1. Are Stellar Eruptions a Common Trait of SNe IIn? Baltimore, MD 06/29/11 Ori Fox NPP Fellow NASA Goddard Based on arXiv:1104.5012

2. Late-time IR Emission From SNe IIn >50% of supernovae with late-time IR emission are SNe IIn. Represent <10% of all CCSNe. In some cases, emission 6 years post- detection! Only a single SN Iin Mid-IR spectrum (05ip; ODF+10). The presence of dust yields various clues about the circumstellar medium, progenitor evolution, and circumstellar environment. Type IIn Undefined before 1990

3. Fox et al. 2009 FanCam SN 2005ip ODF+10 ODF+09

4. Late-Time Spitzer Survey

5. Late-Time Spitzer Photometry

6. Late-Time Spitzer Results

7. Why am I here and what does this have to do with ILRT?

8. Origin and Heating of Warm Dust Origin Pre-existing CSMNewly Formed SN EjectaPost-Shock GasShock Heating Radiative Echo Radioactivity Collisional Radiation Must Consider: 1) Energetic Constraints 2) Dust Temperature Constraints Quick Definition: 1) Blackbody Radius 2) Shock Radius 3) Evaporation Radius 4) Echo Radius

9. What can we rule out? Shock Heated Dust: The predicted mass of shock heated dust is less than the observed mass. Newly Formed Dust: Due to a lack of late-time optical spectra, we cannot confirm the presence or absence of asymmetric lines. But the dust temperatures are all quite cooler than the dust vaporization temperature (~1800 K) and the blackbody (i.e., minimum) radii are typically larger than the radii at which the dust would have likely formed (r s2 ). b) V s2 =2500 km s -1

10. Radiative Heating r SN 2005ip Dwek 1983 ODF+10

11. Late-Time Optical Emission Observations show late time optical emission from CSM interaction is common: *L opt (SN 2005ip) = 10 7.8 L ⊙ on days >900 (Smith et al. 2009), *L opt (SN 2006jd) = 10 7.7 L ⊙ on day 1609 (ODF+arXiv:1104.5012), *and L opt (SN 2007rt) ≈ 10 8 L ⊙ on day 562 (Trundle et al. 2009).

12. Radiative Heating r

13. Likely Heating Mechanisms

14. LBV Progenitor Eruptions? LBV progenitors. Progenitor Eruption.

15. Implications and Future Work

16. In general, the Type IIn subclass seems to have a warm dust component that likely is due to an `IR echo' that forms from the heating of a large, pre-existing dust shell. The heating mechanism is likely the optical luminosity generated from the forward forward shock interaction with the circumstellar medium. Mass-loss rates and progenitor wind speeds suggest LBV progenitors that have undergone eruptive events tens to hundreds of years before going SN. Will be be able to observe the echo turn off? What is the mechanism? And more… –Can these techniques be used for other supernova/transient types? –If LBVs can go supernova, than their cores are significantly more evolved than stellar evolution models predict? –If LBVs yield large amounts of dust in their progenitor winds, then perhaps there is a connection to the large mass stars associated with Pop. III stars in the early universe?

17. Backup Slides

18. CCSNe Classification

19. Physical Mechanism Gal-Yam+07

20. Why do we care about dust? The presence of dust yields various clues about the supernova explosion and the progenitor system, including: –Geometry of circumstellar medium and progenitor evolution –Peak supernova luminosity & explosion mechanics –Shock velocity & circumstellar interaction Observed Models Maiolino+04 The presence of dust also allows us to probe the possibility that supernovae are significant sources of dust in the early universe –Observations reveal large amounts of reddening (i.e. dust) in the early universe (Maiolino+04) –But at less than 1 Gyr (Z>6), the universe was not populated by low-mass AGB stars, which are the dominant sources of dust in our local universe

21. What is a Type IIn SN?

22. Smith+08 New Dust Contribution ODF+10 Ejecta Dust Post-Shock Dust

23. Shock Heating Using simple geometry, one can calculate the mass of the shocked shell, which can be compared to the observed dust mass. The resulting dust-to-gas mass ratio constrains the average dust grain size. RR R ODF+10

24. Physical Mechanism Gal-Yam et al. 2007 Type II-P SNe dominate the observed explosions. Direct observations of progenitors (SNe 2003gd, 2005cs, 2008bk, 2004dj, and 2004am) identify red- supergiant (RSG) progenitors. But all have masses from 8.5-17 M . If true, where are the higher mass RSG progenitors? –New IMF? –New theory of stellar evolution and explosions? –Need to account for dust extinction? Smartt09 Gal-Yam+07

25. Physical Mechanism Gal-Yam+07 Type Ib/c progenitors never observed directly. Lack of H -> progenitor wind -> Wolf-Rayet (WR) stars. But with known galactic WR characteristics, little chance we haven’t directly detected a progenitor yet. Also, Type Ib/c rate would require WR stars to form as low as 16 M . These results suggest 2 progenitor systems: –Interacting binaries –WR stars (But what happens to the WR stars that don’t form SNe?)

26. Physical Mechanism Gal-Yam+ 2007 What is the fate of the most massive stars (i.e., LBVs) w/ masses 80-120 M  ? Evolution theory suggests they lose their H/He envelopes and end up WR stars. And any eventual core-collapse should result in a black hole. Direct detection of a single LBV progenitor (SN2005gl). An additional event (SN2006jc) was observed coincident w/ a prior LBV-like outburst. Furthermore, ultra-bright (10 51 erg), H-rich events (e.g., SNe 2006gy, 2005ap, 2008es, 2006tf) require massive progenitors, consistent with LBVs. But physical mechanism that produces the ultra-bright Type IIn (and II-L) SNe remains controversial and unresolved. If LBVs, this would imply the cores are significantly more evolved than predicted by stellar evolution models. –Perhaps the core-collapse model doesn’t even work in this case (e.g., pair-instability)?

27. Radiative Heating r

28.  and Q Coefficients

29. IR Echo Derivation