Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-16761
Miranda, M; Sereno, M; de Filippis, E; Paolillo, M (2008). The dynamical state of RX J1347.5−1145 from a combined strong lensing and X-ray analysis. Monthly Notices of the Royal Astronomical Society, 385(1):511-518.
We perform a combined X-ray and strong lensing analysis of RX J1347.5-1145, one of the most luminous galaxy clusters at X-ray wavelengths. We show that evidence from strong lensing alone, based on published Very Large Telescope (VLT) and new Hubble Space Telescope (HST) data, strongly argues in favour of a complex structure. The analysis takes into account arc positions, shapes and orientations, and is done thoroughly in the image plane. The cluster inner regions are well fitted by a bimodal mass distribution, with a total projected mass of Mtot = (9.9 +/-0.3) × 1014Msolarh-1 within a radius of 360kpch-1 (1.5arcmin). Such a complex structure could be a signature of a recent major merger as further supported by X-ray data. A temperature map of the cluster, based on deep Chandra observations, reveals a hot front located between the first main component and an X-ray emitting south-eastern subclump. The map also unveils a filament of cold gas in the innermost regions of the cluster, most probably a cooling wake caused by the motion of the cD inside the cool core region. A merger scenario in the plane of the sky between two dark matter subclumps is consistent with both our lensing and X-ray analyses, and can explain previous discrepancies with mass estimates based on the virial theorem.
|Item Type:||Journal Article, refereed, original work|
|Communities & Collections:||07 Faculty of Science > Institute of Theoretical Physics|
|Uncontrolled Keywords:||gravitational lensing , galaxies: clusters: general , galaxies: clusters: individual: RX J1347.5-1145 , X-rays: galaxies: clusters|
|Deposited On:||13 Mar 2009 11:18|
|Last Modified:||23 Nov 2012 14:20|
|Additional Information:||The definitive version is available at www.blackwell-synergy.com|
|Other Identification Number:||doi: 10.1111/j.1365-2966.2008.12855.x|
|WoS Citation Count:||12|
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