Combining strong lensing and dynamics in galaxy clusters: integrating MAMPOSSt within LENSTOOL

I. Application on SL2S J02140-0535^⋆,⋆⋆

¹ Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. postal 106, CP 22800, Ensenada, B.C Mexico
e-mail: tomasv@astrosen.unam.mx
² Instituto de Física y Astronomía, Universidad de Valparaíso, Avenida Gran Bretaña 1111, Valparaíso, Chile
³ Laboratoire d’Astrophysique de Marseille, Université de Provence, CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille Cedex 13, France
⁴ Institut d’Astrophysique de Paris (UMR 7095: CNRS & UPMC), 98bis Bd Arago, 75014 Paris, France
⁵ Max-Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, 85748 Garching, Germany
⁶ INAF−IASF Milano, via E. Bassini 15, 20133 Milano, Italy
⁷ INAF−Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34143 Trieste, Italy
⁸ Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile
⁹ Laboratoire d’Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS, 57 avenue d’Azereix, 65 000 Tarbes, France
¹⁰ Institut Utinam, CNRS UMR 6213, Université de Franche-Comté, OSU THETA Franche-Comté-Bourgogne, Observatoire de Besançon, BP 1615, 25010 Besançon Cedex, France
¹¹ Facultad de Ciencias Físico-Matemáticas, Universidad Autónoma de Nuevo León, San Nicolás de los Garza, Mexico
¹² Department of Physics and Astronomy, University of California, Riverside, CA 92521, USA

Received: 2 April 2016
Accepted: 11 August 2016

Abstract

Context. The mass distribution in galaxy clusters and groups is an important cosmological probe. It has become clear in recent years that mass profiles are best recovered when combining complementary probes of the gravitational potential. Strong lensing (SL) is very accurate in the inner regions, but other probes are required to constrain the mass distribution in the outer regions, such as weak lensing or studies of dynamics.

Aims. We constrain the mass distribution of a cluster showing gravitational arcs by combining a strong lensing method with a dynamical method using the velocities of its 24 member galaxies.

Methods. We present a new framework in which we simultaneously fit SL and dynamical data. The SL analysis is based on the LENSTOOL software and the dynamical analysis uses the MAMPOSSt code, which we integrated into LENSTOOL. After describing the implementation of this new tool, we applied it to the galaxy group SL2S J02140-0535 (z_spec = 0.44), which we had previously studied. We used new VLT/FORS2 spectroscopy of multiple images and group members, as well as shallow X-ray data from XMM.

Results. We confirm that the observed lensing features in SL2S J02140-0535 belong to different background sources. One of these sources is located at z_spec = 1.017 ± 0.001, whereas the other source is located at z_spec = 1.628 ± 0.001. With the analysis of our new and our previously reported spectroscopic data, we find 24 secure members for SL2S J02140-0535. Both data sets are well reproduced by a single NFW mass profile; the dark matter halo coincides with the peak of the light distribution, with scale radius, concentration, and mass equal to r_s = 82⁺⁴⁴_-17 kpc, c₂₀₀ = 10.0^+1.7_-2.5, and M₂₀₀ = 1.0^+0.5_-0.2 × 10¹⁴ M_⊙ respectively. These parameters are better constrained when we fit SL and dynamical information simultaneously. The mass contours of our best model agrees with the direction defined by the luminosity contours and the X-ray emission of SL2S J02140-0535. The simultaneous fit lowers the error in the mass estimate by 0.34 dex, when compared to the SL model, and in 0.15 dex when compared to the dynamical method.

Conclusions. The combination of SL and dynamics tools yields a more accurate probe of the mass profile of SL2S J02140-0535 up to r₂₀₀. However, there is tension between the best elliptical SL model and the best spherical dynamical model. The similarities in shape and alignment of the centroids of the total mass, light, and intracluster gas distributions add to the picture of a non-disturbed system.