J/A+A/621/A109ivo://CDS.VizieR/J/A+A/621/A109doi:10.26093/cds/vizier.36210109CDSBoian I.Groh J.H.2023-12-21T16:37:03Z2019-01-17T08:58:30ZCDS support team

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

cds-question@unistra.frastronomical-modelssupernovaespectroscopyObservational surveys are now able to detect an increasing number of transients, such as core-collapse supernovae (SN) and powerful non-terminal outbursts (SN impostors). Dedicated spectroscopic facilities can follow up these events shortly after detection. Here we investigate the properties of these explosions at early times.We use the radiative transfer code CMFGEN to build an extensive library of spectra simulating the interaction of supernovae and their progenitor's winds/circumstellar medium (CSM).We consider a range of progenitor mass-loss rates (dM/dt=5x10^-4^ to 10^-2^ M_{sun}/yr), abundances (solar, CNO-processed, and He-rich), and SN luminosities (L=1.9x10^8^ to 2.5x10^10^L_{sun}_). The models simulate events ~=1-day after explosion, and we assume a fixed location of the shock front as R_in_=8.6x10^13^cm. We show that the large range of massive star properties at the pre-SN stage causes a diversity of early-time interacting SN and impostors. We identify three main classes of early-time spectra consisting of relatively high-ionisation (e.g. HeII and OVI), medium-ionisation (e.g. CIII and NIII), and low-ionisation lines (e.g. HeI and FeII/III). They are regulated by L and the CSM density. Given a progenitor wind velocity v_inf_, our models also place a lower limit of dM/dt>~5x10^-4^(v_inf_=150km/s)M_{sun}_/yr for detection of CSM interaction signatures in observed spectra. Early-time SN spectra should provide clear constraints on progenitors by measuring H, He, and CNO abundances if the progenitors come from single stars. The connections are less clear considering the effects of binary evolution. Nevertheless, our models provide a clear path for linking the final stages of massive stars to their post-explosion spectra at early times, and guiding future observational follow-up of transients with facilities such as the Zwicky Transient Facility.2019A&A...621A.109Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/621/A109CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/621/A109https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/621/A109http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/621/A109https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/621/A109https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/621/A109http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/621/A109GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/621/A109/listList of model spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLum[19e7/25e9] LuminositysolLumphys.luminositydoubledM/dt[5e-4/1e-2] Mass-loss ratesolMass/yrarith.ratefloatvint[150] Terminal velocitykm/sphys.velocintRin[8.640e13] Inner boundarycmpos.angDistancedoubleTeff[16.1/64.7] Effective Temperature (at optical depth = 10)kKphys.temperature.effectivefloatAbund[he sol nit] Abundance code (1)meta.code;phys.abundcharspShow the spectrummeta.ref.urlcharFileNameName of sht spectrum file in subdirectory spmeta.id;meta.filechar