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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 adense `web' of proto-cluster galaxies. Using the Australia Telescope CompactArray, we detected CO(1-0) emission from cold molecular gas -- the rawingredient for star formation -- across the Spiderweb Galaxy. We infer amolecular gas mass of M(H2) = 6x10^10 M(sun) (for M(H2)/L'(CO)=0.8). While thebulk of the molecular gas coincides with the central radio galaxy, there areindications that a substantial fraction of this gas is associated withsatellite galaxies or spread across the inter-galactic medium on scales of tensof kpc. In addition, we tentatively detect CO(1-0) in the star-formingproto-cluster galaxy HAE 229, 250 kpc to the west. Our observations areconsistent with the fact that the Spiderweb Galaxy is building up its stellarmass through a massive burst of widespread star formation. At maximum starformation efficiency, the molecular gas will be able to sustain the currentstar formation rate (SFR ~ 1400 M(sun)/yr, as traced by Seymour et al.) forabout 40 Myr. This is similar to the estimated typical lifetime of a majorstarburst event in infra-red luminous merger systems.

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