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24 April 2024
 
  » arxiv » 1301.6012

 Article overview


CO(1-0) detection of molecular gas in the massive Spiderweb Galaxy (z=2)
B.H.C. Emonts ; I. Feain ; H.J.A. Roettgering ; G. Miley ; N. Seymour ; R.P. Norris ; C.L. Carilli ; M. Villar-Martin ; M.Y. Mao ; E.M. Sadler ; R.D. Ekers ; G.A. van Moorsel ; R.J. Ivison ; L. Pentericci ; C.N. Tadhunter ; D.J. Saikia ;
Date 25 Jan 2013
AbstractThe 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.
Source arXiv, 1301.6012
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