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A Radio Perspective on the GRB-SN Connection

A Radio Perspective on the GRB-SN Connection . Alicia Soderberg May 25, 2005 – Zwicky Conference. Gamma-Ray Bursts. highly relativistic ( ~100) jets ( ~ few degrees) -ray emission mildly relativistic (<10) ejecta produce “afterglow” emission imply central engine

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A Radio Perspective on the GRB-SN Connection

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  1. A Radio Perspective on the GRB-SN Connection Alicia Soderberg May 25, 2005 – Zwicky Conference

  2. 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

  3. 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 ? Type Ibc Supernovae ~ 0.5 % of SNe Ibc associated with GRBs

  4. Spherical + Jet Framework connection ? GRBs SNe Ibc

  5. GRB980425 and Type Ic SN1998bw“A GRB/SN Connection” • z=0.0085 (~36 Mpc) • SN1998bw discovered within BeppoSAX error box for GRB 980425 • Two key probes: Optical & Radio (Galama et al., 1998; Pian et al. 2000)

  6. (Galama et al. 1998) 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)

  7. 8.5 GHz GRB980425 and Type Ic SN1998bw“The most luminous radio SN” E~ 5 x 1049 erg ~3 ejecta (Kulkarni et al.1998; Li & Chevalier 1999) What fraction of SNe Ibc are like SN1998bw?

  8. 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

  9. VLA Survey of Type Ibc Supernovae Results: 11 detections 82 upper limits Radio bright SN Ibc are rare and diverse. (Soderberg et al. 2005; Berger et al. 2002,03; Kulkarni et al. 1998)

  10. Equipartition Energy and Velocity Out of 93 SNe, none like SN1998bw and/or GRBs < 1% GRB/SN

  11. Radio Analysis of SN 2003L • Detailed Modeling: • E ~ 1049 erg • v ~ 0.2c • r ~ t • B ~r -1 • n ~r -2 • Mdot ~ 10-5 M/yr (Soderberg et al., 2005a)

  12. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time) No -rays seen

  13. “Hidden” GRB Jets in Local SNe Ibc Afterglow begins log (F) log (time)

  14. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time)

  15. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time) Type Ibc SN!

  16. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time)

  17. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time)

  18. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time)

  19. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time)

  20. “Hidden” GRB Jets in Local SNe Ibc log (F) log (time)

  21. “Hidden” GRB Jets in Local SNe Ibc t ~ 1 week to few yrs log (F) log (time)

  22. 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)

  23. OPTICAL: Peak SN magnitudes • GRB-SNe do NOT necessarily synthesize more 56Nithan local SNe Ibc. (Soderberg et al., 2005c)

  24. 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.

  25. Broad-lined SNe Ibc Radio limits imply unusual shock parameters and/or low densities.

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