CO in the ALMA Radio-Source Catalogue (ARC): the molecular gas content of radio galaxies as a function of redshift

TL;DR

This study investigates the molecular gas content in radio galaxies across different redshifts using ALMA data, revealing an increase in H2 mass with redshift and insights into galaxy evolution and AGN activity.

Contribution

It provides the first large archival CO survey of radio galaxies, combining new ALMA data with literature to analyze molecular gas evolution over cosmic time.

Findings

H2 mass in radio galaxies increases with redshift.

At 1<z<2.5, many RGs have gas reservoirs comparable to starburst hosts.

The volume density of molecular gas in the brightest RGs remains similar across epochs.

Abstract

To evaluate the role of radio activity in galaxy evolution, we designed a large archival CO survey of radio galaxies (RGs) to determine their molecular gas masses at different epochs. We used a sample of 120 RGs representative of the NVSS 1.4 GHz survey, when flux limited at 0.4 Jy. Of those, 66 galaxies belonged to the ALMA Radio-source Catalogue (ARC) of calibrators and had spectral window tunings around CO (1-0), (2-1), (3-2), or (4-3). We reduced their ALMA data, determined their H2 mass contents, and combined the results with similar results for the remaining 54 galaxies from the literature. We found that, while at all epochs the majority of RGs have undetectable reservoirs, there is a rapid increase in the H2 mass content of the CO-detected RGs with z. At 1<z<2.5, one-fourth of the RGs have at least as much molecular gas as simulations would indicate for a typical halo mass of that epoch. These galaxies plausibly have ``normal'' or even starburst hosts. Taking into account the completeness correction of the sample, we created the corresponding H$_2$ mass functions at 0.005<z<0.3 and 1<z<2.5. The local mass function reveals that the number density of low-z RGs with detectable molecular gas reservoirs is only a little lower (a factor of ~4) than that of pure (or little star-forming) type 1 and 2 AGN in simulations. At 1<z<2.5, there is a significant decrease in the number density of high-z RGs due to the rarity of bright radio galaxies. An estimate for the missing faint RGs would, nonetheless, bring populations close again. Finally, we find that the volume density of molecular gas locked up in the brightest 1/5000-1/7000 RGs is similar in the examined $z$ bins. This result likely indicates that the inflow rate on one hand and the star-formation depletion rate plus the jet-driven expulsion rate on the other hand counteract each other in the most luminous RGs of each epoch.