Suzaku的软x射线背景。2常温气泡?

IF 2.2 4区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Hayato Sugiyama, Masaki Ueda, Kotaro Fukushima, Shogo B Kobayashi, Noriko Y Yamasaki, Kosuke Sato, Kyoko Matsushita
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引用次数: 0

摘要

观测银河系中发射热x射线的星际介质对于研究恒星反馈和理解星系的形成和演化具有重要意义。我们给出了在75°<下的130个Suzaku观测的软x射线背景发射的测量结果;l, lt;285°和|b| >15°。使用由局部热泡和银河系晕组成的标准软x射线背景模型,在某些区域的光谱中残余结构保持在0.7-1 keV。加入温度为~ 0.8 keV(远高于银河系的虚拟温度)的碰撞电离平衡成分,显著降低了130次观测中56次的推导出的c统计量。0.8 keV分量的发射测量值变化超过一个数量级:假设太阳丰度,中位数为$3 \乘以10^{-4}\,\rm {cm^{-6}\ pc}$,第16 - 84百分位范围为$(1\!-\!8)\乘以10^{-4}\,\rm {cm^{-6}\ pc}$。猎户座-仙女座超级气泡方向的区域,有一个从猎户座OB1关联延伸出来的大空腔,有最高的0.8 keV分量的发射测量。虽然散射很大,但在星系纬度较低的地方,发射量往往更高。我们讨论了太阳风电荷交换、恒星和背景群可能引起的偏差。0.8 keV的成分可能是由银河系盘中的超新星加热的,可能与银河系喷泉有关。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
The soft X-ray background with Suzaku. II. Supervirial temperature bubbles?
Abstract Observations of the hot X-ray emitting interstellar medium in the Milky Way are important for studying the stellar feedback and for understanding the formation and evolution of galaxies. We present measurements of the soft X-ray background emission for 130 Suzaku observations at 75° &lt; l &lt; 285° and |b| &gt; 15°. With the standard soft X-ray background model consisting of the local hot bubble and of the Milky Way halo, residual structures remain at 0.7–1 keV in the spectra of some regions. Adding a collisional-ionization-equilibrium component with a temperature of ∼0.8 keV, much higher than the virial temperature of the Milky Way, significantly reduces the derived C-statistic for 56 out of 130 observations. The emission measure of the 0.8 keV component varies by more than an order of magnitude: assuming the solar abundance, the median value is $3 \times 10^{-4}\, \rm {cm^{-6}\ pc}$ and the 16th–84th percentile range is $(1\!-\!8) \times 10^{-4}\, \rm {cm^{-6}\ pc}$. Regions toward the Orion–Eridanus superbubble, having a large cavity extending from the Ori OB1 association, have the highest emission measures of the 0.8 keV component. While the scatter is large, the emission measures tend to be higher toward lower galactic latitudes. We discuss possible biases caused by the solar wind charge exchange, stars, and background groups. The 0.8 keV component is probably heated by supernovae in the Milky Way disk, possibly related to Galactic fountains.
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来源期刊
Publications of the Astronomical Society of Japan
Publications of the Astronomical Society of Japan 地学天文-天文与天体物理
CiteScore
4.10
自引率
13.00%
发文量
98
审稿时长
4-8 weeks
期刊介绍: Publications of the Astronomical Society of Japan (PASJ) publishes the results of original research in all aspects of astronomy, astrophysics, and fields closely related to them.
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