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The most powerful explosions in the Universe Genesis and evolution of Supernova and

EWASS 2012, Symposium 10: "30 years of Italian participation to ESO ”. The most powerful explosions in the Universe Genesis and evolution of Supernova and Gamma-Ray Burst Italian programs at ESO. Elena Pian - INAF, Trieste Astronomical Observatory. Supernovae.

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The most powerful explosions in the Universe Genesis and evolution of Supernova and

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  1. EWASS 2012, Symposium 10: "30 years of Italian participation to ESO” The most powerful explosions in the Universe Genesis and evolution of Supernova and Gamma-Ray Burst Italian programs at ESO Elena Pian - INAF, Trieste AstronomicalObservatory

  2. Supernovae The detection of SN1987A boosted the Supernova research at ESO In the 1990s, the ESO programs led by the Supernova group in Padova pioneered and developed the concept of Target-of-Opportunity on “unpredictable” sources

  3. Diversity of SNIa Absolute light curves of 87 SN Ia m15(B) No STD candles !!

  4. Normal SNeIa follow Phillips relation! Pskovskii – Phillips relation normal Altavilla et al. 2004

  5. Photospheric velocities of SN Ia . v Si II 6355Å velocity evolution HVG 97 km/s/d LVG 37 km/s/d FAINT 87km/s/d ≈MB ≈MB+2 Benetti et al. 2005

  6. Velocity gradient vs. Δm15 HVG Faint LVG Benetti et al. 2005

  7. orro diagram! Applying density structure of W7 transform vexp(Si) in mass. By adding it to the NSE mass, we obtain a constant mass, 1.05±0.09 Msun , with NO Dependence on m15(B) SNe that produce less 56Ni Synthesize more IME X M (NSE+IME) M (NSE) M (56Ni) M (54Fe + 58Ni) ~0.09Msol ~0.13Msol Mazzali et al. 2007

  8. Gamma-Ray Bursts 28 February 1997: BeppoSAX starts localizing GRBs with arcminute accuracy: the “GRB afterglow era” has started ~100 keV About 250 GRBs have been followed up with ESO telescopes

  9. GRB970228: first detection of X-ray and opticalafterglow NTT + SUSI, 13 March 1997 T0 + 21 hours T0 + 8 days Van Paradijs et al. and the BeppoSAX team 1997 T0 + 8 hours T0 + 3 days BeppoSAXdetection of X-rayafterglow Costa et al 1997

  10. GRB990510 (z = 1.6): optical afterglow Lin. Pol. 1.7±0.2% VLT+FORS ESO NTT and 3.6m The time decay is not a single power-law Israel et al. 1999 Covino et al. 1999

  11. The optically brightest GRB (z = 0.937) (z = 6.29) (z = 1.6) Bloom et al. 2009

  12. GRB080319B: the robotic approach REM+TORTORA Racusin et al. 2008

  13. GRB080319B: VLT in Rapid Response Mode with UVES Fe II λ2374 Fe II λ2396* z = 0.937 Detection of variable absorption lines and identification of 6 absorbers in a velocity range of 100 km/s D’Elia et al. 2009

  14. Metallicity of GRB host galaxies VLT+X-shooter Piranomonte et al. 2011

  15. 25 April 1998: Gamma-Ray Bursts meet Supernovae

  16. GRB980425 Supernova 1998bw (TypeIc) z = 0.0085 Kineticenergy ~e52 erg

  17. Light Curves of GRB and XRF Supernovae at z < 0.3 Pian et al. 2006 Bufano et al. 2012 Melandri et al. 2012

  18. Photospheric velocities of Type IcSNe Pian et al. 2006 Bufano et al. 2012

  19. Summary A constant burned mass and a common explosion mechanism for Type Ia Supernovae: This may help in understanding their role as standard candles GRB optical flashes and afterglows: Study of physics (photometry and multiwavelength comparison) and environments (spectroscopy) GRB and XRF Supernovae: highly energetic Type IcSNe. GRB SNe are more luminous than XRF SNe. Is this telling us something about progenitors and remnants?

  20. The Future NTT Supernova Large Program PI: S. Benetti Public ESO Spectroscopic Survey for Transient Objects (PESSTO) PI: S. Smartt, important Italian role with S. Benetti and S. Valenti VLT FORS Type Ib/c and IIb Supernova program (late phase) PI: P. Mazzali VLT X-Shooter GTO TOO program (Denmark, France, Italy The Netherlands) PI: J. Fynbo, Italian Co-PI: S. Covino VLT X-Shooter GTO program on GRB host galaxies PI: S. Piranomonte VLT FORS GRB and X-ray Flash Supernova program PI: E. Pian and M. Della Valle

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