1. Radio and X-ray observations of SN 2009ip Poonam Chandra National Centre for Radio Astrophysics January 4, 2013 Collaborators: Raffaella Margutti (Harvard), Alicia Soderberg (Harvard), Roger Chevalier (University of Virginia) and more……..

2. Radio Observations: Karl G. Jansky Very Large Array

3. SN 2009ip – Radio Observations Radio observations since September 26, 2012 till Dec 2, 2012, in K (22.5 GHz) and X (8.5 GHz) bands with the JVLA. Date of Obs Frequency (GHz) Flux Density (uJy) Sep 26.1121.19<131 Sep 26.148.94<65 Sep 26.6318<66 (ATCA, Hancock et al. 2012) Oct 16.0621.2579+/-29 Oct 17.1221.19108+/-40 Oct 26.048.8544+/-15 Nov 06.0621.19<94 Nov 12.978.99<92 Dec 01.9921.25<305 Dec 02.938.99<544 Possible Detection?

4. SN 2009ip – X-ray observations

5. X-ray telescopes XMM Swift

6. SN 2009ip- Swift-XRT X-ray observations Swift-XRT observations started from Sep 4 2012 until Dec 2012 in photon counting mode. No X-ray emission during the decay of 2012a outburst i.e t<22 nd Sept (3-sigma~3E-3 cps, 12.2ks). No detection even during the rise time of the 2012b Sept 22 nd < t < Oct 1 st (3-sigma 1.1E-3 cps, 31.4ks). X-ray emission detected starting from Oct 1 st when 2012b outburst in 2012 reaches UV/optical peak. Detection until Oct 16 th and then no detection from Oct 20 th onwards.

7. SN 2009ip – Swift X-ray observations

8. SN 2009ip- XMM-Newton X- ray observations XMM-Newton observations on 3 th Nov 2012. XMM observations for ~60ks for EPIC-PN and MOS in full frame thin filter mode. SN detection, 4.5 sigma for a region of 10” (total 132 photons in 55 ks) Data best fit with T>10 keV and NH~1E21 cm -2 Flux absorbed 1.7E-14 erg/s/cm 2 and unabsorbed 1.9E-14 erg/s/cm 2. We use XMM parameters to fit Swift spectrum as well.

9. SN 2009ip – X-ray observations Excess emission? Swift spectrum around the peak (86ks)

10. Contaminating source Presence of contaminating source ~14” away from the SN (Campana et al. 2012, Atel 4444). XMM, Swift-XRT have not enough spatial resolution to exclude the contaminating source completely. Study contamination by merging Swift non-detections as well as post SN detections. Swift X-ray source at 22 23 09.19, -28 56 48.7 with uncertainty of 3.8” (12” away from SN).

11. SN 2009ip – X-ray observations

12. Contaminating source 3.4 sigma detection of the contaminating source. Contaminating source count rate 3E-4 cps. Source contaminates SN flux at the level of ~1.6E-4 cps or 6x10 -15 erg/s/cm 2. This corresponds to luminosity 5x10 38 erg/s, much less than SN luminosity (~1.5x10 39 erg/s). So not significant contamination.

13. SN 2009ip – radio and X-ray light curves

14. Peak radio and X-ray luminosities 2009ip

15. Thank You.

16. Collaborators Raffaella Margutti, Harvard Alicia Soderberg, Harvard-Smithsonian Roger Chevalier, University of Virginia And more……..

17. Supernova Classification (based on optical spectra and light curve) Supernovae Hydrogen Type II Narrow H lines Type IIn No narrow H lines Type IIP/IIL No Hydrogen Type I Silicon Type Ia No Silicon Type Ib/c Plateau Type IIP Linear Type IIL Helium Type Ib No Helium Type Ic

18. Circumstellar interaction Circumstellar wind (1E-5 Msun/Yr) Explosion center Reverse Shock ~1000 km/s Forward Shock ~10,000 km/s Ejecta Circumst ellar medium density ~1/r 

19. Circumstellar interaction Hot ejecta X-rays Synchrotron Radio Forward Shock ~10 9 K Reverse shock ~ 10 7 K

20. Type IIn supernovae Very diverse stellar evolution and mass loss history. SN 1988z, extremely bright even after 20 years SN 1994w faded only in 130 days. SN 2005gl: LBV progenitor? SN 2006gy, extremely bright: PISN progenitor? SN 2002ic, SN 2005gj: Hybrid between Ia/IIN. SNe 2001em, 1995N, 2008fz: Type Ib/c properties SN 2009ip: episodic ejections before turning into true supernova

21. Multiwaveband campaign to understand Type IIn supernovae Observe most the Type IIN supernovae with the JVLA telescope (PI: Chandra). If detected in radio, follow with Swift-XRT (PI: Soderberg). Follow radio bright and/or Swift detected Type IIN supernova with ChandraXO. Get spectroscopy, separate from nearby contamination (PI: Chandra). If bright enough, do spectroscopy with XMM-Newton (PI: Chandra). NIR photometry with PAIRITEL (PI: Soderberg). Low frequency radio follow up with the GMRT Chandra, Soderberg, Chevalier, Fransson, Chugai

22. SN 2009ip A Very Unique Type IIn supernova in NGC 7259 at 66 million light year away. Earlier supernova imposter which had repeated eruptions, in 2009, 2010. Flared in July 2012 and then exploded as supernova in September 2012 (speed 13,000 km/s) Clear link with LBV progenitors (like SN 2005gl, 2006jc etc.) 10 year before explosion HST image shows the progenitor to be ~50-80Msun (massive blue progenitor) SN 2009ip first SN to have both a massive blue progenitor and LBV like eruptions.