J/A+A/695/A29ivo://CDS.VizieR/J/A+A/695/A29doi:10.26093/cds/vizier.36950029CDSSalmaso I.Cappellaro E.Tartaglia L.Anderson J.P.Benetti S.,Bronikowski M.Cai Y.-Z.Charalampopoulos P.Chen T.-W.Concepcion E.,Elias-Rosa N.Galbany L.Gromadzki M.Gutierrez C.P.Kankare E.,Lundqvist P.Matilainen K.Mazzali P.A.Moran S.Mueller-Bravo T.E.,Nicholl M.Pastorello A.Pessi P.J.Pessi T.Petrushevska T.,Pignata G.Reguitti A.Sollerman J.Srivastav S.Stritzinger M.,Tomasella L.Valerin G.2025-05-21T20:02:47Z2025-02-27T09:55:57ZCDS support team

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

cds-question@unistra.frsupernovaevisible-astronomybroad-band-photometryinfrared-photometryultraviolet-photometryspectroscopyAt late stages, massive stars experience strong mass-loss rates, losing their external layers and thus producing a dense H-rich circumstellar medium (CSM). After the explosion of a massive star, the collision and continued interaction of the supernova (SN) ejecta with the CSM power the SN light curve through the conversion of kinetic energy into radiation. When the interaction is strong, the light curve shows a broad peak and high luminosity that lasts for several months. For these SNe, the spectral evolution is also slower compared to non-interacting SNe. Notably, energetic shocks between the ejecta and the CSM create the ideal conditions for particle acceleration and the production of high-energy (HE) neutrinos above 1TeV. We study four strongly-interacting Type IIn SNe: 2021acya, 2021adxl, 2022qml, and 2022wed to highlight their peculiar characteristics, derive the kinetic energy of the explosion and the characteristics of the CSM, infer clues on the possible progenitors and their environment and relate them to the production of HE neutrinos. We analysed spectro-photometric data of a sample of interacting SNe to determine their common characteristics and derive physical properties (radii and masses) of the CSM and ejecta kinetic energies to compare them to HE neutrino production models. The SNe analysed in this sample exploded in dwarf, star-forming galaxies and they are consistent with energetic explosions and strong interaction with the surrounding CSM. For SNe 2021acya and 2022wed, we find high CSM masses and mass-loss rates, linking them to very massive progenitors. For SN 2021adxl, the spectral analysis and less extreme CSM mass suggest a stripped-envelope massive star as possible progenitor. SN 2022qml is marginally consistent with being a Type Ia thermonuclear explosion embedded in a dense CSM. The mass-loss rates for all SNe are consistent with the expulsion of several solar masses of material during eruptive episodes in the last few decades before the explosion. Finally, we find that the SNe in our sample are marginally consistent with HE neutrino production.2025A&A...695A..29Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/695/A29CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/695/A29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/695/A29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/695/A29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/695/A29https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/695/A29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/695/A29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVOpticalInfrareddefaultJ/A+A/695/A29/ph21acyaPhotometry of SN 2021acya (table C1)l_magLimit flag on magmeta.code.errorcharbandBand (1)instr.bandpasscharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoublemagMagnitude in Bandmagphot.magfloate_mag? Error of magnitude in Bandmagstat.error;phot.magfloatnullableTelTelescope, instrumentinstrcharJ/A+A/695/A29/ph21adxlPhotometry of SN 2021adxl (table C2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoublebandBand (1)instr.bandpasscharl_magLimit flag on magmeta.code.errorcharmagMagnitude in Bandmagphot.magfloate_mag? Error of magnitude in Bandmagstat.error;phot.magfloatnullableTelTelescope, instrumentinstrcharJ/A+A/695/A29/ph22qmlPhotometry of SN 2022qml (table C3)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoublebandBand (1)instr.bandpasscharl_magLimit flag on magmeta.code.errorcharmagMagnitude in Bandmagphot.magfloate_mag? Error of magnitude in Bandmagstat.error;phot.magfloatnullableTelTelescope, instrumentinstrcharJ/A+A/695/A29/ph22wedPhotometry of SN 2022wed (table C4)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoublebandBand (1)instr.bandpasscharl_magLimit flag on magmeta.code.errorcharmagMagnitude in Bandmagphot.magfloate_mag? Error of magnitude in Bandmagstat.error;phot.magfloatnullableTelTelescope, instrumentinstrcharJ/A+A/695/A29/ha21acyaFit on the Halpha for SN 2021acya (table C9)ResFWHM resolution0.1nmspect.resolutionfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHanHalpha narrow wavelength0.1nmem.wlfloatFWHMHanHalpha narrow FWHM0.1nmspect.line.widthfloatFluxHanHalpha narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatlambdaHabHalpha broad wavelength0.1nmem.wlfloatFWHMHabHalpha broad FWHM0.1nmspect.line.widthfloatFluxHabFlux Halpha broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatJ/A+A/695/A29/ha21adxlFit on the Halpha for SN 2021adxl (table C11)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHanHalpha narrow wavelength0.1nmem.wlfloatFWHMHanHalpha narrow FWHM0.1nmspect.line.widthfloatFluxHanHalpha narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatlambdaHabHalpha broad wavelength0.1nmem.wlfloatFWHMHabHalpha broad FWHM0.1nmspect.line.widthfloatFluxHabFlux Halpha broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/ha22qmlFit on the Halpha for SN 2022qml (table C13)ResFWHM resolution0.1nmspect.resolutionfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHanHalpha narrow wavelength0.1nmem.wlfloatFWHMHanHalpha narrow FWHM0.1nmspect.line.widthfloatFluxHanHalpha narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatlambdaHabHalpha broad wavelength0.1nmem.wlfloatFWHMHabHalpha broad FWHM0.1nmspect.line.widthfloatFluxHabFlux Halpha broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatJ/A+A/695/A29/ha22wedFit on the Halpha for SN 2022wed (table C15)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHanHalpha narrow wavelength0.1nmem.wlfloatFWHMHanHalpha narrow FWHM0.1nmspect.line.widthfloatFluxHanHalpha narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatlambdaHabHalpha broad wavelength0.1nmem.wlfloatFWHMHabHalpha broad FWHM0.1nmspect.line.widthfloatFluxHabFlux Halpha broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HalphafloatResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/hb21acyaFit on the Hbeta for SN 2021acya (table C10)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHbn? Hbeta narrow wavelength0.1nmem.wlfloatnullableFWHMHbn? Hbeta narrow FWHM0.1nmspect.line.widthfloatnullableFluxHbn? Hbeta narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullablelambdaHbb? Hbeta broad wavelength0.1nmem.wlfloatnullableFWHMHbb? Hbeta broad FWHM0.1nmspect.line.widthfloatnullableFluxHbb? Hbeta broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullableResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/hb21adxlFit on the Hbeta for SN 2021adxl (table C12)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHbn? Hbeta narrow wavelength0.1nmem.wlfloatnullableFWHMHbn? Hbeta narrow FWHM0.1nmspect.line.widthfloatnullableFluxHbn? Hbeta narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullablelambdaHbb? Hbeta broad wavelength0.1nmem.wlfloatnullableFWHMHbb? Hbeta broad FWHM0.1nmspect.line.widthfloatnullableFluxHbb? Hbeta broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullableResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/hb22qmlFit on the Hbeta for SN 2022qml (table C14)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHbn? Hbeta narrow wavelength0.1nmem.wlfloatnullableFWHMHbn? Hbeta narrow FWHM0.1nmspect.line.widthfloatnullableFluxHbn? Hbeta narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullablelambdaHbb? Hbeta broad wavelength0.1nmem.wlfloatnullableFWHMHbb? Hbeta broad FWHM0.1nmspect.line.widthfloatnullableFluxHbb? Hbeta broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullableResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/hb22wedFit on the Hbeta for SN 2022wed (table C16)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintlambdaHbn? Hbeta narrow wavelength0.1nmem.wlfloatnullableFWHMHbn? Hbeta narrow FWHM0.1nmspect.line.widthfloatnullableFluxHbn? Hbeta narrow flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullablelambdaHbb? Hbeta broad wavelength0.1nmem.wlfloatnullableFWHMHbb? Hbeta broad FWHM0.1nmspect.line.widthfloatnullableFluxHbb? Hbeta broad flux (10^-15^erg/cm^2^/s)1e-18W.m**-2phot.flux;em.line.HbetafloatnullableResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/sp21acyaSpectral log of SN 2021acya (table C5)TelTelescopemeta.id;instr.telcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoublePhasePhase (days after explosion, corrected for time dilation)dtime.phaseintResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/sp21adxlSpectral log of SN 2021adxl (table C6)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoubleTelTelescopemeta.id;instr.telcharPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/sp22qmlSpectral log of SN 2022qml (table C7)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoubleTelTelescopemeta.id;instr.telcharPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintResFWHM resolution0.1nmspect.resolutionfloatJ/A+A/695/A29/sp22wedSpectral log of SN 2022wed (table C8)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian datedtime.epochdoubleTelTelescopemeta.id;instr.telcharPhasePhase (days after explosion, corrected for time dilation)dtime.phaseintResFWHM resolution0.1nmspect.resolutionfloat