J/A+A/713/A29ivo://CDS.VizieR/J/A+A/713/A29CDSErtini K.Anderson J.P.Folatelli G.Gonzalez-Gaitan S.Gutierrez C.P.,Sollerman J.Rodriguez O.Aryan A.Chen T.-W.Concepcion E.,Cosentino S.P.Dennefeld M.Erasmus N.Fraser M.Galbany L.,Gromadzki M.Inserra C.Mueller-Bravo T.E.Pessi P.J.Pessi T.,Petrushevska T.Pignata G.Ragosta F.Srivastav S.Young D.R.2026-09-03T07:52:01Z2026-09-03T08:42:17ZCDS support team

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

cds-question@unistra.frsupernovaegalaxiesredshiftedextinctionobservational-astronomyastronomical-reference-materialsabsolute-magnitudephotometryspectroscopyvisible-astronomyinfrared-astronomyType II supernovae (SNe II) are the most common terminal stellar explosions in the Universe. With SNe now being detected within days after explosion, there is growing evidence that the majority of Type II SNe show signs of interaction with a confined, dense cirumstellar material (CSM) in the first few days post explosion. In this work we aim to bridge the gap between single SN studies showing early-time interaction in their spectra, and the statistical studies of early-time SN light curves, which imply the existence of CSM. We present a sample of 68 Type II SNe with both early photometric data, obtained with the ATLAS survey, and spectroscopic data, obtained with the ePESSTO+ collaboration. A subset of the sample is classified based on the presence or absence of narrow spectral features with electron-scattered broadened wings in the early spectra, indicative of interaction with CSM. We characterise the photometric and spectroscopic properties of the sample by measuring rise times to maximum light, peak magnitudes, decline rates and line velocities. Additionally, we measure the ratio of absorption to emission (a/e) of the Halpha P-Cygni profile. Our analysis reveals that SNe II showing early spectroscopic signs of interaction with CSM decline faster and are brighter than those without. However no difference is found in rise times between the two groups. A clear separation is observed in the a/e ratio: SNe with signs of interaction exhibit lower a/e ratios at all epochs compared to those without. Our results highlight that understanding SN II ejecta-CSM interaction requires large, uniform samples of photometric and spectroscopic data, such as the one presented in this work.2026A&A...713A..29Ehttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/713/A29CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/579/A40 : PESSTO catalog (Smartt+, 2015)J/MNRAS/488/4239 : SNe II and IIb optical light curves comparison (Pessi+,2019)J/MNRAS/483/5459 : SNe II as distance indicators at near-IR (Rodriguez+, 2019)J/MNRAS/442/844 : BVRI light curves of type II-P supernovae (Faran+, 2014)J/MNRAS/412/1441 : SNe luminosity functions (Li+, 2011)J/ApJ/955/71 : The iron yield of core-collapse supernovae (Rodriguez+,2023)J/ApJ/952/119 : SNII during ZTF 1st phase survey with follow-up sp.J/ApJ/912/46 : ZTF Type II supernovae with follow-up obs. (Bruch+, 2021)J/ApJ/902/6 : UV to visible-light observations of SN 2018fifJ/ApJ/885/43 : UBVRI & ugriz photometry of supernova SN 2017gmrJ/ApJ/820/33 : R-band light curves of type II supernovae (Rubin+, 2016)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/713/A29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/713/A29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/713/A29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/713/A29https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/713/A29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/713/A29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/713/A29/tablea1 (Physical properties of the selected SN II sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/713/A29/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/713/A29/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/713/A29/tablea1?GETtext/xml+votable180.050000true23.4038333-38.599750.0055555555555555566/929 4149 4434 4954 8215 8318 8387 8403 8923 10379 10385 12371 16869 17782 18022 18172 18484 18767 19359 19991 20006 20014 20090 21075 21175 21179 21233 21265 22636 22684 23189 23255 24828 25357 25381 25526 25650 26575 27116 27329 27423 27797 32913 34215 35158 35189 35590 35755 35800 36105 36115 36236 36261 36269 36496 38313 38718 38781 38829 39489 40359 40828 43805 43920 44507 46563 46733 47516https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/713/A29?format=asciiOpticalInfrareddefaultJ/A+A/713/A29/tablea1Physical properties of the selected SN II samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSNSupernova name (SN)meta.id;meta.maincharDateLastNonDetDate of the last non-detection (Last_non-detection)dtime.epochdoubleSimbadNameSimbad column added by the CDSmeta.idcharnullablezHeliocentric redshift (z_helio)src.redshiftfloatDistDistance (Distance)Mpcpos.distancefloate_DistDistance error (Distance_error)Mpcstat.errorfloatE(B-V)MWGalactic extinction (EB-V_MW)magphys.absorptionfloatDateDiscoveryDate of discovery (Discovery_Date)dtime.epochdoubleDateFirstLightDate of first light (First_Light_Epoch)dtime.epochdoubleATLASDisplay the ATLAS all-sky stellar ref. catalog, ATLAS-REFCAT2 of Tonry et al. 2018ApJ...867..105T, Cat. J/ApJ/867/105meta.ref.urlintnullableTNSDisplay the TNS database object's pagemeta.ref.urlchar_RAPosition from Simbad and TNS databases (right ascension part)degpos.eq.ra;meta.main_DEPosition from Simbad and TNS databases (declination part)degpos.eq.dec;meta.mainGalaxyHost Galaxy name (Host_Galaxy)meta.id.parentcharJ/A+A/713/A29/tablea2The SN II spectral informationrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSNSupernova name (SN)meta.id;meta.maincharNspNumber of spectra per SN (N_of_spectra)meta.numberintEarToLastEpoch of earliest and latest spectrum (Earliest_and_latest_epoch)time.intervalcharClassEarly classification of SNe based on presence or absence of narrow high ionization features in early spectra as flash F, non-flash NF and ledge L (Classification)src.classcharReferenceReference for the earliest spectrum which was used to classify the SN as F/NF/L (Reference_for_early_spectrum)meta.ref;pos.framecharJ/A+A/713/A29/tablea3Light curve properties compared with previous works in the literaturerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintReferenceReference (Reference) (1)meta.ref;pos.framecharNsnNumber of SNe used in each study (Number_of_SN)meta.numberintFilterFilter information (Filter)meta.note;instr.filterchartrise? Rise time (t_rise)dtime.intervalfloatnullablee_trise? Rise time error (t_rise_err)dstat.errorfloatnullablen_triseNote for interval value (t_rise_err)meta.notecharMmaxMag? Absolute magnitude at maximum light (M_max)magphys.magAbs;em.optfloatnullablee_MmaxMag? Absolute magnitude at maximum light error (M_max_err)magstat.error;phot.magfloatnullableNormMax? Normalised absolute magnitude at maximum light (Normalised_M_max) (2)phys.magAbs;em.optfloatnullableJ/A+A/713/A29/tablec1The photometric properties of the SN II SampleSNSN name (SN)meta.id;meta.maincharomaxMagAbsolute magnitude at maximum light in the o-filter (M_max_o)magphys.magAbs;em.optfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_omaxMagAbsolute magnitude at maximum light in the o-filter error (M_max_o_err )magstat.error;phot.magfloatcmaxMag? Absolute magnitude at maximum light in the c-filter (M_max_c)magphys.magAbs;em.optfloatnullablee_cmaxMag? Absolute magnitude at maximum light in the c-filter error (M_max_c_err)magstat.error;phot.magfloatnullabletriseoRise time in the o-filter (t_rise_o)dtime.intervalfloate_triseoRise time in the o-filter error (t_rise_o_err)dstat.errorfloattrisec? Rise time in the c-filter (t_rise_c)dtime.intervalfloatnullablee_trisec? Rise time in the c-filter error (t_rise_c_err)dstat.errorfloatnullables1oDecline rate of the initial, steeper slope of the light curve in the o-filter (s1_o)stat.fit.paramfloate_s1oDecline rate of the initial, steeper slope of the light curve in the o-filter error (s1_o_err)stat.errorfloats1c? Decline rate of the initial, steeper slope of the light curve in the c-filter (s1_c)stat.fit.paramfloatnullablee_s1c? Decline rate of the initial, steeper slope of the light curve in the c-filter error (s1_c_err)stat.errorfloatnullables2oDecline rate of the second, shallower slope of the light curve in the o-filter (s2_o)stat.fit.paramfloate_s2oDecline rate of the second, shallower slope of the light curve in the o-filter error (s2_o_err)stat.errorfloats2c? Decline rate of the second, shallower slope of the light curve in the c-filter (s2_c)stat.fit.paramfloatnullablee_s2c? Decline rate of the second, shallower slope of the light curve in the c-filter error (s2_c_err)stat.errorfloatnullable