The /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: 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