Going out with a bang: HSTs continuing contribution to
gamma-ray bursts Andrew Levan University of Warwick
Slide 2
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
Slide 3
What are they? What are they useful for? What are they? What
are they useful for? Fermi/LAT
Slide 4
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
Slide 13
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
Slide 14
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
Slide 15
Short-GRB hosts +1 AGN Fong et al., Fruchter et al. in
prep
Slide 16
Contrasting locations Fong et al. 2013, Fruchter et al. in
prep
Slide 17
Kilonovae short bursts Tanvir et al. 2013, Berger et al.
2013
Slide 18
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
Slide 19
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.
Slide 20
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)