Deep CO(1–0) Observations of z = 1.62 Cluster Galaxies with Substantial Molecular Gas Reservoirs and Normal Star Formation Efficiencies
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Final Published Version
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Univ Arizona, Steward ObservIssue Date
2017-10-26Keywords
galaxies: clusters: generalgalaxies: evolution
galaxies: high-redshift
galaxies: ISM
galaxies: star formation
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IOP PUBLISHING LTDCitation
Deep CO(1–0) Observations of z = 1.62 Cluster Galaxies with Substantial Molecular Gas Reservoirs and Normal Star Formation Efficiencies 2017, 849 (1):27 The Astrophysical JournalJournal
The Astrophysical JournalRights
© 2017. The American Astronomical Society. All rights reserved.Collection Information
This 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 repository@u.library.arizona.edu.Abstract
We present an extremely deep CO(1-0) observation of a confirmed z = 1.62 galaxy cluster. We detect two spectroscopically confirmed cluster members in CO(1-0) with signal-to-noise ratio >5. Both galaxies have log (M-star/M-circle dot) > 11 and are gas rich, with M-mol/(M-star + M-mol) similar to 0.17-0.45. One of these galaxies lies on the star formation rate (SFR)-M-star sequence, while the other lies an order of magnitude below. We compare the cluster galaxies to other SFR-selected galaxies with CO measurements and find that they have CO luminosities consistent with expectations given their infrared luminosities. We also find that they have gas fractions and star formation efficiencies (SFE) comparable to what is expected from published field galaxy scaling relations. The galaxies are compact in their stellar light distribution, at the extreme end for all high-redshift star-forming galaxies. However, their SFE is consistent with other field galaxies at comparable compactness. This is similar to two other sources selected in a blind CO survey of the HDF-N. Despite living in a highly quenched protocluster core, the molecular gas properties of these two galaxies, one of which may be in the process of quenching, appear entirely consistent with field scaling relations between the molecular gas content, stellar mass, star formation rate, and redshift. We speculate that these cluster galaxies cannot have any further substantive gas accretion if they are to become members of the dominant passive population in z < 1 clusters.ISSN
1538-4357Version
Final published versionSponsors
HST program [HST-GO-12590.011-A, AR-14310.001]; NSF AST [1211358, 1517815]; Alexander von Humboldt foundation; VIDI research program [639.042.611]; Netherlands Organisation for Scientific Research (NWO); George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and AstronomyAdditional Links
http://stacks.iop.org/0004-637X/849/i=1/a=27?key=crossref.b888d0fdf03a5c9ac272fe5fe875e749Scopus Count
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