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题名: CHANDRA AND XMM-NEWTON OBSERVATIONS OF THE MERGING CLUSTER OF GALAXIES PLCK G036.7+14.9
作者: Zhang, B.1, 2, 3; David, L. P.3; Jones, C.3; Andrade-Santos, F.3; O'Sullivan, E.3; Dahle, H.4; Nulsen, P. E. J.3; Clarke, T. E.5; Pointecouteau, E.6, 7; Pratt, G. W.8; Arnaud, M.8; Vrtilek, J. M.3; Ji Li(纪丽)9; van Weeren, R. J.3; Kraft, R. P.3; Kong, X.1, 2
刊名: ASTROPHYSICAL JOURNAL
出版日期: 2015-05-10
卷号: 804, 期号:2, 页码:129
关键词: cosmology: observations ; galaxies: clusters: general ; galaxies: clusters: individual (PLCK G036.7+14.9) ; X-rays: galaxies: clusters
学科分类: 天文和天体物理
DOI: 10.1088/0004-637X/804/2/129
文章类型: Article
英文摘要: We present Chandra and XMM-Newton observations of PLCK G036.7+14.9 from the Chandra-Planck Legacy Program. The high resolution X-ray observations reveal two close (similar to 72" - 193 kpc in projection) subclusters, G036N and G036S, which were not resolved by previous ROSAT, optical, or recent Planck observations. We perform detailed imaging and spectral analyses and use a simplified model to study the kinematics of this system. The basic picture is that PLCK G036.7+14.9 is undergoing a major merger (mass ratio close to unity) between the two massive subclusters, with the merger largely along the line of sight (similar to 80 degrees between the merger axis and the plane of the sky from the simplified model) and probably at an early stage (less than similar to 0.4-0.7 Gyr since the merger began). G036N hosts a small (similar to 27 kpc), moderate cool core (cooling time t(cool) similar to 2.6-4.7Gyr), while G036S has at most a very weak cool core (t(cool) similar to 5.7-10.3Gyr) in the central similar to 40 kpc region. The difference in core cooling times is unlikely to be caused by the ongoing merger disrupting a pre-existing cool core in G036S. G036N also hosts an unresolved radio source in the center, which may be heating the gas if the radio source is extended. The total mass of the whole cluster determined from XMM-Newton is similar to(5.9-8.0) x 10(14) M-circle dot, and is similar to(6.7-9.9) x 10(14) M-circle dot from Chandra. The Planck derived mass,similar to(5.1-6.0) x 10(14) M-circle dot, is higher than the X-ray measured mass of either subcluster, but is lower than the X-ray measured mass of the whole cluster, due to the fact that Planck does not resolve PLCK G036.7+14.9 into subclusters and interprets it as a single cluster. This mass discrepancy could induce significant bias to the mass function if such previously unresolved systems are common in the Planck cluster sample. High resolution X-ray observations are necessary to identify the fraction of such systems and correct such a bias for the purpose of precision cosmological studies.
WOS标题词: Science & Technology ; Physical Sciences
类目[WOS]: Astronomy & Astrophysics
研究领域[WOS]: Astronomy & Astrophysics
关键词[WOS]: ACTIVE GALACTIC NUCLEI ; INTERACTION CROSS-SECTION ; DIGITAL SKY SURVEY ; X-RAY-CLUSTERS ; COOLING FLOWS ; DARK-MATTER ; COSMOLOGICAL SIMULATIONS ; TEMPERATURE PROFILES ; REPRESENTATIVE SAMPLE ; THERMAL CONDUCTION
收录类别: SCI
所属项目名称: PMO_LIB-IR
语种: 英语
WOS记录号: WOS:000354905000051
Citation statistics:
内容类型: 期刊论文
URI标识: http://libir.pmo.ac.cn/handle/332002/14860
Appears in Collections:星系宇宙学和暗能量研究团组_期刊论文

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作者单位: 1.Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China
2.Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China
3.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
4.Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway
5.Naval Res Lab, Washington, DC 20375 USA
6.Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France
7.CNRS, IRAP, F-31028 Toulouse 4, France
8.Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,IRFU,Serv Astrophys,CEA DSM, F-91191 Gif Sur Yvette, France
9.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China
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