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/GRBSN 980425
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 1999; Bloom et al. 1999 Bloom al. et 1999; Gorosabel & Tirado Castro- 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 al. et Spectral evolution from afterglow power law to Stanek broad-lined Ic supernova like SN 1998bw Hjorth et al. 2003; 2003; Hjorth al. et Hjorth et al. 2003; Patat et al. 2001 -24
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-20 Host galaxy Afterglow (mag) V
M -18 Supernova
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-14 0 10 20 30 40 50 Time since explosion (days) Hjorth 2013 27 GRB-SNe in 19 years
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0 Spectroscopic diversity et al. 2015 al. et Modjaz Spectroscopic diversity et al. 2015 al. et Modjaz 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 al. et 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; al. et GRB 100316D/SN 2010bh -18 Gehrels
-16 Absolute magnitude (mag)
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GRB 060505 al.; et Gal-Yam Valle; Della al.; et 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 050509B GRB
HJorth et al. 2005 GRB 050709 GRB
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)
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GRB 050509B GRB 050709
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0 20 40 60 80 100 2005a,b Hjorth al. et 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