论文标题
在1E 0102.2-7219中推定的中央紧凑型物体的X射线属性上
On the X-ray Properties of the Putative Central Compact Object in 1E 0102.2-7219
论文作者
论文摘要
我们已经分析了小麦芽岩云超新星残留物（SNR）1E 0102.2-7219中紧凑型特征的档案Chandra X射线观测值观测值，最近有人建议将其保留为超新星爆炸后留下的中心紧凑型物体。在我们的分析中，我们对每个档案观测值都使用了适当的，时间依赖的响应，对背景进行了建模，而不是减去它，并拟合了无上线的光谱来保留最大光谱信息。此特征的频谱与周围区域的光谱相似，这些区域的频谱显着增强了O，NE，\＆Mg的丰富度。我们发现先前建议的黑体模型与数据不一致，因为蒙特卡洛模拟表明，超过99 \％的模拟数据集的测试统计值低于数据。通过非平衡电离热模型充分描述了频谱，并具有两个类别的模型，这些模型符合数据的良好模型。一类模型的温度为$ kt \ sim0.79 $ keV，一个电离时间表为$ \ sim3 \ times10^{11} {11} \，\ mathrm {cm}^{ - 3} \ 3} \ mathrm {s} $，以及对O and Ne and Ne and Ne and Ne and Ne and Ne and Ne and Ne and ne and ne and ne and ne and ne and ne and ne and ne and Ne and ne ne and ne温度。 $ \ sim7 \ times10^{10} \，\ mathrm {cm}^{ - 3} \ mathrm {s} $的时尺，以及与本地星际介质值一致的丰度。我们还进行了图像分析，发现计数的空间分布与点源的空间分布不一致。点源分布的假设可以在99.9 \％置信度水平上拒绝。因此，这种紧凑的特征很可能是与反向冲击相关的O和NE富含弹出的结。
We have analyzed the archival Chandra X-ray Observatory observations of the compact feature in the Small Magellanic Cloud supernova remnant (SNR) 1E 0102.2-7219 which has recently been suggested to be the Central Compact Object remaining after the supernova explosion. In our analysis, we have used appropriate, time-dependent responses for each of the archival observations, modeled the background instead of subtracting it, and have fit unbinned spectra to preserve the maximal spectral information. The spectrum of this feature is similar to the spectrum of the surrounding regions which have significantly enhanced abundances of O, Ne, \& Mg. We find that the previously suggested blackbody model is inconsistent with the data as Monte Carlo simulations indicate that more than 99\% of the simulated data sets have a test statistic value lower than that of the data. The spectrum is described adequately by a non-equilibrium ionization thermal model with two classes of models that fit the data equally well. One class of models has a temperature of $kT\sim0.79$ keV, an ionization timescale of $\sim3\times10^{11}\,\mathrm{cm}^{-3}\mathrm{s}$, and marginal evidence for enhanced abundances of O and Ne and the other has a temperature of $kT\sim0.91$ keV, an ionization timescale of $\sim7\times10^{10}\,\mathrm{cm}^{-3}\mathrm{s}$, and abundances consistent with local interstellar medium values. We also performed an image analysis and find that the spatial distribution of the counts is not consistent with that of a point source. The hypothesis of a point source distribution can be rejected at the 99.9\% confidence level. Therefore this compact feature is most likely a knot of O and Ne rich ejecta associated with the reverse shock.
