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dc.contributorVirginia Techen
dc.contributor.authorDowell, C. D.en
dc.contributor.authorConley, A.en
dc.contributor.authorGlenn, J.en
dc.contributor.authorArumugam, V.en
dc.contributor.authorAsboth, V.en
dc.contributor.authorAussel, H.en
dc.contributor.authorBertoldi, F.en
dc.contributor.authorBethermin, M.en
dc.contributor.authorBock, J.en
dc.contributor.authorBoselli, A.en
dc.contributor.authorBridge, C. R.en
dc.contributor.authorBuat, V.en
dc.contributor.authorBurgarella, D.en
dc.contributor.authorCabrera-Lavers, A.en
dc.contributor.authorCasey, C. M.en
dc.contributor.authorChapman, S. C.en
dc.contributor.authorClements, D. L.en
dc.contributor.authorConversi, L.en
dc.contributor.authorCooray, A.en
dc.contributor.authorDannerbauer, H.en
dc.contributor.authorDe Bernardis, F.en
dc.contributor.authorEllsworth-Bowers, T. P.en
dc.contributor.authorFarrah, D.en
dc.contributor.authorFranceschini, A.en
dc.contributor.authorGriffin, M.en
dc.contributor.authorGurwell, M. A.en
dc.contributor.authorHalpern, M.en
dc.contributor.authorHatziminaoglou, E.en
dc.contributor.authorHeinis, S.en
dc.contributor.authorIbar, E.en
dc.contributor.authorIvison, R. J.en
dc.contributor.authorLaporte, N.en
dc.contributor.authorMarchetti, L.en
dc.contributor.authorMartinez-Navajas, P.en
dc.contributor.authorMarsden, G.en
dc.contributor.authorMorrison, G. E.en
dc.contributor.authorNguyen, H. T.en
dc.contributor.authorO'Halloran, B.en
dc.contributor.authorOliver, S. J.en
dc.contributor.authorOmont, A.en
dc.contributor.authorPage, M. J.en
dc.contributor.authorPapageorgiou, A.en
dc.contributor.authorPearson, C. P.en
dc.contributor.authorPetitpas, G.en
dc.contributor.authorPerez-Fournon, I.en
dc.contributor.authorPohlen, M.en
dc.contributor.authorRiechers, D. A.en
dc.contributor.authorRigopoulou, D.en
dc.contributor.authorRoseboom, I. G.en
dc.contributor.authorRowan-Robinson, M.en
dc.contributor.authorSayers, J.en
dc.contributor.authorSchulz, B.en
dc.contributor.authorScott, D.en
dc.contributor.authorSeymour, N.en
dc.contributor.authorShupe, D. L.en
dc.contributor.authorSmith, A. J.en
dc.contributor.authorStreblyanska, A.en
dc.contributor.authorSymeonidis, M.en
dc.contributor.authorVaccari, M.en
dc.contributor.authorValtchanov, I.en
dc.contributor.authorVieira, J. D.en
dc.contributor.authorViero, M.en
dc.contributor.authorWang, L.en
dc.contributor.authorWardlow, J.en
dc.contributor.authorXu, C. K.en
dc.contributor.authorZemcov, M.en
dc.date.accessioned2014-02-25T13:57:03Zen
dc.date.available2014-02-25T13:57:03Zen
dc.date.issued2014-01en
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/780/1/75en
dc.identifier.issn0004-637Xen
dc.identifier.urihttp://hdl.handle.net/10919/25541en
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.en
dc.description.sponsorshipNational Aeronautics and Space Administration 12-ADAP12-0139en
dc.description.sponsorshipNASAen
dc.description.sponsorshipCSA (Canada)en
dc.description.sponsorshipNAOC (China)en
dc.description.sponsorshipCEA (France)en
dc.description.sponsorshipCNES (France)en
dc.description.sponsorshipCNRS (France)en
dc.description.sponsorshipASI (Italy)en
dc.description.sponsorshipMCINN (Spain)en
dc.description.sponsorshipSNSB (Sweden)en
dc.description.sponsorshipSTFC (UK)en
dc.description.sponsorshipNASA (USA)en
dc.description.sponsorshipNational Science Foundation AST-0838261en
dc.description.sponsorshipSmithsonian Institutionen
dc.description.sponsorshipAcademia Sinicaen
dc.description.sponsorshipINSU/CNRS (France)en
dc.description.sponsorshipMPG (Germany)en
dc.description.sponsorshipIGN (Spain)en
dc.description.sponsorshipW. M. Keck Foundationen
dc.language.isoen_USen
dc.publisherIOP Publishing Ltd.en
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectgalaxies: high-redshiften
dc.subjectgalaxies: starbursten
dc.subjectinfrared: galaxiesen
dc.subjectsubmillimeter: galaxiesen
dc.subjectdeep-field-southen
dc.subjectstar-forming galaxiesen
dc.subjectdegree extragalactic surveyen
dc.subjectaztec millimeter surveyen
dc.subjectlarge-scale structureen
dc.subjectsquare degree surveyen
dc.subjectmu-m observationsen
dc.subjectscuba super-mapen
dc.subjectsubmillimeter galaxiesen
dc.subjectnumberen
dc.subjectcountsen
dc.titleHerMES: candidate high-redshift galaxies discovered with Herschel/SPIREen
dc.typeArticle - Refereeden
dc.contributor.departmentPhysicsen
dc.identifier.urlhttp://m.iopscience.iop.org/0004-637X/780/1/75/pdf/0004-637X_780_1_75.pdfen
dc.date.accessed2014-02-05en
dc.title.serialAstrophysical Journalen
dc.identifier.doihttps://doi.org/10.1088/0004-637x/780/1/75en


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