CO(1-0) detection of molecular gas in the massive Spiderweb Galaxy (z=2)

TL;DR

This study reports the detection of CO(1-0) emission indicating substantial cold molecular gas in the Spiderweb Galaxy at z=2, suggesting active star formation and mass assembly in this massive proto-cluster environment.

Contribution

First detection of CO(1-0) in the Spiderweb Galaxy, revealing widespread molecular gas and insights into star formation in a high-redshift proto-cluster.

Findings

Molecular gas mass is approximately 6x10^10 solar masses.

Gas is distributed across the galaxy and inter-galactic medium.

Star formation could be sustained for about 40 million years.

Abstract

The high-redshift radio galaxy MRC 1138-262 (`Spiderweb Galaxy'; z = 2.16), is one of the most massive systems in the early Universe and surrounded by a dense `web' of proto-cluster galaxies. Using the Australia Telescope Compact Array, we detected CO(1-0) emission from cold molecular gas -- the raw ingredient for star formation -- across the Spiderweb Galaxy. We infer a molecular gas mass of M(H2) = 6x10^10 M(sun) (for M(H2)/L'(CO)=0.8). While the bulk of the molecular gas coincides with the central radio galaxy, there are indications that a substantial fraction of this gas is associated with satellite galaxies or spread across the inter-galactic medium on scales of tens of kpc. In addition, we tentatively detect CO(1-0) in the star-forming proto-cluster galaxy HAE 229, 250 kpc to the west. Our observations are consistent with the fact that the Spiderweb Galaxy is building up its stellar mass through a massive burst of widespread star formation. At maximum star formation efficiency, the molecular gas will be able to sustain the current star formation rate (SFR ~ 1400 M(sun)/yr, as traced by Seymour et al.) for about 40 Myr. This is similar to the estimated typical lifetime of a major starburst event in infra-red luminous merger systems.