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Supernova 2014J at M82 - II. Direct analysis of a middle-class Type Ia supernova

AutorVallely, Patrick; Moreno-Raya, M. E.; Baron, E.; Ruiz-Lapuente, Pilar ; Domínguez, I.; Galbany, Lluís; González Hernández, J. I.; Méndez, J.; Hamuy, M.; López-Sánchez, A. R.; Catalán, S.; Cooke, E.; Fariña, C.; Génova-Santos, R.; Karjalainen, R.; Lietzen, H.; McCormac, J.; Riddick, F.; Rubiño-Martín, J. A.; Skillen, I.; Tudor, V.; Vaduvescu, O.
Palabras claveSupernovae: general
Supernovae: individual: 2014J, 2011Fe.
Fecha de publicación9-may-2016
EditorBlackwell Publishing
CitaciónMonthly Notices of the Royal Astronomical Society 460: 1614-1624 (2016)
ResumenWe analyse a time series of optical spectra of SN 2014J from almost two weeks prior to maximum to nearly four months after maximum. We perform our analysis using the SYNOW code, which is well suited to track the distribution of the ions with velocity in the ejecta. We show that almost all of the spectral features during the entire epoch can be identified with permitted transitions of the common ions found in normal supernovae (SNe) Ia in agreement with previous studies. We show that 2014J is a relatively normal SN Ia. At early times the spectral features are dominated by Si II, S II, Mg II, and Ca II. These ions persist to maximum light with the appearance of Na I and Mg I. At later times iron-group elements also appear, as expected in the stratified abundance model of the formation of normal Type Ia SNe. We do not find significant spectroscopic evidence for oxygen, until 100 d after maximum light. The +100 d identification of oxygen is tentative, and would imply significant mixing of unburned or only slight processed elements down to a velocity of 6000 kms-1. Our results are in relatively good agreement with other analyses in the infrared. We briefly compare SN 2011fe to SN 2014J and conclude that the differences could be due to different central densities at ignition or differences in the C/O ratio of the progenitors. 2016 The Authors ; Published by Oxford University Press on behalf of the Royal Astronomical Society
Descripción11 págs.; 6 figs.; 4 tabs.
Versión del editorhttp://doi.org/10.1093/mnras/stw1088
URIhttp://hdl.handle.net/10261/145815
DOI10.1093/mnras/stw1088
Identificadoresdoi: 10.1093/mnras/stw1088
issn: 0035-8711
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