J/MNRAS/483/628 SN Ia properties using bolometric light curves (Scalzo+, 2019)
Probing type Ia supernova properties using bolometric light curves from the
Carnegie Supernova Project and the CfA Supernova Group.
Scalzo R.A., Parent E., Burns C., Childress M., Tucker B.E., Brown P.J.,
Contreras C., Hsiao E., Krisciunas K., Morrell N., Phillips M.M.,
Piro A.L., Stritzinger M., Suntzeff N.
<Mon. Not. R. Astron. Soc., 483, 628-647 (2019)>
=2019MNRAS.483..628S 2019MNRAS.483..628S (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Magnitudes ; Photometry, UBVRI
Keywords: methods: statistical - white dwarfs - supernovae: general -
dark energy
Abstract:
We present bolometric light curves constructed from multiwavelength
photometry of Type Ia supernovae (SNe Ia) from the Carnegie Supernova
Project and the CfA Supernova Group, using near-infrared observations
to provide robust constraints on host galaxy dust extinction. This set
of light curves form a well-measured reference set for comparison with
theoretical models. Ejected mass and synthesized 56Ni mass are
inferred for each SN Ia from its bolometric light curve using a
semi-analytic Bayesian light curve model, and fitting formulas
provided in terms of light curve width parameters from the SALT2 and
SNooPy light curve fitters. A weak bolometric width-luminosity
relation is confirmed, along with a correlation between ejected mass
and the bolometric light curve width. SNe Ia likely to have
sub-Chandrasekhar ejected masses belong preferentially to the
broad-line and cool-photosphere spectroscopic subtypes, and have
higher photospheric velocities and populate older, higher mass host
galaxies than SNe Ia consistent with Chandrasekhar-mass explosions.
Two peculiar events, SN 2006bt and SN 2006ot, have normal peak
luminosities but appear to have super-Chandrasekhar ejected masses.
Description:
The SNe Ia we use for our investigation are drawn from the multiyear
Carnegie Supernova Project (CSP-I; Hamuy et al. 2006PASP..118....2H 2006PASP..118....2H)
and the Harvard-Smithsonian Center for Astrophysics Supernova Group
(CfA) data sets.
We use CSP-I uBVgri photometry from Stritzinger et al.
(2011AJ....142..156S 2011AJ....142..156S, Cat. J/AJ/142/156), and CfA UBVRIr'i' photometry
from Jha, Riess & Kirshner (2007ApJ...659..122J 2007ApJ...659..122J, Cat. J/ApJ/659/122),
Hicken et al. (2009ApJ...700..331H 2009ApJ...700..331H, Cat. J/ApJ/700/331), and Hicken et
al. (2012ApJS..200...12H 2012ApJS..200...12H, Cat. J/ApJS/200/12). Near-infrared (NIR)
photometry is also available from Stritzinger et al.
(2011AJ....142..156S 2011AJ....142..156S, Cat. J/AJ/142/156) for CSP-I targets, and from
Friedman et al. (2015ApJS..220....9F 2015ApJS..220....9F, Cat. J/ApJS/220/9) for CfA
targets.
We use derived spectroscopic quantities published in Blondin et al.
(2012AJ....143..126B 2012AJ....143..126B, Cat. J/AJ/143/126), Silverman et al.
(2012MNRAS.425.1819S 2012MNRAS.425.1819S, J/MNRAS/425/1819), and Folatelli et al.
(2013ApJ...773...53F 2013ApJ...773...53F, Cat. J/ApJ/773/53), including: the heliocentric
and CMB-frame redshifts of the host galaxy; the blueshift velocity
vSi of the SiII λ6355 feature in spectra near maximum light;
the spectroscopic subtype identified by SNID (Blondin & Tonry
2007ApJ...666.1024B 2007ApJ...666.1024B); the Wang et al. (2009ApJ...699L.139W 2009ApJ...699L.139W, Cat.
J/ApJ/699/L139) subtype -'normal' (N) or 'high-velocity' (HV) -
determined by whether vSi is greater or less than 11,800km/s; the
Branch et al. (2006PASP..118..560B 2006PASP..118..560B) subtype, based on measurements of
the equivalent widths and line profile shapes of the SiII λ5972
and SiII λ6355 features in spectra taken near maximum light.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
salt2.dat 59 45 SALT2 light curve fit parameters for CSP and
CfA SNe Ia
snoopy.dat 79 45 SNooPy light curve fit parameters for CSP and
CfA SNe Ia
rbol.dat 49 977 Bolometric light curve information for CSP and
CfA SNe Ia
bololc.dat 74 75 Bolometric light curve properties for CSP and
CfA SNe Ia
alpha.dat 41 21 Predictive mean and variance of empirical alpha
priors
results.dat 99 3440 Marginal distributions of progenitor properties
via MCMC
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Byte-by-byte Description of file: salt2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Supernova name
11- 13 A3 --- Set Survey of light curve data (CSP or CfA)
15- 21 F7.1 d MJDmax Date of B-band maximum light
23- 25 F3.1 d e_MJDmax 1-sigma formal uncertainty on MJDmax
27- 31 F5.2 mag Bmagmax Maximum B-band magnitude
33- 36 F4.2 mag e_Bmagmax 1-sigma formal uncertainty on Bmagmax
38- 42 F5.2 --- x1 Light curve width parameter
44- 47 F4.2 --- e_x1 1-sigma formal uncertainty on x1
49- 53 F5.2 --- c Color parameter
55- 59 F5.3 --- e_c 1-sigma formal uncertainty on c
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Byte-by-byte Description of file: snoopy.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Supernova name
11- 13 A3 --- Set Survey of light curve data (CSP or CfA)
15- 19 F5.3 --- sBV Light curve width parameter
21- 25 F5.3 --- e_sBV 1-sigma formal uncertainty on sBV
27- 32 F6.3 mag Bmagmax Maximum B-band magnitude
34- 38 F5.3 mag e_Bmagmax 1-sigma formal uncertainty on Bmagmax
40- 45 F6.3 mag E(B-V) E(B-V) of host galaxy extinction
47- 51 F5.3 --- rv Host galaxy extinction law slope
53- 59 F7.5 --- covEE Variance of E(B-V)
61- 68 F8.5 --- covRR Variance of rv
70- 77 F8.5 --- covER Covariance of E(B-V) and rv
79 A1 --- n_Name ? Remarks on SN 2006bt and SN 2006ot (1)
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Note (1): Note as follows:
* = SNe 2006bt and 2006ot are peculiar SNe excluded from SNooPy's
training set, believed to have negligible host galaxy extinction
(Foley et al. 2010ApJ...708.1748F 2010ApJ...708.1748F; Stritzinger et al. 2011AJ....142..156S 2011AJ....142..156S,
Cat. J/AJ/142/156)
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Byte-by-byte Description of file: rbol.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Supernova name
11- 15 F5.1 d Phase Light curve phase with respect to bolometric
maximum
17- 23 F7.3 [mW/m2] logFbol log10 of bolometric flux computed for assumed
zero host galaxy dust reddening
25- 29 F5.3 [mW/m2] e_logFbol Error on logFbol
31- 36 F6.3 mag corrC Correction term proportional to E(B-V)
38- 42 F5.3 mag corrRC Correction term proportional to
RVxE(B-V) (1)
44- 49 F6.4 mag2 corrRCC Correction term proportional to
RVxE(B-V)2 (1)
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Note (1): RV is the extinction law slope (RV=AV/E(B-V))
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Byte-by-byte Description of file: bololc.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name IAU or survey-specific SN name
18- 20 A3 --- Set Survey of light curve data (CSP, CfA, SNf;
MPA for models)
22- 25 F4.2 mag dm15mag ? Change in bolometric magnitude between
maximum and day +15
27- 30 F4.2 mag e_dm15mag ? 1-sigma formal uncertainty in dm15mag (1)
32- 35 F4.2 mag dm40mag ? Change in bolometric magnitude between
maximum and day +40
37- 40 F4.2 mag e_dm40mag ? 1-sigma formal uncertainty in dm40mag (1)
42- 46 F5.2 [10-7W] logLmax log10 maximum bolometric luminosity
48- 51 F4.2 [10-7W] e_logLmax ? 1-sigma formal uncertainty in Lmax (1)
53- 57 F5.2 [10-7W] logL40 log10 bolometric flux at day +40
59- 62 F4.2 [10-7W] e_logL40 ? 1-sigma formal uncertainty in L40 (1)
64- 67 F4.1 d thm ? Days between pre-max half-light point and
maximum light
69- 72 F4.1 d thp Days between post-max half-light point and
maximum light
74 I1 --- r_Name ? References for the models (2)
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Note (1): Uncertainties are dominated by systematic errors. Null values
indicate that the measurement could not be made reliably due to gaps
in light curve coverage. For CSP and CfA SNe Ia from this work,
measurements are made by directly evaluating and integrating the
GP model of the multi-band light curve, marginalizing over E(B-V) and
RV from host galaxy extinction. For SNf SNe Ia, and for synthetic
UBVRIYJHK light curves of numerical explosion models (MPA),
all quantities measured by one-dimensional GP interpolation on the
published light curves used in Scalzo et al. 2014MNRAS.440.1498S 2014MNRAS.440.1498S.
Note (2): References as follows:
1 = Fink et al. 2010A&A...514A..53F 2010A&A...514A..53F (explosion model)
and Kromer et al. 2010ApJ...719.1067K 2010ApJ...719.1067K (radiation transfer)
2 = Ruiter et al. 2013MNRAS.429.1425R 2013MNRAS.429.1425R
3 = Seitenzahl 2013A&A...559L...5S 2013A&A...559L...5S (explosion model)
and Roepke et al. 2012ApJ...750L..19R 2012ApJ...750L..19R (radiation transfer)
4 = Pakmor et al. 2012ApJ...747L..10P 2012ApJ...747L..10P; three different views given are
_1:angle-averaged light curve, _2:brightest line of sight and
_3:faintest line of sight
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Byte-by-byte Description of file: alpha.dat
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Bytes Format Units Label Explanations
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1- 4 F4.2 --- fNi 56Ni content as fraction of total ejected mass
6- 10 F5.3 --- HK96hi Predictive mean form factor (α) for
Hoeflich & Khokhlov (1996ApJ...457..500H 1996ApJ...457..500H) model
grid, high-density (Chandrasekhar-mass) models
12- 16 F5.3 --- e_HK96hi Error on HK96hi
18- 22 F5.3 --- HK96lo Predictive mean form factor (α) for
Hoeflich & Khokhlov (1996ApJ...457..500H 1996ApJ...457..500H) model
grid, low-density (Chandrasekhar-mass) models
24- 28 F5.3 --- e_HK96lo Error on HK96lo
30- 34 F5.3 --- B17 Predictive mean form factor (α) for
Blondin et al. (2013MNRAS.429.2127B 2013MNRAS.429.2127B,
2017MNRAS.470..157B 2017MNRAS.470..157B) model grid including all
explosion types
36- 41 F6.4 --- e_B17 Error on B17
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Byte-by-byte Description of file: results.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Supernova name
11- 13 A3 --- Set Survey of light curve data (CSP or CfA)
15- 21 A7 --- run Run as described in the main text (1)
23- 28 A6 --- attr Variable for which marginal distribution is
given (2)
30- 38 F9.3 --- p01 1st percentile of attr
40- 48 F9.3 --- p05 5th percentile of attr
50- 58 F9.3 --- p16 16th percentile of attr (-1sigma)
60- 68 F9.3 --- p50 50th percentile of attr (median)
70- 78 F9.3 --- p84 84th percentile of attr (+1sigma)
80- 88 F9.3 --- p95 95th percentile of attr
90- 99 F10.4 --- p99 99th percentile of attr
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Note (1): Run as follows:
runF = Run F priors based on Scalzo et al. 2014MNRAS.440.1498S 2014MNRAS.440.1498S
B17 = alpha prior from Blondin et al. 2013MNRAS.429.2127B 2013MNRAS.429.2127B,
2017MNRAS.470..157B 2017MNRAS.470..157B
HK96 = alpha prior from Hoeflich & Khokhlov 1996ApJ...457..500H 1996ApJ...457..500H
mirnorm = Run F priors + adjustment to MIR flux based on Chandrasekhar-mass
models of normal SNe Ia
mir91bg = Run F priors + adjustment to MIR flux based on Chandrasekhar-mass
models of 1991bg-like SNe Ia
Note (2): Variable as follows:
Mej = total ejected mass, in solar masses
MNi = 56Ni mass in solar masses
MFe = stable iron-peak element mass in solar masses
MSi = intermediate-mass element mass in solar masses
MCO = unburned carbon/oxygen mass in solar masses
lpc = log10(central density in g/cm3)
Egrv51 = binding energy of progenitor in foe (1044J)
Ekin51 = kinetic energy of explosion in foe (1044J)
alpha = ratio Lbol/Lrad at maximum light (dimensionless)
Q = 56Ni form factor (dimensionless; Scalzo et al.
2014MNRAS.440.1498S 2014MNRAS.440.1498S)
ebmv = host galaxy E(B-V) in mag
Rv = host galaxy extinction law slope RV
muoff = offset from mean redshift-based distance modulus assuming flat
LCDM cosmology (ΩΛ=0.7) (i.e., a nuisance parameter
for distance error)
trise = bolometric rise time in days
t0 = gamma-ray transparency time, days since explosion
vsc = velocity of bulk ejecta in km/s (Scalzo et al. 2014MNRAS.440.1498S 2014MNRAS.440.1498S)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 07-Jul-2022