J/A+A/621/A109 Synthetic spectra of supernovae models (Boian+, 2019)
Diversity of supernovae and impostors shortly after explosion.
Boian I., Groh J.H.
<Astron. Astrophys. 621, A109 (2019)>
=2019A&A...621A.109B 2019A&A...621A.109B (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Supernovae ; Spectroscopy
Keywords: supernovae: general - stars: massive - surveys - stars: winds -
stars: mass-loss - stars: evolution
Abstract:
Observational surveys are now able to detect an increasing number of
transients, such as core-collapse supernovae (SN) and powerful
non-terminal outbursts (SN impostors). Dedicated spectroscopic
facilities can follow up these events shortly after detection. Here we
investigate the properties of these explosions at early times.We use
the radiative transfer code CMFGEN to build an extensive library of
spectra simulating the interaction of supernovae and their
progenitor's winds/circumstellar medium (CSM).We consider a range of
progenitor mass-loss rates (dM/dt=5x10-4 to 10-2 M_☉/yr),
abundances (solar, CNO-processed, and He-rich), and SN luminosities
(L=1.9x108 to 2.5x1010L☉). The models simulate events
~=1-day after explosion, and we assume a fixed location of the shock
front as Rin=8.6x1013cm. We show that the large range of massive
star properties at the pre-SN stage causes a diversity of early-time
interacting SN and impostors. We identify three main classes of
early-time spectra consisting of relatively high-ionisation (e.g. HeII
and OVI), medium-ionisation (e.g. CIII and NIII), and low-ionisation
lines (e.g. HeI and FeII/III). They are regulated by L and the CSM
density. Given a progenitor wind velocity vinf, our models also
place a lower limit of dM/dt≳5x10-4(vinf=150km/s)M☉/yr for
detection of CSM interaction signatures in observed spectra.
Early-time SN spectra should provide clear constraints on progenitors
by measuring H, He, and CNO abundances if the progenitors come from
single stars. The connections are less clear considering the effects
of binary evolution. Nevertheless, our models provide a clear path for
linking the final stages of massive stars to their post-explosion
spectra at early times, and guiding future observational follow-up of
transients with facilities such as the Zwicky Transient Facility.
Description:
The associated files contain the high-resolution synthetic spectra of
each of the supernova models presented in the paper (Table 1, Figs. 1
& 2). The models are computed using the radiative transfer code CMFGEN
(Hillier & Miller, 1998ApJ...496..407H 1998ApJ...496..407H) and simulate supernovae
interacting with their progenitor's wind at early times after
explosion for a large range of supernova and progenitor properties.
There are 48 ascii files, one for each model.
Each file contains a header describing the main model parameters:
luminosity (solar luminosities), mass-loss rate (solar masses/year),
terminal wind velocity (km/s), flux temperature at optical
depth=10(kK), inner boundary radius (cm) and the mass-fractions of H,
He, C, N, O and Fe) and three columns: wavelength (Angstrom), flux at
10Mpc (Janskies), and normalised flux.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 69 48 List of model spectra
sp/* . 48 Individual model spectra
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 E4.2 Lsun Lum [19e7/25e9] Luminosity
6- 9 E4.1 Msun/yr dM/dt [5e-4/1e-2] Mass-loss rate
11- 13 I3 km/s vint [150] Terminal velocity
15- 22 E8.4 cm Rin [8.640e13] Inner boundary
24- 27 F4.1 kK Teff [16.1/64.7] Effective Temperature
(at optical depth = 10)
29- 31 A3 --- Abund [he sol nit] Abundance code (1)
34- 69 A36 --- FileName Name of sht spectrum file in subdirectory sp
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Note (1): Abundance (mass fractions) code as follows:
he = H=1.864e-1, He=8.0e-1, C=5.583e-5, N=8.172e-3, O=1.319e-4, Fe=1.36e-3
sol = H=7.010e-1, He=2.8e-1, C=3.025e-3, N=1.182e-3, O=9.634e-4, Fe=1.36e-3
nit = H=7.054e-1, He=2.8e-1, C=5.583e-5, N=8.172e-3, O=1.319e-4, Fe=1.36e-3
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Byte-by-byte Description of file (#): sp/*
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Bytes Format Units Label Explanations
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4- 20 F17.10 0.1nm lambda Spectral wavelength
29- 45 E17.10 Jy F10Mpc Flux at 10Mpc
52- 69 E18.10 --- FNorm ?=- Normalised flux
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Acknowledgements:
Ioana Boian, boiani(at)tcd.ie
(End) Patricia Vannier [CDS] 05-Dec-2018