论文标题
根据SAAO的光度法，修订的月光天空亮度曲线的修订后的简化散射模型
A revised simplified scattering model for the moonlit sky brightness profile based on photometry at SAAO
论文作者
论文摘要
本文在明亮的月亮在场的情况下，介绍了萨瑟兰南非天文天文台（SAAO）的夜空亮度的多滤器测量。观察结果涵盖了各种各样的天空方向，月相和月球位置。与在天文学研究中经常应用的模型相比，经过修订的简化散射模型是为了估算月光引起的天空亮度，该模型更准确地反映了月球束的大气灭绝。量化了由于月光以外的来源而产生的夜空亮度的贡献，并从总天空背景辐射中减去，以确定散射月光的光谱强度和角度分布。然后，通过将天空变亮与传入的月球强度进行比较，使用新方法估计，从而得出了大气散射相函数。该相函数被证明是与合并理论雷利和MIE散射函数的绝佳匹配，后者具有HENYEY-Greenstein形式，而不是以前研究中经常使用的指数角度关系。在某些频段中，测量和模型天空亮度之间的偏差很明显，这些频段是通过多个散射或气球的贡献来解释的，并相应地量化。该模型构成了在光学波段中预测Saao在SAAO上的天空亮度的有效工具，尤其是在存在明亮的月亮中。该方法也很容易被调整为在其他天文站点。该论文还提供了$ ubv（ri）_c $和str {Ö}的49颗星的mgren光度法，大多数没有此类数据。
This paper presents multi-filter measurements of the night sky brightness at the South African Astronomical Observatory (SAAO) in Sutherland in the presence of a bright moon. The observations cover a wide range of sky directions, lunar phases and lunar positions. A revised simplified scattering model is developed for estimating the sky brightness due to moonlight that more accurately reflects the atmospheric extinction of the lunar beam compared to models frequently applied in astronomical studies. Contributions to night sky brightness due to sources other than moonlight are quantified and subtracted from the total sky background radiation to determine the spectral intensity and angular distribution of scattered moonlight. The atmospheric scattering phase function is then derived by comparing the sky brightening to the strength of the incoming lunar beam, estimated using a novel approach. The phase function is shown to be an excellent match to the combined theoretical Rayleigh and Mie scattering functions, the latter with a Henyey--Greenstein form instead of the exponential angular relationship often used in previous studies. Where deviations between measured and model sky brightness are evident in some bands these are explained by contributions from multiple scattering or airglow, and are quantified accordingly. The model constitutes an effective tool to predict sky brightness at SAAO in optical photometric bands, especially with a bright moon present. The methodology can also be readily be adapted for use at other astronomical sites. The paper furthermore presents $UBV(RI)_c$ and Str{ö}mgren photometry for 49 stars, most with no prior such data.
