J/A+A/695/A142 ZTF hydrogen-rich superluminous supernovae (Pessi+, 2025)
Sample of hydrogen-rich superluminous supernovae from the Zwicky Transient
Facility.
Pessi P.J., Lunnan R., Sollerman J., Schulze S., Gkini A., Gangopadhyay A.,
Yan L., Gal-yam A., Perley D.A., Chen T.-W., Hinds K.R., Brennan S.J.,
Hu Y., Singh A., Andreoni I., Cook D.O., Fremling C., Ho A.Y.Q., Sharma Y.,
Van Velzen S., Kangas T., Wold A., Bellm E.C., Bloom J.S., Graham M.J.,
Kasliwal M.M., Kulkarni S.R., Riddle R., Rusholme B.
<Astron. Astrophys. 695, A142 (2025)>
=2025A&A...695A.142P 2025A&A...695A.142P (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry, SDSS ; Optical ; Ultraviolet
Keywords: methods: data analysis - supernovae: general
Abstract:
Hydrogen-rich superluminous supernovae (SLSNe II) are rare. The exact
mechanism producing their extreme light curve peaks is not understood.
Analysis of single events and small samples suggest that circumstellar
material (CSM) interaction is the main mechanism responsible for the
observed features. However, other mechanisms cannot be discarded.
Large sample analysis can provide clarification.
We aim to characterize the light curves of a sample of 107 SLSNe II to
provide valuable information that can be used to validate theoretical
models.
We analyzed the gri light curves of SLSNe II obtained through ZTF. We
studied the peak absolute magnitudes and characteristic timescales.
When possible, we computed the g-r colors and pseudo-bolometric light
curves, and estimated lower limits for their total radiated energy. We
also studied the luminosity distribution of our sample and estimated
the fraction that would be observable by the LSST. Finally, we
compared our sample to other H-rich SNe and to H-poor SLSNe I.
SLSNe II are heterogeneous. Their median peak absolute magnitude is
~-20.3mag in optical bands. Their rise can take from ∼two weeks to
over three months, and their decline times range from ∼twenty days
to over a year. We found no significant correlations between peak
magnitude and timescales. SLSNe II tend to show fainter peaks, longer
declines, and redder colors than SLSNe I.
We present the largest sample of SLSN II light curves to date,
comprising 107 events. Their diversity could be explained by different
CSM morphologies, although theoretical analysis is needed to explore
alternative scenarios. Other luminous transients, such as active
galactic nuclei, tidal disruption events or SNe Ia-CSM, can easily
become contaminants. Thus, good multiwavelength light curve coverage
becomes paramount. LSST could miss ∼30% of the ZTF events in its gri
band footprint.
Description:
ZTF sample of SLSN-II, comprising 107 objects.
ZTF, ALTAS, Swift and pseudo-bolometric light curves, light curve
parameters and estimated total radiated energy are presented.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 118 107 ZTF SLSNe II sample
tablea2.dat 102 11 ZTF contaminants sample
tablea3.dat 36 20113 ZTF forced photometry
tablea4.dat 36 21662 ATLAS forced photometry
tablea5.dat 37 177 Swift forced photometry
tablea6.dat 80 321 Light curve parameters
tablea7.dat 44 2883 Pseudo-Bolometric light curves
tablea8.dat 19 39 Estimated total radiated energy for events with
available gri photometry
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Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- ZTFName ZTF name (YYYYaaaaaaa)
15- 25 A11 --- IAUName IAU name (SN YYYYaaaa)
27- 28 I2 h RAh Right ascension (J2000)
30- 31 I2 min RAm Right ascension (J2000)
33- 37 F5.2 s RAs Right ascension (J2000)
39 A1 --- DE- Declination sign (J2000)
40- 41 I2 deg DEd Declination (J2000)
43- 44 I2 arcmin DEm Declination (J2000)
46- 50 F5.2 arcsec DEs Declination (J2000)
52- 56 F5.3 --- z Heliocentric redshift
58- 62 F5.3 mag AV Landolt V band absorption value obtained
from NED
64- 82 A19 --- RefDiscov Discovery reference
84-102 A19 --- RefClass Classification reference
104-106 A3 --- LCZFT [ZTF] indicates light curve data in tablea3
108-112 A5 --- LCATLAS [ATLAS] indicates light curve data in tablea4
114-118 A5 --- LCSwift [Swift] indicates light curve data in tablea5
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IAUName IAU name (SN YYYYaaaa)
14- 21 F8.2 d MJD Modified Julian date of observation
23 A1 --- Filter [gri] Filter
25- 29 F5.2 mag mag Magnitude in Filter (AB)
31- 34 F4.2 mag e_mag ?=- Magnitude in Filter error (AB)
36 A1 --- l_mag [FT] Flag (1)
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Note (1): Flag as follows:
F = real detection
T = upper limit
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IAUName SN name (SN YYYYaaaa)
14- 21 F8.2 d MJD Modified Julian date of observation
23 A1 --- Filter [oc] Filter
25- 29 F5.2 mag mag Magnitude in Filter (AB)
31- 34 F4.2 mag e_mag ?=- Magnitude in Filter error (AB)
36 A1 --- l_mag [FT] Flag (1)
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Note (1): Flag as follows:
F = real detection
T = upper limit
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IAUName SN name (SN YYYYaaaa)
14- 21 F8.2 d MJD Modified Julian date of observation
23- 26 A4 --- Filter [UVW2 UVW1 UVM2] Filter
28- 32 F5.2 mag mag Magnitude in Filter (AB)
34- 37 F4.2 mag e_mag ?=- Magnitude in Filter error (AB)
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Byte-by-byte Description of file: tablea6.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IAUName SN name (SN YYYYaaaa)
14 A1 --- Filter [gri] Observed filter
16- 23 F8.2 d PeakMJD ?=- Peak epoch MJD
25- 29 F5.2 d e_PeakMJD ? Peak epoch MJD error (lower value)
31- 36 F6.2 d E_PeakMJD ? Peak epoch MJD error (upper value)
38- 43 F6.2 mag PeakMAG ?=- Peak absolute magnitude
45- 48 F4.2 mag e_PeakMAG ? Peak absolute magnitude error (lower value)
50- 53 F4.2 mag E_PeakMAG ? Peak absolute magnitude error (upper value)
55- 59 F5.2 d trise10 ?=- Rise time, time interval between peak and
10% of the flux, trise,10%
61- 66 F6.2 d trise1/e ?=- Rise time, time interval between peak and
1/e of the flux, trise,1/e
68- 73 F6.2 d tdec1/e ?=- Decline time, time interval between peak
and 1/e of the flux, tdec,1/e
75- 80 F6.2 d tdec10 ?=- Decline time, time interval between peak
and 10% fo the flux, tdec,10%
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Byte-by-byte Description of file: tablea7.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IAUName SN name (SN YYYYaaaa)
15- 22 F8.2 d MJD Modified Julian date of observation
24- 28 F5.2 [10-7W] log(Lbol) Bolometric luminosity
30- 33 F4.2 [10-7W] e_log(Lbol) Bolometric luminosity error
35- 39 F5.2 [10-7W] log(Lbol+UV+NIR) Bolometric + UV + NIR luminosity
41- 44 F4.2 [10-7W] e_log(Lbol+UV+NIR) Bolometric + UV + NIR luminosity error
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Byte-by-byte Description of file: tablea8.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IAUName SN name (SN YYYYaaaa)
13 A1 --- l_logRE Limit flag on logRE
15- 19 F5.2 [10-7J] logRE Radiated energy
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History:
Copied at https://zenodo.org/records/14711673
(End) Patricia Vannier [CDS] 26-May-2025