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1/47 Recent Progress in Gamma-ray Bursts: S. R. Kulkarni California Institute of Technology Image Credit: NASA E/PO, Sonoma State University, Aurore Simonnet Slide 2 2/47 Slide 3 3/47 Long & Short Slide 4 4/47 The Gang and collaborators T. Piran, Hebrew U. P. A. Price, U. Hawaii J. Rich, ANU M. Rauch, Carnegie K. Roth, Gemini Obs M. Roth, Carnegie D. J. Sand, Caltech B. P. Schmidt, ANU S. Shectman, Carnegie A. M. Soderberg, Caltech M. Takada, Tohuku U. T. Totani, Kyoto U. W. T. Vestrand, LANL D. Watson, U. Copenhagen R. White, LANL P. Wozniak, LANL J. Wren, LANL G. Kosugi, NAOJ W. Krzeminski, Carnegie S. R. Kulkarni, Caltech P. Kumar, U. Texas D. C. Leonard, Caltech B. L. Lee, U. Toronto A. MacFadyen, IAS P. J. McCarthy, Carnegie D. -S. Moon, Caltech D. C. Murphy, Carnegie E. Nakar, Caltech H. S. Park, LLNL B. Penprase, Pomona C. S. E. Persson, Carnegie B. A. Peterson, ANU M. M. Phillips, Carnegie K. Aoki, NAOJ E. Berger, Carnegie P. B. Cameron, Caltech R. A. Chevalier, U. Virginia S. B. Cenko, Caltech L. L. Cowie, U. Hawaii A. Dey, NOAO S. Evans, LANL D. B. Fox, Penn S./Caltech D. A. Frail, NRAO H. Furusawa, TIT A. Gal-Yam, Caltech F. A. Harrison, Caltech K. C. Hurley, UC Berkeley M. M. Kasliwal, Caltech N. Kawai, TIT Slide 5 5/47 Collaborators T. Piran, Hebrew U. P. A. Price, U. Hawaii J. Rich, ANU M. Rauch, Carnegie K. Roth, Gemini Obs M. Roth, Carnegie D. J. Sand, Caltech B. P. Schmidt, ANU S. Shectman, Carnegie A. M. Soderberg, Caltech M. Takada, Tohuku U. T. Totani, Kyoto U. W. T. Vestrand, LANL D. Watson, U. Copenhagen R. White, LANL P. Wozniak, LANL J. Wren, LANL G. Kosugi, NAOJ W. Krzeminski, Carnegie S. R. Kulkarni, Caltech P. Kumar, U. Texas D. C. Leonard, Caltech B. L. Lee, U. Toronto A. MacFadyen, IAS P. J. McCarthy, Carnegie D. -S. Moon, Caltech D. C. Murphy, Carnegie E. Nakar, Caltech H. S. Park, LLNL B. Penprase, Pomona C. S. E. Persson, Carnegie B. A. Peterson, ANU M. M. Phillips, Carnegie K. Aoki, NAOJ E. Berger, Carnegie P. B. Cameron, Caltech R. A. Chevalier, U. Virginia S. B. Cenko, Caltech L. L. Cowie, U. Hawaii A. Dey, NOAO S. Evans, LANL D. B. Fox, Penn S./Caltech D. A. Frail, NRAO H. Furusawa, TIT A. Gal-Yam, Caltech F. A. Harrison, Caltech K. C. Hurley, UC Berkeley M. M. Kasliwal, Caltech N. Kawai, TIT Slide 6 6/47 Long Duration Bursts: Collapsar Model: Woosley, Heger, MacFadyen Kulkarni et al. Bloom et al. Frail et al. Berger et al. Soderberg etal Slide 7 7/47 SN 1998bw/GRB 980425 Galama et al. 1998, Kulkarni et al. 1998 E ~10 48 erg (isotropic) Slide 8 8/47 Collapsar: The Movie A Hollywood-Bollywood Production From Bogus Enterprise, A Division of General Propaganda Slide 9 9/47 Slide 10 10/47 With physics and lots of hardwork (MacFadyen) Slide 11 11/47 A New Family of Cosmic Explosions : Soderberg Slide 12 12/47 Keck Laser Guide Star AO Slide 13 13/47 Progenitors of Ibc SNe: A Hot Result Slide 14 14/47 Palomar 60-inch: A second life Slide 15 15/47 Exploitation of GRBs has already begun Reichart et al. 2005 Berger et al. GRB 050904: z=6.2 Observations at 3 hours (P60, optical; SOAR, NIR) Slide 16 16/47 Slide 17 17/47 Two classes of GRBs Short - Hard Long - Soft Slide 18 18/47 Summarizing Four Papers 1.Fox et al. The afterglow of GRB 050709 and the nature of the short-hard -ray bursts, Nature, October 6, 2005 2.Berger et al. A merger origin for short -ray bursts inferred from the afterglow and host galaxy of GRB 050724, Nature, November, 2005 3.Kulkarni Modeling Macronovae 4.Kulkarni et al. Constraints on supernova-like emission associated with the short-hard gamma-ray burst 050509b Slide 19 19/47 Toward the SHB Progenitor: Redux How far away are they? How much energy do they release? is the energy release isotropic or collimated? are the central engines long or short-lived? Is there associated non-relativistic ejecta? What are the progenitors? Clue (macro) = host galaxy + offset Clue (micro) = circumburst environment The key to answering these questions has been the precise positions enabled by the discovery of long-lived afterglows. Slide 20 20/47 GRB 050509B: Swift Detection BAT: very faint GRB XRT: T+62 s detects 11 photons(!) No optical, no radio. very faint limits Low energy event and/or low density medium? Giant elliptical galaxy in cluster. z=0.22 Host? Gehrels et al. 2005 T 90 =40 ms Slide 21 21/47 Bloom et al. 2005 NSC J123610+285901 z=0.225 Slide 22 22/47 Kulkarni et al. 2005 GRB 050505B: Keck/Subaru Error radius = 9.3 arcsec Slide 23 23/47 HST Imaging: No Supernova Kulkarni et al. 2005 Error radius = 9.3 arcsec 4 HST Epochs May 14 to June 10 48 sources in XRT error circle Giant elliptical Bloom et al L=1.5L * SFR 28/47 GRB 050709: Panchromatic Studies X-ray source flares for initial 6 ks of 18 ks in second epoch Long-lived central engine? early and late flux do not fit Optical inconsistent with simple PL decay (slope=-1.3 --> -2.8) jet break at T+10 d SN limits M R >-12 mag Radio violate simple AG model Fox et al. 2005; Hjorth et al. 2005 Slide 29 29/47 GRB 050724: Swift Detection Brightest Swift SHB Hard spike/soft bump X-ray, optical and radio afterglow detected Barthelmy al. 2005 T 90 =40 ms 15-150 keV 15-25 keV T 90 =3 s 250 ms 100 s Slide 30 30/47 Barthelmy al. 2005 Slide 31 31/47 Berger et al. 2005 GRB 050724: Swift Slide 32 32/47 Kulkarn i & C ameron Red elliptical z=0.258 L=1.6 L * SFR 33/47 Toward the SHB Progenitor How far away are they? At least some short bursts are z ~ 0.2 How much energy do they release? About 10 49 to 10 50 erg Evidence for ``jets Is there an associated supernova explosion? Supernova, if any, are faint (M v > -13) What are they? Both elliptical and star-forming host galaxies Slide 34 34/47 Comparison to Long Duratrion Gamma-ray Bursts Slide 35 35/47 Empirical Connection to Ia Supernovae Nakar & Gal-Yam Slide 36 36/47 Binary Coalescence 1 Collapsar Magnetar 1 111 Energy Density Host Offset No SNe 1 1 00 0 0 1 00 1 The Score Card Slide 37 37/47 Holy smokes, he is dead?!! Ph: Glendinning Slide 38 38/47 Coalescence of Neutron Stars (Shibata) Slide 39 39/47 Black Hole-Neutron Star (Rupert, Janka) Slide 40 40/47 Macronova Is there a sub-relativistic explosion accompanying short hard bursts? Li & Paczynski 1998 If so, (observationally) > Nova < Supernova => Mini-supernova or Macronova Kulkarni Slide 41 41/47 Macronova Model Parameters: M ejecta & v= c Composition Free Neutrons Radioactive Nickel Neutron Rich Material (non-radioactive) Injection of energy essential for macronova to shine and be detectable Slide 42 42/47 Nickel Decay Slide 43 43/47 r-process and s-process elements Slide 44 44/47 Slide 45 45/47 Comparison to Data (GRB 050509b) =0.5 =0.05 Slide 46 46/47 The Macronova as a Reprocessor Slide 47 47/47 Slide 48 48/47 Slide 49 49/47 Slide 50 50/47 Quasars: A Historical Analogy, II Scintillation: Interplanetary Scintillation showed that quasars were compact The Central Engine: After three decades we have a working model involving black holes The Pesky Jets: Questions remain FRI and FRII What is the difference between radio quiet and radio loud AGN? Unification: The desire to unify various classes of quasars drove much of quasar research. Slide 51 51/47 Quasars: A Historical Analogy, I Astonished & Impressed: The immense power and energy of quasars resulting from Schmidts discovery of redshift. Amused and Educated: Relativistic effects such as super-luminal motion were anticipated by Rees. Ruthless Exploitation: Ask not why quasars quase but simply use them as light beacons to study the IGM. Slide 52 52/47 The Macronova as a reprocessor Long lived central soure (e.g. magnetar) Long lived accretion disk There are already indications of tremendous late time activity. Slide 53 53/47 SHBs Observational Milestones 050509B rapid arcsecond (+/-9.3) localization of X-ray emission (AG?) tentative host is elliptical galaxy in merging cluster (z=0.225) macronova and SNe limits 050709 sub-arcsecond position of X-ray afterglow unambiguous identification of spiral host galaxy & redshift (z=0.16) discovery of optical afterglow evidence that outflows are jet-like evidence that central engines remain active for days to weeks 050724 discovery of first radio afterglow unambiguous identification of red elliptical host galaxy (z=0.257) Slide 54 54/47 Coalescence --> Black Hole (Shibata) Slide 55 55/47 Gal Yam Slide 56 56/47 Possible SHB Progenitors Magnetar Highly magnetized young neutron star (10 14 -10 15 G) Crustal breaking and magnetic reconnection = hyper-flares short (0.2 s) hard pulse and long (300 s), soft pulse Dominant timescale is Alfven velocity in NS Collapsar Massive star core collapses to black hole + short-lived accretion disk Nicely explains long-soft bursts Dominant timescale is set by jet propagation in CO core (20 s) Shorter timescales = collimated jet that wanders due to instabilities Binary Coalescence Merging compact remnants (WD, NS, & BH) Hypercritical accretion onto a newly formed BH Dominant timescale is set by accretion disk viscosity Slide 57 57/47 Slide 58 58/47 Taken from K.Thorne NSF Review talk Widely expected based on burst brightness distribution =0.39+/0.02 luminosity similar to long bursts but duration 100x less predicts faint AG Future z distribution will constrain merger timescale Tavnir et al (astro-ph) suggests 5-25% SHB are at d 62/47 Use this Slide in Italy. X-ray source flares for initial 6 ks of 18 ks in second epoch Long-lived central engine? early and late flux do not fit Optical inconsistent with simple PL decay ( 1 =-1.3 and 2 =-2.8) jet break at T+10 d SNe limits M R >-12 mag Radio violate simple AG model Fox et al. 2005 Slide 63 63/47 GRB 050709: Optical Afterglow Price et al. 2005 and Hjorth et al 2005 T+1.42 d T+2.39 d TT Decays as t -1.3 1.5m Danish Telescope, La Silla Slide 64 64/47 GRB 050724: Gemini Spectra Prochaska et al. ; Berger et al. 2005 z=0.257 Slide 65 65/47 Short Bursts and Gravitational Waves Slide 66 66/47 Fryer, Woosley & Hartmann 1999 Ruffert & Janka 2001 Slide 67 67/47 Palomar 60-inch: Now a robotic telescope