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首页> 外文期刊>The Astrophysical journal >THE FIRST DETECTIONS OF THE EXTRAGALACTIC BACKGROUND LIGHT AT 3000, 5500, AND 8000 A. Ⅱ. MEASUREMENT OF FOREGROUND ZODIACAL LIGHT
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THE FIRST DETECTIONS OF THE EXTRAGALACTIC BACKGROUND LIGHT AT 3000, 5500, AND 8000 A. Ⅱ. MEASUREMENT OF FOREGROUND ZODIACAL LIGHT

机译：在3000、5500和8000 A时探测外星系背景光的方法。Ⅱ。前兆黄道光的测量

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摘要

We present a measurement of the absolute surface brightness of the zodiacal light (3900-5100 A) toward a fixed extragalactic target at high ecliptic latitude based on moderate-resolution (～1.3 A pixel~(-1)) spectropho-tometry obtained with the du Pont 2.5 m Telescope at the Las Campanas Observatory in Chile. This measurement and contemporaneous Hubble Space Telescope data from the Wide Field Planetary Camera 2 and Faint Object Spectrograph comprise a coordinated program to measure the mean flux of the diffuse extragalactic background light (EBL). The zodiacal light at optical wavelengths results from scattering by interplanetary dust so that the zodiacal light flux toward any extragalactic target varies seasonally with the position of the Earth. This measurement of zodiacal light is therefore relevant to the specific observations (date and target field) under discussion. To obtain this result, we have developed a technique that uses the strength of the zodiacal Fraunhofer lines to identify the absolute flux of the zodiacal light in the multiple-component night-sky spectrum. Statistical uncertainties in the result are 0.6% (1 σ). However, the dominant source of uncertainty is systematic errors, which we estimate to be 1.1% (1 σ). We discuss the contributions included in this estimate explicitly. The systematic errors in this result contribute 25% in quadrature to the final error in our coordinated EBL measurement, which is presented in the first paper of this series.
机译：我们基于中等分辨率（〜1.3 A pixel〜（-1））分光光度法，通过高分辩率获得了黄道纬度上朝向固定河外目标的黄道光（3900-5100 A）的绝对表面亮度的测量结果。杜邦2.5 m望远镜，位于智利拉斯坎帕纳斯天文台。来自广角行星相机2和微弱物体光谱仪的这一测量和同时期的哈勃太空望远镜数据包括一个协调程序，用于测量漫射河外背景光（EBL）的平均通量。光学波长的黄道光是由于行星际尘埃的散射而产生的，因此朝向任何银河外目标的黄道光通量会随着地球的位置而季节性变化。因此，黄道光的这种测量与所讨论的特定观察（日期和目标场）有关。为了获得此结果，我们开发了一种技术，该技术利用黄道弗劳恩霍夫谱线的强度来确定多分量夜空光谱中黄道光的绝对通量。结果的统计不确定性为0.6％（1σ）。但是，不确定性的主要来源是系统误差，我们估计其为1.1％（1σ）。我们将明确讨论此估算中包含的贡献。该结果中的系统误差与我们的协同EBL测量中的最终误差在正交上的贡献为25％，这在本系列的第一篇论文中已有介绍。

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