Insights from Radio Wavelengths into Supernova Progenitors

1. Insights from Radio Wavelengths into Supernova Progenitors Laura Chomiuk Jansky Fellow, Michigan State University

2. Supernova Types: I vs. II Type I: No Hydrogen Thermonuclear WD explosions (Ia) and Core collapse of massive stars stripped of H envelopes (Ib/c) Type II: Show Hydrogen Core collapse of massive stars with H envelope

3. Supernova Types: A Continuum of H-richness

4. A diverse, complicated zoo of massive stars and core-collapse SNe + SNeIa (Smartt 2009)

5. Searching for SN progenitors directly with optical imaging SN 2005gl Before During After

6. Or, constraining SN progenitors indirectly-- in the radio Soderberg et al (2008)

7. SN 1970G: The first SN detected in the radio (Gottesman et al. 1972, Goss et al. 1973)

9. shell

10. synchrotron τ ≈ 1 fading because blast decelerates and CSM decreases in density absorbed (either free-free or synchrotron) SN 1994I @ 20 cm Weiler et al. (2011)

11. vw ≈ 30 km/s vsn ≈ 10,000 km/s SN blast probes ~1 year of mass loss in one day!

12. What makes a SN bright at radio wavelengths? • A fast blastwave • Expansion into dense surroundings

13. Radio bolsters a division in Type I SNe: Type Ib/c: Show radio emission, core collapse Type Ia: No radio emission, thermonuclear (Panagia et al. 1986)

14. Relativistic SN 1998bw associated with GRB 980425 (Galama et al. 1998) (Kulkarni et al. 1998, Wieringa et al. 1999)

15. A diversity of mass loss histories SN 2003bg (Soderberg et al. 2006)

16. Shells, Spirals, and Shelves SN 2007bg (Salas et al. 2012) SN 2001ig (Ryder et al. 2004) SN 1993J (Weiler et al. 2007)

17. SNeIb/c: WR stars or interacting binaries?

18. M yr-1/ km s-1 Mdot/vwind= 10-10 10-9 10-8 10-7 10-6 SNeIb/c show mass loss rates consistent with WR stars.

19. Still no radio emission from SNeIa (Panagia et al. 2006) Radio Luminosity (erg/s/Hz) Time Since Explosion (Days)

20. Different progenitor models predict different circumbinary environments. WD + Sub-giant or Main Sequence WD + Giant WD + WD (NASA/Swift/ AuroreSimonnet, Sonoma State Univ.)

22. VLA ...And still no radio emission from SNeIa! Assumes vw = 50 km/s M = 10-8 M yr-1 . JVLA nISM = 1 cm-3

23. Strong limits on the environment of SN 2011fe from EVLA M = 10-8 M yr-1 . SN 2011fe nISM = 1 cm-3 (Chomiuk et al. 2012, Horesh et al. 2011) assumes vw = 50 km/s

24. Strong limits on the environment of SN 2011fe from EVLA Chomiuk et al. (2012), Margutti et al. (2012)

25. SN 2009ip: Watching an LBV explode (Mauerhan et al. 2012)

26. (Mauerhan et al. 2012) SN 2009ip: No longer an impostor since ~Sept 15 No radio detection yet; VLA monitoring ongoing

27. SN 1970G revisited 33.7 ± 4.3 μJy @ 5 GHz (Dittman et al. in prep)

28. SN 1970G consistently challenges our radio facilities (Stockdale et al. 2001, Dittman et al. in prep)

29. SN 1970G: Decline in Radio + Rise in X-rays = Compact Object? (Dittman et al. in prep)

30. Radio light curves of SNe trace mass loss histories of progenitors. • Diversity of mass loss histories • Ib/c mass loss consistent with WR • No Ia radio detections Discovery of first radio SN Type I SNe split into Ia and Ib/c • Jansky VLA Era: • Sensitivity Bonanza! • Relativistic SNe w/o GRBs • Still no Ia radio detections Long GRB associated with a relat-ivistic SN Theory of radio SN

31. end

32. A continuum in blast wave velocities between normal SNeIb/c and GRBs (Soderberg et al. 2010, more in prep)