Chemical enrichment of the intracluster medium within the A3266 cluster

I. Radial profiles

¹ Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching, Germany
² Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
³ Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
⁴ INAF – IASF Palermo, Via U. La Malfa 153, I-90146 Palermo, Italy
⁵ School of Physics & Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD, UK
⁶ Department of Astronomy, University of Geneva, Ch. d’Ecogia 16, CH-1290 Versoix, Switzerland
⁷ Department of Physics and Astronomy, University of Alabama in Huntsville, Huntsville, AL 35899, USA
⁸ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
⁹ Department of Astrophysical Sciences, Princeton University, NJ 08544, USA

^⋆ Corresponding author: egatuzz@mpe.mpg.de

Received: 9 December 2024
Accepted: 17 April 2025

Abstract

We present a detailed study of the elemental abundances distribution of the intracluster medium (ICM) within the A3266 cluster using XMM-Newton observations. This analysis uses EPIC-pn data, including a new energy scale calibration, which allows us to measure velocities with uncertainties down to Δv ∼ 80 km/s, and MOS observations. We measured radial O, Mg, Si, S, Ar, Ca, and Fe profiles. This is the first study of elemental abundances beyond Fe using X-ray observations within the A3266 cluster. The abundance profiles display discontinuities similar to those obtained for the temperature. We modeled the X/Fe ratio profiles with a linear combination of type Ia supernovae (SNIa) and core-collapse supernovae (SNcc) models. We found that the SNIa ratio over the total cluster enrichment tends to be uniform, with a 42 ± 5% contribution. Such a trend supports an early ICM enrichment scenario, with most metals produced before clustering.