探测与银河系相关的软X射线发射的全天分布
Probing the All-sky Distribution of Soft X-ray Emission Associated with the Milky Way
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中文总结 AI 辅助
利用HaloSat和ROSAT数据对银河系软X射线发射进行全天分析，通过均匀光谱拟合和混合空间框架，发现暖热和热成分的双温度分布，并揭示热发射的复合起源。
中文摘要 AI 辅助
我们利用HaloSat和ROSAT数据对与银河系相关的软X射线发射进行了全天分析，将我们先前对五个银道面区域的研究扩展到全天330个天区。我们使用包含一个未吸收的局部热泡和两个额外吸收的热等离子体成分的模型进行了均匀的光谱拟合，分别代表暖热和热等离子体的发射，同时考虑了太阳风电荷交换和宇宙X射线背景。暖热成分通常被解释为来自星系周介质的发射，而热成分的起源仍不确定。单个天区的拟合通常倾向于包含热成分，天区间的温度分布中位数分别为kT = 0.19和0.74 keV，16-84百分位范围分别为0.17-0.21和0.61-0.90 keV。相应的16-84百分位发射度量范围分别为(1.0-8.2) x 10^-2和(0.5-4.1) x 10^-3 cm^-6 pc。来自60度 <= l <= 180度范围内天区的叠加光谱支持了单个天区的结果。在排除明亮的X射线源和大尺度银河系结构后，我们使用一个包含恒星发射以及盘状和晕状弥散等离子体成分的混合空间框架对178个天区的发射度量分布进行了建模。暖热发射主要由盘状项描述，而热发射主要由恒星发射并附加晕状项描述。这些结果支持广泛存在的双温度描述，并表明热发射具有复合起源。
英文摘要
We present an all-sky analysis of soft X-ray emission associated with the Milky Way using HaloSat and ROSAT data, extending our previous study of five Galactic-plane regions to 330 fields across the sky. We performed uniform spectral fitting with a model including an unabsorbed Local Hot Bubble and two additional absorbed thermal components, representing emission from warm-hot and hot plasma, while accounting for solar wind charge exchange and the cosmic X-ray background. The warm hot component is often interpreted as emission from the circumgalactic medium, whereas the origin of the hot component remains uncertain. Individual-field fits generally favored the inclusion of the hot component, and the field-to-field temperature distributions had medians of kT = 0.19 and 0.74 keV, with 16th-84th percentile ranges of 0.17-0.21 and 0.61-0.90 keV, respectively. The corresponding 16th-84th percentile EM ranges were (1.0-8.2) x 10-2 and (0.5-4.1) x 10-3 cm-6 pc. Stacked spectra from fields within 60 deg. <= l <= 180 deg. supported the individual-field results. After excluding bright X-ray sources and large-scale Galactic structures, we modeled the EM distributions of 178 fields using a hybrid spatial framework comprising stellar emission and disk-like and halo-like diffuse-plasma components. The warm-hot emission was described mainly by the disk-like term, whereas the hot emission was described mainly by stellar emission with an additional halo-like term. These results support a widespread two temperature description and suggest a composite origin for the hot emission.
发表机构
- Tokai National Higher Education and Research System, Nagoya University（东京大学高等教育与研究系统名古屋大学）
- NASA/Marshall Space Flight Center（美国国家航空航天局/马歇尔太空飞行中心）
- Tokyo University of Science（东京理科大学）
- NASA/Goddard Space Flight Center（美国国家航空航天局/戈达德太空飞行中心）
- LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS（大气、气候和地球动力学实验室/IPSL，巴黎萨克雷大学UVSQ分校，索邦大学，法国国家科学研究中心）
- The Henry A. Rowland Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学亨利·A·罗兰尔物理与天文学系）
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