Show simple item record

Disappearance of the progenitor of supernova iptf13bvn

Authordc.contributor.authorFolatelli, Gastón 
Authordc.contributor.authorVan Dyk, Schuyler D. 
Authordc.contributor.authorKuncarayakti, Hanindyo 
Authordc.contributor.authorMaeda, Keiichi 
Authordc.contributor.authorBersten, Melina C. 
Authordc.contributor.authorNomoto, Ken'ichi 
Authordc.contributor.authorPignata Libralato, Giuliano 
Authordc.contributor.authorHamuy Wackenhut, Mario 
Authordc.contributor.authorQuimby, Robert M. 
Authordc.contributor.authorZheng, WeiKang 
Authordc.contributor.authorFilippenko, Alexei V. 
Authordc.contributor.authorClubb, Kelsey I. 
Authordc.contributor.authorSmith, Nathan 
Authordc.contributor.authorElias Rosa, Nancy 
Authordc.contributor.authorFoley, Ryan J. 
Authordc.contributor.authorMiller, Adam A. 
Admission datedc.date.accessioned2016-12-23T16:18:01Z
Available datedc.date.available2016-12-23T16:18:01Z
Publication datedc.date.issued2016
Cita de ítemdc.identifier.citationAstrophysical Journal Letters. Volumen: 825 Número: 2es_ES
Identifierdc.identifier.other10.3847/2041-8205/825/2/L22
Identifierdc.identifier.urihttp://repositorio.uchile.cl/handle/2250/142065
Abstractdc.description.abstractSupernova (SN) iPTF13bvn in NGC 5806 was the first Type Ib SN to have been tentatively associated with a progenitor in pre-explosion images. We performed deep ultraviolet (UV) and optical Hubble Space Telescope observations of the SN site similar to 740 days after explosion. We detect an object in the optical bands that is fainter than the pre-explosion object. This dimming is likely not produced by dust absorption in the ejecta; thus, our finding confirms the connection of the progenitor candidate with the SN. The object in our data is likely dominated by the fading SN, implying that the pre-SN flux is mostly due to the progenitor. We compare our revised pre-SN photometry with previously proposed models. Although binary progenitors are favored, models need to be refined. In particular, to comply with our deep UV detection limit, any companion star must be less luminous than a late-O star or substantially obscured by newly formed dust. A definitive progenitor characterization will require further observations to disentangle the contribution of a much fainter SN and its environment.es_ES
Lenguagedc.language.isoenes_ES
Publisherdc.publisherIOP Publishinges_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/*
Sourcedc.sourceAstrophysical Journal Letterses_ES
Keywordsdc.subjectSupernovae: individual (iPTF13bvn)es_ES
Keywordsdc.subjectSupernovae: generales_ES
Keywordsdc.subjectStars: evolutiones_ES
Keywordsdc.subjectGalaxies: individual (NGC 5806)es_ES
Títulodc.titleDisappearance of the progenitor of supernova iptf13bvnes_ES
Document typedc.typeArtículo de revistaes_ES
Catalogueruchile.catalogadorC. R. B.es_ES
Indexationuchile.indexArtículo de publicación ISIes_ES


Files in this item

Icon

This item appears in the following Collection(s)

Show simple item record

Attribution-NonCommercial-NoDerivs 3.0 Chile
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Chile