X-ray Properties of Young Early Type Galaxies: II. Abundance Ratio in the Hot ISM

TL;DR

This study uses Chandra X-ray data to compare metal abundance ratios in young versus old elliptical galaxies, revealing recent star formation signatures and SNII contributions in young ellipticals.

Contribution

It provides the first detailed comparison of relative metal abundances in young and old elliptical galaxies using X-ray observations, highlighting the impact of recent mergers.

Findings

Super-solar Si/Fe ratio in young ellipticals

Solar O/Mg ratio in young ellipticals

Differences diminish outside galaxy centers

Abstract

Using Chandra X-ray observations of young, post-merger elliptical galaxies, we present X-ray characteristics of age-related observational results, by comparing with typical old elliptical galaxies in terms of metal abundances in the hot interstellar matter (ISM). While the absolute element abundances may be uncertain because of unknown systematic errors and partly because of the smaller amount of hot gas in young ellipticals, the relative abundance ratios (e.g., the alpha-element to Fe ratio, most importantly Si/Fe ratio) can be relatively well constrained. We find that in two young elliptical galaxies (NGC 720 and NGC 3923) the Si to Fe abundance ratio is super-solar (at a 99% significance level), in contrast to typical old elliptical galaxies where the Si to Fe abundance ratio is close to solar. Also the O/Mg ratio is close to solar in the two young elliptical galaxies, as opposed to the sub-solar O/Mg ratio reported in old elliptical galaxies. Both features appear to be less significant outside the effective radius (roughly 30" for the galaxies under study), consistent with the observations that confine to the centermost regions the signatures of recent star formation in elliptical galaxies. Observed differences between young and old elliptical galaxies can be explained by the additional contribution from SNe II ejecta in the former. In young elliptical galaxies, the later star formation associated with recent mergers would have a dual effect, resulting both in galaxy scale winds - and therefore smaller observed amounts of hot ISM - because of the additional SNII heating, and in different metal abundances, because of the additional SNII yields.