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|Title:||The Double Galaxy Cluster A2465. III. X-Ray and Weak-lensing Observations||Authors:||Wegner, Gary A.
Molnar, Sandor M.
Forman, William R.
|Issue Date:||2017||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||844||Issue:||1||First Page:||67||Abstract:||We report Chandra X-ray observations and optical weak-lensing measurements from Subaru/Suprime-Cam images of the double galaxy cluster A2465 (z = 0.245). The X-ray brightness data are fit to a β model to obtain the radial gas density profiles of the northeast (NE) and southwest (SW) subcomponents, which are seen to differ in structure. We determine core radii, central temperatures, the gas masses within r <SUB>500c</SUB>, and the total masses for the broader NE and sharper SW components assuming hydrostatic equilibrium. There is no large X-ray excess between the two components. The central entropy of the NE subcluster is about two times higher than the SW. Along with its structural properties and an apparent radio halo that is a sign of a merger, this suggests that the NE component has undergone merging on its own. The weak-lensing analysis gives virial masses for each substructure, which compare well with earlier dynamical results. The derived outer mass contours of the SW sub-component from weak lensing are more irregular and extended than those of the NE. Although there is a weak enhancement and small offsets between X-ray gas and mass centers from weak lensing, the lack of large amounts of gas between the two subclusters indicates that A2465 is in a pre-merger state. We discuss star formation enhancement in this system resulting from its dynamics and shock-induced star formation scenarios. A dynamical model that is consistent with the observed cluster data, based on the FLASH program and the radial infall model, is constructed, where the subclusters currently separated by ∼1.2 Mpc are approaching each other at ∼2000 km s<SUP>-1</SUP> and will meet in ∼0.4 Gyr. <P />Based in part on data collected at the Subaru Telescope, which is operated by the National Astronomical Society of Japan.||Acknowledgments:||M.N. acknowledges support from PRIN-INAF 2014 1.05.01.94.02||URI:||http://hdl.handle.net/20.500.12386/26776||URL:||https://iopscience.iop.org/article/10.3847/1538-4357/aa784a||ISSN:||0004-637X||DOI:||10.3847/1538-4357/aa784a||Bibcode ADS:||2017ApJ...844...67W||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Sep 20, 2020
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