J/MNRAS/448/2766 Strong lines in the optical/NIR for SN 2002bo (Blondin+, 2015)
A one-dimensional Chandrasekhar-mass delayed-detonation model for
the broad-lined Type Ia supernova 2002bo.
Blondin S., Dessart L., Hillier D.J.
<Mon. Not. R. Astron. Soc., 448, 2766-2797 (2015)>
=2015MNRAS.448.2766B 2015MNRAS.448.2766B (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Models, evolutionary ; Spectroscopy
Keywords: radiative transfer - supernovae: general -
supernovae: individual: SN 2002bo
Abstract:
We present 1D non-local thermodynamic equilibrium time-dependent
radiative transfer simulations of a Chandrasekhar-mass
delayed-detonation model which synthesizes 0.51 M☉ of 56Ni, and
confront our results to the Type Ia supernova (SN Ia) 2002bo over the
first 100d of its evolution. Assuming only homologous expansion, this
same model reproduces the bolometric and multiband light curves, the
secondary near-infrared (NIR) maxima, and the optical and NIR spectra.
The chemical stratification of our model qualitatively agrees with previous
inferences by Stehle et al. (2005MNRAS.360.1231S 2005MNRAS.360.1231S), but reveals significant
quantitative differences for both iron-group and intermediate-mass
elements. We show that ±0.1 M☉ (i.e. ±20 per cent) variations
in 56Ni mass have a modest impact on the bolometric and colour
evolution of our model. One notable exception is the U band, where a
larger abundance of iron-group elements results in less opaque ejecta
through ionization effects, our model with more 56Ni displaying a
higher near-ultraviolet flux level. In the NIR range, such variations
in 56Ni mass affect the timing of the secondary maxima but not their
magnitude, in agreement with observational results. Moreover, the
variation in the I, J, and Ks magnitudes is less than 0.1 mag within
∼ 10d from bolometric maximum, confirming the potential of NIR
photometry of SNe Ia for cosmology. Overall, the delayed-detonation
mechanism in single Chandrasekhar-mass white dwarf progenitors seems
well suited for SN 2002bo and similar SNe Ia displaying a broad SiII
6355Å line. Whatever multidimensional processes are at play during
the explosion leading to these events, they must conspire to produce
an ejecta comparable to our spherically symmetric model.
Description:
Our data on SN 2002bo are mostly taken from Benetti et al.
(2004MNRAS.348..261B 2004MNRAS.348..261B), with additional optical spectra from Blondin et al.
(2012, J/AJ/143/126) and Silverman et al. (2012, J/MNRAS/425/1789). We
use the near-infrared (JHKs) photometry published by Krisciunas et al.
(2004AJ....128.3034K 2004AJ....128.3034K). We select spectra whose relative flux
calibration agrees with photometry-based colours to within 0.1 mag. As
in Blondin et al. (2013MNRAS.429.2127B 2013MNRAS.429.2127B), we adopt a recession velocity
cz=1293 km/s for the host galaxy, a distance modulus µ=31.90±0.20 mag,
and a total reddening E(B-V)=0.41±0.07 mag.
Objects:
--------------------------------------------------------
RA (ICRS) DE Designation(s)
--------------------------------------------------------
10 18 06.51 +21 49 41.7 SN 2002bo = AAVSO 1012+22
--------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tables.dat 24 15 List of tables
tablec1.dat 24 30 Strong lines in the optical and NIR at 4.1 d
past explosion (Δtbol=-13.5 d)
tablec2.dat 24 32 Strong lines in the optical and NIR at 5.4 d
past explosion (Δtbol=-12.1 d)
tablec3.dat 24 34 Strong lines in the optical and NIR at 9.6 d
past explosion (Δtbol=-8.0 d)
tablec4.dat 24 33 Strong lines in the optical and NIR at 12.8 d
past explosion (Δtbol=-4.8 d)
tablec5.dat 24 32 Strong lines in the optical and NIR at 15.5 d
past explosion (Δtbol=-2.1 d)
tablec6.dat 24 30 Strong lines in the optical and NIR at 17.0 d
past explosion (Δtbol=-0.5 d)
tablec7.dat 24 29 Strong lines in the optical and NIR at 22.6 d
past explosion (Δtbol=+5.1 d)
tablec8.dat 24 29 Strong lines in the optical and NIR at 27.4 d
past explosion (Δtbol=+9.8 d)
tablec9.dat 24 29 Strong lines in the optical and NIR at 33.2 d
past explosion (Δtbol=+15.6 d)
tablec10.dat 24 28 Strong lines in the optical and NIR at 44.1 d
past explosion (Δtbol=+26.6 d)
tablec11.dat 24 26 Strong lines in the optical and NIR at 53.4 d
past explosion (Δtbol=+35.8 d)
tablec12.dat 24 32 Strong lines in the optical and NIR at 64.6 d
past explosion (Δtbol=+47.0 d)
tablec13.dat 24 32 Strong lines in the optical and NIR at 71.1 d
past explosion (Δtbol=+53.5 d)
tablec14.dat 24 36 Strong lines in the optical and NIR at 86.0 d
past explosion (Δtbol=+68.4 d)
tablec15.dat 24 31 Strong lines in the optical and NIR at 104.1 d
past explosion (Δtbol=+86.5 d)
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/MNRAS/408/827 : Simulations of supernova explosions (Dessart+, 2010)
J/AJ/143/126 : Spectroscopy of 462 nearby Type Ia supernovae
(Blondin+, 2012)
J/MNRAS/425/1789 : Berkeley supernova Ia program. I. (Silverman+, 2012)
Byte-by-byte Description of file: tables.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 F5.1 d Texp Past-explosion time
7- 11 F5.1 d DeltaTbol Time from bolometric maximum Δtbol
13- 24 A12 --- FileName File name containting data for this time
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Byte-by-byte Description of file: tablec*.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Ion Ion designation
8- 14 F7.2 0.1nm lambda1 [3002.65/9997.58]? Line wavelength in air
(Å)
15- 16 A2 --- n_lambda1 Note on lambda1 (1)
18- 22 F5.3 um lambda2 [1.001/2.473]? Line wavelength in air
23- 24 A2 --- n_lambda2 Note on lambda2 (1)
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Note (1): Note as follows:
] = Forbidden and semiforbidden transitions are noted using the appropriate
brackets around the line wavelength (in air);
D = Transitions connected to the ground state.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 27-Nov-2017