蓝尖”红化测量（Schlafly等人，2010，S10），在去除4%的归一化差异后，发现u-g、g-r、r-i和i-z的红化系数与蓝尖方法的红化系数相差-3%，1%，1%和2%。结果表明，R_V=3.1的Fitzpatrick（1999）红化定律优于O 'Donnell（1994）或Cardelli等（1989）红化定律。我们提供了一个表的转换系数从Schlegel等。（1998年）的地图E（B-V）的消光在88个带通的4个值的R_V，使用这个红化的法律和14%的SFD的重新校准首先报告的S10和确认在这项工作中。
英文摘要：
We present measurements of dust reddening using the colors of stars with spectra in the Sloan Digital Sky Survey. We measure reddening as the difference between the measured and predicted colors of a star, as derived from stellar parameters from the SEGUE Stellar Parameter Pipeline (Lee et al. 2008a). We achieve uncertainties of 56, 34, 25, and 29 mmag in the colors u-g, g-r, r-i, and i-z, per star, though the uncertainty varies depending on the stellar type and the magnitude of the star. The spectrum-based reddening measurements confirm our earlier "blue tip" reddening measurements (Schlafly et al. 2010, S10), finding reddening coefficients different by -3%, 1%, 1%, and 2% in u-g, g-r, r-i, and i-z from those found by the blue tip method, after removing a 4% normalization difference. These results prefer an R_V=3.1 Fitzpatrick (1999) reddening law to O'Donnell (1994) or Cardelli et al. (1989) reddening laws. We provide a table of conversion coefficients from the Schlegel et al. (1998) maps of E(B-V) to extinction in 88 bandpasses for 4 values of R_V, using this reddening law and the 14% recalibration of SFD first reported by S10 and confirmed in this work.
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