超维里气体在哪里？III. 来自X射线阴影观测的见解及软弥散X射线背景的修正模型
Where is the Supervirial Gas? III. Insights from X-ray Shadow Observations and a revised Model for the Soft Diffuse X-ray Background
AI总结：
本文利用朱雀卫星六条视线的X射线阴影观测，排除了SDXB中NVII发射线和超维里温度热成分的本地起源，确认其来自银河系CGM，并提出修正的软弥散X射线背景模型。
摘要：
阴影观测为将软弥散X射线背景（SDXB）的前景成分与背景成分分离开来提供了有力工具。此类观测现已确认，“本地”前景由太阳风电荷交换和本地泡构成，而背景辐射来自银河系延展的环银河系介质（CGM）以及未分解的河外源。近年来，对SDXB的新数据和细致分析带来了两项新发现：（1）约0.5 keV处的过量辐射被证认为NVII发射线；（2）约0.8–1.0 keV处的过量辐射被证认为CGM中额外的超维里温度热成分。本文的目标是利用朱雀卫星沿六条视线进行的阴影观测，确定这两种成分中是否有任何一种来自“本地”源。我们消除了关于NVII辐射起源的模糊性，排除了本地起源。我们确认银河系CGM含有富氮等离子体，其平均（N/O）为超太阳丰度，比值为2.6±0.5，并认为富氮等离子体广泛分布于整个CGM中。我们在两条视线中发现超太阳Ne丰度，同样来自CGM。类似地，我们排除了热成分的本地起源，并确认其存在于遮蔽云之后。此外，我们提出了一个修正的软弥散X射线背景模型，这对河外天文学至关重要。
英文摘要：
Shadow observations provide a powerful tool to separate foreground components of the soft diffuse X-ray background (SDXB) from the background components. Such observations have now established that the ``local'' foreground is made of the solar wind charge exchange and the local bubble, and the background emission is from the extended circumgalactic medium (CGM) of the Milky Way and from the unresolved extragalactic sources. New data and careful analyses of the SDXB led to two new discoveries in recent years: (1) excess emission near 0.5 keV that is identified as the NVII emission line, and (2) excess emission near 0.8-1.0 keV that is identified with an additional, super-virial temperature hot thermal component of the CGM. The goal of this paper is to use Suzaku shadow observations along six sightlines to determine whether either of these components is from the ``local'' sources. We eliminate the ambiguity regarding the origin of NVII emission, ruling out the local origin. We confirm that the Milky Way CGM contains nitrogen-rich plasma, with a super-solar average (N/O) of 2.6+-0.5, and suggest that nitrogen-enhanced plasma is widespread throughout the CGM. We find super-solar Ne abundance in two sighlines, also from the CGM. Similarly, we rule out the local origin of the hot thermal component and confirm that it is present beyond the shadowing clouds. Furthermore, we provide a revised model of the soft diffuse X-ray background, which is crucial for extragalactic astronomy.
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