We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field : molecular gas reservoirs in high-redshift galaxies.

Decarli, R. and Walter, F. and Aravena, M. and Carilli, C. and Bouwens, R. and da Cunha, E. and Daddi, E. and Elbaz, D. and Riechers, D. and Smail, I. and Swinbank, M. and Weiss, A. and Bacon, R. and Bauer, F. and Bell, E.F. and Bertoldi, F. and Chapman, S. and Colina, L. and Cortes, P.C. and Cox, P. and Gónzalez-López, J. and Inami, H. and Ivison, R. and Hodge, J. and Karim, A. and Magnelli, B. and Ota, K. and Popping, G. and Rix, H.-W. and Sargent, M. and van der Wel, A. and van der Werf, P. (2016) 'The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field : molecular gas reservoirs in high-redshift galaxies.', Astrophysical journal., 833 (1). p. 70.


We study the molecular gas properties of high-z galaxies observed in the ALMA Spectroscopic Survey (ASPECS) that targets an ˜1 arcmin2 region in the Hubble Ultra Deep Field (UDF), a blind survey of CO emission (tracing molecular gas) in the 3 and 1 mm bands. Of a total of 1302 galaxies in the field, 56 have spectroscopic redshifts and correspondingly well-defined physical properties. Among these, 11 have infrared luminosities {L}{IR}\gt {10}11 {L}⊙ , i.e., a detection in CO emission was expected. Out of these, 7 are detected at various significance in CO, and 4 are undetected in CO emission. In the CO-detected sources, we find CO excitation conditions that are lower than those typically found in starburst/sub-mm galaxy/QSO environments. We use the CO luminosities (including limits for non-detections) to derive molecular gas masses. We discuss our findings in the context of previous molecular gas observations at high redshift (star formation law, gas depletion times, gas fractions): the CO-detected galaxies in the UDF tend to reside on the low-{L}{IR} envelope of the scatter in the {L}{IR}{--}{L}{CO}\prime relation, but exceptions exist. For the CO-detected sources, we find an average depletion time of ˜1 Gyr, with significant scatter. The average molecular-to-stellar mass ratio ({M}{{H}2}/M *) is consistent with earlier measurements of main-sequence galaxies at these redshifts, and again shows large variations among sources. In some cases, we also measure dust continuum emission. On average, the dust-based estimates of the molecular gas are a factor ˜2-5× smaller than those based on CO. When we account for detections as well as non-detections, we find large diversity in the molecular gas properties of the high-redshift galaxies covered by ASPECS.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Publisher statement:© 2016. The American Astronomical Society. All rights reserved.
Date accepted:06 September 2016
Date deposited:09 March 2017
Date of first online publication:08 December 2016
Date first made open access:09 March 2017

Save or Share this output

Look up in GoogleScholar