Stellar Abundances at the Center of Early Type Galaxies with Fine Structure

TL;DR

This study uses full-spectrum fitting to analyze stellar abundances in three early-type galaxies with fine structures, revealing diverse chemical signatures linked to their merger histories and formation pathways.

Contribution

It provides detailed stellar abundance measurements for three ETGs with fine structures, highlighting the complexity of their formation processes and challenging simple merger models.

Findings

NGC 3818 and NGC 4915 have chemical signatures similar to ETGs without fine structure.

NGC 2865 shows higher Ca, Cr, and Mn abundances, inconsistent with simple gas-rich merger models.

ETGs with fine structure can form through multiple merger pathways.

Abstract

Our understanding of early-type galaxies (ETGs) has grown in the past decade with the advance of full-spectrum fitting techniques used to infer the properties of the stellar populations that make-up the galaxy. We present ages, central velocity dispersions, and abundance ratios relative to Fe of C, N, O, Mg, Si, Ca, Ti, Cr, Mn, Co, Ni, Cu, Sr, Ba, and Eu, derived using full-spectrum fitting techniques for three ETGs NGC 2865, NGC 3818, and NGC 4915. Each of these three galaxies were selected because they have optical, disturbed structures (fine structure) that are linked to major merger events that occurred 1, 7, and 6 Gyr ago, respectively. Two of the ETGs, NGC 3818 and NGC 4915, show chemical signatures similar to ETGs without fine structure, which is consistent with a gas-poor merger of elliptical galaxies in which substantial star formation is not expected. For NGC 2865, we find a statistically higher abundance of Ca (an $\alpha$-element) and Cr and Mn (Fe-peak elements). We show that for NGC 2865, a simple gas-rich merger scenario fails to explain the larger abundance ratios compared to ETGs without fine structure. These three early-type galaxies with fine structure exhibit a range of abundances, suggesting ETGs with fine structure can form via multiple pathways and types of galaxy mergers.