J/ApJ/902/6ivo://CDS.VizieR/J/ApJ/902/6doi:10.26093/cds/vizier.19020006CDSSoumagnac M.T.Ganot N.Irani I.Gal-yam A.Ofek E.O.Waxman E.,Morag J.Yaron O.Schulze S.Yang YiRubin A.Cenko S.B.Sollerman J.,Perley D.A.Fremling C.Nugent P.Neill J.D.Karamehmetoglu E.,Bellm E.C.Bruch R.J.Burruss R.Cunningham V.Dekany R.Golkhou V.Z.,Graham M.J.Kasliwal M.M.Konidaris N.P.Kulkarni S.R.Kupfer T.,Laher R.R.Masci F.J.Riddle R.Rigault M.Rusholme B.van Roestel J.,Zackay B.2022-05-18T13:10:38Z2022-02-23T13:20:31ZCDS support team

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

cds-question@unistra.frultraviolet-photometryinfrared-photometryvisible-astronomybroad-band-photometrysupernovaeabsolute-magnitudeHigh-cadence transient surveys are able to capture supernovae closer to their first light than ever before. Applying analytical models to such early emission, we can constrain the progenitor stars' properties. In this paper, we present observations of SN 2018fif (ZTF18abokyfk). The supernova was discovered close to first light and monitored by the Zwicky Transient Facility (ZTF) and the Neil Gehrels Swift Observatory. Early spectroscopic observations suggest that the progenitor of SN 2018fif was surrounded by relatively small amounts of circumstellar material compared to all previous cases. This particularity, coupled with the high-cadence multiple-band coverage, makes it a good candidate to investigate using shock-cooling models. We employ the SOPRANOS code, an implementation of the model by Sapir & Waxman and its extension to early times by Morag et al. Compared with previous implementations, SOPRANOS has the advantage of including a careful account of the limited temporal validity domain of the shock-cooling model as well as allowing usage of the entirety of the early UV data. We find that the progenitor of SN 2018fif was a large red supergiant with a radius of R=744.0_-128.0_^+183.0^R_{sun}_ and an ejected mass of M_ej_=9.3_-5.8_^+0.4^M_{sun}_. Our model also gives information on the explosion epoch, the progenitor's inner structure, the shock velocity, and the extinction. The distribution of radii is double- peaked, with smaller radii corresponding to lower values of the extinction, earlier recombination times, and a better match to the early UV data. If these correlations persist in future objects, denser spectroscopic monitoring constraining the time of recombination, as well as accurate UV observations (e.g., with ULTRASAT), will help break the extinction/radius degeneracy and independently determine both.2020ApJ...902....6Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/902/6CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/PASP/111/438 : Updated Zwicky catalog (UZC) (Falco+, 1999)J/MNRAS/408/827 : Simulations of supernova explosions (Dessart+, 2010)J/ApJ/736/159 : Photometry monitoring of the SN PTF10vdl (Gal-Yam+, 2011)J/MNRAS/438/L101 : First month on SN 2013ej (Valenti+, 2014)J/A+A/593/A68 : PTF12os & iPTF13bvn spectra & light curves (Fremling+, 2016)J/ApJ/820/33 : R-band light curves of type II supernovae (Rubin+, 2016)J/MNRAS/478/3138 : Luminous supergiants in Magellanic Clouds (Davies+, 2018)J/ApJ/861/63 : Type IIP SN 2016bkv LCs and spectra (Hosseinzadeh+, 2018)J/ApJ/901/61 : LCs of 4 superluminous SNe from ZTF (Lunnan+, 2020)J/A+A/657/A64 : Supernovae ZTF light curves (Sollerman+, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/902/6https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/902/6http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/902/6https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/902/6https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/902/6http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/902/6GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVOpticalInfrareddefaultJ/ApJ/902/6/table2Photometric observations of SN 2018fife_mag[0.01/0.8]? Uncertainty in magmagstat.error;phot.magfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJD[2458321.9/2458490.7] Julian Date of the observationdtime.epochdoublemag[17.5/21.4]? Apparent AB magnitude in Filtmagphot.magfloatnullableFlux[4.8e-49/1.1e-15] Flux density; in erg/s/cm^2^/{AA} unitscW.m**-2.nm**-1meta.unit;phot.fluxdoublee_Flux[4.4e-47/1.7e-14] Uncertainty in FluxcW.m**-2.nm**-1stat.error;phot.fluxdoublen_e_Flux[a] a: uncertainty is very suspicious; note added by CDSmeta.notecharMag[-16.8/-12.9]? Absolute magnitude in Filtmagphys.magAbsfloatnullablee_Mag[0.01/0.8]? Uncertainty in Magmagstat.error;phot.magfloatnullableFiltFilter used in the observationinstr.setup;obscharInstInstrument used in the observation (1)instr.setup;obschar