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dc.contributor.authorConley, A.
dc.contributor.authorCooray, A.
dc.contributor.authorVieira, J.
dc.contributor.authorSolares, E.A.G.
dc.contributor.authorKim, S.
dc.contributor.authorAguirre, J.E.
dc.contributor.authorAmblard, A.
dc.contributor.authorAuld, R.
dc.contributor.authorBaker, A.J.
dc.contributor.authorBeelen, A.
dc.contributor.authorBlain, A.W.
dc.contributor.authorBlundell, R.
dc.contributor.authorBock, J.
dc.contributor.authorBradford, C.M.
dc.contributor.authorBridge, C.
dc.contributor.authorBrisbin, D.
dc.contributor.authorBurgarella, D.
dc.contributor.authorCarpenter, J.M.
dc.contributor.authorChanial, P.
dc.contributor.authorChapin, E.
dc.contributor.authorChristopher, N.
dc.contributor.authorClements, D.
dc.contributor.authorCox, P.
dc.contributor.authorDjorgovski, S.G.
dc.contributor.authorDowell, C.D.
dc.contributor.authorEales, S.
dc.contributor.authorEarle, L.
dc.contributor.authorEllsworth-Bowers, T.P.
dc.contributor.authorFarrah, D.
dc.contributor.authorFranceschini, A.
dc.contributor.authorFrayer, D.
dc.contributor.authorFu, H.
dc.contributor.authorGavazzi, R.
dc.contributor.authorGlenn, J.
dc.contributor.authorGriffin, M.
dc.contributor.authorGurwell, M.A.
dc.contributor.authorHalpern, M.
dc.contributor.authorIbar, E.
dc.contributor.authorIvison, R.J.
dc.contributor.authorJarvis, M.J.
dc.contributor.authorKamenetzky, J.
dc.contributor.authorKrips, M.
dc.contributor.authorLevenson, L.
dc.contributor.authorLupu, R.
dc.contributor.authorMahabal, A.
dc.contributor.authorMaloney, P.D.
dc.contributor.authorMaraston, C.
dc.contributor.authorMarchetti, L.
dc.contributor.authorMarsden, G.
dc.contributor.authorMatsuhara, H.
dc.contributor.authorMortier, A.M.J.
dc.contributor.authorMurphy, E.
dc.contributor.authorNaylor, B.J.
dc.contributor.authorNeri, R.
dc.contributor.authorNguyen, H.T.
dc.contributor.authorOliver, S.
dc.contributor.authorOmont, A.
dc.contributor.authorPage, M.J.
dc.contributor.authorPapageorgiou, A.
dc.contributor.authorPearson, C.
dc.contributor.authorPerez-Fournon, I.
dc.contributor.authorPohlen, M.
dc.contributor.authorRangwala, N.
dc.contributor.authorRawlings, J.I.
dc.contributor.authorRaymond, G.
dc.contributor.authorRiechers, D.
dc.contributor.authorRodighiero, G.
dc.contributor.authorRoseboom, I.G.
dc.contributor.authorRowan-Robinson, M.
dc.contributor.authorSchulz, B.
dc.contributor.authorScott, D.
dc.contributor.authorScott, K.
dc.contributor.authorSerra, P.
dc.contributor.authorSeymour, N.
dc.contributor.authorShupe, D.
dc.contributor.authorSmith, A.J.
dc.contributor.authorSymeonidis, M.
dc.contributor.authorTugwell, K.E.
dc.contributor.authorVaccari, M.
dc.contributor.authorValiante, E.
dc.contributor.authorValtchanov, I.
dc.contributor.authorVerma, A.
dc.contributor.authorViero, M.P.
dc.contributor.authorVigroux, L.
dc.contributor.authorWang, L.
dc.contributor.authorWiebe, D.
dc.contributor.authorWright, G.
dc.contributor.authorXu, C.K.
dc.contributor.authorZeimann, G.
dc.contributor.authorZemcov, M.
dc.contributor.authorZmuidzinas, J.
dc.date.accessioned2011-05-25T14:22:30Z
dc.date.available2011-05-25T14:22:30Z
dc.date.issued2011
dc.identifier.citationConley , A , Cooray , A , Vieira , J , Solares , E A G , Kim , S , Aguirre , J E , Amblard , A , Auld , R , Baker , A J , Beelen , A , Blain , A W , Blundell , R , Bock , J , Bradford , C M , Bridge , C , Brisbin , D , Burgarella , D , Carpenter , J M , Chanial , P , Chapin , E , Christopher , N , Clements , D , Cox , P , Djorgovski , S G , Dowell , C D , Eales , S , Earle , L , Ellsworth-Bowers , T P , Farrah , D , Franceschini , A , Frayer , D , Fu , H , Gavazzi , R , Glenn , J , Griffin , M , Gurwell , M A , Halpern , M , Ibar , E , Ivison , R J , Jarvis , M J , Kamenetzky , J , Krips , M , Levenson , L , Lupu , R , Mahabal , A , Maloney , P D , Maraston , C , Marchetti , L , Marsden , G , Matsuhara , H , Mortier , A M J , Murphy , E , Naylor , B J , Neri , R , Nguyen , H T , Oliver , S , Omont , A , Page , M J , Papageorgiou , A , Pearson , C , Perez-Fournon , I , Pohlen , M , Rangwala , N , Rawlings , J I , Raymond , G , Riechers , D , Rodighiero , G , Roseboom , I G , Rowan-Robinson , M , Schulz , B , Scott , D , Scott , K , Serra , P , Seymour , N , Shupe , D , Smith , A J , Symeonidis , M , Tugwell , K E , Vaccari , M , Valiante , E , Valtchanov , I , Verma , A , Viero , M P , Vigroux , L , Wang , L , Wiebe , D , Wright , G , Xu , C K , Zeimann , G , Zemcov , M & Zmuidzinas , J 2011 , ' Discovery of a multiply lensed submillimeter galaxy in early HerMES Herschel/SPIRE data ' , The Astrophysical Journal , vol. 732 , no. 2 Part II . https://doi.org/10.1088/2041-8205/732/2/L35
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 174058
dc.identifier.otherPURE UUID: 27cdbda1-76c0-46c2-acee-33f3707f91b4
dc.identifier.otherdspace: 2299/5826
dc.identifier.otherScopus: 79955575775
dc.identifier.urihttp://hdl.handle.net/2299/5826
dc.description‘In these times, during the rise in the popularity of institutional repositories, the Society does not forbid authors from depositing their work in such repositories. However, the AAS regards the deposit of scholarly work in such repositories to be a decision of the individual scholar, as long as the individual's actions respect the diligence of the journals and their reviewers.’ Original article can be found at: http://iopscience.iop.org/ Copyright American Astronomical Society
dc.description.abstractWe report the discovery of a bright (f (250 μm)>400 mJy), multiply lensed submillimeter galaxy HERMES J105751.1+573027 in Herschel/SPIRE Science Demonstration Phase data from the HerMES project. Interferometric 880 μm Submillimeter Array observations resolve at least four images with a large separation of ∼9″. A high-resolution adaptive optics Kp image with Keck/NIRC2 clearly shows strong lensing arcs. Follow-up spectroscopy gives a redshift of z = 2.9575, and the lensing model gives a total magnification of μ ∼ 11 ± 1. The large image separation allows us to study the multi-wavelength spectral energy distribution (SED) of the lensed source unobscured by the central lensing mass. The far-IR/millimeter-wave SED is well described by a modified blackbody fit with an unusually warm dust temperature, 88 ± 3 K. We derive a lensing-corrected total IR luminosity of (1.43 ± 0.09) × 1013 L⊙, implying a star formation rate of ∼2500 M⊙ yr-1. However, models primarily developed from brighter galaxies selected at longer wavelengths are a poor fit to the full optical-to-millimeter SED. A number of other strongly lensed systems have already been discovered in early Herschel data, and many more are expected as additional data are collected.en
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectgalaxies : high-redshift
dc.subjectgalaxies : starburst
dc.subjectgravitational lensing : strong
dc.subjectsubmillimeter : galaxies
dc.titleDiscovery of a multiply lensed submillimeter galaxy in early HerMES Herschel/SPIRE dataen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionDepartment of Allied Health Professions and Midwifery
dc.contributor.institutionHealth & Human Sciences Research Institute
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1088/2041-8205/732/2/L35
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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