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The Supernova/Gamma-Ray Burst Connection

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The Supernova/Gamma-Ray Burst Connection The Supernova/Gamma-Ray Burst Connection Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Levan et al. 2014 Levan et al. 2014 Reviews Woosley & Bloom 1996 Hjorth & Bloom 2012 Hjorth 2013 (ultrabrief) Quite some recent developments LGRB-SN properties ULGRB-SLSN SGRB-KN Phillips relation for LGRB-SNe Galama et al. 1998; Fynbo et al. 2000 SN 1998bw/GRB 980425 SN 1998bw/GRB Galama et al. 1998 Collapsar model “We predict that all GRBs produced by the collapsar model will also make supernovae like SN 1998bw” 1999 Woosley & MacFadyen GRB 980326: light curve bump Castro-Tirado & Gorosabel 1999; Bloom et al. 1999 SN 2003dh/GRB 030329 GRB 980425 was an unusual GRB: Low luminosity and no afterglow Search for a SN in a high luminosity, higher redshift, afterglow dominated GRB? 2003 et al. Spectral evolution from afterglow power law to Stanek broad-lined Ic supernova like SN 1998bw Hjorth et al. 2003; 2003; Hjorth et al. Hjorth et al. 2003; Patat et al. 2001 -24 -22 -20 Host galaxy Afterglow (mag) V M -18 Supernova -16 -14 0 10 20 30 40 50 Time since explosion (days) Hjorth 2013 27 GRB-SNe in 19 years 5 4 3 2 1 0 Spectroscopic diversity diversity Spectroscopic Modjaz et al. 2015 Spectroscopic diversity diversity Spectroscopic Modjaz et al. 2015 SNe from different classes of GRBs -20 Low-luminosity GRBs Collapsar GRBs GRB 980425 GRB 030329 -19 (mag) V M -18 -17 48 50 52 54 log E,iso (erg) Hjorth 2013 Long GRBs with no (bright) SN 2007 et al. Ofek Compact object merger progenitor with longer duration? 56 GRB 030329/SN 2003dh Ni fallback? GRB 980425/SN 1998bw GRB 031203/SN 2003lw GRB 060218/SN 2006aj 2006; et al. GRB 100316D/SN 2010bh -18 Gehrels -16 Absolute magnitude (mag) -14 GRB 060505 al.; et Gal-Yam Valle; Della et al.; GRB 060614 -12 0 20 40 60 80 100 Fynbo Time since GRB (days) Greiner et al. 2015 Greiner et al. 2015 Magnetar-powered GRB-SNe? Cano et al. 2016 GRB 050509B HJorth et al. 2005 GRB 050709 HJorth et al. 2005 GRB 030329/SN 2003dh GRB 980425/SN 1998bw GRB 031203/SN 2003lw GRB 060218/SN 2006aj GRB 100316D/SN 2010bh -18 -16 Absolute magnitude (mag) -14 GRB 050509B GRB 050709 -12 0 20 40 60 80 100 2005a,b Hjorth et al. Time since GRB (days) GRB 130603B Tanvir et al. 2013; Berger et al. 2013 Tanvir et al. 2013; Berger et al. 2013 GRB 060614 Yang et al. 2015 LUMINOSITY – WIDTH RELATION Phillips relation for Ia supernovae Phillips 1993; Kasen & Woosley 2007 GRB–SN lightcurves Li & Hjorth 2014 Standardized lightcurves Li & Hjorth 2014 Advantages of using GRB-SNe for cosmography Redshift known right away Host galaxies are faint at high z Can determine the extinction from the afterglow Time of explosion known Can predict the evolution, plan the observing campaign Bright (slightly brighter than SNe Ia) Time stretching Cheaper in terms of HST orbits than SN Ia GRB-SN Hubble diagram Li, Hjorth & Wojtak 2014 2σ evidence for dark energy from 8 GRB-SNe Li, Hjorth & Wojtak 2014 Superluminous supernovae Inserra & Smartt 2014 Simplistic picture for discussion! LLGRBs = engine, SBO, wide opening angles HLGRBs = jetted collapsars, Ni powered ULGRBs = magnetars, SLSNe SGRBs = NS-NS mergers = NIR KNe GRBs with no SNe = NS-NS mergers Origin of luminosity–width relation, usefulness for cosmography .
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