新视野号观测宇宙光学背景
New Horizons Observations of the Cosmic Optical Background
摘要：
我们使用新视野LORRI相机的现有数据来测量七个高银河纬度区域内的光学波段（$0.4\lesssimλ\lesssim0.9{\rmμm}$）天空亮度。当新视野号距离太阳42到45天文单位时，测量到的平均原始水平是$33.2\pm0.5{\rm ~nW ~m^{-2} ~sr^{-1}}.$这是$\sim10\times$，比哈勃太空望远镜可以到达的最暗的天空还要暗，突出了新视野号探测宇宙光学背景（COB）的实用性。分离COB对原始总量的贡献需要减去明亮恒星和星系的散射光，低于视场内光度检测极限的暗淡恒星，以及由红外卷云散射的漫射银河系光。我们从IRIS $100μ$ m所有的天空图中删除新发现的残余黄道光，以产生两种不同的漫射银河光（DGL）的估计。使用这些产生在0.608 $μ$ m的LORRI枢轴波长下在${\rm 15.9\pm 4.2\ (1.8~stat., 3.7~sys.) ~nW ~m^{-2} ~sr^{-1}}$至${\rm 18.7\pm 3.8\ (1.8~stat., 3.3 ~sys.)~ nW ~m^{-2} ~sr^{-1}}$范围内的COB的高度显著的检测。从总COB水平中减去比光度检测极限更暗的星系积分光（IGL），留下了${\rm 8.8\pm4.9\ (1.8 ~stat., 4.5 ~sys.) ~nW ~m^{-2} ~sr^{-1}}$至${\rm 11.9\pm4.6\ (1.8 ~stat., 4.2 ~sys.) ~nW ~m^{-2} ~sr^{-1}}$范围内的未知来源的漫射通量分量。用未探测到的星系来解释它需要在$V>24$处星系计数的暗端斜率明显变陡，或者现有的调查用$V< 30.$遗漏了一半的星系
英文摘要：
We used existing data from the New Horizons LORRI camera to measure the optical-band ($0.4\lesssimλ\lesssim0.9{\rmμm}$) sky brightness within seven high galactic latitude fields. The average raw level measured while New Horizons was 42 to 45 AU from the Sun is $33.2\pm0.5{\rm ~nW ~m^{-2} ~sr^{-1}}.$ This is $\sim10\times$ darker than the darkest sky accessible to the {\it Hubble Space Telescope}, highlighting the utility of New Horizons for detecting the cosmic optical background (COB). Isolating the COB contribution to the raw total requires subtracting scattered light from bright stars and galaxies, faint stars below the photometric detection-limit within the fields, and diffuse Milky Way light scattered by infrared cirrus. We remove newly identified residual zodiacal light from the IRIS $100μ$m all sky maps to generate two different estimates for the diffuse galactic light (DGL). Using these yields a highly significant detection of the COB in the range ${\rm 15.9\pm 4.2\ (1.8~stat., 3.7~sys.) ~nW ~m^{-2} ~sr^{-1}}$ to ${\rm 18.7\pm 3.8\ (1.8~stat., 3.3 ~sys.)~ nW ~m^{-2} ~sr^{-1}}$ at the LORRI pivot wavelength of 0.608 $μ$m. Subtraction of the integrated light of galaxies (IGL) fainter than the photometric detection-limit from the total COB level leaves a diffuse flux component of unknown origin in the range ${\rm 8.8\pm4.9\ (1.8 ~stat., 4.5 ~sys.) ~nW ~m^{-2} ~sr^{-1}}$ to ${\rm 11.9\pm4.6\ (1.8 ~stat., 4.2 ~sys.) ~nW ~m^{-2} ~sr^{-1}}$. Explaining it with undetected galaxies requires the galaxy-count faint-end slope to steepen markedly at $V>24$ or that existing surveys are missing half the galaxies with $V< 30.$
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