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24 April 2024 |
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Article overview
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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 | 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. | Source: | arXiv, 1301.6012 | Services: | Forum | Review | PDF | Favorites |
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