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Going out with a bang: HSTs continuing contribution to gamma-ray bursts Andrew Levan University of Warwick

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Javier Gorosabel Urkia 27 Oct 1969- 21 Apr 2015 A major contributor to the field of gamma-ray bursts from the first afterglows to today

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What are they? What are they useful for? What are they? What are they useful for? Fermi/LAT

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1960 2020 1973 - Discovery of GRBs (VELA, Konus) 1993 - Long bursts / short bursts - (Konus, BATSE) 1997 - Afterglows 2003 - Long bursts - SNe 1997 now: Host galaxies (locations, morphology, LF, probes etc) 2005 - GRBs at z>6 2009 - GRBs at z>8 2005-now - Short GRBs - KNe 2011 GRBs from relativistic tidal flares 2013 - Ultralong GRBs 1993 - Isotropic on sky (very near or far) 2008 Naked eye GRB Vela (0) Konus (0) BATSE (0)BeppoSAX (30)HETE-2 (30)Swift (800) Missions (number located 40 M ), H-poor stars at metalicity < solar Fruchter et al. 2006, Svensson et al. 2010 Larsson et al. 2007 8,20,40,60,80 M See also Blanchard poster for new results

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Long-GRBs as high-z probes T+17h T+19h z=7.9 z=8.2 These sources have H(AB)~23-24 at 2-3 days, possible for WFC grisms Tanvir et al. 2009, Tanvir et al. in prep Afterglow Host galaxy F160W, 26000sF160W, 10000s

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Next goals: Long-GRBs GRBs at z>9 Swift/GROUND/HS T grism Hosts at z>7 HST (if lucky), JWST GRB/SNe as standard candles? HST (to test), JWST (to be useful) Phot-z = 9.4: Cuccharia et al. 2011 A GRB-SNe Philips relation? Cano 2014; Li, Hjorth & Wojtak 2014

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Short-GRB hosts +1 AGN Fong et al., Fruchter et al. in prep

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Contrasting locations Fong et al. 2013, Fruchter et al. in prep

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Kilonovae short bursts Tanvir et al. 2013, Berger et al. 2013

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Next goals: Short-GRBs Kilonovae Direct optical/IR spectrum (grism ideal) Sample, r-process production, ejection into ISM. Gravitational wave counterparts Advanced detectors operation end 2015 Clear distinction between NS-NS and NS-BH Clean rate measurements Simultaneous GW/GRB unambiguous progenitor identification

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Summary Progress in GRBs is a triumph of a multi-wavelength, multi- observatory approach. Swift/Fermi -> Ground -> Chandra/HST/Spitzer Through this we now know the progenitors of both long- and short- GRBs and are deploying them as powerful cosmological probes. Star formation rate Properties of early galaxies Heavy element production Large facilities (HST, JWST, ELTs etc) are crucial, but for GRBs (or any kind of transient) they do not stand alone.

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1960 2020 1973 - Discovery of GRBs (VELA, Konus) 1993 - Long bursts / short bursts - (Konus, BATSE) 1997 - Afterglows 2003 - Long bursts - SNe 1997 now: Host galaxies (locations, morphology, LF, probes etc) 2005 - GRBs at z>6 2009 - GRBs at z>8 2005-now - Short GRBs - KNe 2011 GRBs from relativistic tidal flares 2013 - Ultralong GRBs 1993 - Isotropic on sky (very near or far) 2008 Naked eye GRB Vela (0) Konus (0) BATSE (0)BeppoSAX (30)HETE-2 (30)Swift (800) SVOM Missions (number located 9 Host galaxy detections at z>7 from JWST? Short GRB kilonova characterisation Gravitational-wave counterparts GRB cosmology? Progenitors of new GRB populations (ultralong etc)