J/A+A/659/A39ivo://CDS.VizieR/J/A+A/659/A39doi:10.26093/cds/vizier.36590039CDSMelandri A.Izzo L.Pian E.Malesani D.B.Della Valle M.Rossi A.,D'Avanzo P.Guetta D.Mazzali P.A.Benetti S.Masetti N.Palazzi E.,Savaglio S.Amati L.Antonelli L.A.Ashall C.Bernardini M.G.,Campana S.Carini R.Covino S.D'Elia V.de Ugarte Postigo A.,De Pasquale M.Filippenko A.V.Fruchter A.S.Fynbo J.P.U.Giunta A.,Hartmann D.H.Jakobsson P.Japelj J.Jonker P.G.Kann D.A.Lamb G.P.,Levan A.J.Martin-Carrillo A.Moller P.Piranomonte S.Pugliese G.,Salvaterra R.Schulze S.Starling R.L.C.Stella L.Tagliaferri G.,Tanvir N.Watson D.2022-08-25T11:46:28Z2022-03-01T09:58:04ZCDS support team

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

cds-question@unistra.frgamma-ray-astronomygamma-ray-burstssupernovaephotometryspectroscopyWe observed GRB190114C (redshift z=0.4245), the first gamma-ray burst (GRB) ever detected at TeV energies, at optical and near-infrared wavelengths with several ground-based telescopes and the Hubble Space Telescope, with the primary goal of studying its underlying supernova, SN 2019jrj. The monitoring spanned the time interval between 1.3 and 370 days after the burst, in the observer frame. We find that the afterglow emission can be modelled with a forward shock propagating in a uniform medium modified by time-variable extinction along the line of sight. A jet break could be present after 7 rest-frame days, and accordingly the maximum luminosity of the underlying supernova (SN) ranges between that of stripped-envelope core-collapse SNe of intermediate luminosity and that of the luminous GRB-associated SN 2013dx. The observed spectral absorption lines of SN 2019jrj are not as broad as in classical GRB SNe and are instead more similar to those of less-luminous core-collapse SNe. Taking the broad-lined stripped-envelope core-collapse SN 2004aw as an analogue, we tentatively derive the basic physical properties of SN 2019jrj. We discuss the possibility that a fraction of the TeV emission of this source might have had a hadronic origin and estimate the expected high-energy neutrino detection level with IceCube.2022A&A...659A..39Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/659/A39CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/659/A39https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/659/A39http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/659/A39https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/659/A39https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/659/A39http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/659/A39GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-raydefaultJ/A+A/659/A39/table2Summary of spectroscopic observationsspShow the spectrummeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateObservation datetime.epoch;obsnullablePhasePhase with respect to the time of burst (T0) are in the rest framedtime.epochfloatSlitSlitarcsecmeta.notefloatTexpExposure time (s)time.duration;obs.exposurecharSeeingSeeingarcsecinstr.obsty.seeingfloatTelTelescope/Instrumentmeta.notecharFileNameName of the spectrum file in subdirectory spmeta.id;meta.filecharJ/A+A/659/A39/rbandr-band Photometry table of GRB190114C (Fig. 2) compiled by A. Melandri (data are all dereddened for Galactic extinction)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintInstInstrument (1)meta.id;instrchardtMid-time of the observation from the burststime.epochdoubletexpExposure timestime.duration;obs.exposurefloattstartStarting time of the observation = mid-time-(exposure_time/2)stime.epochdoubletendEnding time of the observation = mid-time+(exposure_time/2)stime.epochdoublefoptOptical flux in filter (2)mJyphot.flux.density;em.optdoublee_foptOptical flux in filter error (2)mJystat.errordoublemagMagnitude in filter (2)magphot.magfloate_magMagnitude in filter error (2)magstat.error;phot.magfloatfHGsubOptical flux in filter, after the Host Galxy flux subtraction (3)phot.flux.density;em.optdoublef(AG)Estimate (from the optical fit) of the afterglow contribution at that epoch (3)phot.flux.density;em.optdoublefSNEstimate of the SN contribution in filter, fSN=fHGsub-f(AG) (3)phot.flux.density;em.optdoubleJ/A+A/659/A39/ibandi-band Photometry table of GRB190114C (Fig. 2) compiled by A. Melandri (data are all dereddened for Galactic extinction)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintInstInstrument (1)meta.id;instrchardtMid-time of the observation from the burststime.epochdoubletexpExposure timestime.duration;obs.exposurefloattstartStarting time of the observation = mid-time-(exposure_time/2)stime.epochdoubletendEnding time of the observation = mid-time+(exposure_time/2)stime.epochdoublefoptOptical flux in filter (2)mJyphot.flux.density;em.optdoublee_foptOptical flux in filter error (2)mJystat.errordoublemagMagnitude in filter (2)magphot.magfloate_magMagnitude in filter error (2)magstat.error;phot.magfloatfHGsubOptical flux in filter, after the Host Galxy flux subtraction (3)phot.flux.density;em.optdoublef(AG)Estimate (from the optical fit) of the afterglow contribution at that epoch (3)phot.flux.density;em.optdoublefSNEstimate of the SN contribution in filter, fSN=fHGsub-f(AG) (3)phot.flux.density;em.optdoubleJ/A+A/659/A39/zbandz-band Photometry table of GRB190114C (Fig. 2) compiled by A. Melandri (data are all dereddened for Galactic extinction)magMagnitude in filter (2)magphot.magfloattstartStarting time of the observation = mid-time-(exposure_time/2)stime.epochdoubletendEnding time of the observation = mid-time+(exposure_time/2)stime.epochdoublefoptOptical flux in filter (2)mJyphot.flux.density;em.optdoublee_foptOptical flux in filter error (2)mJystat.errordoublee_magMagnitude in filter error (2)magstat.error;phot.magfloatfHGsubOptical flux in filter, after the Host Galxy flux subtraction (3)phot.flux.density;em.optdoublef(AG)Estimate (from the optical fit) of the afterglow contribution at that epoch (3)phot.flux.density;em.optdoublefSNEstimate of the SN contribution in filter, fSN=fHGsub-f(AG) (3)phot.flux.density;em.optdoubleInstInstrument (1)meta.id;instrcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintdtMid-time of the observation from the burststime.epochdoubletexpExposure timestime.duration;obs.exposurefloat