J/MNRAS/459/3939 Type II supernova light curves (Valenti+, 2016)
The diversity of Type II supernova versus the similarity in their progenitors.
Valenti S., Howell D.A., Stritzinger M.D., Graham M.L., Hosseinzadeh G.,
Arcavi I., Bildsten L., Jerkstrand A., Mccully C., Pastorello A.,
Piro A.L., Sand D., Smartt S.J., Terreran G., Baltay C., Benetti S.,
Brown P., Filippenko A.V., Fraser M., Rabinowitz D., Sullivan M., Yuan F.
<Mon. Not. R. Astron. Soc., 459, 3939-3962 (2016)>
=2016MNRAS.459.3939V 2016MNRAS.459.3939V (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry
Keywords: supernovae: general - supernovae: individual: SN 2013bu, SN 2013fs,
SN 2014cy, SN 2013ej, ASASSN-14ha, ASASSN-14gm, ASASSN-14dq,
SN 2013ab, SN 2013by, SN 2014G, LSQ13dpa, LSQ14gv, SN 2014G,
SN 2013ab, SN 2015W
Abstract:
High-quality collections of Type II supernova (SN) light curves are
scarce because they evolve for hundreds of days, making follow-up
observations time consuming and often extending over multiple
observing seasons. In light of these difficulties, the diversity of
SNe II is not fully understood. Here we present ultraviolet and
optical photometry of 12 SNe II monitored by the Las Cumbres
Observatory Global Telescope Network during 2013 to 2014, and compare
them with previously studied SNe having well-sampled light curves. We
explore SN II diversity by searching for correlations between the
slope of the linear light-curve decay after maximum light
(historically used to divide SNe II into IIL and IIP) and other
measured physical properties. While SNe IIL are found to be on average
more luminous than SNe IIP, SNe IIL do not appear to synthesize more
56Ni than SNe IIP. Finally, optical nebular spectra obtained for
several SNe in our sample are found to be consistent with models of
red supergiant progenitors in the 12-16M☉ range. Consequently,
SNe IIL appear not to account for the deficit of massive red
supergiants as SN II progenitors.
Description:
Between September 2012 and July 2013, LCOGT deployed eight 1m
telescopes around the world. Commissioning of the telescopes lasted
until 2014 March when the LCOGT network of telescopes become
operational (Brown et al. 2013). It was at this time we initiated our
programme to obtain detailed follow-up observations of SNe II. To
maximize the potential of the LCOGT network to contribute to our
understanding of SNe II, we selected to monitor all objects located
within 40 Mpc and having constraints on the explosion epoch of within
one week or less, or a blue featureless spectrum which is typical of
young SNe II. Objects selected for monitoring were discovered by
various transient search surveys, and our main criterion for selection
was the potential to collect data extending from soon after explosion
to at least the end of the plateau phase.
The sample consists of 16 bright SNe II discovered in 2013 and 2014.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 88 112 Sample of SNe type II
tabled2.dat 124 107 *Slope Data
tabled3.dat 90 39 *Bolometric light curve parameters
tabled4.dat 107 30 Bolometric MCMC light curve parameters
tabled5.dat 105 44 MCMC parameters on V band light curves
refs.dat 73 54 References
tabled1.dat 62 4556 Photometric Data for 12 SNe
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Note on tabled2.dat: The slope is computed with the following equation:
mag = M + s50 x t.
Note on tabled3.dat: The slope is computed with the following equation:
Log10(Lum(t)) = Log10(Lum(0)) + S1 x t.
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1 A1 --- LC [*] * indicates light curves in tabled1.dat
3- 13 A11 --- Name SN name
16- 20 F5.2 --- mu Distance modulus
22- 25 F4.2 --- e_mu rms uncertainty on mu
27 A1 --- r_mu Reference for mu, in refs.dat file
29- 38 F10.2 d Epoch Explosion epoch
40- 43 F4.1 d e_Epoch rms uncertainty on Epoch
45- 46 A2 --- r_Epoch Reference for Epoch, in refs.dat file
48- 51 F4.2 mag E(B-V)h Host redenning
53- 56 F4.2 mag e_E(B-V)h rms uncertainty on E(B-V)h
58- 59 A2 --- r_E(B-V)h Reference for E(B-V)h, in refs.dat file
61- 64 F4.2 mag E(B-V)MW Milky Way redenning
66- 88 A23 --- Host Host galaxy name
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Byte-by-byte Description of file: tabled2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name SN name
17- 21 F5.2 mag Vmag ?=- V magnitude at maximum light
23- 26 F4.2 mag e_Vmag ?=- rms uncertainty on Vmag
28- 35 F8.5 mag s50(V) ?=- Rise time in V band
36- 42 F7.5 mag e_s50(V) ?=- rms uncertainty on s50(V)
43- 46 F4.1 --- phstartV ?=- Starting day in V band
48- 51 F4.1 --- phstopV ?=- Ending day in V band
53- 57 F5.2 mag Rmag ?=- R magnitude at maximum light
59- 62 F4.2 mag e_Rmag ?=- rms uncertainty on Rmag
63 A1 --- n_Rmag [i] i for infinity
64- 71 F8.5 --- s50(R) ?=- Rise time in R band
72- 77 F6.4 --- e_s50(R) ?=- rms uncertainty on s50(R)
78 A1 --- n_s50(R) [i] i for infinity
79- 82 F4.1 --- phstartR ?=- Starting day in R band
84- 87 F4.1 --- phstopR ?=- Ending day in R band
89- 94 F6.2 mag Imag ?=- I magnitude at maximum light
96- 99 F4.2 mag e_Imag ?=- rms uncertainty in Imag
101-108 F8.5 --- s50(I) ?=- Rise time in I band
109-115 F7.5 --- e_s50(I) ?=- rms uncertainty on s50(I)
116-119 F4.1 --- phstartI ?=- Starting day in I band
121-124 F4.1 --- phstopI ?=- Ending day in I band
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Byte-by-byte Description of file: tabled3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name SN name
15- 19 F5.2 [Lsun] logL1(0) ?=- Luminosity of the initial, steeper slope
of the light curve (Log10(Lum1(0))
21- 27 F7.4 --- S1 ?=- Decline rate of the initial, steeper slope
of the light curve
29- 34 F6.4 --- e_S1 ?=- rms uncertainty on S1
35 A1 --- neS1 [i] i for infinity
36- 39 F4.1 d phstart1 ?=- Starting day of initial slope
41- 44 F4.1 d phstop1 ?=- Ending day of initial slope
46- 50 F5.2 [Lsun] logL2(0) ?=- Luminosity of the second, shallower slope
of the light curve (Log10(Lum2(0))
52- 58 F7.4 --- S2 ?=- Decline rate of the second, shallower slope
of the light curve
60- 65 F6.4 --- e_S2 ?=- rms uncertainty on S2
67- 70 F4.1 d phstart2 ?=- Starting day of second slope
72- 76 F5.1 d phstop2 ?=- Ending day of second slope
78- 83 F6.4 Msun MNi ?=- Ni mass
85- 90 F6.4 Msun e_MNi ?=- rms uncertainty on MNi
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Byte-by-byte Description of file: tabled4.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name SN name
16- 20 F5.1 --- Tpt Time of the drop (G1)
22- 25 F4.1 --- e_Tpt rms uncertainty on Tpt
27- 34 F8.5 --- A0 Depth of the drop (G1)
36- 42 F7.5 --- E_A0 Error on A0, upper value
44- 50 F7.5 --- e_A0 Error on A0, lower value
52- 58 F7.5 --- W0 Shape of the drop (G1)
60- 66 F7.5 --- E_W0 Error on W0, upper value
68- 74 F7.5 --- e_W0 Error on W0, lower value
76- 83 F8.5 --- M0 M0 parameter (G1)
85- 91 F7.5 --- E_M0 Error on M0, upper value
93- 99 F7.5 --- e_M0 Error on M0, lower value
101-107 F7.4 --- P0 P0 parameter (G1)
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Byte-by-byte Description of file: tabled5.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name SN name
16- 20 F5.1 --- tpt Time of the drop (G1)
22- 25 F4.1 --- e_tpt rms uncertainty on tpt
27- 33 F7.5 --- a0 Depth of the drop (G1)
35- 41 F7.5 --- E_a0 Error on a0, upper value
43- 49 F7.5 --- e_a0 Error on a0, lower value
51- 57 F7.5 --- w0 Shape of the drop (G1)
59- 65 F7.5 --- E_w0 Error on w0, upper value
67- 73 F7.5 --- e_w0 Error on w0, lower value
75- 82 F8.5 --- m0 m0 parameter (G1)
84- 90 F7.5 --- E_m0 Error on m0, upper value
92- 98 F7.5 --- e_m0 Error on m0, lower value
100-105 F6.4 --- p0 p0 parameter (G1)
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Ref Reference code
4- 22 A19 --- BibCode BibCode
24- 50 A27 --- Aut Author's name
52- 73 A22 --- Com Comment
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Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name SN name
14- 23 A10 "date" Date Observation date
25- 35 F11.3 d JD Julian date
36 A1 --- l_mag Limit flag on mag
37- 42 F6.3 mag mag Magnitude in Filter (1)
44- 48 F5.3 mag e_mag ?=- rms uncertainty on mag
50- 52 A3 --- Filter Filter (2)
54- 62 A9 --- Tel Telescope (3)
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Note (1): Data have not been corrected for extinction.
Note (2): Filters: UBVRI, um2, uw1, uw2 us, bs, vs, g+r, r, i ,z
Note (3): Telescopes as follows:
Swift = Swift Telescope
LSQ = LSQ, La Silla Quest, Chile
1m0-08 = 1m0-08 McDonald Observatory, USA
1m0-10 = 1m0-10, Sutherland, South Africa
1m0-12 = 1m0-12, Sutherland, South Africa
1m0-13 = 1m0-13, Sutherland, South Africa
1m0-04 = 1m0-04, Cerro Tololo, Chile
1m0-05 = 1m0-05, Cerro Tololo, Chile
1m0-09 = 1m0-09, Cerro Tololo, Chile
1m0-03 = 1m0-03, Siding Spring, Australia
1m0-11 = 1m0-11, Siding Spring, Australia
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Global notes:
Note (G1): The parameter tPT is obtained by fitting the SN light curve in
magnitudes around the fall from the plateau with the function
y(t) = -a0/[1+e^(t-tPT)/W0) + (P0 x t ) + M0
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Aug-2017