arXiv 0712.35382007-12-20astro-ph

比较Suzaku和XMM-牛顿观测的软X射线背景：太阳风电荷交换发射的证据

Comparing Suzaku and XMM-Newton Observations of the Soft X-ray Background: Evidence for Solar Wind Charge Exchange Emission

David B. Henley, Robin L. Shelton

备注：: 17 pages, 8 figures. Accepted for publication in the Astrophysical Journal
发表信息：: Astrophys.J. 676:335,2008
DOI：: 10.1086/528924

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摘要：

我们提出了一对朱雀光谱的软X射线背景（SXRB），从点上和关闭附近的阴影在南银河半球的灯丝的分析。由于两个指向方向上的银河柱密度不同，观测到的星系晕辐射在两个光谱中具有不同的形状。我们利用这种差异时，建模的光谱，从未吸收的前景发射从本地气泡（LB）的吸收晕发射分离。我们得到的温度和排放措施是显着不同的，从早期的分析XMM-牛顿光谱从相同的指向。我们将这种差异归因于XMM-牛顿光谱中存在以前未识别的太阳风电荷交换（SWCX）污染，这可能是由于太阳风移动穿过视线的局部增强。ACE的同期太阳风数据显示，在XMM-牛顿观测过程中没有任何异常。因此，我们的研究结果表明，简单地检查同期的太阳风数据可能是不够的，以确定是否频谱的SXRB被污染的SWCX排放。如果我们的朱雀光谱没有受到SWCX辐射的严重污染，我们的最佳拟合LB模型给出的温度为log T = 5.98 + 0.03/-0.04，压力为p/k = 13，100 - 16，100 cm^-3 K。这些值低于从LB的其他最近的观测中获得的值，这表明LB可能不是等温的，可能不是压力平衡的。与此同时，我们的光环模型表明，氖相对于氧和铁可能会增强，这可能是因为氧和铁部分存在于尘埃中。

英文摘要：

We present an analysis of a pair of Suzaku spectra of the soft X-ray background (SXRB), obtained from pointings on and off a nearby shadowing filament in the southern Galactic hemisphere. Because of the different Galactic column densities in the two pointing directions, the observed emission from the Galactic halo has a different shape in the two spectra. We make use of this difference when modeling the spectra to separate the absorbed halo emission from the unabsorbed foreground emission from the Local Bubble (LB). The temperatures and emission measures we obtain are significantly different from those determined from an earlier analysis of XMM-Newton spectra from the same pointing directions. We attribute this difference to the presence of previously unrecognized solar wind charge exchange (SWCX) contamination in the XMM-Newton spectra, possibly due to a localized enhancement in the solar wind moving across the line of sight. Contemporaneous solar wind data from ACE show nothing unusual during the course of the XMM-Newton observations. Our results therefore suggest that simply examining contemporaneous solar wind data might be inadequate for determining if a spectrum of the SXRB is contaminated by SWCX emission. If our Suzaku spectra are not badly contaminated by SWCX emission, our best-fitting LB model gives a temperature of log T = 5.98 +0.03/-0.04 and a pressure of p/k = 13,100-16,100 cm^-3 K. These values are lower than those obtained from other recent observations of the LB, suggesting the LB may not be isothermal and may not be in pressure equilibrium. Our halo modeling, meanwhile, suggests that neon may be enhanced relative to oxygen and iron, possibly because oxygen and iron are partly in dust.

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