PHOTOMETRIC RESPONSE FUNCTIONS OF THE SLOAN DIGITAL SKY SURVEY IMAGER
PHOTOMETRIC RESPONSE FUNCTIONS OF THE SLOAN DIGITAL SKY SURVEY IMAGER
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DOI：
10.1088/0004-6256/139/4/1628
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发表时间：
2010-02
期刊：
影响因子：
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通讯作者：
M. Doi;Masayuki Tanaka;M. Fukugita;J. Gunn;N. Yasuda;Ž. Ivezić;J. Brinkmann;Ernst de Haars
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文献类型：
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作者：
M. Doi;Masayuki Tanaka;M. Fukugita;J. Gunn;N. Yasuda;Ž. Ivezić;J. Brinkmann;Ernst de Haars
建立了一套单色光照明系统，对斯隆数字巡天（SDSS）中镶嵌CCD成像仪的响应函数进行了现场测量。该系统的概述和测量的结果，主要是在第一个六年的SDSS，进行了说明。我们提出了五个颜色通带的参考响应函数来自这些测量，并讨论列到列的变化和时间的变化，以及它们对测光的影响。我们还讨论了所产生的影响，从各种，略有不同的相关检测器系统，用于给SDSS光度的响应函数。我们表明，SDSS的校准程序删除这些变化相当不错，最终的误差从变量响应函数不太可能是大于0.01马格的g，r，i，z波段在整个调查期间。相当大的老化效应在u波段中未被发现，响应函数显示在调查年份期间短波长侧的吞吐量减少30%，这可能导致测光中的系统误差。老化效应与U波段仪器灵敏度的变化一致，U波段的仪器灵敏度已校准。预期的颜色变化与重复测光目录中的测量颜色变化一致。大多数恒星的颜色变化为Δ（u − g）<$0.01等，极端颜色的恒星最多为Δ（u − g）<$0.02等。我们在最终的星表中证实，在测光中没有发现超过0.01等的系统变化，这可以归因于老化和/或季节效应，除了极端颜色的恒星的长期u − g颜色变化。
The monochromatic illumination system is constructed to carry out in situ measurements of the response function of the mosaicked CCD imager used in the Sloan Digital Sky Survey (SDSS). The system is outlined and the results of the measurements, mostly during the first six years of the SDSS, are described. We present the reference response functions for the five color passbands derived from these measurements, and discuss column-to-column variations and variations in time, and also their effects on photometry. We also discuss the effect arising from various, slightly different response functions of the associated detector systems that were used to give SDSS photometry. We show that the calibration procedures of SDSS remove these variations reasonably well with the resulting final errors from variant response functions being unlikely to be larger than 0.01 mag for g, r, i, and z bands over the entire duration of the survey. The considerable aging effect is uncovered in the u band, the response function showing a 30% decrease in the throughput in the short wavelength side during the survey years, which potentially causes a systematic error in photometry. The aging effect is consistent with variation of the instrumental sensitivity in the u band, which is calibrated out. The expected color variation is consistent with measured color variation in the catalog of repeated photometry. The color variation is Δ(u − g) ∼ 0.01 for most stars, and at most Δ(u − g) ∼ 0.02 mag for those with extreme colors. We verified in the final catalog that no systematic variations in excess of 0.01 mag are detected in the photometry which can be ascribed to aging and/or seasonal effects except for the secular u − g color variation for stars with extreme colors.