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We present a generalized analytic formalism for the inverse Compton X-rayemission from hydrogen-poor supernovae and apply this framework to SN2011feusing Swift-XRT, UVOT and Chandra observations. We characterize the opticalproperties of SN2011fe in the Swift bands and find them to be broadlyconsistent with a "normal" SN Ia, however, no X-ray source is detected byeither XRT or Chandra. We constrain the progenitor system mass loss rate to belower than 2x10^-9 M_sun/yr (3sigma c.l.) for wind velocity v_w=100 km/s. Ourresult rules out symbiotic binary progenitors for SN2011fe and argues againstRoche-lobe overflowing subgiants and main sequence secondary stars if >1% ofthe transferred mass is lost at the Lagrangian points. Regardless of thedensity profile, the X-ray non-detections are suggestive of a clean environment(particle density < 150 cm-3) for (2x10^15<R<5x10^16) cm around the progenitorsite. This is either consistent with the bulk of material being confined withinthe binary system or with a significant delay between mass loss and supernovaexplosion. We furthermore combine X-ray and radio limits from Chomiuk et al.2012 to constrain the post shock energy density in magnetic fields. Finally, wesearched for the shock breakout pulse using gamma-ray observations from theInterplanetary Network and find no compelling evidence for asupernova-associated burst. Based on the compact radius of the progenitor starwe estimate that the shock break out pulse was likely not detectable by currentsatellites.

Inverse Compton X-ray Emission from Supernovae with Compact Progenitors: Application to SN2011fe