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dc.contributor.authorChapman, S. C.-
dc.contributor.authorBothwell, M. S.-
dc.contributor.authorNeri, R.-
dc.contributor.authorCox, P.-
dc.contributor.authorBertoldi, F.-
dc.contributor.authorSmail, I.-
dc.contributor.authorCoppin, K.-
dc.contributor.authorSwinbank, A. M.-
dc.contributor.authorCoppin, K.-
dc.contributor.authorGreve, T. R.-
dc.contributor.authorMuxlow, T. W. B.-
dc.contributor.authorBeswick, R. J.-
dc.contributor.authorBlain, A. W.-
dc.contributor.authorGenzel, R.-
dc.contributor.authorOmont, A.-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society , 2011, 415 (3), pp. 2723-2743-
dc.description.abstractWe present interferometric CO observations of 12 z∼ 2 submillimetre-faint, star-forming radio galaxies (SFRGs) which are thought to be ultraluminous infrared galaxies (ULIRGs) possibly dominated by warmer dust (Tdust ≳ 40 K) than submillimetre galaxies (SMGs) of similar luminosities. Four other CO-observed SFRGs are included from the literature, and all the observations are taken at the Plateau de Bure Interferometer (PdBI) in the compact configuration. 10 of the 16 SFRGs observed in CO (63 per cent) are detected at >4σ with a mean inferred molecular gas mass of ∼2 × 1010 M⊙. SFRGs trend slightly above the local ULIRG LFIR–L′CO relation. Since SFRGs are about two times fainter in radio luminosity but exhibit similar CO luminosities to SMGs, this suggests SFRGs are slightly more efficient star formers than SMGs at the same redshifts. SFRGs also have a narrow mean CO linewidth, 320 ± 80 km s−1. Many SMGs have similarly narrow CO linewidths, but very broad features (∼900 km s−1) are present in a few SMGs and are absent from SFRGs. SFRGs bridge the gap between properties of very luminous >5 × 1012 L⊙ SMGs and those of local ULIRGs, and are consistent with intermediate-stage major mergers. We suspect that more moderate luminosity SMGs, not yet surveyed in CO, would show similar molecular gas properties to SFRGs. The active galactic nucleus (AGN) fraction of SFRGs is consistent with SMGs and is estimated to be 0.3 ± 0.1, suggesting that SFRGs are observed near the peak phase of star formation activity and not in a later, post-SMG enhanced AGN phase. The excitation analysis of one SFRG is consistent with the CO excitation observed in SMGs [turning over beyond 12CO(J= 4→3)]. This CO survey of SFRGs serves as a pilot project for the much more extensive survey of Herschel and SCUBA-2 selected sources which only partially overlap with SMGs. Better constraints on the CO properties of a diverse high-z ULIRG population are needed from ALMA to determine the evolutionary origin of extreme starbursts, and what role ULIRGs serve in catalyzing the formation of massive stellar systems in the early Universe.-
dc.publisherOxford University Press (OUP)-
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 the authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.-
dc.titleMolecular gas in submillimetre-faint, star-forming ultraluminous galaxies at z > 1-
dc.typeJournal Article-
dc.description.versionPublisher Version-
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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