文章基本信息

标题：Properties of the cosmological filament between two clusters: A possible detection of a large-scale accretion shock by Suzaku
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作者：H. Akamatsu ; H. Akamatsu ; Y. Fujita 等
期刊名称：Astronomy & Astrophysics
印刷版ISSN：0004-6361
电子版ISSN：1432-0746
出版年度：2017
卷号：606
页码：1-8
DOI：10.1051/0004-6361/201730497
语种：English
出版社：EDP Sciences
摘要：We report on the results of a Suzaku observation of the plasma in the filament located between the two massive clusters of galaxies, Abell 399 and Abell 401. Abell 399 (z = 0.0724) and Abell 401 (z = 0.0737) are expected to be in the initial phase of a cluster merger. In the region between the two clusters, we find a clear enhancement in the temperature of the filament plasma from 4 keV (expected value of a typical cluster temperature profile) to kT ~ 6.5 keV. Our analysis also shows that filament plasma is present out to a radial distance of 15′ (1.3 Mpc) from a line connecting the two clusters. The temperature profile is characterized by an almost flat radial shape with kT ~ 6–7 keV within 10′ or ~0.8 Mpc. Across r = 8′ from the axis, the temperature of the filament plasma shows a drop from 6.3 keV to 5.1 keV, indicating the presence of a shock front. The Mach number based on the temperature drop is estimated to be ℳ ~ 1.3. We also successfully determined the abundance profile up to 15′ (1.3 Mpc), showing an almost constant value (Z = 0.3 solar) at the cluster outskirts. We estimated the Compton y parameter to be ~ 14.5 ± 1.3 × 10-6, which is in agreement with the Planck results (14–17 × 10-6 on the filament). The line-of-sight depth of the filament is l ~ 1.1 Mpc, which indicates that the geometry of filament is likely a pancake shape rather than cylindrical. The total mass of the filamentary structure is ~7.7 × 1013M⊙. We discuss a possible interpretation of the drop of X-ray emission at the rim of the filament, which was pushed out by the merging activity and formed by the accretion flow induced by the gravitational force of the filament.
关键词：enX-rays: galaxies: clustersintergalactic mediumgalaxies: abundanceslarge-scale structure of Universegalaxies: clusters: intracluster medium