论文标题
用苏扎库和钱德拉观测测量的附近星系群的郊区的化学丰度
Chemical abundances in the outskirts of nearby galaxy groups measured with joint Suzaku and Chandra observations
论文作者
论文摘要
我们报告了深苏扎库（Deep Suzaku）的结果，主要是附近四个星系组的Chandra观察结果：MKW4，Antlia，RXJ1159+5531和ESO3060170。它们的峰值温度在2-3 KEV上的变化，使其成为最小的系统，其气体性能约束至病毒半径。郊区的平均fe丰度（R $> $> 0.25r $ _ {200} $）的内部培养基（IGRM）为$ z _ {\ rm fe} = 0.309 \ pm0.018 $ $ $ $ $ $ $ $ $ z_ \ odot $ with $ quest $ quyt $ quyt $ qut^2 $ = 14 $ = 14属于自由度，并且是众所周知的，并且是众所周知的，并且是奇怪的，并且是奇怪的，并且是奇怪的，并且是一个奇异的群体。与Illustristng宇宙学模拟的数值预测完全一致。我们的结果支持银河系系统之间的早期富集场景，甚至在质量的数量级，甚至在它们形成之前。当集成到R $ _ {200} $时，我们开始看到ICM中测得的Fe含量与超新星产量的期望之间的张力。我们进一步限制了他们的O，MG，SI，S和NI丰度。这些元素相对于FE的丰度比与Illustristng的预测（如果有）一致。它们的IA型超新星分数在14％-21％之间变化。可以排除在集团郊区的纯核倒塌的超新星富集。它们在r $ _ {200} $中的累积铁质量比是珀尔修斯集群的一半，这可能意味着星系组并不能保留由于其较浅的重力潜力孔，或者组和簇可能具有不同的星形形成历史。
We report results from deep Suzaku and mostly snapshot Chandra observations of four nearby galaxy groups: MKW4, Antlia, RXJ1159+5531, and ESO3060170. Their peak temperatures vary over 2-3 keV, making them the smallest systems with gas properties constrained to their viral radii. The average Fe abundance in the outskirts (R $>$ 0.25R$_{200}$) of their intragroup medium (IGrM) is $Z_{\rm Fe}=0.309\pm0.018$ $Z_\odot$ with $χ^2$ = 14 for 12 degrees of freedom, which is remarkably uniform and strikingly similar to that of massive galaxy clusters, and is fully consistent with the numerical predictions from the IllustrisTNG cosmological simulation. Our results support an early-enrichment scenario among galactic systems over an order of magnitude in mass, even before their formation. When integrated out to R$_{200}$, we start to see a tension between the measured Fe content in ICM and what is expected from supernovae yields. We further constrain their O, Mg, Si, S, and Ni abundances. The abundance ratios of those elements relative to Fe are consistent with the predictions (if available) from IllustrisTNG. Their Type Ia supernovae fraction varies between 14%-21%. A pure core collapsed supernovae enrichment at group outskirts can be ruled out. Their cumulative iron-mass-to-light ratios within R$_{200}$ are half that of the Perseus cluster, which may imply that galaxy groups do not retain all of their enriched gas due to their shallower gravitational potential wells, or that groups and clusters may have different star formation histories.
