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dc.creatorAravena, Manuel
dc.creatorDecarli, Roberto
dc.creatorGonzález-López, Jorge
dc.creatorBoogaard, Leindert
dc.creatorWalter, Fabian
dc.creatorCarilli, Chris
dc.creatorPopping, Gergoe
dc.creatorWeiss, Axel
dc.creatorC
dc.creatorBacon, Roland
dc.creatorErik Bauer, Franz
dc.creatorBertoldi, Frank
dc.creatorBouwens, Richard
dc.creatorContini, Thierry
dc.creatorCortes, Paulo C
dc.creatorCox, Pierre
dc.creatorda Cunha, Elisabete
dc.creatorDaddi, Emanuele
dc.creatorDíaz-Santos, Tanio
dc.creatorElbaz, David
dc.creatorHodge, Jacqueline
dc.creatorInami, Hanae
dc.creatorIvison, Rob
dc.creatorLe Fevre, Olivier
dc.creatorMagnelli, Benjamin
dc.creatorOesch, Pascal
dc.creatorRiechers, Dominik
dc.creatorSmail, Ian
dc.creatorSomerville, Rachel S
dc.creatorSwinbank, A M
dc.creatorUzgil, Bade
dc.creatorvan der Werf, Paul
dc.creatorWagg, Jeff
dc.creatorWisotzki, Lutz
dc.date.accessioned2021-08-23T22:55:37Z
dc.date.available2021-08-23T22:55:37Z
dc.date.issued2019
dc.identifier.urihttp://hdl.handle.net/10533/251674
dc.description.abstractWe analyze the interstellar medium properties of a sample of 16 bright CO line emitting galaxies identified in the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS) Large Program. This CO-selected galaxy sample is complemented by two additional CO line emitters in the UDF that are identified based on their Multi-Unit Spectroscopic Explorer (MUSE) optical spectroscopic redshifts. The ASPECS CO-selected galaxies cover a larger range of star formation rates (SFRs) and stellar masses compared to literature CO emitting galaxies at z > 1 for which scaling relations have been established previously. Most of ASPECS CO-selected galaxies follow these established relations in terms of gas depletion timescales and gas fractions as a function of redshift, as well as the SFR-stellar mass relation ("galaxy main sequence"). However, we find that similar to 30% of the galaxies (5 out of 16) are offset from the galaxy main sequence at their respective redshift, with similar to 12% (2 out of 16) falling below this relationship. Some CO-rich galaxies exhibit low SFRs, and yet show substantial molecular gas reservoirs, yielding long gas depletion timescales. Capitalizing on the well-defined cosmic volume probed by our observations, we measure the contribution of galaxies above, below, and on the galaxy main sequence to the total cosmic molecular gas density at different lookback times. We conclude that main-sequence galaxies are the largest contributors to the molecular gas density at any redshift probed by our observations (z similar to 1-3). The respective contribution by starburst galaxies above the main sequence decreases from z similar to 2.5 to z similar to 1, whereas we find tentative evidence for an increased contribution to the cosmic molecular gas density from the passive galaxies below the main sequence.
dc.language.isoeng
dc.relation.urihttps://doi.org/10.3847/1538-4357/ab30df
dc.rightsAtribución-NoComercial-SinDerivadas 3.0 Chile
dc.rightshttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/
dc.titleThe ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Evolution of the Molecular Gas in CO-selected Galaxies
dc.typeArticulo
dc.description.conicytinstrumentRegular 2015
dc.identifier.folio1151239
dc.description.conicytprogramFONDECYT
dc.relation.contesthandle/10533/111557
dc.rights.driverinfo:eu-repo/semantics/article
dc.rights.driverinfo:eu-repo/semantics/openAccess
dc.title.journalASTROPHYSICAL JOURNAL
dc.relation.instrumenthandle/10533/111541
dc.relation.programhandle/10533/108045
dc.description.shortconicytprogramFONDECYT
dc.type.openaireinfo:eu-repo/semantics/publishedVersion


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