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