J/ApJ/860/100 LCs of 26 hydrogen-poor superluminous SNe (De Cia+, 2018)
Light curves of hydrogen-poor superluminous supernovae from the Palomar
Transient Factory.
De Cia A., Gal-Yam A., Rubin A., Leloudas G., Vreeswijk P., Perley D.A.,
Quimby R., Yan L., Sullivan M., Flors A., Sollerman J., Bersier D.,
Cenko S.B., Gal-Yam M., Maguire K., Ofek E.O., Prentice S., Schulze S.,
Spyromilio J., Valenti S., Arcavi I., Corsi A., Howell D.A., Mazzali P.,
Kasliwal M.M., Taddia F., Yaron O.
<Astrophys. J., 860, 100 (2018)>
=2018ApJ...860..100D 2018ApJ...860..100D
ADC_Keywords: Supernovae; Photometry, SDSS; Photometry, ultraviolet; Redshifts
Keywords: supernovae: general
Abstract:
We investigate the light-curve properties of a sample of 26
spectroscopically confirmed hydrogen-poor superluminous supernovae
(SLSNe-I) in the Palomar Transient Factory survey. These events are
brighter than SNe Ib/c and SNe Ic-BL, on average, by about 4 and 2mag,
respectively. The peak absolute magnitudes of SLSNe-I in rest-frame g
band span -22≲Mg≲-20mag, and these peaks are not powered by
radioactive 56Ni, unless strong asymmetries are at play. The rise
timescales are longer for SLSNe than for normal SNe Ib/c, by roughly
10 days, for events with similar decay times. Thus, SLSNe-I can be
considered as a separate population based on photometric properties.
After peak, SLSNe-I decay with a wide range of slopes, with no obvious
gap between rapidly declining and slowly declining events. The latter
events show more irregularities (bumps) in the light curves at all
times. At late times, the SLSN-I light curves slow down and cluster
around the 56Co radioactive decay rate. Powering the late-time light
curves with radioactive decay would require between 1 and 10M☉
of Ni masses. Alternatively, a simple magnetar model can reasonably
fit the majority of SLSNe-I light curves, with four exceptions, and
can mimic the radioactive decay of 56Co, up to ∼400days from
explosion. The resulting spin values do not correlate with the
host-galaxy metallicities. Finally, the analysis of our sample cannot
strengthen the case for using SLSNe-I for cosmology.
Description:
The 26 SLSNe discussed in this paper are all the hydrogen-poor SLSNe
discovered between 2009 and 2013 by the (i)PTF survey (PTF mounted on
the Palomar Observatory 48-inch Samuel Oschin Telescope (P48), in
California). The sample is shown in Table 1. The PTF SLSNe in our
sample have been spectroscopically classified as SLSNe-I by
Quimby+ (2018ApJ...855....2Q 2018ApJ...855....2Q).
Follow-up imaging was obtained with the Palomar 60-inch telescope
(P60). The filters employed for our observations are Johnson B, Kron R
(similar to Cousins RC), Sloan i' and z', and Gunn g.
We observed PTF SLSNe at late times using the Low-Resolution Imaging
Spectrometer (LRIS) on the Keck I telescope.
Follow-up imaging was also obtained with the 2m robotic Liverpool
Telescope (LT) at the Roque de los Muchachos Observatory on La Palma,
Spain, with the RATCAM and IO:O optical imagers in g, r, and i filters
(similar to SDSS).
The LCO (Las Cumbres Observatory) data have been reduced and PSF
magnitudes were computed on the subtracted images and transformed to
the standard SDSS filter system (for gri).
We imaged several of the SLSNe in our sample with the Large Monolithic
Imager (LMI) mounted on the 4.3m Discovery Channel Telescope (DCT) in
Happy Jack, AZ.
A number of supernovae in our sample were observed with the
UltraViolet/Optical Telescope (UVOT) on board the Swift Gamma-Ray
Burst Explorer.
Follow-up imaging was obtained with the Palomar 200-inch Hale
Telescope with the LFC (Palomar P200/Large Format Camera).
The SLSNe iPTF 13dcc and iPTF 13ehe were observed with the Advanced
Camera for Surveys in the Wide Field Channel on board the HST with the
F625W filter, as part of the GO-13858 program (PI A. De Cia).
We complement the photometric data set of the SLSNe in our sample with
the data published in Quimby+ (2011, J/other/Nat/474.484),
Pastorello+ (2010ApJ...724L..16P 2010ApJ...724L..16P), Inserra+ (2013ApJ...770..128I 2013ApJ...770..128I),
Nicholl+ (2013Natur.502..346N 2013Natur.502..346N), Chen+ (2015MNRAS.452.1567C 2015MNRAS.452.1567C), and
Vreeswijk+ (2014, J/ApJ/797/24).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 46 26 The PTF sample of 26 hydrogen-poor SLSNe
table3.dat 31 26 Radiated energy and nickel mass estimates from
the peak luminosity and the late-time decay
table9.dat 160 27 Kgr corrections
table10.dat 160 27 Kri corrections
table11.dat 51 2069 PTF photometry data
table12.dat 56 1404 PTF rest-frame g photometry data
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See also:
II/313 : Palomar Transient Factory (PTF) photometric catalog 1.0 (Ofek+, 2012)
J/ApJ/736/159 : Photometry monitoring of the SN PTF10vdl (Gal-Yam+, 2011)
J/other/Nat/491.228 : Light curves of 2 superluminous supernovae (Cooke+, 2012)
J/ApJ/763/42 : X-ray emission from 28 SNe (IIn, Ibn, SLSN-I) (Ofek+, 2013)
J/MNRAS/444/3258 : Velocities and EW of PTF SNe Ia (Maguire+, 2014)
J/ApJ/788/154 : Palomar Transient Factory SNe IIn photometry (Ofek+, 2014)
J/ApJ/781/42 : Optical photometry of SN 2010jl (Ofek+, 2014)
J/ApJ/797/24 : Imaging observations of iPTF 13ajg (Vreeswijk+, 2014)
J/MNRAS/446/3895 : The rising light curves of Type Ia supernovae (Firth+, 2015)
J/MNRAS/448/1206 : Superluminous supernovae in faint galaxies (McCrum+, 2015)
J/A+A/574/A60 : Light curve templates of SNe Ib/c from SDSS (Taddia+, 2015)
J/ApJ/830/13 : Host NUV-NIR data of 32 superluminous SNe (Perley+, 2016)
J/ApJ/820/33 : R-band light curves of type II supernovae (Rubin+, 2016)
J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)
J/ApJ/835/58 : PTF 12dam & iPTF 13dcc follow-up (Vreeswijk+, 2017)
J/ApJ/852/81 : 17 PS1 superluminous SNe LCs + classif. (Lunnan+, 2018)
J/A+A/609/A106 : PTF11mnb Bgri light curves (Taddia+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- PTF PTF identifier
8- 9 I2 h RAh Hour of right ascension (J2000)
11- 12 I2 min RAm Minute of right ascension (J2000)
14- 18 F5.2 s RAs Second of right ascension (J2000)
20 A1 --- DE- Sign of declination (J2000)
21- 22 I2 deg DEd Degree of declination (J2000)
24- 25 I2 arcmin DEm Arcminute of declination (J2000)
27- 30 F4.1 arcsec DEs Arcsecond of declination (J2000)
32- 37 F6.4 --- z [0.05/0.8] Redshift
39- 41 A3 --- Type Type
43- 46 F4.2 mag Av [0.02/1.5] Galactic foreground extinction
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- PTF PTF identifier
8- 11 F4.1 [10-7W] logLbol [43.4/44.6] log of the bolometric peak
luminosity
13- 14 A2 --- l_logErad [≥] Limit flag on logErad
15- 18 F4.1 10-7J logErad [49.3/51.3] log of radiated energy
20- 21 A2 --- l_MNipk [≤] Limit flag on MNipk
22- 25 F4.1 Msun MNipk [3.4/49.5] Nickel mass estimate from
the peak luminosity
27- 28 A2 --- l_MNid [≤] Limit flag on MNid
29- 31 F3.1 Msun MNid [0.8/9.7]? Nickel mass estimate from
the late-time decay
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- ID [-25/321] Supernova identifier
6- 10 F5.2 mag 09as [-0.3/0] Kgr correction for 09as; z=0.1864
12- 16 F5.2 mag 09atu [-0.5/-0.3] Kgr correction for 09atu; z=0.5014
18- 22 F5.2 mag 09cnd [-0.4/-0.1] Kgr correction for 09cnd; z=0.2585
24- 28 F5.2 mag 09cwl [-0.4/-0.3] Kgr correction for 09cwl; z=0.3502
30- 34 F5.2 mag 10aagc [-0.3/-0.04] Kgr correction for 10aagc; z=0.2067
36- 40 F5.2 mag 10bfz [-0.3/0.04] Kgr correction for 10bfz; z=0.1699
42- 46 F5.2 mag 10bjp [-0.4/-0.3] Kgr correction for 10bjp; z=0.3585
48- 52 F5.2 mag 10cwr [-0.3/-0.08] Kgr correction for 10cwr; z=0.2301
54- 58 F5.2 mag 10hgi [-0.2/0.2] Kgr correction for 10hgi; z=0.0982
60- 64 F5.2 mag 10nmn [-0.2/0.2] Kgr correction for 10nmn; z=0.1236
66- 70 F5.2 mag 10uhf [-0.4/-0.1] Kgr correction for 10uhf; z=0.2879
72- 76 F5.2 mag 10vqv [-0.5/-0.3] Kgr correction for 10vqv; z=0.4520
78- 82 F5.2 mag 10vwg [-0.3/-0.01] Kgr correction for 10vwg; z=0.1901
84- 88 F5.2 mag 11dij [-0.2/0.2] Kgr correction for 11dij; z=0.1429
90- 94 F5.2 mag 11hrq [-0.2/0.3] Kgr correction for 11hrq; z=0.0571
96-100 F5.2 mag 11rks [-0.3/-0.01] Kgr correction for 11rks; z=0.1924
102-106 F5.2 mag 12dam [-0.2/0.2] Kgr correction for 12dam; z=0.1075
108-112 F5.2 mag 12gty [-0.3/0.02] Kgr correction for 12gty; z=0.1768
114-118 F5.2 mag 12hni [-0.2/0.2] Kgr correction for 12hni; z=0.1056
120-124 F5.2 mag 12mxx [-0.4/-0.2] Kgr correction for 12mxx; z=0.3274
126-130 F5.2 mag 13ajg [-0.9/-0.1] Kgr correction for 13ajg; z=0.7403
132-136 F5.2 mag 13bdl [-0.4/-0.3] Kgr correction for 13bdl; z=0.4030
138-142 F5.2 mag 13bjz [-0.4/-0.1] Kgr correction for 13bjz; z=0.2712
144-148 F5.2 mag 13cjq [-0.4/-0.3] Kgr correction for 13cjq; z=0.3962
150-154 F5.2 mag 13dcc [-0.4/-0.3] Kgr correction for 13dcc; z=0.4308
156-160 F5.2 mag 13ehe [-0.4/-0.2] Kgr correction for 13ehe; z=0.3434
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Byte-by-byte Description of file: table10.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- ID [-25/321] Supernova identifier
6- 10 F5.2 mag 09as [-0.2/-0.1] Kri correction for 09as; z=0.1864
12- 16 F5.2 mag 09atu [-0.7/-0.4] Kri correction for 09atu; z=0.5014
18- 22 F5.2 mag 09cnd [-0.3/-0.2] Kri correction for 09cnd; z=0.2585
24- 28 F5.2 mag 09cwl [-0.5/-0.2] Kri correction for 09cwl; z=0.3502
30- 34 F5.2 mag 10aagc [-0.2/-0.1] Kri correction for 10aagc; z=0.2067
36- 40 F5.2 mag 10bfz [-0.2/-0.1] Kri correction for 10bfz; z=0.1699
42- 46 F5.2 mag 10bjp [-0.5/-0.3] Kri correction for 10bjp; z=0.3585
48- 52 F5.2 mag 10cwr [-0.3/-0.2] Kri correction for 10cwr; z=0.2301
54- 58 F5.2 mag 10hgi [-0.3/-0.05] Kri correction for 10hgi; z=0.0982
60- 64 F5.2 mag 10nmn [-0.3/-0.08] Kri correction for 10nmn; z=0.1236
66- 70 F5.2 mag 10uhf [-0.3/-0.22] Kri correction for 10uhf; z=0.2879
72- 76 F5.2 mag 10vqv [-0.7/-0.4] Kri correction for 10vqv; z=0.4520
78- 82 F5.2 mag 10vwg [-0.2/-0.1] Kri correction for 10vwg; z=0.1901
84- 88 F5.2 mag 11dij [-0.3/-0.09] Kri correction for 11dij; z=0.1429
90- 94 F5.2 mag 11hrq [-0.2/0.02] Kri correction for 11hrq; z=0.0571
96-100 F5.2 mag 11rks [-0.2/-0.1] Kri correction for 11rks; z=0.1924
102-106 F5.2 mag 12dam [-0.3/-0.06] Kri correction for 12dam; z=0.1075
108-112 F5.2 mag 12gty [-0.2/-0.1] Kri correction for 12gty; z=0.1768
114-118 F5.2 mag 12hni [-0.3/-0.06] Kri correction for 12hni; z=0.1056
120-124 F5.2 mag 12mxx [-0.4/-0.2] Kri correction for 12mxx; z=0.3274
126-130 F5.2 mag 13ajg [-1/-0.4] Kri correction for 13ajg; z=0.7403
132-136 F5.2 mag 13bdl [-0.6/-0.3] Kri correction for 13bdl; z=0.4030
138-142 F5.2 mag 13bjz [-0.3/-0.2] Kri correction for 13bjz; z=0.2712
144-148 F5.2 mag 13cjq [-0.6/-0.3] Kri correction for 13cjq; z=0.3962
150-154 F5.2 mag 13dcc [-0.6/-0.3] Kri correction for 13dcc; z=0.4308
156-160 F5.2 mag 13ehe [-0.5/-0.2] Kri correction for 13ehe; z=0.3434
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- PTF Supernova PTF identifier
8- 16 F9.3 d MJD [54910.4/57070] Modified Julian Date
18- 24 F7.2 d Phase [-104/716] Phase; rest-frame days
with respect to peak
26- 30 F5.2 mag mag [16.4/25.3] Apparent AB magnitude in Filter (1)
32- 35 F4.2 mag e_mag [0.01/0.7] Uncertainty in mag
37- 40 A4 --- Filt Filter used
42- 51 A10 --- Tel Telescope identifier (G1)
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Note (1): The UV photometry fom Swift was not corrected from host-galaxy
contribution, but this should be minimal (see Sect. 3.7).
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Byte-by-byte Description of file: table12.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- PTF Supernova PTF identifier
8- 16 F9.3 d MJD [54918.1/57070] Modified Julian Date
18- 24 F7.2 d Phase [-104/716] Phase; rest-frame days
with respect to peak
26- 30 F5.2 mag gmag [16.8/26.4] Apparent g band AB magnitude
32- 35 F4.2 mag e_gmag [0.01/0.6] Uncertainty in gmag
37- 42 F6.2 mag gMag [-22.7/-13.2] Absolute rest-frame g band
AB magnitude (1)
44- 52 A9 --- Tel Telescope identifier (G1)
54- 56 A3 --- Ref Reference code (2)
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Note (1): The absolute magnitudes in rest-frame g-band are derived from
gMag = rmag - DM - Kgr, where DM is the distance modulus, rmag is
corrected for foreground Galactic extinction (Table 1), and Kgr is
the k-correction (Table C2), as described in Sect. 3.12.
Note (2): Reference code as follows:
I = Quimby et al. (2011Natur.474..487Q 2011Natur.474..487Q);
II = Pastorello et al. (2010ApJ...724L..16P 2010ApJ...724L..16P);
III = Inserra et al. (2013ApJ...770..128I 2013ApJ...770..128I);
IV = Nicholl et al. (2013Natur.502..346N 2013Natur.502..346N),
Chen et al. (2015MNRAS.452.1567C 2015MNRAS.452.1567C);
V = Vreeswijk et al. (2014, J/ApJ/797/24).
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Global Note:
Note (G1): Telescope as follows:
p48 = Palomar 48 inch telescope;
p60 = Palomar 60 inch telescope;
Swift/UVOT = Gehrels Swift UltraViolet/Optical Telescope;
Keck = Keck I 10m telescope;
p200 = Palomar 200 inch Hale telescope;
LT = Liverpool 2m Telescope;
LCOGT = Las Cumbres Observatory;
DCT = Discovery Channel 4.3m Telescope;
HST = Hubble Space Telescope;
PS1 = Pan-STARRS1 Medium Deep Survey in Lunnan+, 2018, J/ApJ/852/81
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 04-Jul-2019