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Title: MC2: Subaru and Hubble Space Telescope Weak-lensing Analysis of the Double Radio Relic Galaxy Cluster PLCK G287.0+32.9

Abstract

The second most significant detection of the Planck Sunyaev-Zel'dovich survey, PLCK G287.0+32.9 (z = 0.385), boasts two similarly bright radio relics and a radio halo. One radio relic is located $$\sim 400\,\mathrm{kpc}$$ NW of the X-ray peak and the other $$\sim 2.8$$ Mpc to the SE. This large difference suggests that a complex merging scenario is required. A key missing puzzle for the merging scenario reconstruction is the underlying dark matter distribution in high resolution. Here, we present a joint Subaru Telescope and Hubble Space Telescope weak-lensing analysis of the cluster. Our analysis shows that the mass distribution features four significant substructures. Of the substructures, a primary cluster of mass $${M}_{200{\rm{c}}}={1.59}_{-0.22}^{+0.25}\times {10}^{15}\ {h}_{70}^{-1}\ {M}_{\odot }$$ dominates the weak-lensing signal. This cluster is likely to be undergoing a merger with one (or more) subcluster whose mass is approximately a factor of 10 lower. One candidate is the subcluster of mass $${M}_{200{\rm{c}}}={1.16}_{-0.13}^{+0.15}\times {10}^{14}\ {h}_{70}^{-1}\ {M}_{\odot }$$ located $$\sim 400\,\mathrm{kpc}$$ to the SE. The location of this subcluster suggests that its interaction with the primary cluster could be the source of the NW radio relic. Another subcluster is detected $$\sim 2$$ Mpc to the SE of the X-ray peak with mass $${M}_{200{\rm{c}}}={1.68}_{-0.20}^{+0.22}\times {10}^{14}\ {h}_{70}^{-1}\ {M}_{\odot }$$. This SE subcluster is in the vicinity of the SE radio relic and may have created the SE radio relic during a past merger with the primary cluster. The fourth subcluster, $${M}_{200{\rm{c}}}={1.87}_{-0.22}^{+0.24}\times {10}^{14}\ {h}_{70}^{-1}\ {M}_{\odot }$$, is NW of the X-ray peak and beyond the NW radio relic.

Authors:
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3]; ORCiD logo [4]; ORCiD logo [5]; ORCiD logo [6]; ORCiD logo [7];  [4]; ORCiD logo [8]
  1. Yonsei Univ., Seoul (Korea). Dept. of Astronomy
  2. Yonsei Univ., Seoul (Korea). Dept. of Astronomy; Univ. of California, Davis, CA (United States). Dept. of Physics
  3. Univ. of California, Davis, CA (United States). Dept. of Physics; Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  4. Univ. of California, Davis, CA (United States). Dept. of Physics
  5. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  6. SLAC National Accelerator Lab., Menlo Park, CA (United States); Stanford Univ., CA (United States). Dept. of Physics, KIPAC
  7. Space Telescope Science Inst., Baltimore, MD (United States)
  8. Univ. Observatory Munich, Munich (Germany); Max Planck Inst. for Extraterrestrial Physics, Garching (Germany)
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Sponsoring Org.:
USDOE; National Science Foundation (NSF); National Aeronautics and Space Administration (NASA)
OSTI Identifier:
1417013
Alternate Identifier(s):
OSTI ID: 1430983
Report Number(s):
LLNL-JRNL-744497
Journal ID: ISSN 1538-4357; TRN: US1800987
Grant/Contract Number:  
AC02-76SF00515; 1518246; PF5-160138; NAS8-03060; AC52-07NA27344
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 851; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; cosmology: observations; dark matter; galaxies: clusters: individual (PLCK G287.0+32.9); gravitational lensing: weak; X-rays: galaxies: clusters

Citation Formats

Finner, Kyle, Jee, M. James, Golovich, Nathan, Wittman, David, Dawson, William, Gruen, Daniel, Koekemoer, Anton M., Lemaux, Brian C., and Seitz, Stella. MC2: Subaru and Hubble Space Telescope Weak-lensing Analysis of the Double Radio Relic Galaxy Cluster PLCK G287.0+32.9. United States: N. p., 2017. Web. https://doi.org/10.3847/1538-4357/aa998c.
Finner, Kyle, Jee, M. James, Golovich, Nathan, Wittman, David, Dawson, William, Gruen, Daniel, Koekemoer, Anton M., Lemaux, Brian C., & Seitz, Stella. MC2: Subaru and Hubble Space Telescope Weak-lensing Analysis of the Double Radio Relic Galaxy Cluster PLCK G287.0+32.9. United States. https://doi.org/10.3847/1538-4357/aa998c
Finner, Kyle, Jee, M. James, Golovich, Nathan, Wittman, David, Dawson, William, Gruen, Daniel, Koekemoer, Anton M., Lemaux, Brian C., and Seitz, Stella. Mon . "MC2: Subaru and Hubble Space Telescope Weak-lensing Analysis of the Double Radio Relic Galaxy Cluster PLCK G287.0+32.9". United States. https://doi.org/10.3847/1538-4357/aa998c. https://www.osti.gov/servlets/purl/1417013.
@article{osti_1417013,
title = {MC2: Subaru and Hubble Space Telescope Weak-lensing Analysis of the Double Radio Relic Galaxy Cluster PLCK G287.0+32.9},
author = {Finner, Kyle and Jee, M. James and Golovich, Nathan and Wittman, David and Dawson, William and Gruen, Daniel and Koekemoer, Anton M. and Lemaux, Brian C. and Seitz, Stella},
abstractNote = {The second most significant detection of the Planck Sunyaev-Zel'dovich survey, PLCK G287.0+32.9 (z = 0.385), boasts two similarly bright radio relics and a radio halo. One radio relic is located $\sim 400\,\mathrm{kpc}$ NW of the X-ray peak and the other $\sim 2.8$ Mpc to the SE. This large difference suggests that a complex merging scenario is required. A key missing puzzle for the merging scenario reconstruction is the underlying dark matter distribution in high resolution. Here, we present a joint Subaru Telescope and Hubble Space Telescope weak-lensing analysis of the cluster. Our analysis shows that the mass distribution features four significant substructures. Of the substructures, a primary cluster of mass ${M}_{200{\rm{c}}}={1.59}_{-0.22}^{+0.25}\times {10}^{15}\ {h}_{70}^{-1}\ {M}_{\odot }$ dominates the weak-lensing signal. This cluster is likely to be undergoing a merger with one (or more) subcluster whose mass is approximately a factor of 10 lower. One candidate is the subcluster of mass ${M}_{200{\rm{c}}}={1.16}_{-0.13}^{+0.15}\times {10}^{14}\ {h}_{70}^{-1}\ {M}_{\odot }$ located $\sim 400\,\mathrm{kpc}$ to the SE. The location of this subcluster suggests that its interaction with the primary cluster could be the source of the NW radio relic. Another subcluster is detected $\sim 2$ Mpc to the SE of the X-ray peak with mass ${M}_{200{\rm{c}}}={1.68}_{-0.20}^{+0.22}\times {10}^{14}\ {h}_{70}^{-1}\ {M}_{\odot }$. This SE subcluster is in the vicinity of the SE radio relic and may have created the SE radio relic during a past merger with the primary cluster. The fourth subcluster, ${M}_{200{\rm{c}}}={1.87}_{-0.22}^{+0.24}\times {10}^{14}\ {h}_{70}^{-1}\ {M}_{\odot }$, is NW of the X-ray peak and beyond the NW radio relic.},
doi = {10.3847/1538-4357/aa998c},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 851,
place = {United States},
year = {2017},
month = {12}
}

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