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A Radio Perspective on the GRB-SN Connection Alicia Soderberg May 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 10 2 Gpc -3 yr -1
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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 10 4 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 Nickel v ~ 60,000 km/s (Iwamoto et al.1998; Woosley et al. 1999) (Galama et al. 1998)
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8.5 GHz E ~ 5 x 10 49 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 Survey of 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
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Radio Analysis of SN 2003L (Soderberg et al., 2005a) Detailed Modeling: E ~ 10 49 erg v ~ 0.2c r ~ t B ~ r -1 n ~ r -2 M dot ~ 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 56 Ni 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 Ibc Radio limits imply unusual shock parameters and/or low densities.
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