HI in radio galaxies: prospects for upcoming wide-field surveys

TL;DR

This study investigates the large-scale properties of neutral hydrogen in nearby radio galaxies, revealing differences based on radio source size and suggesting that low-power radio-AGN activity may be a transient phase in early-type galaxy evolution.

Contribution

It provides new insights into the HI content of radio galaxy hosts, highlighting differences between extended and compact sources and emphasizing the importance of upcoming HI surveys.

Findings

Extended FR-I radio hosts are HI poor and show no signs of recent mergers.

Compact radio sources often contain large HI discs/rings, indicating different fueling mechanisms.

Overall HI properties are similar to radio-quiet early-type galaxies, suggesting transient AGN activity.

Abstract

We present results of an ongoing systematic study of the large-scale properties of neutral hydrogen (HI) gas in nearby radio galaxies. Our main goal is to investigate the importance of gas-rich galaxy mergers and interactions among radio-loud AGN. From an HI study of a complete sample of classical low-power radio galaxies we find that the host galaxies of extended Fanaroff & Riley type-I radio sources are generally HI poor (< 10E8 M_sun) and show no indications for gas-rich galaxy mergers or ongoing gas-rich interactions. In contrast, the host galaxies of a significant fraction of low-power compact radio sources contain enormous discs/rings of HI gas (with sizes up to 190 kpc and masses up to 2 x 10E10 M_sun). This segregation in HI mass with radio source size likely indicates that these compact radio sources are either confined by large amounts of gas in the central region, or that their fueling is inefficient and different from the fueling process of classical FR-I radio sources. To a first order, the overall HI properties of our complete sample (detection rate, mass and morphology) appear similar to those of radio-quiet early-type galaxies. If confirmed by better statistics, this would imply that low-power radio-AGN activity may be a short phase that occurs at some point during the lifetime of many early-type galaxies. We discuss how upcoming HI surveys (e.g. with ASKAP and Apertif) are essential for studying in a statistical way the the connection between the presence and morphology of a radio-loud AGN and the properties of the cold HI gas associated with its host galaxy.