X-Ray Observation of a Magnetized Hot Gas Outflow in the Galactic Center Region
X-Ray Observation of a Magnetized Hot Gas Outflow in the Galactic Center Region
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DOI：
10.3847/1538-4357/ab0d82
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发表时间：
2019-03
期刊：
影响因子：
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通讯作者：
S. Nakashima;K. Koyama;Q. Wang;R. Enokiya
中科院分区：
文献类型：
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作者：
S. Nakashima;K. Koyama;Q. Wang;R. Enokiya
我们报道了在银河系北部中心(GC)区域用Suzaku观测到的1°尺度的X射线羽流。该羽状物位于前人报道的射电波瓣以东的(L，b)∼(0.°2，0.°6)。射电波瓣内部或以西没有发现明显的X射线超标。羽流的光谱显示出由高度电离的镁、硅和S产生的强发射线，这些谱线是由KT∼为0.7keV、太阳金属丰度为0.7keV的薄热等离子体模型重现的。不存在非平衡电离的特征。在1.5-3.0keV波段，未吸收表面亮度为3×10−14erg cm−2 S−1 Argmin−2。在软X射线波段的强星际吸收表明，该羽流不是前景源，而是位于GC距离处，其物理尺寸为∼100pC，密度为0.1cm−3，热压为1×10−10erg cm−3，质量为600M⊙，热能为7×1050erg。根据与偏振射电发射的明显联系，我们认为X射线羽流是从GC流出的磁化热气。
We report the discovery of a 1° scale X-ray plume in the northern Galactic Center (GC) region observed with Suzaku. The plume is located at (l, b) ∼ (0.°2, 0.°6), east of the radio lobe reported by previous studies. No significant X-ray excesses are found inside or to the west of the radio lobe. The spectrum of the plume exhibits strong emission lines from highly ionized Mg, Si, and S that are reproduced by a thin thermal plasma model with kT ∼ 0.7 keV and solar metallicity. There is no signature of non-equilibrium ionization. The unabsorbed surface brightness is 3 × 10−14 erg cm−2 s−1 arcmin−2 in the 1.5–3.0 keV band. Strong interstellar absorption in the soft X-ray band indicates that the plume is not a foreground source but is at the GC distance, giving a physical size of ∼100 pc, density of 0.1 cm−3, thermal pressure of 1 × 10−10 erg cm−3, mass of 600 M⊙, and thermal energy of 7 × 1050 erg. From the apparent association with a polarized radio emission, we propose that the X-ray plume is a magnetized hot gas outflow from the GC.