天鹅座环东北至西南边缘的朱雀观测
Suzaku Observations across the Cygnus Loop from the Northeastern to the Southwestern Rim
摘要：
我们已经观察到天鹅座环从东北（NE）边缘到西南（SW）边缘使用朱雀在10点，这是刚刚北部的先前XMM牛顿观测。将获得的观测数据划分为45个矩形区域，其中宽度被配置为使得每个区域保持8000个$-$ 12000光子。用单kTe组分非平衡电离（NEI）模型或双kTe组分NEI模型对每个区域的光谱进行拟合。两kTe分量模型在几乎所有的非边缘区域中产生显著更好的拟合。从丰度和通量判断，高kTe组分（$-$ 0.8keV）应是喷出物的来源，而低\kTe组分（$\sim$ 0.3keV）则来自上扫物质。我们发现，在环中心的西南方，被扫起的物质壳层非常薄。结合以前的观测，我们估计这个薄壳区域的直径为$1^{\circ}$。在天鹅座圈的中心位置，O、Ne和Mg的喷出物分布较为均匀，Si和Fe的喷出物分布较为集中，而O、Ne和Mg的喷出物分布较集中，而Si和Fe的喷出物分布较集中，主要集中在天鹅座圈的西南部。我们计算了各种金属的质量，并估计天鹅座环的起源是12- 15 M的$_\odot$核心坍塌爆炸。
英文摘要：
We have observed the Cygnus Loop from the northeast (NE) rim to the southwest (SW) rim using Suzaku in 10 pointings that is just north of previous XMM-Newton observations. The observation data obtained were divided into 45 rectangular regions where the width were configured so that each region holds 8000$-$12000 photons. The spectrum acquired from each region was fitted either with one-kTe-component non-equilibrium ionization (NEI) model or with two-kTe-component NEI model. The two-kTe-component model yields significantly better fit in almost all the non-rim regions. Judging from abundances and flux, the high-kTe-component (0.4$-$0.8keV) must be the ejecta origin, while the low-\kTe-component ($\sim$0.3keV) comes from the swept-up matter. We found that swept-up matter shell is very thin in just southwest of center of the Loop. Together with previous observations, we estimate the diameter of this thin shell region to be $1^{\circ}$. We also found that the ejecta distributions were asymmteric to the geometric center: the ejecta of O, Ne and Mg were distributed more in the NE, while the ejecta of Si and Fe were distributed more in the SW of the Cygnus Loop. We calculated the masses for various metals and estimated the origin of the Cygnus Loop as the 12-15M$_\odot$ core-collapse explosion.
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