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A Radio Perspective on the GRB-SN Connection
Alicia SoderbergMay 25, 2005 – Zwicky Conference
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Gamma-Ray Bursts
• highly relativistic (~100) jets ( ~ few degrees) -ray emission
• mildly relativistic (<10) ejecta produce “afterglow” emission
• imply central engine
• spherical explosion produces non-relativistic (<1) optical SN emission (Type Ibc)
• Rate: ~2.5 x 102 Gpc-3 yr-1
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Type Ibc Supernovae
?
Type Ibc Supernovae
• NO H in optical spectra (10%)
• NO -ray emission
• NON-relativistic, <1, synchrotron emission from mildly asymmetric ejecta
• NO evidence for central engines
• spherical explosion drives non-relativistic optical SN
• Rate: 4.8 x 104 Gpc-3 yr-1~ 0.5 % of SNe Ibc associated with GRBs
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GRBs
?
SNe Ibc
Spherical + Jet Framework
connection
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(Galama et al., 1998; Pian et al. 2000)
z=0.0085 (~36 Mpc)
SN1998bw discovered within BeppoSAX error box for GRB 980425
Two key probes:
Optical & Radio
GRB980425 and Type Ic SN1998bw“A GRB/SN Connection”
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GRB980425 and Type Ic SN1998bw“A luminous local SN”
Optical emission requires:
~ 0.5 M Nickelv ~ 60,000 km/s
(Iwamoto et al.1998; Woosley et al. 1999)
(Galama et al. 1998)
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8.5 GHzE ~ 5 x 1049 erg
~3 ejecta
(Kulkarni et al.1998; Li & Chevalier 1999)
What fraction of SNe Ibc are like SN1998bw?
GRB980425 and Type Ic SN1998bw“The most luminous radio SN”
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RADIO is most sensitive to relativistic ejecta
1. Synchrotron emission traces the fastest ejecta
2. The synchrotron peak is near/below the radio band.
3. Higher frequencies dominated by other processes.
Observe EVERY (optically selected) SN Ibc within 100 Mpc
Caltech/NRAO/ATCA Radio Type Ibc SN Survey
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VLA Surveyof Type Ibc Supernovae
Results:11 detections
82 upper limits
(Soderberg et al. 2005; Berger et al. 2002,03; Kulkarni et al. 1998)Radio bright SN Ibc are rare and diverse.
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Equipartition Energy and Velocity
Out of 93 SNe, none like SN1998bw and/or GRBs
< 1% GRB/SN
€
∝ d−1/17Fν ,p8 /17ν p
−1 μas
E ∝ d2Fν ,p4 ν p
−7θ−6 erg
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Radio Analysis of SN 2003L
(Soderberg et al., 2005a)
Detailed Modeling: E ~ 1049 erg
v ~ 0.2c
r ~ t
B ~ r -1
n ~ r -2
Mdot ~ 10-5 M/yr
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
No -rays seen
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
Afterglow begins
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
Type Ibc SN!
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
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log (time)
log
(F)
“Hidden” GRB Jets in Local SNe Ibc
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log (time)
log
(F)
t ~ 1 week to few yrs
“Hidden” GRB Jets in Local SNe Ibc
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Constraints on Off-Axis GRBs
Out of 53 SNe Ibc,
None house GRBs
< 2% GRB/SN
Broad-lined events
are NO exception
< 20% GRB/BL
(Soderberg et al. in prep)
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OPTICAL: Peak SN magnitudes
(Soderberg et al., 2005c)
GRB-SNe do NOT necessarily synthesize more 56Ni than local SNe Ibc.
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Conclusions & Future Progress
Radio SNe Ibc are rare and diverse. Their optical properties are similarly diverse and overlap with GRBs
~10 % are radio bright
< 1% with relativistic ejecta
< 2% with off-axis GRB jets
ATA will enable further progress, but SN studies will still be limited by optical discoveries.
We need MORE small telescope campaigns.
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Broad-lined SNe IbcRadio limits
imply unusual
shock parameters and/or low densities.