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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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摘要

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及其邻近区域的朱雀数据，以研究其周围的扩展发射。M 86核心、羽流和向西北方向延伸的尾部以及周围延伸的光晕都被清晰地探测到。从类似45度的位置角度。接近275度。，核心和扩展晕的表面亮度分布相对较好地用一个类似于0.5到15'-20'的β模型来表示。核心的X射线光谱用类似于0.9 keV和0.6 keV的kT双温模型表示。核心和晕的温度在星系中有一个正梯度，在r类似于7'时达到最大值kT，类似于1.0 keV，表明晕气体位于比星系更大的标度势结构中。羽流和尾部的温度分别为0.86+/-0.01千电子伏和1.00+/-0.01千电子伏。我们首次成功地分别测定了核心、羽流、尾和晕的α元素丰度。除Ne外，Fe的丰度比与各地的太阳比一致。核心和羽流中的铁丰度与0.7相似，而尾部的铁丰度与1.0相似，但考虑到ICM的不确定性，差异不显著。晕的丰度在r之前几乎相同，类似于10'，然后在r大于或类似于10时变得显著更小（0.2-0.3），表明金属丰度的气体仍保留在外晕中。根据表面亮度分布，我们估算了r<100 kpc时的气体质量（类似于3 x 10（10）M圆点）和动力学质量（类似于3 x 10（12）M圆点）。气体质量与动态质量之比为10（-3）-10（-2），表明大部分晕气体已被剥离。

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