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dc.contributor.authorCanameras, R.
dc.contributor.authorNesvadba, N. P. H.
dc.contributor.authorKneissl, R.
dc.contributor.authorLimousin, M.
dc.contributor.authorGavazzi, R.
dc.contributor.authorScott, D.
dc.contributor.authorDole, H.
dc.contributor.authorFrye, B.
dc.contributor.authorKoenig, S.
dc.contributor.authorLe Floc'h, E.
dc.contributor.authorOteo, I.
dc.date.accessioned2017-06-23T22:39:03Z
dc.date.available2017-06-23T22:39:03Z
dc.date.issued2017-03-24
dc.identifier.citationPlanck's dusty GEMS III. A massive lensing galaxy with a bottom-heavy stellar initial mass function at z=1.5 2017, 600:L3 Astronomy & Astrophysicsen
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.doi10.1051/0004-6361/201630359
dc.identifier.urihttp://hdl.handle.net/10150/624365
dc.description.abstractWe study the properties of the foreground galaxy of the Ruby, the brightest gravitationally lensed high-redshift galaxy on the sub-millimeter sky as probed by the Planck satellite, and part of our sample of Planck's dusty GEMS. The Ruby consists of an Einstein ring of 1.4" diameter at z = 3.005 observed with ALMA at 0.1" resolution, centered on a faint, red, massive lensing galaxy seen with HST/WFC3, which itself has an exceptionally high redshift, z = 1.525 +/- 0.001, as confirmed with VLT/X-shooter spectroscopy. Here we focus on the properties of the lens and the lensing model obtained with LENSTOOL. The rest-frame optical morphology of this system is strongly dominated by the lens, while the Ruby itself is highly obscured, and contributes less than 10% to the photometry out to the K band. The foreground galaxy has a lensing mass of (3.70 +/- 0.35) x 10(11) M-Theta Magnification factors are between 7 and 38 for individual clumps forming two image families along the Einstein ring. We present a decomposition of the foreground and background sources in the WFC3 images, and stellar population synthesis modeling with a range of star-formation histories for Chabrier and Salpeter initial mass functions (IMFs). Only the stellar mass range obtained with the latter agrees well with the lensing mass. This is consistent with the bottom-heavy IMFs of massive high-redshift galaxies expected from detailed studies of the stellar masses and mass profiles of their low-redshift descendants, and from models of turbulent gas fragmentation. This may be the first direct constraint on the IMF in a lens at z = 1.5, which is not a cluster central galaxy.
dc.description.sponsorshipCNRS; CNES; ERC program [321302]; COSMICISMen
dc.language.isoenen
dc.publisherEDP SCIENCES S Aen
dc.relation.urlhttp://www.aanda.org/10.1051/0004-6361/201630359en
dc.rights© ESO, 2017en
dc.subjectgalaxies: high-redshiften
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: star formationen
dc.subjectgalaxies: stellar contenten
dc.subjectinfrared: galaxiesen
dc.subjectsubmillimeter: galaxiesen
dc.titlePlanck's dusty GEMS III. A massive lensing galaxy with a bottom-heavy stellar initial mass function at z=1.5en
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalAstronomy & Astrophysicsen
dc.description.noteOpen access journal.en
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
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-11T20:24:59Z
html.description.abstractWe study the properties of the foreground galaxy of the Ruby, the brightest gravitationally lensed high-redshift galaxy on the sub-millimeter sky as probed by the Planck satellite, and part of our sample of Planck's dusty GEMS. The Ruby consists of an Einstein ring of 1.4" diameter at z = 3.005 observed with ALMA at 0.1" resolution, centered on a faint, red, massive lensing galaxy seen with HST/WFC3, which itself has an exceptionally high redshift, z = 1.525 +/- 0.001, as confirmed with VLT/X-shooter spectroscopy. Here we focus on the properties of the lens and the lensing model obtained with LENSTOOL. The rest-frame optical morphology of this system is strongly dominated by the lens, while the Ruby itself is highly obscured, and contributes less than 10% to the photometry out to the K band. The foreground galaxy has a lensing mass of (3.70 +/- 0.35) x 10(11) M-Theta Magnification factors are between 7 and 38 for individual clumps forming two image families along the Einstein ring. We present a decomposition of the foreground and background sources in the WFC3 images, and stellar population synthesis modeling with a range of star-formation histories for Chabrier and Salpeter initial mass functions (IMFs). Only the stellar mass range obtained with the latter agrees well with the lensing mass. This is consistent with the bottom-heavy IMFs of massive high-redshift galaxies expected from detailed studies of the stellar masses and mass profiles of their low-redshift descendants, and from models of turbulent gas fragmentation. This may be the first direct constraint on the IMF in a lens at z = 1.5, which is not a cluster central galaxy.


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