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dc.contributor.authorPapadopoulos, Andreaspt_BR
dc.contributor.authorD'Andrea, Christopher B.pt_BR
dc.contributor.authorSullivan, Markpt_BR
dc.contributor.authorNichol, Robert C.pt_BR
dc.contributor.authorBarbary, Kylept_BR
dc.contributor.authorBiswas, Rahulpt_BR
dc.contributor.authorBrown, Peter J.pt_BR
dc.contributor.authorCovarrubias, Ricardo A.pt_BR
dc.contributor.authorFinley, David A.pt_BR
dc.contributor.authorFischer, John A.pt_BR
dc.contributor.authorFoley, Ryan Josephpt_BR
dc.contributor.authorGoldstein, Daniel Abrahampt_BR
dc.contributor.authorGupta, Ravi R.pt_BR
dc.contributor.authorKessler, Richard S.pt_BR
dc.contributor.authorKovacs, Eve Veronikapt_BR
dc.contributor.authorKuhlmann, Stephen Eugenept_BR
dc.contributor.authorLidman, Chrispt_BR
dc.contributor.authorMarch, Marisa Cristinapt_BR
dc.contributor.authorNugent, Peter Edwardpt_BR
dc.contributor.authorSako, Masaopt_BR
dc.contributor.authorSmith, Robert Christopherpt_BR
dc.contributor.authorSpinka, Harold M.pt_BR
dc.contributor.authorWester, William Carlpt_BR
dc.contributor.authorAbbott, Timothy M. C.pt_BR
dc.contributor.authorAbdalla, Filipe B.pt_BR
dc.contributor.authorAllam, Sahar S.pt_BR
dc.contributor.authorBanerji, M.pt_BR
dc.contributor.authorBernstein, Joseph P.pt_BR
dc.contributor.authorBernstein, Rebecca A.pt_BR
dc.contributor.authorCarnero Rosell, Aureliopt_BR
dc.contributor.authorCosta, Luiz N. dapt_BR
dc.contributor.authorDePoy, Darren L.pt_BR
dc.contributor.authorDesai, S.pt_BR
dc.contributor.authorDiehl, H. Thomaspt_BR
dc.contributor.authorEifler, Timpt_BR
dc.contributor.authorEvrard, August E.pt_BR
dc.contributor.authorFlaugher, Brennapt_BR
dc.contributor.authorFrieman, Joshua A.pt_BR
dc.contributor.authorGerdes, David W.pt_BR
dc.contributor.authorGruen, Danielpt_BR
dc.contributor.authorHonscheid, K.pt_BR
dc.contributor.authorJames, David J.pt_BR
dc.contributor.authorKuehn, Kylerpt_BR
dc.contributor.authorKuropatkin, Nikolay P.pt_BR
dc.contributor.authorLahav, Oferpt_BR
dc.contributor.authorMaia, Marcio Antonio Geimbapt_BR
dc.contributor.authorMakler, Martínpt_BR
dc.contributor.authorMarshall, Jennifer L.pt_BR
dc.contributor.authorMerritt, K. Wyattpt_BR
dc.contributor.authorMiller, Christopher J.pt_BR
dc.contributor.authorMiquel, Ramonpt_BR
dc.contributor.authorOgando, Ricardo L.C.pt_BR
dc.contributor.authorPlazas Malagón, Andrés Alejandropt_BR
dc.contributor.authorRoe, Natalie A.pt_BR
dc.contributor.authorRomer, Anita K.pt_BR
dc.contributor.authorRykoff, Elipt_BR
dc.contributor.authorSanchez-Alvaro, Eusebiopt_BR
dc.contributor.authorSantiago, Basilio Xavierpt_BR
dc.contributor.authorScarpine, Victor Emanuelpt_BR
dc.contributor.authorSchubnell, Michaelpt_BR
dc.contributor.authorSevilla Noarbe, Ignaciopt_BR
dc.contributor.authorSoares-Santos, Marcellept_BR
dc.contributor.authorSuchyta, Ericpt_BR
dc.contributor.authorSwanson, Molly E. C.pt_BR
dc.contributor.authorTarle, Gregorypt_BR
dc.contributor.authorThaler, Jon J.pt_BR
dc.contributor.authorTucker, Douglas L.pt_BR
dc.contributor.authorWechsler, Risa H.pt_BR
dc.contributor.authorZuntz, J.pt_BR
dc.date.accessioned2015-09-18T01:58:25Zpt_BR
dc.date.issued2015pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/126975pt_BR
dc.description.abstractWe present DES13S2cmm, the first spectroscopically-confirmed superluminous supernova (SLSN) from the Dark Energy Survey (DES).We briefly discuss the data and search algorithm used to find this event in the first year of DES operations, and outline the spectroscopic data obtained from the European Southern Observatory (ESO) Very Large Telescope to confirm its redshift (z = 0.663 ± 0.001 based on the host-galaxy emission lines) and likely spectral type (Type I). Using this redshift, we find M peak U = −21.05+0.10 −0.09 for the peak, rest-frame U-band absolute magnitude, and find DES13S2cmm to be located in a faint, low-metallicity (subsolar), low stellar-mass host galaxy (log (M/M ) = 9.3 ± 0.3), consistent with what is seen for other SLSNe-I. We compare the bolometric light curve of DES13S2cmm to 14 similarly well-observed SLSNe-I in the literature and find that it possesses one of the slowest declining tails (beyond +30 d rest-frame past peak), and is the faintest at peak. Moreover, we find the bolometric light curves of all SLSNe-I studied herein possess a dispersion of only 0.2–0.3 mag between +25 and +30 d after peak (rest frame) depending on redshift range studied; this could be important for ‘standardizing’ such supernovae, as is done with the more common Type Ia. We fit the bolometric light curve of DES13S2cmm with two competing models for SLSNe-I – the radioactive decay of 56Ni, and a magnetar – and find that while the magnetar is formally a better fit, neither model provides a compelling match to the data. Although we are unable to conclusively differentiate between these two physical models for this particular SLSN-I, further DES observations of more SLSNe-I should break this degeneracy, especially if the light curves of SLSNe-I can be observed beyond 100 d in the rest frame of the supernova.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the Royal Astronomical Society. Oxford. Vol. 449, no. 2 (May 2015), p. 1215-1227pt_BR
dc.rightsOpen Accessen
dc.subjectSurveysen
dc.subjectVia lácteapt_BR
dc.subjectSupernovae: generalen
dc.subjectSupernovae: individual: DES13S2cmmen
dc.titleDES13S2cmm : the first superluminous supernova from the Dark Energy Surveypt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000972678pt_BR
dc.type.originEstrangeiropt_BR


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