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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/28649
Title: The ALMA Spectroscopic Survey in the HUDF: CO Luminosity Functions and the Molecular Gas Content of Galaxies through Cosmic History
Authors: DECARLI, ROBERTO 
Walter, Fabian
Gónzalez-López, Jorge
Aravena, Manuel
Boogaard, Leindert
Carilli, Chris
Cox, Pierre
Daddi, Emanuele
Popping, Gergö
Riechers, Dominik
Uzgil, Bade
Weiss, Axel
Assef, Roberto J.
Bacon, Roland
Bauer, Franz Erik
Bertoldi, Frank
Bouwens, Rychard
Contini, Thierry
Cortes, Paulo C.
da Cunha, Elisabete
Díaz-Santos, Tanio
Elbaz, David
Inami, Hanae
Hodge, Jacqueline
Ivison, Rob
Le Fèvre, Olivier
Magnelli, Benjamin
Novak, Mladen
Oesch, Pascal
Rix, Hans-Walter
Sargent, Mark T.
Smail, Ian
Swinbank, A. Mark
Somerville, Rachel S.
van der Werf, Paul
Wagg, Jeff
Wisotzki, Lutz
Issue Date: 2019
Journal: THE ASTROPHYSICAL JOURNAL 
Number: 882
Issue: 2
First Page: 138
Abstract: We use the results from the ALMA large program ASPECS, the spectroscopic survey in the Hubble Ultra Deep Field (HUDF), to constrain CO luminosity functions of galaxies and the resulting redshift evolution of ρ(H<SUB>2</SUB>). The broad frequency range covered enables us to identify CO emission lines of different rotational transitions in the HUDF at z > 1. We find strong evidence that the CO luminosity function evolves with redshift, with the knee of the CO luminosity function decreasing in luminosity by an order of magnitude from ∼2 to the local universe. Based on Schechter fits, we estimate that our observations recover the majority (up to ∼90%, depending on the assumptions on the faint end) of the total cosmic CO luminosity at z = 1.0-3.1. After correcting for CO excitation, and adopting a Galactic CO-to-H<SUB>2</SUB> conversion factor, we constrain the evolution of the cosmic molecular gas density ρ(H<SUB>2</SUB>): this cosmic gas density peaks at z ∼ 1.5 and drops by a factor of {6.5}<SUB>-1.4</SUB><SUP>+1.8</SUP> to the value measured locally. The observed evolution in ρ(H<SUB>2</SUB>), therefore, closely matches the evolution of the cosmic star formation rate density ρ <SUB>SFR</SUB>. We verify the robustness of our result with respect to assumptions on source inclusion and/or CO excitation. As the cosmic star formation history can be expressed as the product of the star formation efficiency and the cosmic density of molecular gas, the similar evolution of ρ(H<SUB>2</SUB>) and ρ <SUB>SFR</SUB> leaves only little room for a significant evolution of the average star formation efficiency in galaxies since z ∼ 3 (85% of cosmic history).
URI: http://hdl.handle.net/20.500.12386/28649
URL: https://iopscience.iop.org/article/10.3847/1538-4357/ab30fe
ISSN: 0004-637X
DOI: 10.3847/1538-4357/ab30fe
Bibcode ADS: 2019ApJ...882..138D
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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