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 10 2 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 10 4 Gpc -3 yr -1 ~ 0.5 % of SNe Ibc associated with GRBs

4. GRBs ? SNe Ibc Spherical + Jet Framework connection

5. (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”

6. 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)

7. 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”

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 (Soderberg et al. 2005; Berger et al. 2002,03; Kulkarni et al. 1998) Radio bright SN Ibc are rare and diverse.

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

11. 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

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

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

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

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

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

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

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

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

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

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

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 (Soderberg et al., 2005c)  GRB-SNe do NOT necessarily synthesize more 56 Ni than local SNe Ibc.

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.