Temperature and abundance profiles of hot gas in galaxy groups - I. Results and statistical analysis

TL;DR

This study analyzes temperature and metal abundance profiles in 15 galaxy groups, revealing similarities to clusters at large radii and providing insights into chemical enrichment and supernova contributions.

Contribution

It presents detailed radial profiles of temperature and metal abundances in galaxy groups, including new fitting formulas and analysis of supernova enrichment patterns.

Findings

Most groups have cool cores with sizes correlating with mean temperature.

Temperature profiles are similar across groups when scaled, flatter inward of the peak.

Fe abundance shows central excess and declines with radius, with supernova type Ia dominating core enrichment.

Abstract

The distribution of metals in groups of galaxies holds important information about the chemical enrichment history of the Universe. Here we present radial profiles of temperature and the abundance of iron and silicon of the hot intragroup medium for a sample of 15 nearby groups of galaxies observed by Chandra, selected for their regular X-ray morphology. All but one group display a cool core, the size of which is found to correlate with the mean temperature of the group derived outside this core. When scaled to this mean temperature, the temperature profiles are remarkably similar, being analogous to those of more massive clusters at large radii but significantly flatter inwards of the temperature peak. The Fe abundance generally shows a central excess followed by a radial decline, reaching a typical value of 0.1 solar within r_500, a factor of two lower than corresponding results for clusters. Si shows less systematic radial variation, on average displaying a less pronounced decline than Fe and showing evidence for a flattening at large radii. Off-centre abundance peaks are seen both for Fe and Si in a number of groups with well-resolved cores. Derived abundance ratios indicate that supernovae type Ia are responsible for 80 per cent of the Fe in the group core, but the type II contribution increases with radius and completely dominates at r_500. We present fitting formulae for the radial dependence of temperature and abundances, to facilitate comparison to results of numerical simulations of group formation and evolution. In a companion paper, we discuss the implications of these results for feedback and enrichment in galaxy groups.