我们分析了钱德拉X射线天文台对小麦哲伦云超新星遗迹（SNR）1 E 0102.2-7219的紧凑特征的档案观测，该超新星遗迹最近被认为是超新星爆炸后残留的中心紧凑物体。在我们的分析中，我们对每个存档观测结果使用了适当的时间依赖性响应，对背景进行了建模而不是减去它，并拟合了未合并的光谱以保留最大的光谱信息。该特征的光谱与具有显著增强的O、Ne、I和Mg丰度的周围区域的光谱相似。通过蒙特卡罗模拟，发现99%以上的模拟数据集的检验统计量低于实际数据，从而证明了黑体模型与实际数据的不一致性。的光谱是充分描述的非平衡电离热模型与两类模型，同样适合的数据。一类模型的温度为$kT\sim0.79$ keV，电离时标为$\sim3\times10^{11}\,\mathrm{cm}^{-3}\mathrm{s}$，O和Ne丰度增强的边缘证据，另一类模型的温度为$kT\sim0.91$ keV，电离时标为$\sim7\times10^{10}\,\mathrm{cm}^{-3}\mathrm{s}$，丰度与当地星际介质值一致。我们还进行了图像分析，发现计数的空间分布是不一致的点源。在99.9%置信水平下，点源分布的假设可被拒绝。因此，这种致密的特征很可能是与反向激波有关的富含O和Ne的喷出物的结。
英文摘要：
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.
The cooling of the Central Compact Object in Cas A from 2006 to 2020
本文报道了用ACIS仪器在子阵模式下对仙后座A超新星遗迹中心致密天体（CCO）的六次Chandra观测（四个历元）的研究。此模式最大限度地减少频谱失真的仪器效应，如堆积。数据采集时间跨度约为14年。如果假设这个最年轻的已知CCO为非磁性碳大气，那么对于恒定或变化的吸收氢柱密度，温度变化被约束为$\dot{T}=-2900\pm 600$ K yr $^{-1}$或$\dot{T}=-4500\pm 800 $ K yr $^{-1}$（$1σ$不确定性）。这些值分别对应于每10年$-1.5 \pm 0.3$ %和每10年$-2.3 \pm 0.4$ %的冷却速率。我们讨论了一个明显的增加，在过去的五年中的冷却速率和推断的吸收氢柱密度之间的时代的变化。综合考虑，这些变化可能表明系统性影响，例如，ACIS过滤器污染增加的不完美校准。
Pulsed radio emission from a Central Compact Object
Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理与超级计算中心）；New Cornerstone Science Laboratory, Department of Astronomy, Tsinghua University（清华大学天文系新Cornerstone科学实验室）；School of Arts and Sciences, Qingdao Binhai University（青岛滨海学院文理学院）；South African Radio Astronomy Observatory（南非射电天文观测站）；Department of Physics and Astronomy, Haverford College（哈弗福德学院物理与天文学系）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Department of Physics, CCIS 4-183, University of Alberta（阿尔伯塔大学物理系）
