Recent Progress in Gamma-ray Bursts:

1. Recent Progress in Gamma-ray Bursts: S. R. Kulkarni California Institute of Technology Image Credit: NASA E/PO, Sonoma State University, Aurore Simonnet

3. Long & Short

4. 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 The Gang and collaborators 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

5. 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 Collaborators 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

6. Long Duration Bursts: Kulkarni et al. Bloom et al. Frail et al. Berger et al. Soderberg etal Collapsar Model: Woosley, Heger, MacFadyen

7. SN 1998bw/GRB 980425 E~1048 erg (isotropic) Galama et al. 1998, Kulkarni et al. 1998

8. Collapsar: The Movie A Hollywood-Bollywood Production From Bogus Enterprise, A Division of General Propaganda

10. With physics and lots of hardwork (MacFadyen)

11. A New Family of Cosmic Explosions: Soderberg

12. Keck Laser Guide Star AO

13. Progenitors of Ibc SNe: A Hot Result

14. Palomar 60-inch: A second life

15. Exploitation of GRBs has already begun GRB 050904: z=6.2 Observations at 3 hours (P60, optical; SOAR, NIR) Berger et al. Reichart et al. 2005

17. Two classes of GRBs Short - Hard Long - Soft

18. Summarizing Four Papers • Fox et al. “The afterglow of GRB 050709 and the nature of the short-hard γ-ray bursts”, Nature, October 6, 2005 • Berger et al. “A merger origin for short γ-ray bursts inferred from the afterglow and host galaxy of GRB 050724”, Nature, November, 2005 • Kulkarni “Modeling Macronovae” • Kulkarni et al. “Constraints on supernova-like emission associated with the short-hard gamma-ray burst 050509b

19. 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.

20. 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? GRB 050509B: Swift Detection Gehrels et al. 2005 T90=40 ms

21. NSC J123610+285901 z=0.225 Bloom et al. 2005

22. HST Imaging: No Supernova 48 sources in XRT error circle Error radius = 9.3 arcsec 4 HST Epochs May 14 to June 10 Giant elliptical Bloom et al L=1.5L* SFR<0.1 M yr-1 Kulkarni et al. 2005

23. A Hard spike, 84 keV A Soft (PL) bump (alpha=-2) Roughly equal energy in each component GRB 050709: HETE Detection Villasenor et al. 2005 T90=70 ms

24. GRB 050709: Accurate Localization GRB SXC c Fox et al. 2005

25. HST imaging & search for supernova explosion Fox et al. 2005

26. 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 MR>-12 mag • Radio • violate simple AG model Fox et al. 2005; Hjorth et al. 2005

27. Brightest Swift SHB Hard spike/soft bump X-ray, optical and radio afterglow detected GRB 050724: Swift Detection 15-150 keV 250 ms T90=3 s Barthelmy al. 2005 T90=40 ms 15-25 keV 100 s

28. Barthelmy al. 2005

29. GRB 050724: Swift Berger et al. 2005

30. Red elliptical z=0.258 L=1.6 L* SFR<0.03 M yr-1 Kulkarni & Cameron

31. 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 1049 to 1050 erg • Evidence for ``jets’’ • Is there an associated supernova explosion? • Supernova, if any, are faint (Mv > -13) • What are they? • Both elliptical and star-forming host galaxies

32. Comparison to Long Duratrion Gamma-ray Bursts

33. Empirical Connection to Ia Supernovae Nakar & Gal-Yam

34. The Score Card Energy Density Host Offset No SNe Magnetar 0 0 1 0 1 Collapsar 1 1 0 0 0 Binary Coalescence 1 1 1 1 1

35. Holy smokes, he is dead?!! Ph: Glendinning

36. Coalescence of Neutron Stars (Shibata)

37. Black Hole-Neutron Star (Rupert, Janka)

38. Macronova • Is there a sub-relativistic explosion accompanying short hard bursts? Li & Paczynski 1998 • If so, (observationally) > Nova < Supernova => “Mini-supernova” or “Macronova” Kulkarni

39. Macronova Model • Parameters: Mejecta & v=c • Composition • Free Neutrons • Radioactive Nickel • Neutron Rich Material (non-radioactive) • Injection of energy essential for macronova to shine and be detectable

40. Nickel Decay

41. r-process and s-process elements

43. Comparison to Data (GRB 050509b) =0.5 =0.05

44. The Macronova as a Reprocessor

48. 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.

49. Quasars: A Historical Analogy, I • Astonished & Impressed: The immense power and energy of quasars resulting from Schmidt’s 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.

50. 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.