J/ApJ/933/14 LC analysis of type I superluminous SNe (Hosseinzadeh+, 2022)
Bumpy declining light curves are common in hydrogen-poor superluminous
supernovae.
Hosseinzadeh G., Berger E., Metzger B.D., Gomez S., Nicholl M.,
Blanchard P.
<Astrophys. J., 933, 14 (2022)>
=2022ApJ...933...14H 2022ApJ...933...14H
ADC_Keywords: Supernovae ; Photometry ; Spectra, optical
Keywords: Circumstellar matter ; Circumstellar shells ; Magnetars ;
Supernovae
Abstract:
Recent work has revealed that the light curves of hydrogen-poor
(TypeI) superluminous supernovae (SLSNe), thought to be powered by
magnetar central engines, do not always follow the smooth decline
predicted by a simple magnetar spin-down model. Here we present the
first systematic study of the prevalence and properties of "bumps" in
the post-peak light curves of 34 SLSNe. We find that the majority
(44%-76%) of events cannot be explained by a smooth magnetar model
alone. We do not find any difference in supernova properties between
events with and without bumps. By fitting a simple Gaussian model to
the light-curve residuals, we characterize each bump with an
amplitude, temperature, phase, and duration. We find that most bumps
correspond with an increase in the photospheric temperature of the
ejecta, although we do not see drastic changes in spectroscopic
features during the bump. We also find a moderate correlation
(ρ∼0.5; p∼0.01) between the phase of the bumps and the rise time,
implying that such bumps tend to happen at a certain "evolutionary
phase," (3.7±1.4)trise. Most bumps are consistent with having
diffused from a central source of variable luminosity, although
sources further out in the ejecta are not excluded. With this
evidence, we explore whether the cause of these bumps is intrinsic to
the supernova (e.g., a variable central engine) or extrinsic (e.g.,
circumstellar interaction). Both cases are plausible, requiring low-
level variability in the magnetar input luminosity, small decreases in
the ejecta opacity, or a thin circumstellar shell or disk.
Description:
Aside from published and publicly available photometry, we obtained
additional photometric observations of SNe 2017egm, 2018bym, 2018fcg,
2019neq, and 2019ujb. These data are listed in Table 3.
The majority of observations were taken in the gri bands using
KeplerCam on the 1.2m telescope at Fred Lawrence Whipple Observatory.
We also obtained three epochs of BVgri imaging of SN 2017egm using the
Sinistro camera on Las Cumbres Observatory's 1m telescope at McDonald
Observatory, one epoch of griz imaging of SN 2017egm using the
Templeton camera on the 1.3m McGraw-Hill Telescope at MDM Observatory,
and one epoch of r-band imaging of SN 2018bym (from the acquisition
image for our spectrum) using the Gemini Multi-object Spectrograph
(GMOS) on the Gemini-North telescope.
Throughout this work, BV magnitudes are in the Vega system and griz
magnitudes are in the AB system.
The two spectra of SN 2018bym plotted in Figure 9 are also presented here
for the first time. The first was obtained with the Blue Channel
spectrograph on the MMT telescope on 2018-09-09 (UT) and the second with
GMOS on Gemini-North.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 180 34 Final superluminous supernova (SLSN) sample
table3.dat 67 304 New photometry of 5 SLSNe
fig4.dat 113 33 Bump properties of 26 supernovae
sp/* . 2 The two spectra of SN 2018bym in ASCII format
as downloaded on WISeREP (http://www.wiserep.org/)
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+, 2016)
J/ApJ/696/870 : Catalina Real-time Transient Survey (CRTS) (Drake+, 2009)
J/other/Nat/474.484 : Light curves of 4 supernovae (Quimby+, 2011)
J/MNRAS/437/656 : SN PS1-11ap light curves (McCrum+, 2014)
J/ApJ/797/24 : Imaging observations of iPTF 13ajg (Vreeswijk+, 2014)
J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)
J/ApJ/836/25 : Swift UVOT light curves of ASASSN-15lh (Margutti+, 2017)
J/ApJ/835/58 : PTF 12dam & iPTF 13dcc follow-up (Vreeswijk+, 2017)
J/ApJ/860/100 : LCs of 26 hydrogen-poor superluminous SNe (De Cia+, 2018)
J/ApJ/852/81 : 17 PS1 superluminous SNe LCs + classif. sp. (Lunnan+, 2018)
J/ApJ/901/61 : LCs of 4 SLSNe from the ZTF survey (Lunnan+, 2020)
J/ApJ/902/L8 : Opt & NIR spectra of ZTF19aawfbtg (SN2019hge) (Yan+, 2020)
http://gsaweb.ast.cam.ac.uk/alerts : Gaia Photometric Science Alerts homepage
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Set Set (1)
3- 12 A10 --- Name Name of the SN
14 A1 --- f_Name Flag on Name (2)
16- 20 F5.3 --- z [0.03/0.87] Redshift
22- 141 A120 --- Ref Reference (3)
143-180 A38 --- ModRef MOSFiT model reference
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Note (1): Flag as follows:
g = gold sample (15 occurrences)
s = silver sample (11 occurrences)
c = control sample (8 occurrences)
Note (2): Flag as follows:
a = Light curves show two distinct bumps
b = Light curves show two distinct bumps and spectra show helium lines
c = Previously published under the name iPTF13dcc
d = Previously published under the name iPTF15esb
Note (3):
Public photometry sources :
Asteroid Terrestrial-impact Last Alert System :
ATLAS, 2018PASP..130f4505T 2018PASP..130f4505T
Cambridge Photometric Calibration Server :
CPCS, http://gsaweb.ast.cam.ac.uk/followup/)
Catalina Sky Survey :
CSS, 2009ApJ...696..870D 2009ApJ...696..870D
Gaia Photometric Science Alerts :
http://gsaweb.ast.cam.ac.uk/alerts
Panoramic Survey Telescope and Rapid Response System 1 :
PS1, 2016arXiv161205560C 2016arXiv161205560C
Swift Optical/Ultraviolet Supernova Archive :
SOUSA, 2014Ap&SS.354...89B 2014Ap&SS.354...89B
Zwicky Transient Facility
ZTF, 2019PASP..131a8002B 2019PASP..131a8002B
Photometry aggregators and brokers:
Finding Luminous and Exotic Extragalactic Transients
2020ApJ...904...74G 2020ApJ...904...74G
Make Alerts Really Simple :
https://mars.lco.global
Open Supernova Catalog :
2017ApJ...835...64G 2017ApJ...835...64G
Transient Name Server :
https://wis-tns.org
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Supernova name
12- 20 F9.3 d MJD Modified Julian Date of observation
(JD-2400000.5)
22 A1 --- Filt Filter (BVgriz)
24 A1 --- l_omag Upper limit flag on omag
27- 32 F6.3 mag omag [14.57/22.72] Apparent magnitude in Filt
34- 38 F5.3 mag e_omag [0.005/0.4]? Uncertainty in omag
40- 57 A18 --- Tel Telescope
59- 67 A9 --- Inst Instrument
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Byte-by-byte Description of file: fig4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Supernova name
12- 18 E7.1 W.d Eint [1e+40/1.4e+50] Bump integrated energy
(model independent)
20- 24 F5.3 --- Amp [0.16/3.3] Bump amplitude
26- 30 F5.3 --- e_Amp [0.01/2] Uncertainty in Amp
32- 38 F7.1 d MJDpk [54357.9/58890.2] Peak MJD of the bump
40- 43 F4.1 d e_MJDpk [0.3/81.1] Uncertainty in MJDpk
45- 49 F5.1 d FWHM [7.4/146] FWHM of the bump, observer frame
51- 54 F4.1 d e_FWHM [0.5/93] Uncertainty in FWHM
56- 62 E7.1 10-7J Ebump [1e+40/1.5e+50] Bump integrated energy
(model)
64- 70 E7.1 10-7J e_Ebump [1e+40/3.6e+49] Uncertainty in Ebump
72- 76 I5 d2 phase-dur [323/20622] Bump phase times bump duration,
rest frame
78- 82 I5 d2 e_phase-dur [39/16811] Uncertainty in phase-dur
84- 87 F4.1 kK Tbump [4.4/12.2] Bump temperature
89- 91 F3.1 kK e_Tbump [0.4/1.2] Uncertainty in Tbump
93- 97 F5.1 d phase [46.5/257] Bump phase, rest frame
99- 102 F4.1 d e_phase [0.4/58.1] Uncertainty in phase
104- 108 F5.1 d dur [6.4/104.6] Bump duration, rest frame
110- 113 F4.1 d e_dur [0.5/87.2] Uncertainty in dur
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History:
From electronic version of the journal for the tables
Spectra downloaded from WISeREP:
http://www.wiserep.org/search/spectra?name=2018bym
(End) Prepared by [AAS], Katia van der Woerd [CDS] 28-Mar-2024