Simulations of galactic winds and starbursts in galaxy clusters
Simulations of galactic winds and starbursts in galaxy clusters
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星系团中的星系风和星暴的模拟
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发表时间：
2005
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通讯作者：
Uk
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作者：
W. Kapferer;C. Ferrari;W. Domainko;M. Mair;T. Kronberger;S. Schindler;S. Kimeswenger;E. V. Kampen;D. O. Astrophysics;U. Innsbruck;Austria Institute of Astrophysics;U. Goettingen;G. I. F. Astronomy;U. Vienna;Austria School of Mathematics;U. Edinburgh;Uk
爱丁堡大学数学学院，英国苏格兰爱丁堡EH9 3JZ -/-我们提出了一项由星系风和合并驱动的星暴引起的星团内介质（ICM）金属富集的研究。我们将n -体/流体动力学模拟与半数值星系形成模型相结合。通过计算由热、宇宙射线和MHD波压驱动的稳态外流的跨音速解，获得了星系风的质量损失。这些过程引起的金属分布的不均匀性是揭示星系团动态状态的理想工具。我们展示了我们的模型星团的表面亮度、x射线辐射加权温度和金属图，因为它们将被xmm -牛顿等x射线望远镜观测到。我们发现x射线加权金属图通过比较金属丰度分布和星系密度分布来区分合并前或合并后的星系团：合并前的子星系团之间有金属丰度差距，合并后的子星系团之间有高金属丰度。我们将我们的方法应用于两个观测到的星系团，Abell 3528和Abell 3921，以显示它们是合并前还是合并后的系统。在我们的模拟中发现的金属丰度分布的不均匀性的生存时间可达几个Gyr。我们表明，星系风和合并驱动的星暴在星系团中心（~ 3 Mpc半径）区域的z=1之后非常有效地丰富了ICM。关键字。星系：星团：一般-星系：丰度-星系：相互作用-星系：ISM - x射线：星系：星团
School of Mathematics, University of Edinburgh, Edinburgh EH9 3JZ, Scotland, UK-/-Abstract. We present an investigation of the metal enrichmentof the intra-cluster medium (ICM) bygalactic windsand merger-driven starbursts. We use combined N-body/hydrodynamic simulations with a semi-numerical galaxyformation model. The mass loss by galactic winds is obtained by calculating transonic solutions of steady stateoutflows, driven by thermal, cosmic ray and MHD wave pressure. The inhomogeneities in the metal distributioncaused by these processes are an ideal tool to reveal the dynamical state of a galaxy cluster. We present surfacebrightness, X-ray emission weighted temperature and metal maps of our model clusters as they would be observedby X-ray telescopes like XMM-Newton. We show that X-ray weighted metal maps distinguish between pre- orpost-merger galaxy clusters by comparing the metallicity distribution with the galaxy-density distribution: pre-mergers have a metallicity gap between the subclusters, post-mergers a high metallicity between subclusters. Weapply our approach to two observed galaxy clusters, Abell 3528 and Abell 3921, to show whether they are pre-or post-merging systems. The survival time of the inhomogeneities in the metallicity distribution found in oursimulations is up to several Gyr. We show that galactic winds and merger-driven starbursts enrich the ICM veryefficiently after z=1 in the central (∼ 3 Mpc radius) region of a galaxy cluster.Key words. Galaxies: clusters: general - Galaxies: abundances - Galaxies: interactions - Galaxies: ISM - X-ray:galaxies: clusters