J/ApJ/932/1ivo://CDS.VizieR/J/ApJ/932/1doi:10.26093/cds/vizier.19320001CDSRossi A.Rothberg B.Palazzi E.Kann D.A.D'Avanzo P.Amati L.,Klose S.Perego A.Pian E.Guidorzi C.Pozanenko A.S.Savaglio S.,Stratta G.Agapito G.Covino S.Cusano F.D'Elia V.De Pasquale M.,Valle M.D.Kuhn O.Izzo L.Loffredo E.Masetti N.Melandri A.,Minaev P.Y.Guelbenzu A.N.Paris D.Paiano S.Plantet C.Rossi F.,Salvaterra R.Schulze S.Veillet C.Volnova A.A.2024-11-06T20:26:02Z2024-05-16T13:57:57ZCDS support team

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

cds-question@unistra.frgamma-ray-astronomygamma-ray-burstsgalaxiesspectroscopyvisible-astronomyGamma-ray bursts (GRBs) are classified into long and short events. Long GRBs (LGRBs) are associated with the end states of very massive stars, while short GRBs (SGRBs) are linked to the merger of compact objects. GRB 200826A was a peculiar event, because by definition it was an SGRB, with a rest-frame duration of ~0.5s. However, this event was energetic and soft, which is consistent with LGRBs. The relatively low redshift (z=0.7486) motivated a comprehensive, multiwavelength follow-up campaign to characterize its host, search for a possible associated supernova (SN), and thus understand the origin of this burst. To this aim we obtained a combination of deep near-infrared (NIR) and optical imaging together with spectroscopy. Our analysis reveals an optical and NIR bump in the light curve whose luminosity and evolution are in agreement with several SNe associated to LGRBs. Analysis of the prompt GRB shows that this event follows the Ep,i-Eiso relation found for LGRBs. The host galaxy is a low-mass star-forming galaxy, typical of LGRBs, but with one of the highest star formation rates, especially with respect to its mass (logM_*_/M_{sun}_=8.6, SFR~4.0M_{sun}_/yr). We conclude that GRB 200826A is a typical collapsar event in the low tail of the duration distribution of LGRBs. These findings support theoretical predictions that events produced by collapsars can be as short as 0.5s in the host frame and further confirm that duration alone is not an efficient discriminator for the progenitor class of a GRB.2022ApJ...932....1Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/932/1CatalogResearchIsServedByTAP VizieR generic servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)J/ApJ/678/1127 : Optical photometry of GRB 070610 (Kasliwal+, 2008)J/ApJ/701/824 : Afterglows of short & long-duration GRBs (Nysewander+, 2009)J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010)J/ApJ/778/128 : GRB-host galaxies photometry (Perley+, 2013)J/A+A/570/A11 : The Hawk-I UDS and GOODS Survey (HUGS) (Fontana+, 2014)J/ApJ/789/23 : Properties of SN host galaxies (Kelly+, 2014)J/A+A/609/A30 : Conversion factors to LIR & Mdust (Schreiber+, 2018)J/MNRAS/486/L46 : Gamma-ray burst redshifts (Amati+, 2019)J/A+A/625/A152 : Light-curve models of black hole (Barbieri+, 2019)J/MNRAS/492/1919 : Type I GRBs & the new classification method (Minaev+, 2020)J/MNRAS/493/3379 : Comparison between GRB afterglows & AT2017gfo (Rossi+, 2020)J/A+A/646/A50 : GRB 190829A/SN 2019oyw spectra (Hu+, 2021)J/ApJ/916/89 : 85 short GRB kilonovae opt. & NIR obs. (Rastinejad+, 2021)J/A+A/659/A39 : GRB190114C spectra and light curves (Melandri+, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/932/1https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/932/1http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/932/1https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/932/1https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/932/1http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/932/1GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-rayOpticaldefaultJ/ApJ/932/1/fig10LBT/MODS observed spectrum of the host galaxy of GRB 200826ArecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[3800.23/10100] Wavelength; Angstroms0.1nmem.wldoubleFlux[-6.42e-18/4.1e-17] Flux density; erg/s/cm^2^/Angstrom (1)cW.m**-2.nm**-1phot.fluxdouble