J/A+A/702/A212ivo://CDS.VizieR/J/A+A/702/A212doi:10.26093/cds/vizier/bc-ny/lcbcCDSReynolds T.M.Nagao T.Gottumukkala R.Gutierrez C.P.Kangas T.,Kravtsov T.Kuncarayakti H.Maeda K.Elias-Rosa N.Fraser M.Kotak R.,Mattila S.Pastorello A.Pessi P.J.Cai Y.-Z.Fynbo J.P.U.Kawabata M.,Lundqvist P.Matilainen K.Moran S.Reguitti A.Taguchi K.Yamanaka M.2026-08-03T06:58:04Z2025-10-24T10:02:12ZCDS support team

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

cds-question@unistra.frsupernovaephotometryvisible-astronomySome core-collapse supernovae (CCSNe) are too luminous and radiate too much total energy to be powered by the release of thermal energy from the ejecta and radioactive-decay energy from the synthesised ^56^Ni/^56^Co. A source of additional power is the interaction between the supernova (SN) ejecta and a massive circumstellar material (CSM). This is an important power source in Type IIn SNe, which show narrow spectral lines arising from the unshocked CSM, but not all interacting SNe show such narrow lines. We present photometric and spectroscopic observations of the hydrogen-rich SN 2021irp, which is both luminous, with M_o_<-19.4mag, and long-lived, remaining brighter than M_o_=-18mag for ~250d. We show that an additional energy source is required to power such a SN, and determine the nature of the source. We also investigate the properties of the pre-existing and newly formed dust associated with the SN. Photometric observations show that the luminosity of the SN is an order of magnitude higher than typical Type II SNe and persists for much longer. We detect a infrared excess attributed to dust emission. Spectra show multi-component line profiles, an Fe II pseudo-continuum, and a lack of absorption lines, all typical features of Type IIn SNe. We detect a narrow (<85km/s) P-Cygni profile associated with the unshocked CSM. An asymmetry in emission line profiles indicates dust formation occurring from 250-300d. Analysis of the SN blackbody radius evolution indicates asymmetry in the shape of the emitting region. We identify the main power source of SN 2021irp as extensive interaction with a massive CSM, and that this CSM is distributed asymmetrically around the progenitor star. The infrared excess is explained with emission from newly formed dust although there is also some evidence of an IR echo from pre-existing dust at early times.2025A&A...702A.212Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/702/A212CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/702/A213 : SN 2021irp polarisation spectra (Reynolds+, 2025)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/702/A212https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/702/A212http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/702/A212https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/702/A212https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/702/A212http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/702/A212GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/702/A212/tablea1Photometry of SN 2021irprecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPhasePhase (rest frame days with respect to our estimated explosion epoch)dtime.phasefloatMJDModified Julian datedtime.epochdoublel_magLimit flag on magmeta.code.errorcharmagMagnitude in Band (1)magphot.magfloate_mag? Magnitude in Band errormagstat.error;phot.magfloatnullableBand[G BVJHK riz co W1 W2] Observed bandinstr.bandpasscharTel+InstTelescopemeta.id;instr.telchar