J/MNRAS/488/4239 SNe II and IIb optical light curves comparison (Pessi+, 2019)
Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type
II supernovae.
Pessi P.J., Folatelli G., Anderson J.P., Bersten M., Burns C.,
Contreras C., Davis S., Englert B., Hamuy M., Hsiao E.Y., Martinez L.,
Morrell N., Phillips M.M., Suntzeff N., Stritzinger M.D.
<Mon. Not. R. Astron. Soc., 488, 4239-4257 (2019)>
=2019MNRAS.488.4239P 2019MNRAS.488.4239P (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Redshifts ; Optical
Keywords: supernovae: general - supernovae: individual (SN 2001fa, SN 2004ff,
SN 2006Y, SN 2007fz, SN 2008M, SN 2013ai, SN 2013fs)
Abstract:
Type II supernovae (SNe II) show strong hydrogen features in their
spectra throughout their whole evolution, while type IIb supernovae
(SNe IIb) spectra evolve from dominant hydrogen lines at early times
to increasingly strong helium features later on. However, it is
currently unclear whether the progenitors of these SN types form a
continuum in pre-SN hydrogen mass or whether they are physically
distinct. SN light-curve morphology directly relates to progenitor and
explosion properties such as the amount of hydrogen in the envelope,
the pre-SN radius, the explosion energy, and the synthesized mass of
radioactive material. In this work, we study the morphology of the
optical-wavelength light curves of hydrogen-rich SNe II and
hydrogen-poor SNe IIb to test whether an observational continuum
exists between the two. Using a sample of 95 SNe (73 SNe II and 22 SNe
IIb), we define a range of key observational parameters and present a
comparative analysis between both types. We find a lack of events that
bridge the observed properties of SNe II and IIb. Light-curve
parameters such as rise times and post-maximum decline rates and
curvatures clearly separate both SN types and we therefore conclude
that there is no continuum, with the two SN types forming two
observationally distinct families. In the V band a rise time of 17d
(SNe II lower and SNe IIb higher), and a magnitude difference between
30 and 40d post-explosion of 0.4mag (SNe II lower and SNe IIb higher)
serve as approximate thresholds to differentiate both types.
Description:
Our sample includes 73 SNe II (see Table A1), with 64 taken from the
Carnegie Type II Supernova Program (CATS; Galbany et al.
2016AJ....151...33G 2016AJ....151...33G, Cat. J/AJ/151/33; PI: Hamuy, 2002-2003) and the
Carnegie Supernova Project (CSP-I; Hamuy et al. 2006PASP..118....2H 2006PASP..118....2H;
PIs: Phillips and Hamuy, 2004-2009) samples from the work of Anderson
et al. (2014ApJ...786...67A 2014ApJ...786...67A). This sample was selected as it
originated from a well-defined data set that was observed, reduced and
calibrated in a consistent manner. Additionally, nine objects having
well-defined light-curve maxima were included from the literature. All
the objects with well defined light-curve maxima were then used as
templates to obtain the date of maximum light for the rest of the
sample.
In the case of SNe IIb, no sufficiently large sample exists from a
single follow-up program. Therefore, we collate all SNe IIb from the
literature (see Table A2) that fit our selection criteria. First, we
require at least nine data points in our primary photometric band (V),
in order to have a good approximation of the intrinsic shape of the
light curve. Second, existing photometric data points around maximum
light for SNe IIb and prior to ∼25d after explosion for SNe II to have
a dense enough coverage of the early part of the light curve. This
means that our SN II light curves do not necessarily cover the epoch
of maximum light. Third, when the explosion date is not well
constrained by prediscovery non-detections, at least three available
spectra in order to be able to estimate the explosion dates through
spectral matching.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 99 73 SNe II sample
tablea2.dat 115 22 SNe IIb sample
table1.dat 40 11 Comparison between the explosion epochs obtained
from non-detection constraints and those
calculated using SNID for SNe IIb
table2.dat 44 35 Comparison between the date of maximum light in
the V band obtained directly from SN photometry
and that obtained from SNID for SNe II and
SNe IIb
tablea3.dat 55 2 SNe IIb with no observed maximum sample
tablea4.dat 227 95 Parameters obtained with respect to explosion
epoch
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Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Supernova name (YYYYaa or YYYYA)
8- 13 F6.4 --- z Heliocentric redshift of the host obtained
from NED
15- 21 F7.1 d texpl Explosion epoch of the supernova obtained
from non-detections
23 A1 --- r_texpl [abc] Reference for texpl (1)
25- 28 F4.1 d e_texpl Error on texpl
30- 36 F7.1 d tVmax Epoch of maximum light of the SN light curve
in the V band
38 A1 --- r_tVmax [c] Reference for tVmax (1)
40- 42 F3.1 d e_tVmax Error on tVmax
44- 50 F7.1 d tBmax Epoch of maximum light of the SN light curve
in the B band
52 A1 --- r_tBmax [d] Reference for tBmax (2)
54- 56 F3.1 d e_tBmax Error on tBmax
58- 64 F7.1 d trmax Epoch of maximum light of the SN light curve
in the r band
66 A1 --- r_trmax [d] Reference for trmax (2)
68- 70 F3.1 d e_trmax Error on trmax
72- 73 I2 --- phref Photometry reference (3)
75- 89 A15 --- spref Spectral references (4)
91- 99 A9 --- circular Reference of the discovery circular
--------------------------------------------------------------------------------
Note (1): References as follows:
a = Explosion epoch from Gutierrez et al. (2017ApJ...850...89G 2017ApJ...850...89G)
b = Explosion epoch estimation from spectral matching
c = Maximum light epoch from spectral matching
Note (2): Reference as follows:
d = Maximum light epoch with respect to average in V band from those SNe
that have data points around maximum
Note (3): References as follows:
1 = Leonard et al. (2002AJ....124.2490L 2002AJ....124.2490L)
2 = Galbany et al. (2016AJ....151...33G 2016AJ....151...33G, Cat. J/AJ/151/33)
3 = Anderson et al. (2014ApJ...786...67A 2014ApJ...786...67A) and Contreras et al.
(in preparation)
4 = Takats et al. (2015MNRAS.450.3137T 2015MNRAS.450.3137T, Cat. J/MNRAS/450/3137)
5 = Dall'Ora et al. (2014ApJ...787..139D 2014ApJ...787..139D)
6 = Valenti et al. (2016MNRAS.459.3939V 2016MNRAS.459.3939V, Cat. J/MNRAS/459/3939)
7 = Valenti et al. (2015MNRAS.448.2608V 2015MNRAS.448.2608V, Cat. J/MNRAS/448/2608)
8 = Yuan et al. (2016MNRAS.461.2003Y 2016MNRAS.461.2003Y, Cat. J/MNRAS/461/2003)
9 = Huang et al. (2016ApJ...832..139H 2016ApJ...832..139H)
10 = Terreran et al. (2016MNRAS.462..137T 2016MNRAS.462..137T)
Note (4): References as follows:
1 = WISeREP (Yaron & Gal-Yam 2012PASP..124..668Y 2012PASP..124..668Y)
2 = Gutierrez et al. (2017ApJ...850...89G 2017ApJ...850...89G)
3 = Leonard et al. (2002AJ....124.2490L 2002AJ....124.2490L)
4 = Shivvers et al. (2017PASP..129e4201S 2017PASP..129e4201S)
5 = Takats et al. (2015MNRAS.450.3137T 2015MNRAS.450.3137T, Cat. J/MNRAS/450/3137)
6 = Dall'Ora et al. (2014ApJ...787..139D 2014ApJ...787..139D)
7 = Childress et al. (2016PASA...33...55C 2016PASA...33...55C)
8 = Valenti et al. (2015MNRAS.448.2608V 2015MNRAS.448.2608V, Cat. J/MNRAS/448/2608)
9 = Black et al. (2017ApJ...848....5B 2017ApJ...848....5B)
10 = Yuan et al. (2016MNRAS.461.2003Y 2016MNRAS.461.2003Y, Cat. J/MNRAS/461/2003)
11 = Valenti et al. (2014MNRAS.438L.101V 2014MNRAS.438L.101V, Cat. J/MNRAS/438/L101)
12 = Dhungana et al. (2016ApJ...822....6D 2016ApJ...822....6D)
13 = Bose et al. (2015ApJ...806..160B 2015ApJ...806..160B)
14 = Yaron et al. (2017NatPh..13..510Y 2017NatPh..13..510Y)
15 = Terreran et al. (2016MNRAS.462..137T 2016MNRAS.462..137T)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Supernova name (YYYYaa, YYYYaaa or YYYYA)
9 A1 --- f_Name [*] Flag on Name (1)
11- 17 F7.4 --- z Heliocentric redshift of the host obtained
from NED
19- 25 F7.1 d texpl Explosion epoch of the supernova obtained
from non-detections
27 A1 --- r_texpl [a] Reference for texpl (2)
29- 31 F3.1 d e_texpl Error on texpl
33- 39 F7.1 d tVmax Epoch of maximum light of the SN light curve
in the V band
41- 44 F4.1 d e_tVmax Error on tVmax
46- 52 F7.1 d tBmax Epoch of maximum light of the SN light curve
in the B band
54 A1 --- r_tBmax [b] Reference for tBmax (3)
56- 58 F3.1 d e_tBmax Error on tBmax
60- 66 F7.1 d trmax Epoch of maximum light of the SN light curve
in the r band
68 A1 --- r_trmax [b] Reference for trmax (3)
70- 73 F4.1 d e_trmax Error on trmax
75- 93 A19 --- phref Photometry reference (4)
95-103 A9 --- spref Spectral references (5)
105-115 A11 --- circular Reference of the discovery circular
--------------------------------------------------------------------------------
Note (1): Flag as follows:
* = This object last non-detection and first detection dates in
Drout et al. (2011ApJ...741...97D 2011ApJ...741...97D, Cat. J/ApJ/741/97) differs from said
dates in the discovery circular. We use the date that appear in
Drout et al. (2011ApJ...741...97D 2011ApJ...741...97D, Cat. J/ApJ/741/97) since they are
more constraining.
Note (2): Reference as follows:
a = Explosion epoch estimation from spectral matching
Note (3): Reference as follows:
b = Maximum light epoch with respect to average in V band from those SNe
that have data points around maximum
Note (4): References as follows:
1 = Stritzinger et al. (2018A&A...609A.134S 2018A&A...609A.134S, Cat. J/A+A/609/A134)
2 = The Open Supernova Catalog (Guillochon et al. 2017ApJ...835...64G 2017ApJ...835...64G)
3 = Morales-Garoffolo et al. (2014MNRAS.445.1647M 2014MNRAS.445.1647M);
Morales-Garoffolo, Elias-Rosa & Isern (2015hsa8.conf..518M)
4 = Bersten et al. (2018Natur.554..497B 2018Natur.554..497B)
5 = Bianco et al. (2014ApJS..213...19B 2014ApJS..213...19B, Cat. J/ApJS/213/19)
6 = Brown et al. (2014Ap&SS.354...89B 2014Ap&SS.354...89B)
7 = Okyudo et al. (1993PASJ...45L..63O 1993PASJ...45L..63O)
8 = van Driel et al. (1993PASJ...45L..59V 1993PASJ...45L..59V)
9 = Benson et al. (1994AJ....107.1453B 1994AJ....107.1453B, Cat. J/AJ/107/1453)
10 = Richmond et al. (1994AJ....107.1022R 1994AJ....107.1022R, Cat. J/AJ/107/1022)
11 = Metlova et al. (1995AstL...21..598M 1995AstL...21..598M)
12 = Barbon et al. (1995A&AS..110..513B 1995A&AS..110..513B)
13 = Richmond et al. (1996AJ....112..732R 1996AJ....112..732R)
14 = Qiu et al. (1999AJ....117..736Q 1999AJ....117..736Q)
15 = Galbany et al. (2016AJ....151...33G 2016AJ....151...33G, Cat. J/AJ/151/33)
16 = Drout et al. (2011ApJ...741...97D 2011ApJ...741...97D, Cat. J/ApJ/741/97)
17 = Tsvetkov et al. (2009PZ.....29....2T 2009PZ.....29....2T, Cat. J/other/PZ/29.2)
18 = Pastorello et al. (2008MNRAS.389..955P 2008MNRAS.389..955P, Cat. J/MNRAS/389/955)
19 = Ergon et al. (2014A&A...562A..17E 2014A&A...562A..17E, Cat. J/A+A/562/A17)
20 = Kumar et al. (2013MNRAS.431..308K 2013MNRAS.431..308K, Cat. J/MNRAS/431/308)
21 = Morales-Garoffolo et al. (2015MNRAS.454...95M 2015MNRAS.454...95M, Cat. J/MNRAS/454/95)
22 = Bufano et al. (2014MNRAS.439.1807B 2014MNRAS.439.1807B)
Note (5): References as follows:
1 = Yaron & Gal-Yam (2012PASP..124..668Y 2012PASP..124..668Y)
2 = Holmbo et al. (in preparation)
3 = Matheson et al. (2000AJ....120.1487M 2000AJ....120.1487M)
4 = Barbon et al. (1995A&AS..110..513B 1995A&AS..110..513B)
5 = Jerkstrand et al. (2015A&A...573A..12J 2015A&A...573A..12J, Cat. J/A+A/573/A12)
6 = Modjaz et al. (2014AJ....147...99M 2014AJ....147...99M, Cat. J/AJ/147/99)
7 = Hamuy et al. (2009ApJ...703.1612H 2009ApJ...703.1612H)
8 = Pastorello et al. (2008MNRAS.389..955P 2008MNRAS.389..955P, Cat. J/MNRAS/389/955)
9 = Taubenberger et al. (2011MNRAS.413.2140T 2011MNRAS.413.2140T)
10 = Oates et al. (2012MNRAS.424.1297O 2012MNRAS.424.1297O)
11 = Arcavi et al. (2011ApJ...742L..18A 2011ApJ...742L..18A, Cat. J/ApJ/742/L18)
12 = Ergon et al. (2014A&A...562A..17E 2014A&A...562A..17E, Cat. J/A+A/562/A17)
13 = Ergon et al. (2015A&A...580A.142E 2015A&A...580A.142E, Cat. J/A+A/580/A142)
14 = Milisavljevic et al. (2013ApJ...767...71M 2013ApJ...767...71M)
15 = Kumar et al. (2013MNRAS.431..308K 2013MNRAS.431..308K, Cat. J/MNRAS/431/308)
16 = Morales-Garoffolo et al. (2015MNRAS.454...95M 2015MNRAS.454...95M, Cat. J/MNRAS/454/95)
17 = Bufano et al. (2014MNRAS.439.1807B 2014MNRAS.439.1807B)
18 = Childress et al. (2016PASA...33...55C 2016PASA...33...55C)
19 = Szalai et al. (2016MNRAS.460.1500S 2016MNRAS.460.1500S)
20 = Kilpatrick et al. (2017MNRAS.465.4650K 2017MNRAS.465.4650K)
21 = Shivvers et al. (2019MNRAS.482.1545S 2019MNRAS.482.1545S, Cat. J/MNRAS/482/1545)
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Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Supernova name (YYYYaa, YYYYaaa or YYYYA)
9- 15 F7.1 d teSNID Explosion epoch calculated using SNID for
SNe IIb (G1)
17- 21 F5.2 d e_teSNID Error on SNID
23- 29 F7.1 d teobs Explosion epoch obtained from non-detection
constraints
31- 34 F4.2 d e_teobs Error on tobs
36- 40 F5.1 d Diffte Difference between tSNID and tobs
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- Type Supernova type (II or IIb)
5- 11 A7 --- Name Supernova name (YYYYaa, YYYYaaa or YYYYA)
13- 19 F7.1 d tmSNID ? Date of maximum light in the V band obtained
from SNID (G1)
21- 24 F4.2 d e_tmSNID ? Error on tmSNID
26- 32 F7.1 d tmobs Date of maximum ligt in the V band obtained
directly from SN photometry
34- 38 F5.2 d e_tmobs Error on tmobs
40- 44 F5.1 d Difftm ? Difference between tmSNID and tmobs
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Supernova name (YYYYaa)
8- 15 F8.6 --- z Heliocentric redshift of the host obtained
from NED
17- 23 F7.1 d texpl Explosion epoch of the supernova
25- 29 F5.2 d e_texpl Error on texpl
31- 37 F7.1 d tVmax Epoch of maximum light of the supernova light
curve in the V band
39- 41 F3.1 d e_tVmax Error on tVmax
43 I1 --- phref Photometry reference (1)
45 I1 --- spref Spectral reference (2)
47- 55 A9 --- circular Reference of the discovery circular
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Note (1): Reference as follows:
1 = Stritzinger et al. (2018A&A...609A.134S 2018A&A...609A.134S, Cat. J/A+A/609/A134)
Note (2): Reference as follows:
1 = Holmbo et al. (in preparation)
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- Type Supernova type (II or IIb)
5- 11 A7 --- Name Supernova name (YYYYaa, YYYYaaa or YYYYA)
13- 16 F4.1 d triseB Time to maximum light or rise time in the
B band (1)
18- 21 F4.1 d e_triseB Error on triseB
23- 27 F5.3 10-2mag/d2 dm1B ? Earliest maximum of the first light-curve
derivative after maximum light in the
B band (2)
29- 34 F6.4 10-2mag/d2 e_dm1B ? Error on dm1B (5)
36- 39 F4.1 d tdm1B ? Phase corresponding to dm1B
41- 44 F4.1 d e_tdm1B ? Error on tdm1B (6)
46- 53 F8.5 10-2mag/d2 dm2B ? Earliest minimum of the second light-curve
derivative after maximum light in the
B band (3)
55- 61 F7.5 10-2mag/d2 e_dm2B ? Error on dm2B (5)
63- 66 F4.1 d tdm2B ? Phase corresponding to dm2B
68- 71 F4.1 d e_tdm2B ? Error on tdm2B (6)
73- 76 F4.2 mag DB4030 ? Magnitude difference between phases 30
and 40d post-explosion in the B band (4)
78- 82 F5.3 mag e_DB4030 ? Error on DB4030
84- 87 F4.1 d triseV Time to maximum light or rise time in the
V band (1)
89- 92 F4.1 d e_triseV Error on triseV
94- 98 F5.3 10-2mag/d2 dm1V ? Earliest maximum of the first light-curve
derivative after maximum light in the
V band (2)
100-105 F6.4 10-2mag/d2 e_dm1V ? Error on dm1V (5)
107-110 F4.1 d tdm1V ? Phase corresponding to dm1V
112-115 F4.1 d e_tdm1V ? Error on tdm1V (6)
117-124 F8.5 10-2mag/d2 dm2V ? Earliest minimum of the second light-curve
derivative after maximum light in the
V band (3)
126-132 F7.5 10-2mag/d2 e_dm2V ? Error on dm2V (5)
134-137 F4.1 d tdm2V ? Phase corresponding to dm2V
139-142 F4.1 d e_tdm2V ? Error on tdm2V (6)
144-149 F6.3 mag DV4030 ? Magnitude difference between phases 30
and 40d post-explosion in the V band (4)
151-155 F5.3 mag e_DV4030 ? Error on DV4030
157-160 F4.1 d triser Time to maximum light or rise time in the
r band (1)
162-165 F4.1 d e_triser Error on triser
167-171 F5.3 10-2mag/d2 dm1r ? Earliest maximum of the first light-curve
derivative after maximum light in the
r band (2)
173-178 F6.4 10-2mag/d2 e_dm1r ? Error on dm1r (5)
180-183 F4.1 d tdm1r ? Phase corresponding to dm1r
185-188 F4.1 d e_tdm1r ? Error on tdm1r (6)
190-197 F8.5 10-2mag/d2 dm2r ? Earliest minimum of the second light-curve
derivative after maximum light in the
r band (3)
199-205 F7.5 10-2mag/d2 e_dm2r ? Error on dm2r (5)
207-210 F4.1 d tdm2r ? Phase corresponding to dm2r
212-215 F4.1 d e_tdm2r ? Error on tdm2r (6)
217-221 F5.2 mag Dr4030 ? Magnitude difference between phases 30
and 40d post-explosion in the r band (4)
223-227 F5.3 mag e_Dr4030 ? Error on Dr4030
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Note (1): trise is considered to be the elapsed time between the date of
explosion and the date of maximum light
Note (2): This parameter captures the maximum rate at which the light curve
declines after peak
Note (3): This parameter gives an idea of how much the curvature of the
light-curve changes in the region where it changes the most
Note (4): The phases are chosen in order to capture the post-maximum behaviour
of both SN types. This parameter is similar to dm1 defined below in
the sense that it measures a slope of the light curve. We include it
here because it is easier to visualize and to measure when data are
sparse.
Note (5): The Monte Carlo method was used to obtain the errors for dm1 and dm2
Note (6): The errors in the dm phases are considered to be the maximum between
the error in the explosion epoch and the error obtained using the
Monte Carlo method
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Global Notes:
Note (G1): We use spectral matching tool SNID to derive an explosion date
(Supernova Identification software, Blondin & Tonry
2007ApJ...666.1024B 2007ApJ...666.1024B)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 16-Dec-2022