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Title: MC2: Mapping the dark matter distribution of the “Toothbrush” cluster RX J0603.3+4214 with Hubble Space Telescope and Subaru weak lensing

Journal Article · · The Astrophysical Journal (Online)
 [1];  [2];  [3];  [4];  [5];  [6];  [4];  [3]
  1. Yonsei Univ. (Korea, Republic of); Univ. of California, Davis, CA (United States)
  2. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  3. Leiden Univ. (Netherlands)
  4. Univ. of California, Davis, CA (United States)
  5. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  6. Hamburg Sternwarte (Germany)
+ Show Author Affiliations

The galaxy cluster RX J0603.3+4214 at z = 0:225 is one of the rarest clusters boasting an extremely large ( 2 Mpc) radio relic. Because of the remarkable morphology of the relic, the cluster is nicknamed the \Toothbrush Cluster". Although the cluster's underlying mass distribution is one of the critical pieces of information needed to reconstruct the merger scenario responsible for the puzzling radio relic morphology, its proximity to the Galactic plane b 10 has imposed signi cant observational challenges. We present a high-resolution weak-lensing study of the cluster with Subaru/Suprime Cam and Hubble Space Telescope imaging data. Our mass reconstruction reveals that the cluster is composed of complicated dark matter substructures closely tracing the galaxy distribution, in contrast, however, with the relatively simple binary X-ray morphology. Nevertheless, we nd that the cluster mass is still dominated by the two most massive clumps aligned north-south with a 3:1 mass ratio (M200 = 6:29+2:24 -1:62 X 1014M⊙ and 1:98+1:24 -0:74 X 1014M⊙ for the northern and southern clumps, respectively). The southern mass peak is 20 o set toward the south with respect to the corresponding X-ray peak, which has a \bullet"-like morphology pointing south. Comparison of the current weak- lensing result with the X-ray, galaxy, and radio relic suggests that perhaps the dominant mechanism responsible for the observed relic may be a high-speed collision of the two most massive subclusters, although the peculiarity of the morphology necessitates involvement of additional subclusters. Careful numerical simulations should follow in order to obtain more complete understanding of the merger scenario utilizing all existing observations.

Research Organization:
Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)
Sponsoring Organization:
USDOE
Grant/Contract Number:
AC52-07NA27344
OSTI ID:
1430965
Report Number(s):
LLNL-JRNL-737792; TRN: US1803006
Journal Information:
The Astrophysical Journal (Online), Vol. 817, Issue 2; ISSN 1538-4357
Publisher:
Institute of Physics (IOP)Copyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 26 works
Citation information provided by
Web of Science

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Cited By (12)

Diffuse Radio Emission from Galaxy Clusters journal February 2019
MC 2 : A Deeper Look at ZwCl 2341.1+0000 with Bayesian Galaxy Clustering and Weak Lensing Analyses journal May 2017
Deep VLA Observations of the Cluster 1RXS J0603.3+4214 in the Frequency Range of 1–2 GHz journal January 2018
A massive cluster at z = 0.288 caught in the process of formation: The case of Abell 959 journal May 2019
Dark matter dynamics in Abell 3827: new data consistent with standard cold dark matter journal April 2018
Merging Cluster Collaboration: Optical and Spectroscopic Survey of a Radio-selected Sample of 29 Merging Galaxy Clusters journal February 2019
Merging Cluster Collaboration: A Panchromatic Atlas of Radio Relic Mergers journal September 2019
MC 2 : Multiwavelength and Dynamical Analysis of the Merging Galaxy Cluster ZwCl 0008.8+5215: An Older and Less Massive Bullet Cluster journal March 2017
Multiwavelength Analysis of the Merging Galaxy Cluster A115 journal April 2019
Dark matter dynamics in Abell 3827: New data consistent with standard cold dark matter text January 2018
Merging Cluster Collaboration: A Panchromatic Atlas of Radio Relic Mergers text January 2018
A Massive Cluster at z = 0.288 Caught in the Process of Formation: The Case of Abell 959 text January 2019

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