We present an in-depth analysis and results of eleven XMM–Newton data sets, spanning 2000–2016, of the anomalous X-ray Pulsar CXOU J010043.1−721134 that has been classified as a magnetar. We find a spin period of 8.0275(1) s as of December 2016 and calculate the period derivative to be (1.76 ± 0.02) × 10−11 s s−1, which translate to a dipolar magnetic field strength of 3.8 × 1014 G and characteristic age of ∼7200 yr for the magnetar. It has a double-peaked pulse profile, with one broad and one narrow peak, in both soft (0.3–1.3 keV) and hard (1.3–8 keV) energy bands. The pulse fractions in the two energy bands are found to be consistent with constant values. These results are in agreement with previously published results for this source. Although two-component models produce acceptable fits to its energy spectra, single component models are much simpler and are able to explain the similarity of the pulse profiles in the low- and high-energy bands. We attempt fitting with four different single-component models and find that the best fit to the spectra is obtained by fitting a thermal Comptonization model with the photon index (Γ) between 2.0 and 2.7, and the electron temperature ( kTe) between 0.5 and 0.9 keV, for a seed blackbody photon distribution of 0.2 keV. Finally, we conclude by discussing our results briefly.

中文翻译：

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磁星 CXOU J010043.1−721134 的长期 XMM-牛顿视图：综合光谱和时间结果

我们对被归类为磁星的异常 X 射线脉冲星 CXOU J010043.1-721134 的 11 个 XMM-Newton 数据集（跨越 2000-2016 年）进行了深入分析和结果。我们发现截至 2016 年 12 月的自旋周期为 8.0275(1) s，并计算出周期导数为 (1.76 ± 0.02) × 10−11 ss−1，这转化为 3.8 × 1014 G 的偶极磁场强度和特征磁星的年龄约为 7200 年。它在软（0.3-1.3 keV）和硬（1.3-8 keV）能带中具有双峰脉冲轮廓，具有一个宽峰和一个窄峰。发现两个能带中的脉冲分数与恒定值一致。这些结果与该来源先前公布的结果一致。尽管双分量模型对其能谱产生了可接受的拟合，单分量模型要简单得多，并且能够解释低能带和高能带中脉冲轮廓的相似性。我们尝试用四种不同的单分量模型进行拟合，发现通过拟合热康普顿模型，光子指数 (Γ) 介于 2.0 和 2.7 之间，电子温度 (kTe) 介于 0.5 和 0.9 之间，可以获得对光谱的最佳拟合keV，用于 0.2 keV 的种子黑体光子分布。最后，我们通过简要讨论我们的结果来结束。对于 0.2 keV 的种子黑体光子分布，电子温度 (kTe) 在 0.5 和 0.9 keV 之间。最后，我们通过简要讨论我们的结果来结束。对于 0.2 keV 的种子黑体光子分布，电子温度 (kTe) 在 0.5 和 0.9 keV 之间。最后，我们通过简要讨论我们的结果来结束。