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dc.contributor.authorEstrada-Carpenter, Vicente
dc.contributor.authorPapovich, Casey
dc.contributor.authorMomcheva, Ivelina
dc.contributor.authorBrammer, Gabriel
dc.contributor.authorLong, James
dc.contributor.authorQuadri, Ryan F.
dc.contributor.authorBridge, Joanna
dc.contributor.authorDickinson, Mark
dc.contributor.authorFerguson, Henry
dc.contributor.authorFinkelstein, Steven
dc.contributor.authorGiavalisco, Mauro
dc.contributor.authorGosmeyer, Catherine M.
dc.contributor.authorLotz, Jennifer
dc.contributor.authorSalmon, Brett
dc.contributor.authorSkelton, Rosalind E.
dc.contributor.authorTrump, Jonathan R.
dc.contributor.authorWeiner, Benjamin
dc.date.accessioned2019-05-29T17:40:50Z
dc.date.available2019-05-29T17:40:50Z
dc.date.issued2019-01-10
dc.identifier.citationVicente Estrada-Carpenter et al 2019 ApJ 870 133en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aaf22e
dc.identifier.urihttp://hdl.handle.net/10150/632418
dc.description.abstractWe use deep Hubble Space Telescope spectroscopy to constrain the metallicities and (light-weighted) ages of massive (log M-*/M-circle dot greater than or similar to 10) galaxies selected to have quiescent stellar populations at 1.0 < z < 1.8. The data include twelve-orbit depth coverage with the WFC3/G102 grism covering similar to 8000 < lambda < 11,500 angstrom at a spectral resolution of R similar to 210 taken as part of the CANDELS Ly alpha Emission at Reionization (CLEAR) survey. At 1.0 < z < 1.8, the spectra cover important stellar population features in the rest-frame optical. We simulate a suite of stellar population models at the grism resolution, fit these to the data for each galaxy, and derive posterior likelihood distributions for metallicity and age. We stack the posteriors for subgroups of galaxies in different redshift ranges that include different combinations of stellar absorption features. Our results give light-weighted ages of t(z similar to 1.1) = 3.2 +/- 0.7 Gyr, t(z similar to 1.2) = 2.2 +/- 0.6 Gyr, t(z similar to 1.3) = 3.1 +/- 0.6 Gyr, and t(z similar to 1.6) = 2.0 +/- 0.6 Gyr for galaxies at z similar to 1.1, 1.2, 1.3, and 1.6, respectively. This implies that most of the massive quiescent galaxies at 1 < z < 1.8 had formed >68% of their stellar mass by z > 2. The posteriors give metallicities of Z(z similar to 1.1) = 1.16 +/- 0.29 Z(circle dot), Z(z similar to 1.2) = 1.05 +/- 0.34 Z(circle dot), Z(z similar to 1.3) = 1.00 +/- 0.31 Z(circle dot), and Z(z similar to 1.6) = 0.95 +/- 0.39 Z(circle dot). This is evidence that massive galaxies had enriched rapidly to approximately solar metallicities as early as z similar to 3.en_US
dc.description.sponsorshipHagler Institute for Advanced Study at Texas AM University; George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Hubble Space Telescope [GO 14227]; NASA through a grant from the Space Telescope Science Institute [GO 14227, NAS5-26555]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/870/i=2/a=133?key=crossref.8be9c0bfe71409d9c318b08490a1542fen_US
dc.rights© 2019. The American Astronomical Society. All rights reserved.en_US
dc.subjectgalaxies: evolutionen_US
dc.titleCLEAR. I. Ages and Metallicities of Quiescent Galaxies at 1.0 < z < 1.8 Derived from Deep Hubble Space Telescope Grism Dataen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, MMT Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis 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.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume870
dc.source.issue2
dc.source.beginpage133
refterms.dateFOA2019-05-29T17:40:51Z


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