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arXiv 1111.2136astro-ph.GA
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漫射H α背景与FUV连续统背景的比较--关于漫射H α背景的起源

Comparison of the Diffuse Halpha and FUV Continuum Backgrounds: On the Origins of the Diffuse Halpha Background

Kwang-Il Seon, Adolf Witt, Il-Joong Kim, Jong-Ho Shinn, Jerry Edelstein, Kyoung-Wook Min, Wonyong Han

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12 pages, 6 figures, accepted for publication in ApJ
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摘要：

我们比较了银河系的漫射H $α$图和FUV（1370- 1710）连续谱图。H $α$强度与FUV强度良好相关。H $α$ /FUV强度比一般随H $α$强度和FUV硬度比的增加而增加（1370- 1520 ~ 1560- 1710），这意味着晚OB星可能是高纬H $α$复合线的主要来源。H $α$强度随银河系纬度的变化也与FUV强度的变化非常相似。结果可能表明，不仅H $α$和FUV背景的原始辐射源，而且负责漫射背景的辐射转移机制在很大程度上是共同的。因此，我们提出了一个方案，其中在高纬度的H $α$背景主要由两个组成部分，H $α$光子产生的原位复合在电离区周围的晚OB星和尘埃散射光的H $α$光子起源于晚OB星。

英文摘要：

We compare the diffuse H$α$ map of our Galaxy with the FUV (1370-1710Å) continuum map. The H$α$ intensity correlates well with the FUV intensity. The H$α$/FUV intensity ratio increases in general with the H$α$ intensity and the FUV hardness ratio (1370-1520Å to 1560-1710Å), implying that late OB stars may be the main source of the H$α$ recombination line at high latitudes. The variation of the H$α$ intensity as a function of the Galactic latitude is also very similar to that of the FUV intensity. The results likely suggest that not only the original radiation sources of the H$α$ and FUV backgrounds but also the radiative transfer mechanisms responsible for the diffuse backgrounds are largely common. Therefore, we propose a scenario wherein the H$α$ background at high latitudes is mostly composed of two components, H$α$ photons produced by in-situ recombination at the ionized regions around late OB stars and dust-scattered light of the H$α$ photons originating from late OB stars.

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