Villanueva, V., Ibar, E., Hughes, T.M., Lara-Lopez, M.A., Dunne, L., Eales, S., Ivison, R.J., Aravena, M., Baes, M., Bourne, N., Cassata, P., Cooray, A., Dannerbauer, H., Davies, L.J.M., Driver, S.P., Dye, S., Furlanetto, C., Herrera-Camus, R., Maddox, S.J., Michałowski, M.J., Molina, J., Riechers, D., Sansom, A.E., Smith, M.W.L., Rodighiero, G., Valiante, E. and van der Werf, P.
(2017)
VALES I: the molecular gas content in star-forming dusty H-ATLAS galaxies up to z = 0.35.
Monthly Notices of the Royal Astronomical Society, 470
(4).
pp. 3775-3805.
ISSN 1365-2966
Abstract
We present an extragalactic survey using observations from the Atacama Large Millimeter/submillimeter Array (ALMA) to characterize galaxy populations up to z = 0.35: the Valpara´ıso ALMA Line Emission Survey (VALES). We use ALMA Band-3 CO(1–0) observations to study the molecular gas content in a sample of 67 dusty normal star-forming galaxies selected from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We have spectrally detected 49 galaxies at >5σ significance and 12 others are seen at low significance in stacked spectra. CO luminosities are in the range of (0.03–1.31) × 1010 K km s−1 pc2, equivalent to log(Mgas/M) = 8.9–10.9 assuming an αCO = 4.6 (K km s−1 pc2) −1, which perfectly complements the parameter space previously explored with local and high-z normal galaxies. We compute the optical to CO size ratio for 21 galaxies resolved by ALMA at ∼3.5 arcsec resolution (6.5 kpc), finding that the molecular gas is on average ∼ 0.6 times more compact than the stellar component. We obtain a global Schmidt–Kennicutt relation, given by log[[ΣSFR/(M yr−1 kpc−2)] = (1.26 ± 0.02) × log[ΣMH2 /(M pc−2)] − (3.6 ± 0.2). We find a significant fraction of galaxies lying at ‘intermediate efficiencies’ between a longstanding mode of star formation activity and a starburst, specially at LIR = 1011–12 L. Combining our observations with data taken from the literature, we propose that star formation efficiencies can be parametrized by log [SFR/MH2 ] = 0.19 × (log LIR − 11.45) − 8.26 − 0.41 × arctan[−4.84 (logLIR − 11.45)]. Within the redshift range we explore (z < 0.35), we identify a rapid increase of the gas content as a function of redshift.
| Item Type: |
Article
|
| Additional Information: |
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
| Keywords: |
ISM: lines and bands, galaxies: high-redshift, galaxies: ISM, infrared: galaxies, submillimetre: galaxies |
| Schools/Departments: |
University of Nottingham, UK > Faculty of Science > School of Physics and Astronomy |
| Identification Number: |
https://doi.org/10.1093/mnras/stx1338 |
| Depositing User: |
Eprints, Support
|
| Date Deposited: |
25 Aug 2017 09:31 |
| Last Modified: |
18 Oct 2017 17:30 |
| URI: |
https://eprints.nottingham.ac.uk/id/eprint/45138 |
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