1. Gamma-Ray Bursts and Supernovae Tsinghua Transient Workshop 8 Nov 2012 Elena Pian INAF-Trieste Astronomical Observatory, Italy & Scuola Normale Superiore di Pisa, Italy

2. GRBs are brief flashes of soft  -ray radiation (  100 keV), discovered in the 1970’s, the origin of which was not known until 1997 CGRO-BATSE

3. 1960-1970: Vela satellites 1991-2000: BATSE onboard the Compton Gamma Ray Observatory

4. The GRB distribution is isotropic

5. Light curves of GRBs Fluence ~ if cosmological relativistic conditions are implied: Lorentz factor  CGRO-BATSE (Fishman & Meegan 1995)

6. CGRO spectrum of a GRB

7. Bimodal distribution of GRB durations short long Different progenitors: SNe vs binary NS mergers Kulkarni 2000 Duration (s)

8. 1 degree5 arcmin Comparison between CGRO-BATSE and BeppoSAX accuracy BATSE BSAX

9. 1996-2002: The BeppoSAX revolution Wide Field Cameras

10. 8 hours3 days GRB970228: first detection of X-ray and optical afterglow 6 months later Costa et al. 1997 Van Paradijs et al. 1997

11. z = 0.8 GRB990123 (z = 1.6) V ~ 23.5 GRB020405 (z = 0.7) GRB990510 (z = 1.6) V(host) = 28.5 ! z = 0.7z = 0.8 Optical fields of long GRBs

12. GRB and Core Collapse SNe hosts observed with Hubble Space Telescope Fruchter et al.2006 CC-SNe from Hubble High-z SN Search + HST GOODS GRBs The morphologies are significantly different

13. Short GRB050509b (z = 0.22) Bloom et al. 2005 Host galaxy

14. Swift localization of GRBs

15. Early Multiwavelength Counterparts (z = 0.937) Bloom et al. 2008 (z = 6.29) (z = 1.6)

16. Redshift Measurement Djorgovski et al. 1999

17. Bloom et al. 1998,1999 Host galaxies exhibit emission lines of star formation: [O II], [O III], Balmer and Paschen series

18. Isotropic irradiated  –ray energy vs redshift Long GRB Short GRB

19. GRB model: a stellar collapse Or merger produces a relativistic jet  ~ 100  ~ 10

20. GRB980425 Supernova 1998bw (Type Ic) z = 0.0085 Galama et al. 1998

21. GRB-Supernovae with ESO VLT+FORS z = 0.168 z = 0.105 GRB031203/SN2003lw GRB-SNe have kinetic energies exceeding those of normal SNe by an order of magnitude (e52 erg) Hjorth et al. 2003 Malesani et al. 2004

22. X-ray Flashes

23. Swift was triggered by XRF060218 on Feb 18.149, 2006 UT Prompt event afterglow Shock breakout or jet cocoon interaction with CSM, Or central engine, or synchrotron + inverse Compton ? Campana et al. 2006 SN UVOT z = 0.033

24. VLT-FORS and Lick 3m monitoring of SN2006aj Pian et al. 2006; Mazzali et al. 2006; Ferrero et al. 2006 SN2006aj (z = 0.033)

25. The modelling of the light curve and spectra of SN2006aj requires: And suggests that: Neutron Star?

26. GRB vs XRF: is the central remnant A black hole or neutron star?  ~ 100  ~ 10

27. Starling et al. 2011 X-ray light curves of low-redshift GRBs

28. Shock breakout in SN2010bh (z = 0.059) Cano et al. 2011 Gemini-South, Faulkes telescope, HST

29. GRB120422A/SN2012bz (z = 0.283) Perley et al. 2012 26 April 2012

30. Light Curves of GRB and XRF Supernovae at z < 0.3 Melandri et al. 2012

31. GRB980425 GRBs with supernovae GRB030329 GRB031203 GRB120422A

32. Photospheric velocities of Type Ic SNe Pian et al. 2006 Bufano et al. 2012

33. GRB091127/SN2009nz (z = 0.49) Cobb et al. 2010 Gemini/GMOS, Berger et al. 2011

34. Properties of SNe Ibc as f(M prog ) 2010bh 2010ah A minimum mass and energy seem to be required for GRBs: Need more data and analysis to understand trend (Courtesy: P. Mazzali) SN 2012bz/ GRB120422A SN 2012bz/ GRB120422A

35. light curves of the optical afterglow of the “normal” long GRB060614 (z = 0.125) Della Valle et al. 2006 Gal-Yam et al. 2006

36. spectra of GRB060614 (z = 0.125): no SN features GMOS, 15 Jul 06 VLT, 29 Jul 06 Della Valle et al. 2006Gal-Yam et al. 2006

37. Long GRB060505 (z = 0.089): supernova search Fynbo et al. 2006

38. Light curves of Ic SNe: GRB-SNe, broad-lined SNe, normal SNe -14 GRB060614 GRB060505 Della Valle et al. 2006 Fynbo et al. 2006 Gal-Yam et al. 2006

39. GRB060614: “long” GRB (z = 0.125) GRB050709: short GRB (z = 0.16) Comparison of temporal profiles of long and short GRBs: soft tails Swift/BAT Dt < 20 ms Gehrels et al. 2006 Villasenor et al. 2005 HETE2/WXM HETE2/FREGATE

40. GRB060505: Swift/BAT and Suzaku/WAM time profiles Time delay between BAT and WAM is inconsistent with short GRB: Dt = 0.36 +- 0.05 seconds McBreen et al. 2008

41. Summary and open problems All long GRBs and XRFs at z < 0.3 (with 2 exceptions) are associated with energetic spectroscopically identified Type Ic Sne. However, most broad-lined energetic Ic SNe are not associated with GRBs. SNe associated with GRBs are more luminous than both XRF-Sne and broad-lined Ic Sne with no GRB Mechanisms: Collapsar: a BH forms after the core collapses, and rapid accretion on it feeds the GRB jet. Magnetar: the NS spin-down powers a relativistic jet Is the early high energy emission due to an engine (jet) or to shock breakout? Are energetic, GRB-less Ic Sne the Progenitors of misaligned GRBs?

42. Simulated and analytical radio emission of GRBs 8.46 GHz Van Eerten, Zhang, MacFadyen 2010

43. HST Fields of GRBs (physical scale across each image is about 7 kpc) Starling et al. 2011

44. GRB/XRFs associated with supernovae Zhang et al. 2012, arXiv:1206.0298