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Strong near-infrared carbon in the Type Ia supernova iPTF13ebh

Authordc.contributor.authorHsiao, Eric 
Authordc.contributor.authorBurns, C.R. 
Authordc.contributor.authorContreras, C. 
Authordc.contributor.authorHöflich, P. 
Authordc.contributor.authorSand, D. 
Authordc.contributor.authorMarion, G.H. 
Authordc.contributor.authorPhillips, M. M. 
Authordc.contributor.authorStritzinger, M. 
Authordc.contributor.authorGonzález Gaitán, Santiago 
Authordc.contributor.authorMason, R. E. 
Authordc.contributor.authorFolatelli, Gastón 
Authordc.contributor.authorParent, E. 
Authordc.contributor.authorGall, C. 
Authordc.contributor.authorAmanullah, R. 
Authordc.contributor.authorAnupama, G. C. 
Authordc.contributor.authorArcavi, I. 
Authordc.contributor.authorBanerjee, D. P. K. 
Authordc.contributor.authorBeletsky, Y. 
Authordc.contributor.authorBlanc Mendiberri, Guillermo 
Authordc.contributor.authorBloom, J. S. 
Authordc.contributor.authorBrown, P. J. 
Authordc.contributor.authorCampillay, A. 
Authordc.contributor.authorCao, Y. 
Authordc.contributor.authorCia, A. de 
Authordc.contributor.authorDiamond, T. 
Authordc.contributor.authorFreedman, W. L. 
Authordc.contributor.authorGonzález, C. 
Authordc.contributor.authorGoobar, A. 
Authordc.contributor.authorHolmbo, S. 
Authordc.contributor.authorHowell, D. A. 
Authordc.contributor.authorJohansson, J. 
Authordc.contributor.authorKasliwal, M. M. 
Authordc.contributor.authorKirshner, R. P. 
Authordc.contributor.authorKrisciunas, K. 
Authordc.contributor.authorKulkarni, S. R. 
Authordc.contributor.authorMaguire, K. 
Authordc.contributor.authorMilne, P. A. 
Authordc.contributor.authorMorrell, N. 
Authordc.contributor.authorNugent, P. E. 
Authordc.contributor.authorOfek, E. O. 
Authordc.contributor.authorOsip, D. 
Authordc.contributor.authorPalunas, P. 
Authordc.contributor.authorPerley, D. A. 
Authordc.contributor.authorPersson, S. E. 
Authordc.contributor.authorPiro, A. L. 
Authordc.contributor.authorRabus, M. 
Authordc.contributor.authorRoth, M. 
Authordc.contributor.authorSchiefelbein, J. M. 
Authordc.contributor.authorSrivastav, S. 
Authordc.contributor.authorSullivan, M. 
Authordc.contributor.authorSuntzeff, Nicholas B. 
Authordc.contributor.authorSurace, J. 
Authordc.contributor.authorWózniak, P. R. 
Authordc.contributor.authorYaron, O. 
Admission datedc.date.accessioned2015-10-07T14:57:22Z
Available datedc.date.available2015-10-07T14:57:22Z
Publication datedc.date.issued2015
Cita de ítemdc.identifier.citationAstronomy & Astrophysics Volumen: 578 Número de artículo: A9en_US
Identifierdc.identifier.other10.1051/0004-6361/201425297
Identifierdc.identifier.urihttp://repositorio.uchile.cl/handle/2250/134204
General notedc.descriptionArtículo de publicación ISIen_US
Abstractdc.description.abstractWe present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2 : 3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C I lines, and the C I lambda 1.0693 mu m line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C II counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C I compared to the weaker optical C II appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Delta m(15)(B) = 1.79 +/- 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si II lambda 0.6355 mu m line, implying a long dark phase of similar to 4 days.en_US
Patrocinadordc.description.sponsorshipCONICYT through FONDECYT 3130680en_US
Lenguagedc.language.isoenen_US
Publisherdc.publisherESOen_US
Type of licensedc.rightsAtribución-NoComercial-SinDerivadas 3.0 Chile*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/*
Keywordsdc.subjectinfrared: generalen_US
Keywordsdc.subjectsupernovae: generalen_US
Keywordsdc.subjectsupernovae: individual: iPTF13ebhen_US
Títulodc.titleStrong near-infrared carbon in the Type Ia supernova iPTF13ebhen_US
Document typedc.typeArtículo de revistaen_US


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Except where otherwise noted, this item's license is described as Atribución-NoComercial-SinDerivadas 3.0 Chile