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サトウ コウスケ
SATO KOSUKE
佐藤 浩介 所属 京都産業大学 理学部 宇宙物理・気象学科 職種 教授 |
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| 言語種別 | 英語 |
| 発行・発表の年月 | 2022/10 |
| 形態種別 | 研究論文 |
| 査読 | 査読あり |
| 標題 | XMM-Newton view of the shock heating in an early merging cluster, CIZA J1358.9$-$4750 |
| 執筆形態 | 共著 |
| 掲載誌名 | Publications of the Astronomical Society of Japan |
| 掲載区分 | 国外 |
| 巻・号・頁 | 75(1),pp.37-51 |
| 著者・共著者 | Y. Omiya,K. Nakazawa,K. Matsushita,S. B. Kobayashi,N. Okabe,K. Sato,T. Tamura,Y. Fujita,L. Gu,T. Kitayama,T. Akahori,K. Kurahara,T. Yamaguchi |
| 概要 | CIZA J1358.9-4750 is a nearby galaxy cluster in the early phase of a major
merger. The two-dimensional temperature map using XMM-Newton EPIC-PN observation confirms the existence of a high temperature region, which we call the "hot region", in the "bridge region" connecting the two clusters. The ~ 500 kpc wide region between the southeast and northwest boundaries also has higher pseudo pressure compared to the unshocked regions, suggesting the existence of two shocks. The southern shock front is clearly visible in the X-ray surface brightness image and has already been reported by Kato et al. (2015). The northern one, on the other hand, is newly discovered. To evaluate their Mach number, we constructed a three-dimensional toy merger model with overlapping shocked and unshocked components in line of sight. The unshocked and preshock ICM conditions are estimated based on those outside the interacting bridge region assuming point symmetry. The hot region spectra are modeled with two-temperature thermal components, assuming that the shocked condition follows the Rankin-Hugoniot relation with the preshock condition. As a result, the shocked region is estimated to have a line-of-sight depth of ~ 1 Mpc with a Mach number of ~ 1.3 in the southeast shock and ~ 1.7 in the northwest shock. The age of the shock waves is estimated to be ~ 260 Myr. This three dimensional merger model is consistent with the Sunyaev-Zeldovich signal obtained using the Planck observation within the CMB fluctuations. The total flow of the kinetic energy of the ICM through the southeast shock was estimated to be ~ 2.2 x $10^{42}$ erg/s. Assuming that 10 % of this energy is converted into ICM turbulence, the line-of-sight velocity dispersion is calculated to be ~ 200 km/s, which is basically resolvable via coming high spectral resolution observations. |
| DOI | 10.1093/pasj/psac087 |
| PermalinkURL | http://arxiv.org/abs/2210.02145v2 |
| researchmap用URL | http://arxiv.org/pdf/2210.02145v2 |