A Caltech Library Service

CLUMP-3D: Three-dimensional Shape and Structure of 20 CLASH Galaxy Clusters from Combined Weak and Strong Lensing

Chiu, I-Non and Umetsu, Keiichi and Sereno, Mauro and Ettori, Stefano and Meneghetti, Massimo and Merten, Julian and Sayers, Jack and Zitrin, Adi (2018) CLUMP-3D: Three-dimensional Shape and Structure of 20 CLASH Galaxy Clusters from Combined Weak and Strong Lensing. Astrophysical Journal, 860 (2). Art. No. 126. ISSN 0004-637X.

[img] PDF - Published Version
Creative Commons Attribution.

[img] PDF - Accepted Version
See Usage Policy.


Use this Persistent URL to link to this item:


We perform a three-dimensional triaxial analysis of 16 X-ray regular and 4 high-magnification galaxy clusters selected from the CLASH survey by combining two-dimensional weak-lensing and central strong-lensing constraints. In a Bayesian framework, we constrain the intrinsic structure and geometry of each individual cluster assuming a triaxial Navarro–Frenk–White halo with arbitrary orientations, characterized by the mass M_(200c), halo concentration c_(200c), and triaxial axis ratios q_a ⩽ q_b, and investigate scaling relations between these halo structural parameters. From triaxial modeling of the X-ray-selected subsample, we find that the halo concentration decreases with increasing cluster mass, with a mean concentration of c_(200c) = 4.82 ± 0.30 at the pivot mass M_(200c) = 10^(15) M_⊙ h^(-1). This is consistent with the result from spherical modeling, c_(200c) = 4.51 ± 0.14. Independently of the priors, the minor-to-major axis ratio q_a of our full sample exhibits a clear deviation from the spherical configuration q_a = 0.52 ± 0.04 at 10^(15) M_⊙ h^(-1) with uniform priors), with a weak dependence on the cluster mass. Combining all 20 clusters, we obtain a joint ensemble constraint on the minor-to-major axis ratio of q_a = 0.652_(-0.078)^(+0.162) and a lower bound on the intermediate-to-major axis ratio of q_b > 0.63 at the 2σ level from an analysis with uniform priors. Assuming priors on the axis ratios derived from numerical simulations, we constrain the degree of triaxiality for the full sample to be T = 0.79 ± 0.03 at 10^(15) M_⊙ h^(-1), indicating a preference for a prolate geometry of cluster halos. We find no statistical evidence for an orientation bias (f_(geo) = 0.93 ± 0.07), which is insensitive to the priors and in agreement with the theoretical expectation for the CLASH clusters.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Chiu, I-Non0000-0002-5819-6566
Umetsu, Keiichi0000-0002-7196-4822
Sereno, Mauro0000-0003-0302-0325
Ettori, Stefano0000-0003-4117-8617
Meneghetti, Massimo0000-0003-1225-7084
Sayers, Jack0000-0002-8213-3784
Zitrin, Adi0000-0002-0350-4488
Additional Information:© 2018. The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2018 March 31; revised 2018 May 8; accepted 2018 May 11; published 2018 June 20. We thank Tetsu Kitayama and Daichi Suto for providing us with simulated data points that are presented in Figure 8. We thank the anonymous referee for providing constructive suggestions that lead to the improvement of this paper. K.U. acknowledges support from the Ministry of Science and Technology of Taiwan (grants MoST 103-2112-M-001-030-MY3 and MoST 106-2628-M-001-003-MY3) and from the Academia Sinica Investigator Award. M.S. acknowledges financial 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. J.S. was supported by NSF/AST-1617022. M.M., M.S., S.E., J.S. acknowledge support from the Italian Ministry of Foreign Affairs and International Cooperation, Directorate General for Country Promotion (Project "Crack the lens"). This work was made possible by the availability of high-quality lensing data produced by the CLASH survey. This paper made use of the code colossus (Diemer 2017) and the packages from Bocquet and Carter (2016) and Hinton (2016) for plotting. This work made use of the IPython package (Pérez & Granger 2007), SciPy (Jones et al. 2001), TOPCAT, an interactive graphical viewer and editor for tabular data (Taylor 2005), matplotlib, a Python library for publication quality graphics (Hunter 2007), Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), NumPy (Van Der Walt et al. 2011).
Funding AgencyGrant Number
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 SinicaUNSPECIFIED
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
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Ministero degli affari esteri e della cooperazione internazionale (MAECI)UNSPECIFIED
Subject Keywords:cosmology: observations; dark matter; galaxies: clusters: general; gravitational lensing: weak; gravitational lensing: strong
Issue or Number:2
Record Number:CaltechAUTHORS:20180626-135119115
Persistent URL:
Official Citation:I-Non Chiu et al 2018 ApJ 860 126
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:87353
Deposited By: George Porter
Deposited On:26 Jun 2018 21:21
Last Modified:03 Oct 2019 19:55

Repository Staff Only: item control page