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On the X-Ray Properties of the Putative Central Compact Object in 1E 0102.2−7219
The Astrophysical Journal ( IF 4.9 ) Pub Date : 2020-11-23 , DOI: 10.3847/1538-4357/abc075
Xi Long 1, 2, 3 , Terrance J. Gaetz 1 , Paul P. Plucinsky 1
Affiliation  

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.

中文翻译:

1E 0102.2−7219 中假定的中心致密天体的 X 射线特性

我们已经分析了钱德拉 X 射线天文台对小麦哲伦星云超新星遗迹 (SNR) 1E 0102.2-7219 中致密特征的档案观测,该遗迹最近被认为是超新星爆炸后剩余的中央致密天体。在我们的分析中,我们对每个存档观察使用了适当的时间相关响应,对背景进行建模而不是减去它,并拟合未分箱的光谱以保留最大的光谱信息。该特征的光谱与周围区域的光谱相似,O、Ne、\& Mg 的丰度显着增加。我们发现之前建议的黑体模型与数据不一致,因为 Monte Carlo 模拟表明超过 99\% 的模拟数据集具有低于数据的测试统计值。光谱由非平衡电离热模型充分描述,其中两类模型同样适合数据。一类模型的温度为 $kT\sim0.79$ keV,电离时间标度为 $\sim3\times10^{11}\,\mathrm{cm}^{-3}\mathrm{s}$,并且O 和 Ne 丰度增强的边际证据,另一个的温度为 $kT\sim0.91$ keV,电离时间标度为 $\sim7\times10^{10}\,\mathrm{cm}^{-3} \mathrm{s}$,以及与当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\% 置信水平下被拒绝。因此,这种紧凑的特征很可能是与反向激波相关的富含 O 和 Ne 的喷射物结。
更新日期:2020-11-23
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