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Authordc.contributor.authorGonzález Gaitán, Santiago 
Authordc.contributor.authorTominaga, N. 
Authordc.contributor.authorMolina, J. 
Authordc.contributor.authorGalbany, Lluis 
Authordc.contributor.authorBufano, Filomena 
Authordc.contributor.authorAnderson, J. 
Authordc.contributor.authorGutiérrez, C. 
Authordc.contributor.authorFörster, Francisco 
Authordc.contributor.authorPignata Libralato, Giuliano 
Authordc.contributor.authorBersten, M. 
Authordc.contributor.authorHowell, D. A. 
Authordc.contributor.authorSullivan, M. 
Authordc.contributor.authorCarlberg, R. 
Authordc.contributor.authorDe Jaeger, Thomas 
Authordc.contributor.authorHamuy Wackenhut, Mario 
Authordc.contributor.authorBaklanov, P. 
Authordc.contributor.authorBlinnikov, S. 
Admission datedc.date.accessioned2015-08-17T20:02:05Z
Available datedc.date.available2015-08-17T20:02:05Z
Publication datedc.date.issued2015
Cita de ítemdc.identifier.citationMNRAS 451, 2212–2229 (2015)en_US
Identifierdc.identifier.otherdoi:10.1093/mnras/stv1097
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/132787
General notedc.descriptionArtículo de publicación ISIen_US
Abstractdc.description.abstractWe investigate the early-time light curves of a large sample of 223 Type II supernovae (SNe II) from the Sloan Digital Sky Survey and the Supernova Legacy Survey. Having a cadence of a few days and sufficient non-detections prior to explosion, we constrain risetimes, i.e. the durations from estimated first to maximum light, as a function of effective wavelength. At rest-frame g band (λeff = 4722 Å), we find a distribution of fast rise-times with median of (7.5 ± 0.3) d. Comparing these durations with analytical shock models of Rabinak & Waxman and Nakar & Sari, and hydrodynamical models of Tominaga et al., which are mostly sensitive to progenitor radius at these epochs, we find a median characteristic radius of less than 400 solar radii. The inferred radii are on average much smaller than the radii obtained for observed red supergiants (RSG). Investigating the post-maximum slopes as a function of effective wavelength in the light of theoretical models, we find that massive hydrogen envelopes are still needed to explain the plateaus of SNe II. We therefore argue that the SN II rise-times we observe are either (a) the shock cooling resulting from the core collapse of RSG with small and dense envelopes, or (b) the delayed and prolonged shock breakout of the collapse of an RSG with an extended atmosphere or embedded within pre-SN circumstellar material.en_US
Lenguagedc.language.isoenen_US
Publisherdc.publisherRoyal Astronomical Societyen_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.subjectsupergiantsen_US
Keywordsdc.subjectsupernoave: general.en_US
Títulodc.titleThe rise-time of Type II supernovaeen_US
Document typedc.typeArtículo de revista


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