A puzzle solved after two decades: SN 2002gh among the brightest of superluminous supernovae

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dc.contributor.authorCartier, Regis
dc.contributor.authorHamuy, Mario
dc.contributor.authorContreras, Carlos
dc.contributor.authorAnderson, Joseph P.
dc.contributor.authorPhillips, Mark M.
dc.contributor.authorMorrell, Nidia
dc.contributor.authorStritzinger, Maximilian D.
dc.contributor.authorHueichapan, Emilio D.
dc.contributor.authorClocchiatti, Alejandro
dc.contributor.authorRoth, Miguel
dc.contributor.authorThomas-Osip, Joanna
dc.contributor.authorGonzalez, Luis E.
dc.date.accessioned2025-01-20T21:05:14Z
dc.date.available2025-01-20T21:05:14Z
dc.date.issued2022
dc.description.abstractWe present optical photometry and spectroscopy of the superluminous SN 2002gh from maximum light to +204 d, obtained as part of the Carnegie Type II Supernova (CATS) project. SN 2002gh is among the most luminous discovered supernovae ever, yet it remained unnoticed for nearly two decades. Using Dark Energy Camera archival images we identify the potential supernova (SN) host galaxy as a faint dwarf galaxy, presumably having low metallicity, and in an apparent merging process with other nearby dwarf galaxies. We show that SN 2002gh is among the brightest hydrogen-poor SLSNe with M-V = -22.40 +/- 0.02, with an estimated peak bolometric luminosity of 2.6 +/- 0.1 x 10(44) erg s(-1). We discount the decay of radioactive nickel as the main SN power mechanism, and assuming that the SN is powered by the spin-down of a magnetar we obtain two alternative solutions. The first case, is characterized by significant magnetar power leakage, and M-ej between 0.6 and 3.2 M-circle dot, P-spin = 3.2 ms, and B = 5 x 10(13) G. The second case does not require power leakage, resulting in a huge ejecta mass of about 30 M-circle dot, a fast spin period of P-spin similar to 1 ms, and B similar to 1.6 x 10(14) G. We estimate a zero-age main-sequence mass between 14 and 25 M-circle dot for the first case and of about 135 M-circle dot for the second case. The latter case would place the SN progenitor among the most massive stars observed to explode as an SN.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stac1371
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stac1371
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93296
dc.identifier.wosidWOS:000813872600006
dc.issue.numero2
dc.language.isoen
dc.pagina.final2649
dc.pagina.inicio2627
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectsupernovae: general
dc.subjectsupernovae: individual: SN2002gh
dc.titleA puzzle solved after two decades: SN 2002gh among the brightest of superluminous supernovae
dc.typeartículo
dc.volumen514
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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