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Persistent Cii Absorption In the Normal TYPE Ia Supernova 2002fk∗

Universidad de Chile. Repositorio Académico

 
Título Persistent Cii Absorption In the Normal TYPE Ia Supernova 2002fk∗
 
Autor Contreras, Carlos
Cartier, Regis
Clocchiatti, Alejandro
Coppi, Paolo
González, Luis
Suntzeff, Nicholas B.
Krisciunas, Kevin
Zelaya, Paula
Folatelli, Gaston
Roth, Miguel
Gonzalez, Sergio
Phillips, Mark M.
Koviak, Kathleen
Morrell, Nidia
Huerta Cancino, Leonor Patricia
Maza Sancho, José María
Hamuy Wackenhut, Mario Andrés
 
Tema Key words: cosmological parameters
 
Descripción Artículo de publicación ISI.
We present well-sampled UBVRIJHK photometry of SN 2002fk starting 12 days before maximum light through
122 days after peak brightness, along with a series of 15 optical spectra from −4 to +95 days since maximum. Our
observations show the presence of C ii lines in the early-time spectra of SN 2002fk, expanding at 11,000 km s−1 and persisting until 8 days past maximum light with a velocity of ∼9000 km s−1. SN 2002fk is characterized
by a small velocity gradient of v˙Si ii = 26 km s−1 day−1, possibly caused by an off-center explosion with the ignition region oriented toward the observer. The connection between the viewing angle of an off-center explosion
and the presence of C ii in the early-time spectrum suggests that the observation of Cii could be also due to a
viewing angle effect. Adopting the Cepheid distance to NGC 1309 we provide the first H0 value based on near infrared (near-IR) measurements of a Type Ia supernova (SN) between 63.0 ± 0.8 (±3.4 systematic) and 66.7 ± 1.0
(±3.5 systematic) km s−1 Mpc−1, depending on the absolute magnitude/decline rate relationship adopted. It appears
that the near-IR yields somewhat lower (6%–9%) H0 values than the optical. It is essential to further examine this issue by (1) expanding the sample of high-quality near-IR light curves of SNe in the Hubble flow, and (2) increasing
the number of nearby SNe with near-IR SN light curves and precise Cepheid distances, which affords the promise to deliver a more precise determination of H0.
 
Fecha 2014-09-16T13:26:01Z
2015-03-13T13:01:15Z
2014-09-16T13:26:01Z
2015-03-13T13:01:15Z
2014-07-01
 
Tipo Artículo de revista
 
Enlace The Astrophysical Journal, 789:89 (22pp), 2014 July 1
doi:10.1088/0004-637X/789/1/89
http://repositorio.uchile.cl/handle/2250/126472
 
Idioma en_US
 
Publicador The American Astronomical Society