TY - JOUR
T1 - Supernova 2014J at M82-II. Direct analysis of a middle-class type Ia supernova
AU - Vallely, Patrick
AU - Moreno-Raya, M. E.
AU - Baron, E.
AU - Ruiz-Lapuente, Pilar
AU - Domínguez, I.
AU - Galbany, Lluís
AU - González Hernández, J. I.
AU - Méndez, J.
AU - Hamuy, M.
AU - López-Sánchez, A. R.
AU - Catalán, S.
AU - Cooke, E.
AU - Fariña, C.
AU - Génova-Santos, R.
AU - Karjalainen, R.
AU - Lietzen, H.
AU - McCormac, J.
AU - Riddick, F.
AU - Rubiño-Martín, J. A.
AU - Skillen, I.
AU - Tudor, V.
AU - Vaduvescu, O.
PY - 2016/8/1
Y1 - 2016/8/1
N2 - We 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 iand 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.
AB - We 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 iand 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.
KW - supernovae: general
KW - supernovae: individual: 2014J, 2011Fe
UR - http://www.scopus.com/inward/record.url?scp=84983059162&partnerID=8YFLogxK
U2 - 10.1093/mnras/stw1088
DO - 10.1093/mnras/stw1088
M3 - Article
AN - SCOPUS:84983059162
SN - 0035-8711
VL - 460
SP - 1614
EP - 1624
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -