论文标题
在IA型超新星残留N103B中定位CSM发射
Locating the CSM Emission within the Type Ia Supernova Remnant N103B
论文作者
论文摘要
我们提出了Chandra对IA型超新星残留物（SNR）0509-68.7（也称为N103B）的深度观察结果，位于大型麦哲伦云（LMC）中。残留物显示出亮度的不对称性，西半球的表现明显比东半部明亮。以前的多波长观察结果将差异归因于密度梯度和建议的偶然物质起源，这与Kepler的SNR相似。我们将聚类技术与传统成像分析相结合，在残留物中空间定位各种发射组件。我们发现O和MG发射沿爆炸波最强，并且与非辐射冲击的尘埃发射和光学发射相吻合。相对于平均LMC的丰度，在这些区域中，O和MG的丰度增强了，与射流产物相比，它是独特的空间分布，支持偶然培养基（CSM）解释。我们还发现，CR的空间分布与残留物内部的FE相同，并且与O和MG发射完全不合时间。
We present results from deep Chandra observations of the young Type Ia supernova remnant (SNR) 0509-68.7, also known as N103B, located in the Large Magellanic cloud (LMC). The remnant displays an asymmetry in brightness, with the western hemisphere appearing significantly brighter than the eastern half. Previous multi-wavelength observations have attributed the difference to a density gradient and suggested circumstellar material origins, drawing similarities to Kepler's SNR. We apply a clustering technique combined with traditional imaging analysis to spatially locate various emission components within the remnant. We find that O and Mg emission is strongest along the blast wave, and coincides with Spitzer observations of dust emission and optical emission from the non-radiative shocks. The abundances of O and Mg in these regions are enhanced relative to the average LMC abundances and appear as a distinct spatial distribution compared to the ejecta products, supporting the circumstellar medium (CSM) interpretation. We also find that the spatial distribution of Cr is identical to that of Fe in the interior of the remnant, and does not coincide at all with the O and Mg emission.
