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Shapes and Centroids of 39 Strong Lensing Galaxy Clusters from the Sloan Giant Arcs Survey

Published online by Cambridge University Press:  04 March 2024

Raven Gassis*
Affiliation:
Department of Physics, University of Cincinnati
Matthew B. Bayliss
Affiliation:
Department of Physics, University of Cincinnati
Keren Sharon
Affiliation:
Department of Astronomy, University of Michigan
Guillaume Mahler
Affiliation:
Centre for Extragalactic Astronomy, Durham University
Michael D. Gladders
Affiliation:
Department of Astronomy and Astrophysics/Kavli Institute for Cosmological Physics, University of Chicago
Håkon Dahle
Affiliation:
Institute of Theoretical Astrophysics, University of Oslo
Michael K. Florian
Affiliation:
Steward Observatory
Jane R. Rigby
Affiliation:
University of Arizona, Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center
Lauren Elicker
Affiliation:
Department of Physics, University of Cincinnati
M. Riley Owens
Affiliation:
Department of Physics, University of Cincinnati
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Abstract

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Strong lensing galaxy clusters provide a powerful observational test of Cold Dark Matter (CDM) structure predictions derived from simulation. Specifically, the shape and relative alignments of the dark matter halo, stars, and hot intracluster gas tells us the extent to which theoretical structure predictions hold for clusters in various dynamical states. We measure the position angles, ellipticities, and locations/centroids of the brightest cluster galaxy (BCG), intracluster light (ICL), the hot intracluster medium (ICM), and the core lensing mass for a sample of strong lensing galaxy clusters from the SDSS Giant Arcs Survey (SGAS). We use iterative elliptical isophote fitting methods and GALFIT modeling on HST WFC3/IR imaging data to extract ICL and BCG information and use CIAO’s Sherpa modeling on Chandra ACIS-I X-ray data to make measurements of the ICM. Using this multicomponent approach, we attempt to constrain the physical state of these strong lensing clusters and evaluate the different observable components in terms of their ability to trace out the gravitational potential of the cluster.

Type
Contributed Paper
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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