Molecular gas in galaxies of Hickson compact groups

TL;DR

This study observes molecular gas in galaxies within Hickson compact groups, revealing enhanced central gas concentrations likely driven by tidal interactions, and compares their properties with other galaxy samples to understand star formation and merging processes.

Contribution

First comprehensive CO observations of Hickson compact group galaxies, highlighting gas concentration effects and star formation efficiency differences compared to other environments.

Findings

Enhanced molecular gas ratios in compact group galaxies.

Molecular gas content similar to galaxy pairs and starburst samples.

Star formation efficiency appears lower in compact groups.

Abstract

We have observed 70 galaxies belonging to 45 Hickson compact groups in the CO(1-0) and CO(2-1) lines, in order to determine their molecular content. We detected 57 galaxies, corresponding to a detection rate of 81%. We compare the gas content relative to blue and FIR luminosities of galaxies in compact groups with respect to other samples in the literature, including various environments and morphological types. We find that there is some hint of enhanced M(H2)/Lb and M(dust)/Lb ratios in the galaxies from compact group with respect to our control sample, especially for the most compact groups, suggesting that tidal interactions can drive the gas component inwards, by removing its angular momentum, and concentrating it in the dense central regions, where it is easily detected. The molecular gas content in compact group galaxies is similar to that in pairs and starburst samples. However, the total L(FIR) luminosity of HCGs is quite similar to that of the control sample, and therefore the star formation efficiency appears lower than in the control galaxies. However this assumes that the FIR spatial distributions are similar in both samples which is not the case at radio frequencies. Higher spatial resolution FIR data are needed to make a valid comparison. Given their short dynamical friction time-scale, it is possible that some of these systems are in the final stage before merging, leading to ultra-luminous starburst phases. We also find for all galaxy samples that the \htwo content (derived from CO luminosity and normalised to blue luminosity) is strongly correlated to the L(FIR)luminosity, while the total gas content H2+HI is not.