银极处的宇宙紫外背景
The Cosmic Ultraviolet Background at the Galactic Poles
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中文总结 AI 辅助
研究人员借助GALEX数据将银极宇宙紫外背景分解为尘埃散射光与偏移量，通过单次散射模型获尘埃颗粒特性，估算偏移量的未解释部分，明确偏移量恒定且方差小。
中文摘要 AI 辅助
我们利用存档的GALEX数据，将银极处的宇宙紫外背景分解为尘埃散射光和一个偏移量两个组分。我们用单次散射模型对尘埃散射光进行建模，得到在1530埃处反照率（a）的1σ限为0.54至0.71，相位函数非对称因子（g）为0.74至0.83；在2360埃处反照率（a）为0.66至0.73，相位函数非对称因子（g）为0.71至0.77，这表明尘埃颗粒具有中等反射性且高度前向散射。在1530埃处偏移量为277至284光子单位，在2360埃处为513至520光子单位。我们估算了偏移量的其他银内和银外贡献源，发现1530埃处有161±18光子单位未被解释，2360埃处有335±38光子单位未被解释，且这些区域的偏移量是恒定的，方差为20至30光子单位。
英文摘要
We have used archival GALEX data to separate the cosmic ultraviolet background at the Galactic Poles into two components: the dust scattered light and an offset. We have modeled the dust-scattered light using a single- scattering model finding 1 sigma limits of 0.54 -- 0.71 for the albedo (a) and 0.74 -- 0.83 for the phase function asymmetry factor (g) at 1530 Å and 0.66 -- 0.73 for a and 0.71 -- 0.77 for g at 2360 Å, that is, the grains are moderately reflective and highly forward-scattering. The offsets are 277 -- 284 photon units at 1530 Å and 513 -- 520 photon units at 2360 Å. We have estimated other Galactic and extragalactic contributors to the offset finding that 161 +- 18 photon units is unaccounted for at 1530 Å and 335 +- 38 at 2360 Å. The offsets are constant over these regions with variances of 20 -- 30 photon units.
