CaltechAUTHORS
Published June 10, 2018 | Version Published + Submitted
Journal Article Open

CLUMP-3D: Testing ΛCDM with Galaxy Cluster Shapes

Creators

  • 1. ROR icon University of Bologna
  • 2. ROR icon Institute of Astronomy and Astrophysics, Academia Sinica
  • 3. ROR icon INFN Sezione di Bologna
  • 4. ROR icon California Institute of Technology
  • 5. ROR icon Institute of Physics of Cantabria
  • 6. ROR icon University of Pennsylvania
  • 7. ROR icon Ben-Gurion University of the Negev

Abstract

The ΛCDM model of structure formation makes strong predictions on the concentration and shape of dark matter (DM) halos, which are determined by mass accretion processes. Comparison between predicted shapes and observations provides a geometric test of the ΛCDM model. Accurate and precise measurements needs a full three-dimensional (3D) analysis of the cluster mass distribution. We accomplish this with a multi-probe 3D analysis of the X-ray regular Cluster Lensing and Supernova survey with Hubble (CLASH) clusters combining strong and weak lensing, X-ray photometry and spectroscopy, and the Sunyaev–Zel'dovich effect (SZe). The cluster shapes and concentrations are consistent with ΛCDM predictions. The CLASH clusters are randomly oriented, as expected given the sample selection criteria. Shapes agree with numerical results for DM-only halos, which hints at baryonic physics being less effective in making halos rounder.

Additional Information

© 2018 The American Astronomical Society. Received 2018 March 30; revised 2018 May 5; accepted 2018 May 18; published 2018 June 7. The authors thank Rossella Cassano and Gianfranco Brunetti for useful discussions, and Gustavo Yepes for supplying the MUSIC-2 simulations performed at the Barcelona Supercomputing Center, Spain. M.S. and S.E. acknowledge support from the contracts ASI-INAF I/009/10/0, NARO15 ASI-INAF I/037/12/0, ASI 2015-046-R.0 and ASI-INAF n.2017-14-H.0. K.U. acknowledges support from the Ministry of Science and Technology of Taiwan (grants 103-2112-M-001-030-MY3 and 106-2628-M-001-003-MY3) and from the Academia Sinica Investigator Award. J.S. was supported by NSF/AST-1617022. M.M. acknowledges support from MAECI and contracts ASI-INAF/I/023/12/0 and ASI n. I/023/12/0. J.V.-F. was supported by AYA2015-64508-P (MINECO/FEDER).

Attached Files

Published - Sereno_2018_ApJL_860_L4.pdf

Submitted - 1804.00667.pdf

Files

1804.00667.pdf

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Additional details

Identifiers

Eprint ID
86882
Resolver ID
CaltechAUTHORS:20180607-104511392

Related works

Describes
https://arxiv.org/abs/1804.00667 (URL)

Funding

Agenzia Spaziale Italiana (ASI)
I/009/10/0
Agenzia Spaziale Italiana (ASI)
I/037/12/0
Agenzia Spaziale Italiana (ASI)
2015-046-R.0
Agenzia Spaziale Italiana (ASI)
2017-14-H.0
Ministry of Science and Technology (Tapei)
103-2112-M-001-030-MY3
Ministry of Science and Technology (Tapei)
106-2628-M-001-003-MY3
Academia Sinica
NSF
AST-1617022
Agenzia Spaziale Italiana (ASI)
I/023/12/0
Agenzia Spaziale Italiana (ASI)
I/023/12/0
Ministerio de Economía, Industria y Competitividad (MINECO)
AYA2015-64508-P

Dates

Created
2018-06-07
Created from EPrint's datestamp field
Updated
2021-11-15
Created from EPrint's last_modified field