The morphology and kinematics of the galaxy group AM 1054-325: A MUSE perspective

TL;DR

This study uses MUSE data to analyze how galaxy interactions in the group AM 1054-325 influence morphology, star formation, and chemical properties, revealing tidal effects and gas dynamics.

Contribution

It provides a detailed spatial and spectral analysis of galaxy interactions, star formation, and metallicity variations within the group using MUSE observations.

Findings

Star-forming clumps along tidal tails have higher metallicities.

Galaxy B shows quenched star formation and disturbed gas kinematics.

Tidal interactions contribute significantly to stellar mass growth.

Abstract

Galaxy interactions in groups can lead to intense starbursts and the activation of active galactic nuclei (AGNs). The stripped gas from the outer disk can lead to star-forming clumps along the tidal tails or sometimes tidal dwarf galaxies. We investigate the impact of interaction on various galaxy properties, including morphology, star formation rates, and chemical composition in the galaxy group AM\,1054-325 using Multi Unit Spectroscopic Explorer (MUSE) data. We conduct a comprehensive spatially and spectrally resolved investigation of the star formation rate, star formation histories, metallicity, and AGN activity. The galaxy subgroup AM\,1054-325A shows multiple star-forming clumps in H$\alpha$ emission along the western tidal tail, which are formed due to tidal stripping. These clumps also have higher metallicities. AM\,1054-325B is quenched and shows disturbed gas kinematics and the signature of gas accretion in the H$\alpha$ map. The specific star formation along the tidal tail is higher, contributing to the galaxy's overall stellar mass growth.