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Published March 1, 2016 | Submitted + Published
Journal Article Open

The Morphologies and Alignments of Gas, Mass, and the Central Galaxies of CLASH Clusters of Galaxies

Abstract

Morphology is often used to infer the state of relaxation of galaxy clusters. The regularity, symmetry, and degree to which a cluster is centrally concentrated inform quantitative measures of cluster morphology. The Cluster Lensing and Supernova survey with Hubble Space Telescope (CLASH) used weak and strong lensing to measure the distribution of matter within a sample of 25 clusters, 20 of which were deemed to be "relaxed" based on their X-ray morphology and alignment of the X-ray emission with the Brightest Cluster Galaxy. Toward a quantitative characterization of this important sample of clusters, we present uniformly estimated X-ray morphological statistics for all 25 CLASH clusters. We compare X-ray morphologies of CLASH clusters with those identically measured for a large sample of simulated clusters from the MUSIC-2 simulations, selected by mass. We confirm a threshold in X-ray surface brightness concentration of C ≳ 0.4 for cool-core clusters, where C is the ratio of X-ray emission inside 100 h_(70)^(−1) kpc compared to inside 500 h_(70)^(-1)kpc. We report and compare morphologies of these clusters inferred from Sunyaev–Zeldovich Effect (SZE) maps of the hot gas and in from projected mass maps based on strong and weak lensing. We find a strong agreement in alignments of the orientation of major axes for the lensing, X-ray, and SZE maps of nearly all of the CLASH clusters at radii of 500 kpc (approximately 1/2 R_(500) for these clusters). We also find a striking alignment of clusters shapes at the 500 kpc scale, as measured with X-ray, SZE, and lensing, with that of the near-infrared stellar light at 10 kpc scales for the 20 "relaxed" clusters. This strong alignment indicates a powerful coupling between the cluster- and galaxy-scale galaxy formation processes.

Additional Information

© 2016 The American Astronomical Society. Received 2015 October 6; accepted 2016 January 11; published 2016 February 25. M.D. was partially supported by an STScI/NASA award HST-GO-12065.07-A and NASA ADAP award NNX13AI41G. A.B. was partially supported by the same NASA ADAP award NNX13AI41G and a Chandra archive grant SAO AR3-14013X. E.R. was supported by FP7-PEOPLE-2013-IIF (Grant Agreement PIIF-GA-2013-627474) and NSF AST-1210973. S.E. acknowledges the financial contribution from contracts ASI-INAF I/009/10/0 and PRIN-INAF 2012. This work was supported in part by National Science Foundation Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. J.S. was supported by NSF/AST-0838261, NASA/NNX11AB07G, and the Norris Foundation CCAT Postdoctoral Fellowship. N.G.C. was partially supported by a NASA Graduate Student Research Fellowship. The Bolocam observations were partially supported by the Gordon and Betty Moore Foundation. This research made use of the Caltech Submillimeter Observatory, which was operated at the time by the California Institute of Technology under cooperative agreement with the National Science Foundation (NSF/AST-0838261). G.Y. acknowledges financial support from MINECO's grant AYA2012-31101. The MUSIC simulations have been performed in the Marenostrum Supercomputer at the Barcelona Supercomputer Center, thanks to time granted by the Red Española de Supercomputación. Facilities: Chandra X-ray Observatory - , Hubble Space Telescope/ACS - , Hubble Space Telescope/WFC3 - , Caltech Submillimeter Observatory. -

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Submitted - 1601.04947v1.pdf

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Additional details

Created:
August 22, 2023
Modified:
February 24, 2024