A survey of molecular gas in luminous sub-millimetre galaxies

M. S. Bothwell*, Ian Smail, S. C. Chapman, R. Genzel, R. J. Ivison, L. J. Tacconi, S. Alaghband-Zadeh, F. Bertoldi, A. W. Blain, C. M. Casey, P. Cox, T. R. Greve, D. Lutz, R. Neri, A. Omont, A. M. Swinbank

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

Abstract

We present the results from a survey of 12CO emission in 40 luminous sub-millimetre galaxies (SMGs), with 850-μm fluxes of S850μm = 4-20 mJy, conducted with the Plateau de Bure Interferometer. We detect 12CO emission in 32 SMGs at z ~ 1.2-4.1, including 16 SMGs not previously published. Using multiple 12CO line (Jup = 2-7) observations, we derive a median spectral line energy distribution for luminous SMGs. We report the discovery of a fundamental relationship between 12CO FWHM and 12CO line luminosity in high-redshift starbursts, which we interpret as a natural consequence of the baryon-dominated dynamics within the regions probed by our observations. We use far-infrared luminosities to assess the star formation efficiency in our SMGs, finding that the slope of the L' CO -LFIR relation is close to linear. We derive molecular gas masses, finding a mean gas mass of (5.3 ± 1.0) × 10)10 M. Combining these with dynamical masses, we determine the redshift evolution of the gas content of SMGs, finding that they do not appear to be significantly more gas rich than less vigorously star-forming galaxies at high redshifts. Finally, we collate X-ray observations, and study the interdependence of gas and dynamical properties of SMGs with their AGN activity and supermassive black holemasses (MBH), finding that SMGs lie significantly below the local MBH-σ relation.

Original languageEnglish
Pages (from-to)3047-3067
Number of pages21
JournalMonthly Notices of the Royal Astronomical Society
Volume429
Issue number4
DOIs
Publication statusPublished - 17 Jan 2013

Keywords

  • Cosmology: observations
  • Galaxies: evolution
  • Galaxies: formation
  • Galaxies: ISM

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