SNhunt151: An explosive event inside a dense cocoon

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dc.contributor.authorElias-Rosa N.
dc.contributor.authorBenetti S.
dc.contributor.authorCappellaro E.
dc.contributor.authorPastorello A.
dc.contributor.authorTerreran G.
dc.contributor.authorMorales-Garoffolo A.
dc.contributor.authorHowerton S.C.
dc.contributor.authorValenti S.
dc.contributor.authorKankare E.
dc.contributor.authorDrake A.J.
dc.contributor.authorDjorgovski S.G.
dc.contributor.authorTomasella L.
dc.contributor.authorTartaglia L.
dc.contributor.authorKangas T.
dc.contributor.authorOchner P.
dc.contributor.authorFilippenko A.V.
dc.contributor.authorCiabattari F.
dc.contributor.authorGeier S.l
dc.contributor.authorHowell D.A.
dc.contributor.authorIsern J.
dc.contributor.authorLeonini S.
dc.contributor.authorPignata G.
dc.contributor.authorTuratto M.
dc.date.accessioned2022-08-22T16:30:59Z
dc.date.available2022-08-22T16:30:59Z
dc.date.issued2018-04
dc.descriptionIndexación Scopuses
dc.description.abstractSNhunt151 was initially classified as a supernova (SN) impostor (nonterminal outburst of a massive star). It exhibited a slow increase in luminosity, lasting about 450 d, followed by a major brightening that reaches MV ≈ -18 mag. No source is detected to MV ≳ -13 mag in archival images at the position of SNhunt151 before the slow rise. Low-to-mid-resolution optical spectra obtained during the pronounced brightening show very little evolution, being dominated at all times by multicomponent Balmer emission lines, a signature of interaction between the material ejected in the new outburst and the pre-existing circumstellar medium. We also analysed mid-infrared images from the Spitzer Space Telescope, detecting a source at the transient position in 2014 and 2015. Overall, SNhunt151 is spectroscopically a Type IIn SN, somewhat similar to SN 2009ip. However, there are also some differences, such as a slow pre-discovery rise, a relatively broad light-curve peak showing a longer rise time (~50 d), and a slower decline, along with a negligible change in the temperature around the peak (T ≤ 104 K). We suggest that SNhunt151 is the result of an outburst, or an SN explosion, within a dense circumstellar nebula, similar to those embedding some luminous blue variables like η Carinae and originating from past mass-loss events. © 2017 The Author(s).es
dc.description.urihttps://authors.library.caltech.edu/85510/1/sty009.pdf
dc.identifier.citationMonthly Notices of the Royal Astronomical Society Volume 475, Issue 2, Pages 2614 - 26311 April 2018es
dc.identifier.doi10.1093/mnras/sty009
dc.identifier.issn00358711
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/23592
dc.language.isoenes
dc.publisherOxford University Presses
dc.rights.licenseCC BY 4.0
dc.subjectSupernovaees
dc.subjectLight Curvees
dc.subjectWolf-Rayet Starses
dc.subjectInfrared imaginges
dc.subjectSpace telescopeses
dc.titleSNhunt151: An explosive event inside a dense cocoones
dc.typeArtículoes
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