3D mapping of the Crab Nebula with SITELLE – I. Deconvolution and kinematic reconstruction
3D mapping of the Crab Nebula with SITELLE – I. Deconvolution and kinematic reconstruction
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DOI：
10.1093/mnras/staa4046
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发表时间：
2021-01
期刊：
影响因子：
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通讯作者：
T. Martin;D. Milisavljevic;Laurent Drissen D'epartement de physique;D. d'optique;Universit'e Laval;Qc
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文献类型：
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作者：
T. Martin;D. Milisavljevic;Laurent Drissen D'epartement de physique;D. d'optique;Universit'e Laval;Qc
我们提出了一个高光谱立方体的蟹状星云获得的成像傅里叶变换光谱仪SITELLE的加拿大-法国-夏威夷望远镜。我们描述了我们的技术用于去卷积310 000个单独的光谱（R = 9600）包含Hα，[N ii] λλ6548，6583，和[S ii] λλ6716，6731发射线，并创建一个详细的三维重建的超新星遗迹假设均匀的全球扩张。我们发现，一般边界的3D体积所占据的螃蟹是不严格的椭圆形的，因为通常假设，而是出现遵循一个“心形”的分布，是对称的脉冲星风环的平面。明显的限制气体的散装分布与约束膨胀一致的位置的黑暗海湾和东西带的氦丰富的灯丝，这可能与相互作用与预先存在的拱盘。细丝的分布遵循复杂的蜂窝状排列，在大小尺度上具有直的和圆的边界，这些边界与距膨胀中心的距离反相关。这种分布与超新星遗迹3C 58和仙后座A中观察到的大规模环没有什么不同，在那里它被归因于湍流混合过程，鼓励向外膨胀的放射性56 Ni丰富的喷出物羽状物。这些特征反映了公元1054年的原始超新星及其前身星星的关键细节，可能有利于铁核前身的低能量爆炸。我们证明，我们的主要研究结果是强大的，尽管区域的非同源膨胀驱动的加速物质的脉冲星风星云。
We present a hyperspectral cube of the Crab Nebula obtained with the imaging Fourier transform spectrometer SITELLE on the Canada-France-Hawaii telescope. We describe our techniques used to deconvolve the 310 000 individual spectra (R = 9600) containing Hα, [N ii] λλ6548, 6583, and [S ii] λλ6716, 6731 emission lines and create a detailed three-dimensional reconstruction of the supernova remnant assuming uniform global expansion. We find that the general boundaries of the 3D volume occupied by the Crab are not strictly ellipsoidal as commonly assumed, and instead appear to follow a “heart-shaped” distribution that is symmetrical about the plane of the pulsar wind torus. Conspicuous restrictions in the bulk distribution of gas consistent with constrained expansion coincide with positions of the dark bays and east-west band of He-rich filaments, which may be associated with interaction with a pre-existing circumstellar disk. The distribution of filaments follows an intricate honeycomb-like arrangement with straight and rounded boundaries at large and small scales that are anti-correlated with distance from the center of expansion. The distribution is not unlike the large-scale rings observed in supernova remnants 3C 58 and Cassiopeia A, where it has been attributed to turbulent mixing processes that encouraged outwardly expanding plumes of radioactive 56Ni-rich ejecta. These characteristics reflect critical details of the original supernova of 1054 CE and its progenitor star, and may favour a low-energy explosion of an iron-core progenitor. We demonstrate that our main findings are robust despite regions of non-homologous expansion driven by acceleration of material by the pulsar wind nebula.