450 d of Type II SN 2013ej in optical and near-infrared

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dc.contributor.authorYuan, Fang
dc.contributor.authorJerkstrand, A.
dc.contributor.authorValenti, S.
dc.contributor.authorSollerman, J.
dc.contributor.authorSeitenzahl, I. R.
dc.contributor.authorPastorello, A.
dc.contributor.authorSchulze, S.
dc.contributor.authorChen, T. W.
dc.contributor.authorChildress, M. J.
dc.contributor.authorFraser, M.
dc.contributor.authorFremling, C.
dc.contributor.authorKotak, R.
dc.contributor.authorRuiter, A. J.
dc.contributor.authorSchmidt, B. P.
dc.contributor.authorSmartt, S. J.
dc.contributor.authorTaddia, F.
dc.contributor.authorTerreran, G.
dc.contributor.authorTucker, B. E.
dc.contributor.authorBarbarino, C.
dc.contributor.authorBenetti, S.
dc.contributor.authorElias Rosa, N.
dc.contributor.authorGal Yam, A.
dc.contributor.authorHowell, D. A.
dc.contributor.authorInserra, C.
dc.contributor.authorKankare, E.
dc.contributor.authorLee, M. Y.
dc.contributor.authorLi, K. L.
dc.contributor.authorMaguire, K.
dc.contributor.authorMargheim, S.
dc.contributor.authorMehner, A.
dc.contributor.authorOchner, P.
dc.contributor.authorSullivan, M.
dc.contributor.authorTomasella, L.
dc.contributor.authorYoung, D. R.
dc.date.accessioned2024-01-10T13:10:47Z
dc.date.available2024-01-10T13:10:47Z
dc.date.issued2016
dc.description.abstractWe present optical and near-infrared photometric and spectroscopic observations of SN 2013ej, in galaxy M74, from 1 to 450 d after the explosion. SN 2013ej is a hydrogen-rich supernova, classified as a Type IIL due to its relatively fast decline following the initial peak. It has a relatively high peak luminosity (absolute magnitude M-V =-17.6) but a small 56Ni production of similar to 0.023 M-circle dot. Its photospheric evolution is similar to other Type II SNe, with shallow absorption in the H a profile typical for a Type IIL. During transition to the radioactive decay tail at similar to 100 d, we find the SN to grow bluer in B - V colour, in contrast to some other Type II supernovae. At late times, the bolometric light curve declined faster than expected from Co-56 decay and we observed unusually broad and asymmetric nebular emission lines. Based on comparison of nebular emission lines most sensitive to the progenitor core mass, we find our observations are best matched to synthesized spectral models with a M-ZAMS = 12-15 M-circle dot progenitor. The derived mass range is similar to but not higher than the mass estimated for Type IIP progenitors. This is against the idea that Type IIL are from more massive stars. Observations are consistent with the SN having a progenitor with a relatively low-mass envelope.
dc.description.funderESO
dc.description.funderRobert Martin Ayers Sciences Fund
dc.description.funderNational Aeronautics and Space Administration
dc.description.funderAustralian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO)
dc.description.funderARC
dc.description.funderPRIN-INAF
dc.description.funderCONICYT-Chile FONDECYT
dc.description.funderBasal-CATA
dc.description.funder'Millennium Institute of Astrophysics (MAS)' of Initiative Cientifica Milenio del Ministerio de Economia, Fomento y Turismo
dc.description.funderEuropean Union FP7 programme through ERC
dc.description.funderSTFC through an Ernest Rutherford Fellowship
dc.description.funderSTFC
dc.description.funderEU/FP7ERC grant
dc.description.funderEU/FP7 via ERC
dc.description.funderQuantum Universe I-CORE Program by Israeli Committee for Planning and Budgeting
dc.description.funderIsrael Science Foundation (ISF)
dc.description.funderMinerva grant
dc.description.funderISF grant
dc.description.funderWeizmann-UK making connections programme
dc.description.funderKimmel award
dc.description.funderARCHES award
dc.description.funderScience and Technology Facilities Council
dc.fechaingreso.objetodigital2024-04-29
dc.format.extent16 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stw1419
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stw1419
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77933
dc.identifier.wosidWOS:000383273600064
dc.information.autorucFísica;Schulze S ;S/I;237742
dc.issue.numero2
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final2018
dc.pagina.inicio2003
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsacceso restringido
dc.subjectsupernovae: general
dc.subjectsupernovae: individual: SN 2013ej
dc.subjectFIELD SPECTROGRAPH WIFES
dc.subjectCORE-COLLAPSE SUPERNOVAE
dc.subjectLIGHT-CURVES
dc.subjectCARBON-MONOXIDE
dc.subjectSHOCK BREAKOUT
dc.subjectMASSIVE STARS
dc.subjectP SUPERNOVA
dc.subjectPLATEAU SUPERNOVAE
dc.subjectPROGENITOR STARS
dc.subjectEMISSION-LINES
dc.subject.ods07 Affordable and Clean Energy
dc.subject.odspa07 Energía asequible y no contaminante
dc.title450 d of Type II SN 2013ej in optical and near-infrared
dc.typeartículo
dc.volumen461
sipa.codpersvinculados237742
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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