Energy spectra of the soft X-ray diffuse emission in fourteen fields observed with Suzaku
Energy spectra of the soft X-ray diffuse emission in fourteen fields observed with Suzaku
复制标题
DOI：
10.1093/pasj/61.4.805
复制
发表时间：
2009-03
影响因子：
2.3
通讯作者：
T. Yoshino;K. Mitsuda;N. Yamasaki;Y. Takei;T. Hagihara;K. Masui;Michael W. Bauer;D. McCammon;R. Fujimoto;Q. Wang;Y. Yao;Y. Yao
中科院分区：
文献类型：
--
作者：
T. Yoshino;K. Mitsuda;N. Yamasaki;Y. Takei;T. Hagihara;K. Masui;Michael W. Bauer;D. McCammon;R. Fujimoto;Q. Wang;Y. Yao;Y. Yao
文中给出了用Suzaku观测到的12个场的软漫射X射线发射，以及以前分析得到的另外两个场。它们都有银河系经度65度，L和295度，以避免来自从银河系中心延伸至少30度的非常明亮的漫射源的贡献。苏扎库9个无污染区域的地表亮度与RASS值在统计上是一致的，R45波段的差异上限为17×10~(-6)c S^~(-1)阿明~(-2)。Ovii和Oviii的强度之间有很好的相关性，Ovii的发射在~2个光子S^{-1}cm^{-2str^-1}(LU)处有一个强度底。高纬Oviii排放与地面以上Ovii过量排放密切相关，(Oviii强度)=0.5x[(Ovii强度)-2LU]，表明不同视线上的平均温度在~0.2keV附近具有较窄的分布。我们认为，Ovii的偏置强度来自日球层的太阳风电荷交换，可能来自局地热泡，而过剩的Ovii(2-7LU)是来自银河系较远部分的排放。该星系辐射的总测辐射光度为4×10^{39}尔格S^{-1}，其特征温度可能与银河系的维里温度有关。
The soft diffuse X-ray emission of twelve fields observed with Suzaku are presented together with two additional fields from previous analyses. All have galactic longitudes 65 deg < l < 295 deg to avoid contributions from the very bright diffuse source that extends at least 30 deg from the Galactic center. The surface brightnesses of the Suzaku nine fields for which apparently uncontaminated ROSAT All Sky Survey (RASS) were available were statistically consistent with the RASS values, with an upper limit for differences of 17 x 10^{-6} c s^{-1} amin^{-2} in R45}-band. The Ovii and Oviii intensities are well correlated to each other, and Ovii emission shows an intensity floor at ~2 photons s^{-1} cm^{-2 str^{-1} (LU). The high-latitude Oviii emission shows a tight correlation with excess of Ovii emission above the floor, with (Oviii intensity) = 0.5 x [(Ovii intensity) -2 LU], suggesting that temperatures averaged over different line-of-sight show a narrow distribution around ~0.2 keV. We consider that the offset intensity of Ovii arises from the Heliospheric solar wind charge exchange and perhaps from the local hot bubble, and that the excess Ovii (2-7 LU) is emission from more distant parts of the Galaxy. The total bolometric luminosity of this galactic emission is estimated to be 4 x 10^{39} erg s^{-1}, and its characteristic temperature may be related to the virial temperature of the Galaxy.