论文标题
从观察到集体内气体的观察结果排名理论超新星爆炸模型
Ranking Theoretical Supernovae Explosion Models from Observations of the Intracluster Gas
论文作者
论文摘要
簇内培养基（ICM）是由宇宙历史上不同超新星（SNE）类型合成的重元素的储层。不同的富集机制贡献了不同的相对金属产生，主要由不同的SNE类型优势引起。使用空间分辨的X射线光谱，可以探测每个金属富集机制的贡献。但是，各种各样的物理可行的超新星爆炸模型使对ICM富集历史的分析更加不确定。本文提出了非参数PDF分析，通过将其性能与观察结果进行比较，从而对不同的理论SNE产生了模型。具体而言，我们将这种新方法应用于核心折叠SN和IA型SN模型的7192组合，使用来自$ Suzaku $观测的8个Galaxy Systems（群集和组）的8个丰度比率来测试其预测。这项新型技术可以比较许多SN模型并最大程度地提取光谱信息提取，并考虑所有可测量的丰度比及其不确定性。我们发现，具有非零初始金属性祖细胞的II型超新星的表现优于配对SN和Hypernova型号，以及3D SNIA模型（WD祖细胞中央密度为$ 2.9 \ times10^9 \ Mathrm {G \ g \，cm^{ - 3}} $中的所有测试模型。
The intracluster medium (ICM) is a reservoir of heavy elements synthesized by different supernovae (SNe) types over cosmic history. Different enrichment mechanisms contribute a different relative metal production, predominantly caused by different SNe Type dominance. Using spatially resolved X-ray spectroscopy, one can probe the contribution of each metal enrichment mechanism. However, a large variety of physically feasible supernova explosion models make the analysis of the ICM enrichment history more uncertain. This paper presents a non-parametric PDF analysis to rank different theoretical SNe yields models by comparing their performance against observations. Specifically, we apply this new methodology to rank 7192 combinations of core-collapse SN and Type Ia SN models using 8 abundance ratios from $Suzaku$ observations of 18 galaxy systems (clusters and groups) to test their predictions. This novel technique can compare many SN models and maximize spectral information extraction, considering all the individual measurable abundance ratios and their uncertainties. We find that Type II Supernova with nonzero initial metallicity progenitors in general performed better than Pair-Instability SN and Hypernova models and that 3D SNIa models (with the WD progenitor central density of $2.9\times10^9 \mathrm{g\,cm^{-3}}$) performed best among all tested SN model pairs.
