Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055
Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055
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DOI：
10.1093/mnras/stz2437
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发表时间：
2019-08
影响因子：
4.8
通讯作者：
C. Braun;S. Safi-Harb;Chris Fryer
中科院分区：
文献类型：
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作者：
C. Braun;S. Safi-Harb;Chris Fryer
我们对超新星遗迹RCW 103（G332.4 - 00.4）进行了钱德拉和XMM-牛顿成像和光谱研究，其中包含中心致密天体1 E 161348 - 5055。高分辨率的钱德拉X射线图像显示，东南部和西北部地区的辐射增强。使用XMM-牛顿数据的Fe L，Mg，Si和S的等效宽度线图像被用来映射喷出物的分布。SNR被分成56个区域，最好的特点是由两个组件的热模型。较硬的成分（kT = 0.6 keV）可以用VPSHOCK非平衡电离模型来拟合，电离时间尺度净值为1011-1012 cm−3 s，丰度略高于太阳值。用APEC模型拟合的软分量（kT 0.2 keV）可以用碰撞电离平衡下的等离子体很好地描述，其丰度与太阳值一致。假设距离为3.1千秒差距，Sedov阶段膨胀到均匀介质中，我们估计SNR年龄为4.4千年，上扫质量Msw = 16 $f_\mathrm { s}^{-1/2}$ D$_{3.1}^{5/2}$ M，低爆炸能量E* = 3.7 × 1049 $f\mathrm{ s}^{-1/2}$ D $3.1}^{5/2}$ erg。如果我们放松Sedov假设，等离子体具有低填充因子，等离子体温度被低估，或者如果SNR扩展到祖先的风吹气泡中，那么这个能量可能会高出一个数量级。标准的爆炸模型并不符合喷出物的产量。通过将拟合的丰度与最新的核心坍缩核合成模型进行比较，我们的最佳估计产生了大约12-13 M的低质量祖先，低于以前的报道。我们讨论了模型拟合中的简并性，特别是改变爆炸能量对母体质量估计的影响。
We present a Chandra and XMM–Newton imaging and spectroscopic study of the supernova remnant (SNR) RCW 103 (G332.4−00.4) containing the central compact object 1E 161348−5055. The high-resolution Chandra X-ray images reveal enhanced emission in the south-eastern and north-western regions. Equivalent width line images of Fe L, Mg, Si, and S using XMM–Newton data were used to map the distribution of ejecta. The SNR was sectioned into 56 regions best characterized by two-component thermal models. The harder component (kT ∼ 0.6 keV) is adequately fitted by the VPSHOCK non-equilibrium ionization model with an ionization time-scale net ∼ 1011–1012 cm−3 s, and slightly enhanced abundances over solar values. The soft component (kT ∼ 0.2 keV), fitted by the APEC model, is well described by plasma in collisional ionization equilibrium with abundances consistent with solar values. Assuming a distance of 3.1 kpc and a Sedov phase of expansion into a uniform medium, we estimate an SNR age of 4.4 kyr, a swept-up mass Msw = 16$f_\mathrm{ s}^{-1/2}$ D$_{3.1}^{5/2}$ M⊙, and a low explosion energy E* = 3.7 × 1049 $f_\mathrm{ s}^{-1/2}$ D$_{3.1}^{5/2}$ erg. This energy could be an order of magnitude higher if we relax the Sedov assumption, the plasma has a low filling factor, the plasma temperature is underestimated, or if the SNR is expanding into the progenitor’s wind-blown bubble. Standard explosion models did not match the ejecta yields. By comparing the fitted abundances to the most recent core-collapse nucleosynthesis models, our best estimate yields a low-mass progenitor of around 12–13 M⊙, lower than previously reported. We discuss degeneracies in the model fitting, particularly the effect of altering the explosion energy on the progenitor mass estimate.