软X射线背景的XMM-牛顿巡天。I. O VII和O VIII在l=120和l=240之间的直线
An XMM-Newton Survey of the Soft X-ray Background. I. The O VII and O VIII Lines Between l=120 and l=240
摘要：
我们目前的测量软X射线背景（SXRB）O VII和O VIII之间的强度$l = 120\degr$和$l = 240\degr$，第一个结果的SXRB使用档案XMM-牛顿观测的调查。我们并不局限于空白天空的观测，而是尽可能多地使用观测，必要时用手去除明亮或延伸的光源。氧强度通常为~0.5-10光子/cm ^2/s/sr（线单位，L. U.）对于O VII和~0-5 L.U.第八章我们的数据集包括69个方向，具有多个观测值，其氧强度变化可用于约束SWCX模型。一个观察结果显示O VII增强约25 L. U。超过2个相同方向的其他观察结果，尽管大多数SWCX增强是$\la 4$ L. U。对于O VII和$\la 2$ L. U。第八章我们没有发现明确的趋势O VII质心移动到禁止线的能量与明亮的SWCX增强的意见。增强SWCX排放和增加太阳风通量或视线靠近磁鞘的太阳下区域之间也没有普遍的联系。在删除可能被日光层SWCX辐射污染的观测数据后，我们用我们的结果来研究星系晕。有一个简单的平面平行模型的预测晕强度的一些分散，指示斑块的晕发射。O VII/O VIII强度比表明晕圈温度约为2.0-2.5 MK，与以前的研究结果一致。（节录）
英文摘要：
We present measurements of the soft X-ray background (SXRB) O VII and O VIII intensity between $l = 120\degr$ and $l = 240\degr$, the first results of a survey of the SXRB using archival XMM-Newton observations. We do not restrict ourselves to blank-sky observations, but instead use as many observations as possible, removing bright or extended sources by hand if necessary. The oxygen intensities are typically ~0.5-10 photons/cm^2/s/sr (line units, L.U.) for O VII and ~0-5 L.U. for O VIII. Our dataset includes 69 directions with multiple observations, whose oxygen intensity variations can be used to constrain SWCX models. One observation exhibits an O VII enhancement of ~25 L.U. over 2 other observations of the same direction, although most SWCX enhancements are $\la 4$ L.U. for O VII and $\la 2$ L.U. for O VIII. We find no clear tendency for the O VII centroid to shift toward the forbidden line energy in observations with bright SWCX enhancements. There is also no universal association between enhanced SWCX emission and increased solar wind flux or the closeness of the sightline to the sub-solar region of the magnetosheath. After removing observations likely to be contaminated by heliospheric SWCX emission, we use our results to examine the Galactic halo. There is some scatter in the halo intensity about the predictions of a simple plane-parallel model, indicating a patchiness to the halo emission. The O VII/O VIII intensity ratio implies a halo temperature of ~2.0-2.5 MK, in good agreement with previous studies. (Abridged)
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