ASCA Observations of the Crab-Like Supernova Remnant 3C 58
ASCA Observations of the Crab-Like Supernova Remnant 3C 58
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DOI：
10.1093/pasj/52.5.875
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发表时间：
2000-06
影响因子：
2.3
通讯作者：
K. Torii;P. Slane;K. Kinugasa;K. Hashimotodani;H. Tsunemi
中科院分区：
文献类型：
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作者：
K. Torii;P. Slane;K. Kinugasa;K. Hashimotodani;H. Tsunemi
本文报道了用ASCA对蟹状超新星遗迹（SNR） 3C 58的x射线观测。我们发现星云上的积分能谱与先前的结果一致，显示出光子指数为7 = 2.2-2.4的幂律谱，被星际吸收约（3-4）x 10 21 cm -2修正。包括黑体成分，这是归因于中心致密源，显著改善了光谱拟合。建立了任何发射薄热等离子体线的严格上限。我们首次发现，星云光谱在信噪比的中心部分较硬，在外围变得较软，而吸收柱在整个星云中是均匀的。相应地，星云的大小随着光子能量的增加而减小，其与半径的关系比蟹状星云更陡峭。结果与同步加速器能量损失模型>进行了比较，并讨论了假定脉冲星的性质。对中心致密源的脉冲x射线发射进行了时序分析。未观察到明显的脉动；并给出了脉冲分数的上限。
We present here X-ray observation of a Crab-like supernova remnant (SNR) 3C 58 with ASCA. We find that the integrated energy spectrum over the nebula is consistent with previous results, showing a power-law spectrum with the photon index of 7 = 2.2-2.4, modified by interstellar absorption of about (3-4) x 10 21 cm -2 . The inclusion of a blackbody component, which is attributable to the central compact source, significantly improves the spectral fit. Stringent upper limits for any line emitting thin hot plasma are established. We find for the first time that the nebular spectrum is harder in the central part of the SNR, becoming softer toward the periphery, while the absorption column is uniform across the nebula. Correspondingly, the nebular size decreases with increasing photon energy, which is a steeper function of the radius than that of the Crab nebula. The results are compared with synchrotron energy-loss models> and the nature of the putative pulsar is discussed. A timing analysis was performed to search for pulsed X-ray emission from the central compact source. No significant pulsations were observed; and we present the upper limit for the pulsed fraction.