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首页> 外文会议>The energetic cosmos : from Suzaku to ASTRO-H >Metal enrichment histories from galaxies to clusters
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Metal enrichment histories from galaxies to clusters

机译：从星系到星团的金属富集历史

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With Suzaku, we derived O, Mg, S, Si and Fe abundances of hot intracluster medium (ICM) in clusters of galaxies, and groups of galaxies, and hot interstellar medium (ISM) in elliptical, SO, and spiral galaxies. Especially for regions of low surface brightness, the XIS provides better sensitivity to faint lines of O and Mg, which are predominantly synthesized by supernovae (SN) II.rnThe derived abundance ratios, O/Fe, Mg/Fe, Si/Fe and S/Fe of the ICM, scatter around unity, i.e., the solar ratio, adopting the new solar abundances defined by Lodders (2003). Observed clusters and groups of galaxies with a bright central galaxy show similar Fe abundances of about 0.5 solar at 0.1-0.2r180. In contrast, the metal-mass-to-light ratios for clusters of galaxies tend to be higher than those in groups of galaxies. If metal enrichment occurred before the cluster or group formations, the poor systems would carry relatively smaller metal mass with smaller gas mass, while metal abundance would be similar.rnThe derived Fe abundances of the ISM in elliptical galaxies are about 0.5-1.0 solar, indicating a low rate of present metal supply into the ICM. To account for Fe mass in the ICM, the past average rate of SNe Ia was much larger. The derived 0 and Mg abundances of the ISM in these galaxies are consistent with stellar metallicity which reflects formation histories of these galaxies. Observed low O/Fe ratio of the ISM in a SO galaxy, NGC 4382, indicates different formation histories between this SO galaxy and elliptical galaxies. The abundance pattern of the hot ISM in spiral galaxies may depend on their starburst activities.
机译：利用朱雀，我们得出了星系群和星系群中的集群内热介质（ICM）的O，Mg，S，Si和Fe的丰度，而椭圆形，SO和螺旋星系中的星际热介质（ISM）的O，Mg，S，Si和Fe丰度也很高。特别是对于表面亮度较低的区域，XIS对主要由超新星（SN）II合成的O和Mg弱线提供了更好的灵敏度.rn得出的丰度比O / Fe，Mg / Fe，Si / Fe和S ICM的/ Fe，采用Lodders（2003）定义的新的太阳丰度，围绕着单位散射，即太阳比率。观测到的具有明亮中央星系的星系团和星团在0.1-0.2r180处显示相似的铁丰度，约为0.5太阳。相反，星系团的金属质轻比往往高于星系组。如果金属富集发生在团簇或群形成之前，那么较差的系统将携带相对较小的金属质量而气体质量较小，而金属丰度将相似.rn椭圆星系中ISM的Fe丰度约为0.5-1.0太阳，表明当前向ICM供应的金属的比率较低。要考虑到ICM中的铁质量，过去的SNe Ia平均速率要大得多。在这些星系中，ISM的0和Mg丰度与恒星的金属性一致，这反映了这些星系的形成历史。在SO星系NGC 4382中观察到的ISM的低O / Fe比值表明该SO星系和椭圆星系之间的形成历史不同。螺旋星系中热ISM的丰度模式可能取决于其星爆活动。

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