利用新视野号对高银纬线和连续谱发射（912 - 1600 Å）的观测
Observations of High Galactic Latitude Line and Continuum Emission (912 - 1600 Å) with New Horizons
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中文总结 AI 辅助
该研究利用新视野号对912 - 1600 Å的宇宙紫外背景进行观测，检测到多种发射线，确认1135 Å处发射线源于银河系，分析了尘埃散射连续谱，给出尘埃颗粒反照率等结果，发现与之前研究一致的偏移量，确认大部分发射来自CUVB未识别成分。
中文摘要 AI 辅助
我们利用新视野号航天器上爱丽丝光谱仪的斯特恩孔径，在距离太阳56天文单位处对912 - 1600 Å的宇宙紫外背景（CUVB）进行了观测，为漫射源提供了9 Å的光谱分辨率。我们在3σ水平上检测到CIII（977 Å）和CIV（1548/1551 Å）发射线，强度分别为4200±1500和4100±1200 ph cm⁻² s⁻¹ sr⁻¹，还对OVI（1032/1038 Å）进行了边缘检测，强度为1400±1300 ph cm⁻² s⁻¹ sr⁻¹。我们报告在1135 Å处有3σ的发射线检测，已确定为N I共振三重态。首次确认它一定起源于银河系。尘埃散射连续谱由少数（N < 100）O9 - B2恒星主导，显示出恒星光谱中1000 Å附近的深吸收特征。模型表明，对于相位函数不对称性g < 0.6的尘埃颗粒，在大部分光谱（950 - 1550 Å）上反照率a < 0.5。我们发现一个偏移量，包括河外背景光和晕贡献者，与我们之前从Box得到的结果一致，包括莱曼极限附近偏移量的下降。我们确认大部分发射一定来自CUVB中未识别的成分。
英文摘要
We present observations of the cosmic ultraviolet background (CUVB) from 912 - 1600 A using the Stem aperture of the Alice spectrograph on the New Horizons spacecraft at 56 AU from the Sun, providing a spectral resolution of 9 A for diffuse sources. We detect emission lines of CIII (977 A) and CIV (1548/1551 A) at the 3 sigma level with strengths of 4200 +/- 1500 and 4100 +/- 1200 ph cm(-2) s(-1) sr(-1), respectively, and a marginal detection of OVI (1032/1038 A) at 1400 +/- 1300 ph cm(-2) s(-1) sr(-1). We report a 3 sigma detection of an emission line at 1135 A, which we have identified with the N I resonance triplet. Although this line had earlier been observed in FUSE and SPEAR data, it had been attributed to airglow or instrumental effects. We confirm, for the first time, that it must originate in the Galaxy. The dust-scattered continuum is dominated by a small number (N < 100) of O9 - B2 stars and shows the deep absorption feature near 1000 A seen in the stellar spectrum. Our models suggest an albedo of a < 0.5 over most of the spectrum (950 -- 1550 A) for the dust grains with the phase function asymmetry of g < 0.6. We find an offset, comprising the extragalactic background light and halo contributors, consistent with our earlier results from the Box, including the decline in the offset near the Lyman limit. We confirm that much of the emission must be from an unidentified component of the CUVB.
