J/A+A/677/A28ivo://CDS.VizieR/J/A+A/677/A28doi:10.26093/cds/vizier.36770028CDSPessi T.Prieto J.L.Anderson J.P.Galbany L.Lyman J.D.Kochanek C.,Dong S.Forster F.Gonzalez-Diaz R.Gonzalez-Gaitan S.Gutierrez C.P.,Holoien T.W.-S.James P.A.Jimenez-Palau C.Johnston E.J.,Kuncarayakti H.Rosales-Ortega F.Sanchez S.F.Schulze S.Shappee B.2026-04-30T20:02:44Z2023-08-29T08:23:22ZCDS support team

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

cds-question@unistra.frsupernovaeredshiftedchemical-abundancesphotometryvisible-astronomyThe analysis of core-collapse supernova (CCSN) environments can provide important information on the life cycle of massive stars and constrain the progenitor properties of these powerful explosions. The MUSE instrument at the Very Large Telescope (VLT) enables detailed local environment constraints of the progenitors of large samples of CCSNe. Using a homogeneous SN sample from the All-Sky Automated Survey for Supernovae (ASAS-SN) survey, an untargeted and spectroscopically complete transient survey, has enabled us to perform a minimally biased statistical analysis of CCSN environments. We analyze 111 galaxies observed by MUSE that hosted 112 CCSNe - 78 II, nine IIn, seven IIb, four Ic, seven Ib, three Ibn, two Ic-BL, one ambiguous Ibc, and one superluminous SN - detected or discovered by the ASAS-SN survey between 2014 and 2018. The majority of the galaxies were observed by the the All-weather MUse Supernova Integral field Nearby Galaxies (AMUSING) survey. Here we analyze the immediate environment around the SN locations and compare the properties between the different CCSN types and their light curves. We used stellar population synthesis and spectral fitting techniques to derive physical parameters for all HII regions detected within each galaxy, including the star formation rate (SFR), H{alpha} equivalent width (EW), oxygen abundance, and extinction. Results. We found that stripped-envelope (SE) SNe occur in environments with a higher median SFR, H{alpha} EW, and oxygen abundances than SNe II and SNe IIn/Ibn. Most of the distributions have no statistically significant differences, except between oxygen abundance distributions of SESNe and SNe II, and between H{alpha} EW distributions of SESNe and SNe II. The distributions of SNe II and IIn are very similar, indicating that these events explode in similar environments. For the SESNe, SNe Ic have higher median SFRs, H{alpha} EWs, and oxygen abundances than SNe Ib. SNe IIb have environments with similar SFRs and H{alpha} EWs to SNe Ib, and similar oxygen abundances to SNe Ic. We also show that the postmaximum decline rate, s, of SNe II correlates with the H{alpha} EW, and that the luminosity and the {DELTA}m15 parameter of SESNe correlate with the oxygen abundance, H{alpha} EW, and SFR at their environments. This suggests a connection between the explosion mechanisms of these events to their environment properties.2023A&A...677A..28Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A28CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/677/A28https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/677/A28http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/677/A28https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/677/A28https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/677/A28http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/677/A28GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/677/A28/table1 (General properties of the SNe and their host galaxies (updated version from erratum, 2026A&A...705C...1P, 10-Dec-2025))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/677/A28/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/677/A28/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/677/A28/table1?GETtext/xml+votable180.050000true307.049875-3.1370750.0055555555555555566/11 564 8501 8506 8829 9099 9217 16411 16433 16442 17032 17056 17207 17870 17901 17974 18013 18365 18507 18578 18708 18757 18846 19607 19614 19810 19872 19996 20139 20177 21051 22611 23827 24765 24960 25079 25181 25211 25277 25336 25389 25535 25839 25889 26171 26217 26372 26433 26448 27656 28073 28167 28422 29974 29983 31383 31998 32129 32183 32642 33179 33500 33614 33921 34050 34654 34694 35252 35531 35691 35788 36773 37014 37109 37399 38343 38350 38797 39000 39025 40393 40448 40841 41065 42010 42056 43192 43234 43305 43488 43610 43732 43886 43963 44544 44718 44848 45283 45486 45693 46491 46525 46684 46690 46903 46999 47160 47919 48213 48290https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/677/A28?format=asciiOpticaldefaultJ/A+A/677/A28/table1General properties of the SNe and their host galaxies (updated version from erratum, 2026A&A...705C...1P, 10-Dec-2025)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSN namemeta.id;meta.maincharSimbadNameSimbad column added by the CDSmeta.idnullableTypeSN typesrc.classcharRAJ2000SN Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000SN Declination (J2000)pos.eq.dec;meta.mainHostHost galaxy namemeta.id.parentcharzHost? Host galaxy redshiftsrc.redshift;pos.heliocentricdoublenullableAvMW? Galactic extinction towards the host galaxymagphys.absorptionfloatnullableBMAGhost? Host galaxy absolute magnitudes in B bandmagphys.magAbsfloatnullableJ/A+A/677/A28/table2Distance properties of the HII regions related to each SNrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSN namemeta.id;meta.maincharzcmbCMB redshiftsrc.redshiftdoubleDLLuminosity distance to SNMpcpos.distancefloatdprojDistance between the SN and HII regionpcpos.distancedoublerRadius of HII regionpcphys.size.radius;obs.fielddoubleAreaArea of HII regionkpc**2phys.areadoubleJ/A+A/677/A28/tabled1Measured fluxes of different emission lines at the neares HII region to each SNrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSN namemeta.id;meta.maincharFHa? H{alpha} flux (in 10^-17^erg/s/cm^2^)1e-20W.m**-2phot.flux;em.line.Halphadoublenullablee_FHa? H{alpha} flux error (in 10^-17^erg/s/cm^2^)1e-20W.m**-2stat.errordoublenullableFHb? H{beta} flux (in 10^-17^erg/s/cm^2^)1e-20W.m**-2phot.flux;em.line.Hbetadoublenullablee_FHb? H{beta} flux error (in 10^-17^erg/s/cm^2^)1e-20W.m**-2stat.errordoublenullableFOIII? OIII flux (in 10^-17^erg/s/cm^2^)1e-20W.m**-2phot.fluxdoublenullablee_FOIII? OIII flux error (in 10^-17^erg/s/cm^2^)1e-20W.m**-2stat.errordoublenullableFNII? NII flux (in 10^-17^erg/s/cm^2^)1e-20W.m**-2phot.fluxdoublenullablee_FNII? NII flux error (in 10^-17^erg/s/cm^2^)1e-20W.m**-2stat.errordoublenullableFSII? SII flux (in 10^-17^erg/s/cm^2^)1e-20W.m**-2phot.fluxdoublenullablee_FSII? SII flux error (in 10^-17^erg/s/cm^2^)1e-20W.m**-2stat.errordoublenullableJ/A+A/677/A28/tabled2Physical properties of the HII region related to each SN12+log(O/H)D16Oxygen abundance in the D16 indexphys.abunddoublee_12+log(O/H)D16Error of the oxygen abundance in the D16 indexstat.errordoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSN namemeta.id;meta.maincharEWHa? H{alpha} equivalent width0.1nmspect.line.eqWidthdoublenullablee_EWHa? H{alpha} equivalent width error0.1nmstat.errordoublenullable12+log(O/H)N2? Oxygen abundance in the N2 indexphys.abunddoublenullablee_12+log(O/H)N2? Error of the oxygen abundance in the N2 indexstat.errordoublenullable12+log(O/H)O3N2? Oxygen abundance in the O3N2 indexphys.abunddoublenullablee_12+log(O/H)O3N2? Error of the oxygen abundance in the O3N2 indexstat.errordoublenullablelogSigmaSFR? Star formation rate surface densitylog(solMass.yr**-1.kpc**-2)phys.SFRdoublenullablee_logSigmaSFR[]? Star formation rate surface density errorlog(solMass.yr**-1.kpc**-2)stat.errordoublenullableE(B-V)? Host galaxy extinctionmagphot.color.excessdoublenullablee_E(B-V)? Host galaxy extinction errormagstat.errordoublenullableJ/A+A/677/A28/tableg1Light curve parameters of the SNe IIrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSN namemeta.id;meta.maincharVmag? Magnitude at peak brightness in V bandmagphot.mag;em.opt.Vdoublenullablee_Vmag? Error of magnitude at peak brightness in V bandmagstat.error;phot.magdoublenullables2V? Light curve decline rate in V bandmag/dphot.mag;arith.diffdoublenullablee_s2V? Error of light curve decline rate in V bandmag/dstat.errordoublenullableBmag? Magnitude at peak brightness in B bandmagphot.mag;em.opt.Bdoublenullablee_Bmag? Error of magnitude at peak brightness in B bandmagstat.error;phot.magdoublenullables2B? Light curve decline rate in B bandmag/dphot.mag;arith.diffdoublenullablee_s2B? Error of light curve decline rate in B bandmag/dstat.errordoublenullablermag? Magnitude at peak brightness in r bandmagphot.mag;em.opt.Rdoublenullablee_rmag? Error of magnitude at peak brightness in r bandmagstat.error;phot.magdoublenullables2r? Light curve decline rate in r bandmag/dphot.mag;arith.diffdoublenullablee_s2r? Error of light curve decline rate in r bandmag/dstat.errordoublenullable