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dc.contributorVirginia Tech
dc.contributor.authorDowell, C. D.
dc.contributor.authorConley, A.
dc.contributor.authorGlenn, J.
dc.contributor.authorArumugam, V.
dc.contributor.authorAsboth, V.
dc.contributor.authorAussel, H.
dc.contributor.authorBertoldi, F.
dc.contributor.authorBethermin, M.
dc.contributor.authorBock, J.
dc.contributor.authorBoselli, A.
dc.contributor.authorBridge, C.
dc.contributor.authorBuat, V.
dc.contributor.authorBurgarella, D.
dc.contributor.authorCabrera-Lavers, A.
dc.contributor.authorCasey, C. M.
dc.contributor.authorChapman, S. C.
dc.contributor.authorClements, D. L.
dc.contributor.authorConversi, L.
dc.contributor.authorCooray, A.
dc.contributor.authorDannerbauer, H.
dc.contributor.authorDe Bernardis, F.
dc.contributor.authorEllsworth-Bowers, T. P.
dc.contributor.authorFarrah, D.
dc.contributor.authorFranceschini, A.
dc.contributor.authorGriffin, M.
dc.contributor.authorGurwell, M. A.
dc.contributor.authorHalpern, M.
dc.contributor.authorHatziminaoglou, E.
dc.contributor.authorHeinis, S.
dc.contributor.authorIbar, E.
dc.contributor.authorIvison, R. J.
dc.contributor.authorLaporte, N.
dc.contributor.authorMarchetti, L.
dc.contributor.authorMartinez-Navajas, P.
dc.contributor.authorMarsden, G.
dc.contributor.authorMorrison, G. E.
dc.contributor.authorNguyen, H. T.
dc.contributor.authorO'Halloran, B.
dc.contributor.authorOliver, S. J.
dc.contributor.authorOmont, A.
dc.contributor.authorPage, M. J.
dc.contributor.authorPapageorgiou, A.
dc.contributor.authorPearson, C. P.
dc.contributor.authorPetitpas, G.
dc.contributor.authorPerez-Fournon, I.
dc.contributor.authorPohlen, M.
dc.contributor.authorRiechers, D.
dc.contributor.authorRigopoulou, D.
dc.contributor.authorRoseboom, I. G.
dc.contributor.authorRowan-Robinson, M.
dc.contributor.authorSayers, J.
dc.contributor.authorSchulz, B.
dc.contributor.authorScott, D.
dc.contributor.authorSeymour, N.
dc.contributor.authorShupe, D. L.
dc.contributor.authorSmith, A. J.
dc.contributor.authorStreblyanska, A.
dc.contributor.authorSymeonidis, M.
dc.contributor.authorVaccari, M.
dc.contributor.authorValtchanov, I.
dc.contributor.authorVieira, J. D.
dc.contributor.authorViero, M.
dc.contributor.authorWang, L.
dc.contributor.authorWardlow, J.
dc.contributor.authorXu, C. K.
dc.contributor.authorZemcov, M.
dc.date.accessioned2014-02-25T13:57:03Z
dc.date.available2014-02-25T13:57:03Z
dc.date.issued2014-01
dc.identifier.citationC. Darren Dowell et al. 2014. "herMES: candidate high-redshift galaxies discovered with herschel/spire," ApJ 780 75 doi:10.1088/0004-637X/780/1/75
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/10919/25541
dc.description.abstractWe present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 mu m flux densities to search for red sources. We apply this method to 21 deg(2) of data from the HerMES survey to produce a catalog of 38 high-z candidates. Follow-up of the first five of these sources confirms that this method is efficient at selecting high-z DSFGs, with 4/5 at z = 4.3-6.3 (and the remaining source at z = 3.4), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e. g., 850 mu m) and in single-band surveys, shows that our method is much more efficient at selecting high-z DSFGs, in the sense that a much larger fraction are at z > 3. Correcting for the selection completeness and purity, we find that the number of bright (S-500 (mu m) >= 30 mJy), red Herschel sources is 3.3 +/- 0.8 deg(-2). This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-z DSFGs is similar to that at z similar to 2, rest-frame UV based studies may be missing a significant component of the star formation density at z = 4-6, even after correction for extinction.
dc.description.sponsorshipNational Aeronautics and Space Administration 12-ADAP12-0139
dc.description.sponsorshipNASA
dc.description.sponsorshipCSA (Canada)
dc.description.sponsorshipNAOC (China)
dc.description.sponsorshipCEA (France)
dc.description.sponsorshipCNES (France)
dc.description.sponsorshipCNRS (France)
dc.description.sponsorshipASI (Italy)
dc.description.sponsorshipMCINN (Spain)
dc.description.sponsorshipSNSB (Sweden)
dc.description.sponsorshipSTFC (UK)
dc.description.sponsorshipNASA (USA)
dc.description.sponsorshipNational Science Foundation AST-0838261
dc.description.sponsorshipSmithsonian Institution
dc.description.sponsorshipAcademia Sinica
dc.description.sponsorshipINSU/CNRS (France)
dc.description.sponsorshipMPG (Germany)
dc.description.sponsorshipIGN (Spain)
dc.description.sponsorshipW. M. Keck Foundation
dc.language.isoen_US
dc.publisherIOP Publishing Ltd.
dc.subjectgalaxies: high-redshift
dc.subjectgalaxies: starburst
dc.subjectinfrared: galaxies
dc.subjectsubmillimeter: galaxies
dc.subjectdeep-field-south
dc.subjectstar-forming galaxies
dc.subjectdegree extragalactic survey
dc.subjectaztec millimeter survey
dc.subjectlarge-scale structure
dc.subjectsquare degree survey
dc.subjectmu-m observations
dc.subjectscuba super-map
dc.subjectsubmillimeter galaxies
dc.subjectnumber
dc.subjectcounts
dc.titleherMES: candidate high-redshift galaxies discovered with herschel/spire
dc.typeArticle
dc.identifier.urlhttp://m.iopscience.iop.org/0004-637X/780/1/75/pdf/0004-637X_780_1_75.pdf
dc.date.accessed2014-02-05
dc.title.serialAstrophysical Journal
dc.identifier.doihttps://doi.org/10.1088/0004-637x/780/1/75


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