ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CO LUMINOSITY FUNCTIONS AND THE EVOLUTION OF THE COSMIC DENSITY OF MOLECULAR GAS
Carilli, Chris L.
da Cunha, Elisabete
Ivison, R. J.
Riechers, Dominik A.
Smail, Ian R.
Bauer, Franz E.
Bell, Eric F.
Cortes, Paulo C.
Fevre, Olivier Le
van der Wel, Arjen
van der Werf, Paul
AffiliationUniv Arizona, Steward Observ
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PublisherIOP PUBLISHING LTD
CitationALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CO LUMINOSITY FUNCTIONS AND THE EVOLUTION OF THE COSMIC DENSITY OF MOLECULAR GAS 2016, 833 (1):69 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2016. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractIn this paper we use ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field in band. 3 and band. 6, to place blind constraints on the CO luminosity function and the evolution of the cosmic molecular gas density as a function of redshift up to z similar to 4.5. This study is based on galaxies that have been selected solely through their CO emission and not through any other property. In all of the redshift bins the ASPECS measurements reach the predicted "knee" of the CO luminosity function (around 5 x 10(9) K km s(-1) pc(2)). We find clear evidence of an evolution in the CO luminosity function with respect to z similar to 0, with more CO-luminous galaxies present at z similar to 2. The observed galaxies at z similar to 2 also appear more gas-rich than predicted by recent semi-analytical models. The comoving cosmic molecular gas density within galaxies as a function of redshift shows a drop by a factor of 3-10 from z similar to 2 to z similar to 0 (with significant error bars), and possibly a decline at z > 3. This trend is similar to the observed evolution of the cosmic star formation rate density. The latter therefore appears to be at least partly driven by the increased availability of molecular gas reservoirs at the peak of cosmic star formation (z similar to 2).
VersionFinal published version
SponsorsFONDECYT [1140099, 1151408]; National Science Foundation [AST-1614213]; Concicyt grant Basal-CATA [PFB-06/2007]; Concicyt grant Anilo [ACT1417]; FONDECYT Regular ; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; STFC [ST/L00075X/1]; Collaborative Research Council 956, sub-project A1 - Deutsche Forschungsgemeinschaft (DFG); German ARC; ERC grant COSMIC-DAWN; ERC grant DUSTYGAL; ERC grant COSMICISM