J/A+A/708/A136ivo://CDS.VizieR/J/A+A/708/A136CDSOtaki K.Schneider R.Graziani L.Bonella A.Marassi S.Limongi M.,Bianchi S.2026-05-04T07:43:19Z2026-04-01T09:36:54ZCDS support team

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

cds-question@unistra.frsupernovaestellar-massesastronomical-modelsSupernovae (SNe) are believed to be the dominant sources of dust production at high redshift. However, the reverse shock generated by the interaction of the SN forward shock and the interstellar medium (ISM) can significantly reduce the mass of newly formed dust in SN ejecta. This study quantifies the mass, composition, and grain size distribution of surviving dust after the passage of the reverse shock using the GRASHrev model. Our analysis covers a grid of SN models with progenitor masses 13M_{sun}_<=m_star_<=120M_{sun}_, metallicity -3<=[Fe/H]=0, and explores, for the first time, the effect of stellar rotation, considering two initial velocities v=0 and 300km/s. The SN explosions are assumed to occur in a uniform ISM with densities n_ISM_=0.05, 0.5, and 5cm^-3^. We find that the larger grains (>=10nm) are more resistant to destruction by the reverse shock, with amorphous carbon dominating the surviving dust mass in most models. The surviving dust mass decreases with increasing ISM density. For non-rotating progenitors, the maximum mass of dust surviving the passage of the reverse shock is ~0.02M_{sun}_ released by SN explosions of a 120 Msun progenitor with [Fe/H]=0 in the ISM density 0.5cm^-3^, corresponding to ~4% of the initial dust mass before the passage of the reverse shock. Similarly, among the rotating progenitors, a maximum surviving mass fraction is ~5% with a final dust mass ~0.03M_{sun}_ in [Fe/H]=-1 models. Although the reverse shock has a strong destructive impact, our results indicate that, on very short timescales of <30Myr since the onset of star formation, SNe can enrich the ISM with carbonaceous grains ranging in size from approximately 1nm to 100nm (up to ~1um in non-rotating models). This is especially notable given the recent detection of the 2175{AA} UV extinction bump in galaxies at z>6, suggesting the early presence of such dust.2026A&A...708A.136Ohttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/708/A136CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/708/A136https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/708/A136http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/708/A136https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/708/A136https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/708/A136http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/708/A136GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/708/A136/tablea1Initial dust yields for non-rotating modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[Fe/H][-3/0] Initial metallicityphys.abund.ZintMstarProgenitor mass (13/15/20/25/30/40/60/80/120)solMassphys.massintMdustTotal dust masssolMassphys.massdoubleMAl2O3Al2O3 masssolMassphys.massdoubleMFeFe masssolMassphys.massdoubleMFe3O4Fe3O4 masssolMassphys.massdoubleMMgSiO3MgSiO3 masssolMassphys.massdoubleMMg2SiO4Mg2SiO4 masssolMassphys.massdoubleMACAC masssolMassphys.massdoubleMSiO2SiO2 masssolMassphys.massdoublemuMean molecular weightstat.weightdoubleJ/A+A/708/A136/tablea2Initial dust yields for rotating modelsrecnoRecord number assigned by the VizieR team. 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