the most powerful explosions in the universe genesis and evolution of supernova and
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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. - PowerPoint PPT PresentationTRANSCRIPT
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The most powerful explosions in the Universe Genesis and evolution of Supernova and Gamma-Ray Burst Italian programs at ESO
EWASS 2012, Symposium 10: "30 years of Italian participation to ESO”
Elena Pian - INAF, Trieste Astronomical Observatory
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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
Supernovae
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Absolute light curves of 87 SN Ia
Diversity of SNIa
m15(B)
No STD candles !!
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Normal SNe Ia follow Phillips relation!
Altavilla et al. 2004
Pskovskii – Phillips relation
normal
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vv .. HVG 97 km/s/d HVG 97 km/s/d
LVG 37 km/s/dLVG 37 km/s/dFAINT 87km/s/dFAINT 87km/s/d
Si II 6355Si II 6355ÅÅ velocity evolution velocity evolution
≈≈MMBB
≈≈MMBB+2+2
Photospheric velocities of SN IaPhotospheric velocities of SN Ia
Benetti et al. 2005
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Velocity gradient vs. Velocity gradient vs. ΔΔmm1515
HVG
LVG
Faint
Benetti et al. 2005
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~0.13Msol~0.13Msol
~0.09Msol~0.09Msol
Applying density structure of W7Applying density structure of W7transform vtransform vexpexp(Si) in mass. (Si) in mass.
ByBy a adding it to the NSE mass, dding it to the NSE mass, wwe e oobtain a constant mass, btain a constant mass, 1.05±0.09 M1.05±0.09 Msunsun , with NO , with NO
DDependence on ependence on mm1515(B)(B)
SNe that produce less SNe that produce less 5656Ni Ni SSynthesize more IMEynthesize more IME
Mazzali et al. 2007
orro diagram!orro diagram! X M (NSE+IME) M (NSE) M (56Ni) M (54Fe + 58Ni)
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28 February 1997:
BeppoSAX starts localizing GRBs with arcminute accuracy: the “GRB afterglow era” has started
About 250 GRBs have been followed up with ESO telescopes
~100 keV
Gamma-Ray Bursts
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GRB970228: first detection of X-ray and optical afterglow
Van Paradijs et al. and the BeppoSAX team 1997
T0 + 21 hours T0 + 8 days
BeppoSAX detection of X-ray afterglowCosta et al 1997
NTT + SUSI, 13 March 1997
T0 + 8 hours T0 + 3 days
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GRB990510 (z = 1.6): optical afterglow
ESO NTT and 3.6m
The time decay is not a single power-law
Israel et al. 1999
Lin. Pol. 1.7±0.2%
VLT+FORS
Covino et al. 1999
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The optically brightest GRB
(z = 0.937)
Bloom et al. 2009
(z = 6.29)
(z = 1.6)
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GRB080319B: the robotic approach
Racusin et al. 2008
REM+TORTORA
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GRB080319B: VLT in Rapid Response Mode with UVES
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
Fe II λ2374 Fe II λ2396*
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Metallicity of GRB host galaxies
VLT+X-shooter
Piranomonte et al. 2011
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25 April 1998:
Gamma-Ray Bursts meet Supernovae
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z = 0.0085
GRB980425Supernova 1998bw (Type Ic)
Kinetic energy ~e52 erg
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Light Curves of GRB and XRF Supernovae at z < 0.3
Pian et al. 2006Bufano et al. 2012Melandri et al. 2012
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Photospheric velocities of Type Ic SNe
Pian et al. 2006Bufano et al. 2012
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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 Ic SNe.
GRB SNe are more luminous than XRF SNe. Is this telling us something about progenitors and remnants?
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The Future
NTT Supernova Large ProgramPI: 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 galaxiesPI: S. Piranomonte
VLT FORS GRB and X-ray Flash Supernova programPI: E. Pian and M. Della Valle