J/A+A/683/A223ivo://CDS.VizieR/J/A+A/683/A223doi:10.26093/cds/vizier.36830223CDSSchulze S.Fransson C.Kozyreva A.Chen T.-W.Yaron O.Jerkstrand A.,Gal-Yam A.Sollerman J.Yan L.Kangas T.Leloudas G.Omand C.M.B.,Smartt S.J.Yang Y.Nicholl M.Sarin N.Yao Y.Brink T.G.Sharon A.,Rossi A.Chen P.Chen Z.Cikota A.De K.Drake A.J.Filippenko A.V.,Fremling C.Freour L.Fynbo J.P.U.Ho A.Y.Q.Inserra C.Irani I.,Kuncarayakti H.Lunnan R.Mazzali P.Ofek E.O.Palazzi E.Perley D.A.,Pursiainen M.Rothberg B.Shingles L.J.Smith K.Taggart K.,Tartaglia L.Zheng W.Anderson J.P.Cassara L.Christensen E.,Djorgovski S.G.Galbany L.Gkini A.Graham M.J.Gromadzki M.,Groom S.L.Hiramatsu D.Howell D.A.Kasliwal M.M.McCully C.,Mueller-Bravo T.E.Paiano S.Paraskeva E.Pessi P.J.Polishook D.,Rau A.Rigault M.Rusholme B.2024-11-07T20:01:51Z2024-03-21T10:05:50ZCDS support team

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

cds-question@unistra.frsupernovaeinfrared-photometryvisible-astronomybroad-band-photometryultraviolet-photometryStars with zero-age main sequence masses between 140 and 260 solar masses are thought to explode as pair-instability supernovae (PISNe). During their thermonuclear runaway, PISNe can produce up to several tens of solar masses of radioactive nickel, resulting in luminous transients similar to some superluminous supernovae (SLSNe). Yet, no unambiguous PISN has been discovered so far. SN 2018ibb is a hydrogen-poor SLSN at z=0.166 that evolves extremely slowly compared to the hundreds of known SLSNe. Between mid 2018 and early 2022, we monitored its photometric and spectroscopic evolution from the UV to the near-infrared (NIR) with 2-10m class telescopes. SN 2018ibb radiated >3*10^51^erg during its evolution, and its bolometric light curve reached >2*10^44^erg/s at its peak. The long-lasting rise of >93 rest-frame days implies a long diffusion time, which requires a very high total ejected mass. The PISN mechanism naturally provides both the energy source (Ni-56) and the long diffusion time. Theoretical models of PISNe make clear predictions as to their photometric and spectroscopic properties. SN 2018ibb complies with most tests on the light curves, nebular spectra and host galaxy, and potentially all tests with the interpretation we propose. Both the light curve and the spectra require 25-44 solar masses of freshly nucleosynthesised Ni-56, pointing to the explosion of a metal-poor star with a helium core mass of 120-130 solar masses at the time of death. This interpretation is also supported by the tentative detection of [CoII]-1.025um, which has never been observed in any other PISN candidate or SLSN before. We observe a significant excess in the blue part of the optical spectrum during the nebular phase, which is in tension with predictions of existing PISN models. However, we have compelling observational evidence for an eruptive mass-loss episode of the progenitor of SN 2018ibb shortly before the explosion, and our dataset reveals that the interaction of the SN ejecta with this oxygen-rich circumstellar material contributed to the observed emission. That may explain this specific discrepancy with PISN models. Powering by a central engine, such as a magnetar or a black hole, can be excluded with high confidence. This makes SN 2018ibb by far the best candidate for being a PISN, to date.2024A&A...683A.223Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/683/A223CatalogResearchIsServedByTAP VizieR generic servicerelated-tohttps://www.wiserep.org/object/10471 : SN 2018ibb Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/683/A223https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/683/A223http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/683/A223https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/683/A223https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/683/A223http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/683/A223GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVOpticalInfrareddefaultJ/A+A/683/A223/tablea1Multi-band photometryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTel/InstName of telescope and instrumentmeta.id;instrcharFilterFilter namemeta.id;instr.filtercharMJDModified Julian Datedtime.epochdoublemagApparent magnitude in Filter (1)magphot.magfloate_mag1-sigma error on apparent magnitudemagstat.error;phot.magfloatJ/A+A/683/A223/tablec1Bolometric light curve and blackbody propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhaseRest-frame days since peakdtime.phasefloatlogLbol? Bolometric luminosity (scale: log10)log(1e-07W)phys.luminosityfloatnullableE_logLbol? Upper 1-sigma error on bolometric luminositylog(1e-07W)stat.error;stat.maxfloatnullablee_logLbol? Lower 1-sigma error on bolometric luminositylog(1e-07W)stat.errorfloatnullablelogR? Blackbody radius (scale: log10) (1)log(cm)phys.size.radiuscharE_logR? Upper 1-sigma error on logRlog(cm)stat.error;stat.maxchare_logR? Lower 1-sigma error on logRlog(cm)stat.errorcharT? Blackbody temperature (2)Kphys.temperaturechare_T? 1-sigma error on blackbody temperatureKstat.errorchar