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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >X-ray study of extended emission around M 86 observed with Suzaku
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X-ray study of extended emission around M 86 observed with Suzaku

机译：用舒萨库观察M 86周围延长发射的X射线研究

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We analyzed the Suzaku data of M 86 and its adjacent regions to study the extended emission around it. The M 86 core, the plume, and the tail extending toward the northwest were clearly detected, as well as the extended halo around them. From the position angle similar to 45 degrees. to similar to 275 degrees., the surface brightness distribution of the core and the extended halo was represented relatively well with a single beta-model of beta similar to 0.5 up to 15'-20' . The X-ray spectra of the core were represented with a two-temperature model of kT similar to 0.9 keV and similar to 0.6 keV. The temperatures of the core and the halo have a positive gradient in the and reach a maximum of kT similar to 1.0 keV at r similar to 7' , indicating that the halo gas is located in a larger-scale potential structure than that of the galaxy. The temperatures of the plume and the tail were 0.86 +/- 0.01 keV and 1.00 +/- 0.01 keV. We succeeded in determining the abundances of alpha-element separately for the core, the plume, the tail, and the halo for the first time. Abundance ratios with respect to Fe were consistent with the solar ratios everywhere, except for Ne. The abundance of Fe was similar to 0.7 in the core and in the plume, while that in the tail was similar to 1.0, but the difference was not significant considering the uncertainties of the ICM. The abundance of the halo was almost the same up to r similar to 10', and then it becomes significantly smaller (0.2-0.3) at r greater than or similar to 10 indicating that gas with metal abundance still remains in the outer halo. From the surface brightness distribution, we estimated the gas mass (similar to 3 x 10(10) M-circle dot ) and the dynamical mass(similar to 3 x 10(12) M-circle dot) in r < 100 kpc. The gas mass to the dynamical mass ratio was 10(-3)-10(-2), suggesting a significant fraction of the halo gas has been stripped.
机译：我们分析了M 86的Suzaku数据及其相邻地区，以研究其周围的延长排放。明确地检测到朝向西北部延伸的M 86芯，羽毛和尾部，以及周围的延长光晕。从类似于45度的位置角度。与275度相似。，核心和延伸光晕的表面亮度分布与类似于0.5至15'-20'的单一β模型相对较好地表示。芯的X射线光谱用两种类似的KT模型表示，类似于0.9keV，类似于0.6keV。芯的温度和晕圈在类似于7'的R中的阳性梯度达到相似的KT，并且达到与1.0keV相似的千kt，表明晕气体位于比星系的较大潜在结构中的较大潜在结构。 。羽流和尾部的温度为0.86 +/- 0.01 keV和1.00 +/- 0.01 keV。我们首次成功地确定了核心，羽流，尾部和光环的亚α元素的丰富。除了NE外，相对于Fe的丰富比率与无处不在的太阳能比一致。核心和羽毛中的Fe的丰度类似于0.7，而尾部的尾部类似于1.0，但考虑到ICM的不确定性，差异并不重要。卤素的丰度与10'相似的r几乎相同，然后r大于或类似于10的r变得明显更小（0.2-0.3），表明用金属丰度仍然存在于外光环中。从表面亮度分布，我们估计气体质量（类似于3×10（10）m圆点）和动态质量（类似于R <100kpc的3×10（12）m圆点）。气体质量与动态质量比为10（-3）-10（-2），表明已经剥离了卤素气体的显着分数。

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