Supernova 2011jd

dc.catalogadordfo
dc.contributor.authorDrake, A. J.
dc.contributor.authorDjorgovski, S. G.
dc.contributor.authorGraham, M. J.
dc.contributor.authorMahabal, A.
dc.contributor.authorWilliams, R.
dc.contributor.authorPrieto, J. L.
dc.contributor.authorCatelan, Marcio
dc.contributor.authorBeshore, E. C.
dc.contributor.authorLarson, S. M.
dc.contributor.authorChristensen, E.
dc.contributor.authorTomasella, L.
dc.contributor.authorBenetti, S.
dc.contributor.authorPastorello, A.
dc.contributor.authorValenti, S.
dc.contributor.authorBufano, F.
dc.date.accessioned2024-03-05T15:15:30Z
dc.date.available2024-03-05T15:15:30Z
dc.date.issued2011
dc.description.abstractReport the discovery of an apparent supernova in unfiltered Catalina Sky Survey (CSS) images: SN 2011 UT R.A. (2000.0) Decl. Mag. Offset 2011jd Nov. 19.17 0 22 54.27 +13 52 22.4 18.3 0".2 W, 2".2 N Further CSS magnitudes for 2011jd: Oct. 15.36 UT, [19.5; Nov. 27.20, 18.1. L. Tomasella, S. Benetti, A. Pastorello, S. Valenti, and F. Bufano, Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Padova, on behalf of a larger collaboration, report that a spectrogram of 2011jd, obtained on Dec. 18.87 UT with the Asiago 1.82-m Copernico Telescope (+ AFOSC; range 350-820 nm; resolution 2.4 nm), shows it to be a type-Ia supernova. The best fit to this spectrum found by GELATO (Harutyunyan et al. 2008, A.Ap. 488, 383; available at website URL https://gelato.tng.iac.es/login.cgi) suggests that 2011jd is similar to type-Ia supernovae between three and four weeks after maximum light, if a redshift of 0.079 is assumed for the host galaxy....
dc.fuente.origenORCID
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/84194
dc.information.autorucInstituto de Astrofísica; Catelan , Marcio; 0000-0001-6003-8877; 1001556
dc.language.isoen
dc.nota.accesocontenido parcial
dc.rightsacceso restringido
dc.titleSupernova 2011jd
dc.typeinforme
sipa.codpersvinculados1001556
sipa.trazabilidadORCID;2024-01-22
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