Probing the cool ISM in galaxies via 21cm HI absorption

TL;DR

This study investigates 21cm HI absorption in young radio AGN to understand cold gas distribution and evolution in host galaxies, revealing diverse absorption profiles and host galaxy types.

Contribution

It introduces a Bayesian spectral-line detection method and presents new HI absorption detections in young radio AGN, expanding knowledge of cold gas in different galaxy types.

Findings

Detected two new HI absorbers and one known system.

Observed both narrow and broad absorption components.

Host galaxies include gas-rich spirals and early-type galaxies.

Abstract

Recent targeted studies of associated HI absorption in radio galaxies are starting to map out the location, and potential cosmological evolution, of the cold gas in the host galaxies of Active Galactic Nuclei (AGN). The observed 21 cm absorption profiles often show two distinct spectral-line components: narrow, deep lines arising from cold gas in the extended disc of the galaxy, and broad, shallow lines from cold gas close to the AGN (e.g. Morganti et al. 2011). Here, we present results from a targeted search for associated HI absorption in the youngest and most recently-triggered radio AGN in the local universe (Allison et al. 2012b). So far, by using the recently commissioned Australia Telescope Compact Array Broadband Backend (CABB; Wilson et al. 2011), we have detected two new absorbers and one previously-known system. While two of these show both a broad, shallow component and a narrow, deep component (see Fig. 1), one of the new detections has only a single broad, shallow component. Interestingly, the host galaxies of the first two detections are classified as gas-rich spirals, while the latter is an early-type galaxy. These detections were obtained using a spectral-line finding method, based on Bayesian inference, developed for future large-scale absorption surveys (Allison et al. 2012a).