Gamma-Ray Bursts and Supernovae Tsinghua Transient Workshop 8 Nov 2012 Elena Pian INAF-Trieste Astronomical Observatory, Italy & Scuola Normale Superiore di Pisa, Italy
Jan 12, 2016
Gamma-Ray Bursts and Supernovae
Tsinghua Transient Workshop 8 Nov 2012
Elena Pian
INAF-Trieste Astronomical Observatory, Italy & Scuola Normale Superiore di Pisa, Italy
Bimodal distribution of GRBdurations
short
long
Different progenitors: SNevs binary NS mergers
Kulkarni 2000Duration (s)
z = 0.8
GRB990123 (z = 1.6)
V ~ 23.5
GRB020405 (z = 0.7)
GRB990510 (z = 1.6)V(host) = 28.5 !
z = 0.7 z = 0.8
Optical fields of long GRBs
Short GRB050509b (z = 0.22)
Bloom et al. 2005
Host galaxy
Early Multiwavelength Counterparts
(z = 0.937)
Bloom et al. 2008
(z = 6.29)
(z = 1.6)
Isotropic irradiated –ray energy vs redshift
Long GRB
Short GRB
GRB980425Supernova 1998bw (Type Ic)
z = 0.0085
Galama et al. 1998
GRB-Supernovae with ESO VLT+FORS
z = 0.168
z = 0.105
GRB031203/SN2003lw
GRB-SNe have kinetic energies exceeding those of normal SNe byan order of magnitude (e52 erg)Hjorth et al. 2003
Malesani et al. 2004
X-ray Flashes
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
VLT-FORS and Lick 3m monitoring of SN2006aj
Pian et al. 2006; Mazzali et al. 2006; Ferrero et al. 2006
SN2006aj (z = 0.033)
The modelling of the light curve and spectra of SN2006aj requires:
And suggests that:
Neutron Star?
GRB vs XRF: is the central remnantA black hole or neutron star?
~ 100~ 10
Starling et al. 2011
X-ray light curves of low-redshift GRBs
Shock breakout in SN2010bh (z = 0.059)
Cano et al. 2011
Gemini-South, Faulkes telescope, HST
GRB120422A/SN2012bz (z = 0.283)
Perley et al. 2012
26 April 2012
Light Curves of GRB and XRF Supernovae at z < 0.3
Melandri et al. 2012
GRB980425
GRBs with supernovae
GRB030329
GRB031203
GRB120422A
GRB120422A
Photospheric velocities of Type Ic SNe
Pian et al. 2006Bufano et al. 2012
Properties of SNe Ibc as f(Mprog)
2010bh
2010bh2010ah
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
light curves of the optical afterglow of the “normal” long GRB060614 (z = 0.125)
Della Valle et al. 2006
Gal-Yam et al. 2006
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
Long GRB060505 (z = 0.089): supernova search
Fynbo et al. 2006
Light curves of Ic SNe: GRB-SNe, broad-lined SNe, normal SNe
-14 GRB060614GRB060505
Della Valle et al. 2006Fynbo et al. 2006Gal-Yam et al. 2006
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. 2006Villasenor et al. 2005
HETE2/WXM
HETE2/WXM
HETE2/FREGATE
HETE2/FREGATE
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
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 theProgenitors of misaligned GRBs?
Simulated and analytical radio emission of GRBs
8.46 GHz
Van Eerten, Zhang, MacFadyen 2010