The merging cluster Abell 1758 revisited: multi-wavelength observations and numerical simulations^⋆

¹ UPMC Université Paris 06, UMR 7095, Institut d’Astrophysique de Paris, 75014 Paris, France
e-mail: durret@iap.fr
² CNRS, UMR 7095, Institut d’Astrophysique de Paris, 75014 Paris, France
³ IAG, USP, R. do Matão 1226, 05508-090 São Paulo/SP, Brazil
⁴ Inst. of Astro and Particle Physics, University of Innsbruck, 6020 Innsbruck, Austria

Received: 22 October 2010
Accepted: 4 February 2011

Abstract

Context. Cluster properties can be more distinctly studied in pairs of clusters, where we expect the effects of interactions to be strong.

Aims. We here discuss the properties of the double cluster Abell 1758 at a redshift z ~ 0.279. These clusters show strong evidence for merging.

Methods. We analyse the optical properties of the North and South cluster of Abell 1758 based on deep imaging obtained with the Canada-France-Hawaii Telescope (CFHT) archive Megaprime/Megacam camera in the g′ and r′ bands, covering a total region of about 1.05 × 1.16 deg², or 16.1 × 17.6 Mpc². Our X-ray analysis is based on archive XMM-Newton images. Numerical simulations were performed using an N-body algorithm to treat the dark-matter component, a semi-analytical galaxy-formation model for the evolution of the galaxies and a grid-based hydrodynamic code with a parts per million (PPM) scheme for the dynamics of the intra-cluster medium. We computed galaxy luminosity functions (GLFs) and 2D temperature and metallicity maps of the X-ray gas, which we then compared to the results of our numerical simulations.

Results. The GLFs of Abell 1758 North are well fit by Schechter functions in the g′ and r′ bands, but with a small excess of bright galaxies, particularly in the r′ band; their faint-end slopes are similar in both bands. In contrast, the GLFs of Abell 1758 South are not well fit by Schechter functions: excesses of bright galaxies are seen in both bands; the faint-end of the GLF is not very well defined in g′. The GLF computed from our numerical simulations assuming a halo mass-luminosity relation agrees with those derived from the observations. From the X-ray analysis, the most striking features are structures in the metal distribution. We found two elongated regions of high metallicity in Abell 1758 North with two peaks towards the centre. In contrast, Abell 1758 South shows a deficit of metals in its central regions. Comparing observational results to those derived from numerical simulations, we could mimic the most prominent features present in the metallicity map and propose an explanation for the dynamical history of the cluster. We found in particular that in the metal-rich elongated regions of the North cluster, winds had been more efficient than ram-pressure stripping in transporting metal-enriched gas to the outskirts.

Conclusions. We confirm the merging structure of the North and South clusters, both at optical and X-ray wavelengths.