J/ApJ/902/86ivo://CDS.VizieR/J/ApJ/902/86doi:10.26093/cds/vizier.19020086CDSHo A.Y.Q.Kulkarni S.R.Perley D.A.Cenko S.B.Corsi A.Schulze S.,Lunnan R.Sollerman J.Gal-Yam A.Anand S.Barbarino C.Bellm E.C.,Bruch R.J.Burns E.De K.Dekany R.Delacroix A.Duev D.A.,Frederiks D.D.Fremling C.Goldstein D.A.Golkhou V.Z.Graham M.J.,Hale D.Kasliwal M.M.Kupfer T.Laher R.R.Martikainen J.Masci F.J.,Neill J.D.Ridnaia A.Rusholme B.Savchenko V.Shupe D.L.,Soumagnac M.T.Strotjohann N.L.Svinkin D.S.Taggart K.Tartaglia L.,Yan L.Zolkower J.2022-06-09T12:15:55Z2022-05-10T12:15:55ZCDS support team

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

cds-question@unistra.frsupernovaeinfrared-photometryvisible-astronomybroad-band-photometryultraviolet-photometryWe present optical, radio, and X-ray observations of SN 2020bvc (=ASASSN-20bs, ZTF 20aalxlis), a nearby (z=0.0252; d = 114Mpc) broad-line (BL) Type Ic supernova (SN) and the first double-peaked Ic-BL discovered without a gamma-ray burst (GRB) trigger. Our observations show that SN 2020bvc shares several properties in common with the Ic-BL SN 2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10GHz radio luminosity (L_radio_~10^37^erg/s) is brighter than ordinary core-collapse SNe but fainter than LLGRB SNe such as SN 1998bw (associated with LLGRB980425). We model our VLA observations (spanning 13-43days) as synchrotron emission from a mildly relativistic (v>~0.3c) forward shock. Second, with Swift and Chandra, we detect X-ray emission (L_X_~10^41^erg/) that is not naturally explained as inverse Compton emission or part of the same synchrotron spectrum as the radio emission. Third, high-cadence (6x night^-1^) data from the Zwicky Transient Facility (ZTF) show a double-peaked optical light curve, the first peak from shock cooling of extended low-mass material (mass M_e_<10^-2^M_{sun}_ at radius R_e_>10^12^cm) and the second peak from the radioactive decay of ^56^Ni. SN 2020bvc is the first double-peaked Ic-BL SN discovered without a GRB trigger, so it is noteworthy that it shows X-ray and radio emission similar to LLGRB SNe. For four of the five other nearby (z<~0.05) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN 2006aj and SN 2020bvc, i.e., that lasts ~1day and reaches a peak luminosity M~-18. Follow-up X-ray and radio observations of Ic-BL SNe with well-sampled early optical light curves will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission.2020ApJ...902...86Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/902/86CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/MNRAS/383/1485 : BVRI light curves of SN 2003jd (Valenti+, 2008)J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)J/ApJ/702/226 : Swift/UVOT panchromatic obs. of SN 2008D (Modjaz+, 2009)J/other/Nat/463.513 : Radio observations of SN 2009bb (Soderberg+, 2010)J/ApJ/742/L18 : Follow-up photometry of SNIIb PTF11eon (Arcavi+, 2011)J/AJ/141/163 : Ultimate LC of SN 1998bw/GRB 980425 (Clocchiatti+, 2011)J/MNRAS/412/1441 : SNe luminosity functions (Li+, 2011)J/ApJ/759/107 : Core-collapse SNe and host galaxies (Kelly+, 2012)J/ApJS/213/19 : Optical & near-IR light curves of 64 SNe (Bianco+, 2014)J/ApJ/781/37 : Multi-band photometry of GRB 130427A (Perley+, 2014)J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)J/ApJS/211/13 : The second Fermi/GBM GRB cat. (4yr) (von Kienlin+, 2014)J/ApJS/219/8 : SFR for WISE + SDSS spectroscopic galaxies (Chang+, 2015)J/A+A/593/A68 : PTF12os & iPTF13bvn spectra & LCs (Fremling+, 2016)J/A+A/594/A116 : HI4PI spectra and column density maps (HI4PI team+, 2016)J/ApJ/832/108 : Spectral data of Type Ic & Ic-bl SNe (Modjaz+, 2016)J/ApJ/851/107 : iPTF 16asu photometry follow-up (Whitesides+, 2017)J/other/Sci/362.201 : iPTF 14gqr (SN 2014ft) photometry (De+, 2018)J/ApJ/887/169 : UV-Opt light curves of the type Ic SN 2018gep (Ho+, 2019)J/ApJ/886/152 : ZTF early obs. of Type Ia SNe. I. LCs (Yao+, 2019)J/ApJ/895/32 : Zwicky Transient Facility BTS. I. (Fremling+, 2020)J/ApJ/893/132 : Optical follow-up of SNIc ZTF18aaqjovh (Ho+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/902/86https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/902/86http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/902/86https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/902/86https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/902/86http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/902/86GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVOpticalInfrareddefaultJ/ApJ/902/86/tablea1UV-to-IR photometry for SN2020bvc, corrected for Milky Way extinctionrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJD[58883.3/58912.6] Modified Julian Datedtime.epochdoubleDeltaT[0.67/29.88] Time since t_0_; 2020 Feb 03.67 UTCdtime.epochfloatInstInstrument used (1)instr.setupcharFiltFilter usedinstr.setup;instr.filtercharmag[16.26/22.23] Apparent AB magnitude in Filtmagphot.magfloate_mag[0.01/0.1] Uncertainty in magmagstat.error;phot.magfloatJ/ApJ/902/86/fig4Optical spectra of SN2020bvcrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintt0[0.76/47.9] Time since reference epoch: 2020 Feb 03.67 UTCdtime.intervalfloatlambda[3061.6/10305] Wavelength in Angstroms0.1nmem.wldoubleFlux[-0.44/2.04]? Flux density in erg/s/cm^2^/{AA} (1)cW.m**-2.nm**-1phot.flux.densitydoublenullable