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GRB-Supernova observations: S tate of the art

Probing the Supernova Mechanism by Observations 16 July 2012. GRB-Supernova observations: S tate of the art. Elena Pian INAF, Trieste Astronomical Observatory & Scuola Normale Superiore di Pisa, Italy.

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GRB-Supernova observations: S tate of the art

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  1. Probing the Supernova Mechanism by Observations 16 July 2012 GRB-Supernova observations: State of the art Elena Pian INAF, Trieste Astronomical Observatory & 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. The GRB distribution is isotropic

  4. GRB970228: first detection of X-ray and optical afterglow 8 hours 3 days Van Paradijs et al. 1997 6 months later Costa et al. 1997

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

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

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

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

  9. Relativistic jet model of a GRB: “Unified scheme” for GRBs and Sne?

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

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

  12. X-ray Flashes

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

  14. M(56Ni) = 0.2 Msun M(progenitor) = 20 Msun Mass of remnant is compatible With neutron star rather than Black hole SN2006aj (z = 0.033) Pian et al. 2006; Mazzali et al. 2006; Ferrero et al. 2006

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

  16. Shock breakout in SN2010bh (Cano et al. 2011) Starling derives an initial radius of 8e11 cm from X-ray spectroscopy

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

  18. z = 0.28

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

  20. VLT FORS spectra of GRB120422A/SN2012bz z = 0.283 SN1998bw SN2006aj

  21. GRB091127/SN2009nz (z = 0.49) Berger et al. 2011 Cobb et al. 2010

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

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

  24. Properties of GRB-SNe Berger et al. 2011

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

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

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

  28. Summary Most long GRBs and XRFs are associated with energetic spectroscopically identified Type Ic Sne. SNe associated with GRBs are more luminous than XRF-SNe 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 Not all long GRBs are accompanied by energetic Type Ic Sne Is the early high energy emission due to an engine (jet) or to shock breakout? Late time SN spectroscopy may be a tool to investigate this via reconstruction of supernova explosion geometry (VLT; Subaru)

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