The H$\alpha$ kinematics of interacting galaxies in 12 compact groups

TL;DR

This study uses Fabry-Perot observations to analyze the kinematics of 42 galaxies in 12 compact groups, revealing diverse interaction stages and their effects on galaxy gas content and star formation.

Contribution

First detailed kinematic analysis of galaxies in compact groups using Fabry-Perot data, linking interaction stages with gas removal and star formation activity.

Findings

Most galaxies show disturbed velocity fields due to interactions.

Some galaxies lack Hα emission, indicating possible gas removal or observational limits.

Only two galaxies have undisturbed rotation curves, suggesting varied interaction effects.

Abstract

We present new Fabry-Perot observations for a sample of 42 galaxies located in twelve compact groups of galaxies: HCG 1, HCG 14, HCG 25, HCG 44, HCG 53, HCG 57, HCG 61, HCG 69, HCG 93, VV 304, LGG 455 and Arp 314. From the 42 observed galaxies, a total of 26 objects are spiral galaxies, which range from Sa to Im morphological types. The remaining 16 objects are E, S0 and S0a galaxies. Using these observations, we have derived velocity maps, monochromatic and velocity dispersion maps for 24 galaxies, where 18 are spiral, three are S0a, two are S0 and one is an Im galaxy. From the 24 velocity fields obtained, we could derive rotation curves for 15 galaxies; only two of them exhibit rotation curves without any clear signature of interactions. Based on kinematic information, we have evaluated the evolutionary stage of the different groups of the current sample. We identify groups that range from having no H$\alpha$ emission to displaying an extremely complex kinematics, where their members display strongly perturbed velocity fields and rotation curves. In the case of galaxies with no H$\alpha$ emission, we suggest that past galaxy interactions removed their gaseous components, thereby quenching their star formation. However, we can not discard that the lack of H$\alpha$ emission is linked with the detection limit for some of our observations.