Multi-wavelength multi-site
Monitoring of Gamma-Ray
Burst-associated Supernovae
19 July 2012
Burst-associated Supernovae
Elena Pian
INAF-Trieste Astronomical Observatory and
Scuola Normale Superiore di Pisa, Italy
GRBs are brief flashes of soft γ-ray radiation (∼100 keV),
discovered in the 1970’s, the origin of which was not known
until 1997
CGRO-BATSE
8 hours 3 days
GRB970228: first detection of X-ray and optical afterglow
Van Paradijs et al. 1997
6 months
later
Costa et al. 1997
t−1.3
Bimodal
distribution
of GRB
durations
short
long
Different Different
progenitors:
SNe
vs binary NS
mergers
Kulkarni 2000Duration (s)
GRB-Supernovae with ESO VLT+FORS
z = 0.168
GRB031203/SN2003lw
z = 0.105
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
Swift was triggered by XRF060218 on Feb 18.149, 2006 UT
Prompt
event
afterglow
Campana et al. 2006
UVOT
Shock breakout or jet cocoon interaction with CSM,
Or central engine, or synchrotron + inverse Compton ?
SN
z = 0.033
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
SN2010bh (z = 0.059)
PROMPT, VLT/FORS, VLT/XS
Gemini-S/GMOS and Magellan Echellette
Bufano et al. 2012Chornock et al. 2010
UVOT
XRF080109/SN2008D (25 Mpc)
Gemini/GMOS
Palomar 60in
S-LOTIS
Swift/XRT
Soderberg et al. 2008
XRT observations
Of XRF080109
~e46 erg
VLT FORS spectra of SN2008D:
Broad lines disappear near main maximum and at the same time He lines develop: the He envelope brakes the high velocity material and prevents the formation of a powerful jet
Broad lines
Mazzali et al. 2008
He lines
Props of SNe Ibc as f(Mprog)
2010bh
SN 2012bz/
GRB120422A
SN 2012bz/
GRB120422A
2010bh
A minimum mass and energy seem to be required for GRBs:
Need more data and analysis to understand trend(Courtesy: P.Mazzali; K. Nomoto)
Summary and open problems
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. 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?
Not all Type Ic SNe make GRBs. Can these be misaligned with Respect to the line of sight?
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