J/A+A/695/A142ivo://CDS.VizieR/J/A+A/695/A142doi:10.26093/cds/vizier.36950142CDSPessi 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.2026-08-28T11:35:08Z2025-07-25T09:51:07ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frsupernovaevisible-astronomysloan-photometryultraviolet-astronomyHydrogen-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.2025A&A...695A.142Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/695/A142CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/695/A142https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/695/A142http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/695/A142https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/695/A142https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/695/A142http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/695/A142GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/695/A142/tablea1 (ZTF SLSNe II sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/695/A142/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/695/A142/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/695/A142/tablea1?GETtext/xml+votable180.050000true176.76719.55080560.005555555555555556Cone search capability for table J/A+A/695/A142/tablea2 (ZTF contaminants sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/695/A142/tablea2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/695/A142/tablea2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/695/A142/tablea2?GETtext/xml+votable180.050000true257.278541726.85569440.0055555555555555566/2 447 602 2053 2335 2350 2617 3080 4319 4462 5507 5742 5925 6000 6109 6130 6336 6459 6515 6937 6961 7239 7252 8280 8285 8298 8619 8736 8745 8769 8960 9018 9563 9603 9662 9738 9815 9886 9978 10142 10163 10312 10463 10727 10878 11318 11366 11424 11508 11514 11591 11603 11719 11824 12028 12543 13067 13464 13745 13753 14972 14975 15777 15847 15884 17292 17423 17656 17680 18015 18063 18254 18398 18598 18649 18681 18709 18831 19076 19091 19383 19630 19808 19883 20003 20377 21207 22560 23034 23206 23296 24901 25052 25391 25669 26009 26096 26444 26618 26637 26696 27694 28041 28249 28262 29328 30015 31326 31418 32451 32504 36343 36719 36850 44865 49029 49032https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/695/A142?format=asciiUVOpticaldefaultJ/A+A/695/A142/tablea1ZTF SLSNe II sampleJ/A+A/695/A142/tablea2ZTF contaminants sampleJ/A+A/695/A142/tablea3ZTF forced photometryJ/A+A/695/A142/tablea4ATLAS forced photometryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIAUNameSN name (SN YYYYaaaa)meta.id;meta.maincharMJDModified Julian date of observationdtime.epochdoubleindexedFilter[oc] Filtermeta.id;instr.filtercharmagMagnitude in Filter (AB)magphot.magfloate_mag? Magnitude in Filter error (AB)magstat.error;phot.magfloatnullablel_mag[FT] Flag (1)meta.code.errorcharJ/A+A/695/A142/tablea5Swift forced photometryIAUNameSN name (SN YYYYaaaa)meta.id;meta.maincharFilter[UVW2 UVW1 UVM2] Filtermeta.id;instr.filtercharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian date of observationdtime.epochdoublemagMagnitude in Filter (AB)magphot.magfloate_mag? Magnitude in Filter error (AB)magstat.error;phot.magfloatnullableJ/A+A/695/A142/tablea6Light curve parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIAUNameSN name (SN YYYYaaaa)meta.id;meta.maincharFilter[gri] Observed filtermeta.id;instr.filtercharPeakMJD? Peak epoch MJDdtime.epochdoublenullablee_PeakMJD? Peak epoch MJD error (lower value)dstat.errorfloatnullableE_PeakMJD? Peak epoch MJD error (upper value)dstat.error;stat.maxfloatnullablePeakMAG? Peak absolute magnitudemagphys.magAbsfloatnullablee_PeakMAG? Peak absolute magnitude error (lower value)magstat.error;phot.magfloatnullableE_PeakMAG? Peak absolute magnitude error (upper value)magstat.error;stat.maxfloatnullabletrise10? Rise time, time interval between peak and 10% of the flux, t_rise,10%_dtime.epoch;stat.maxfloatnullabletrise1/e? Rise time, time interval between peak and 1/e of the flux, t_rise,1/e_dtime.epoch;stat.maxfloatnullabletdec1/e? Decline time, time interval between peak and 1/e of the flux, t_dec,1/e_dtime.epoch;stat.maxfloatnullabletdec10? Decline time, time interval between peak and 10% fo the flux, t_dec,10%_dtime.epoch;stat.maxfloatnullableJ/A+A/695/A142/tablea7Pseudo-Bolometric light curvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIAUNameSN name (SN YYYYaaaa)meta.id;meta.maincharMJDModified Julian date of observationdtime.epochdoublelog(Lbol)Bolometric luminositylog(1e-07W)phys.luminosityfloate_log(Lbol)Bolometric luminosity errorlog(1e-07W)stat.errorfloatlog(Lbol+UV+NIR)Bolometric + UV + NIR luminositylog(1e-07W)phys.luminosityfloate_log(Lbol+UV+NIR)Bolometric + UV + NIR luminosity errorlog(1e-07W)stat.errorfloatJ/A+A/695/A142/tablea8Estimated total radiated energy for events with available gri photometryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIAUNameSN name (SN YYYYaaaa)meta.id;meta.maincharl_logRELimit flag on logREmeta.code.errorcharlogRERadiated energylog(1e-07J)phys.energyfloat