Xrf 060218/sn2006aj: Thermal Emission From A Hot Cocoon And The Spectral Lag Behavior Of The Non-thermal Emission

Details Xrf 060218/sn2006aj: Thermal Emission From A Hot Cocoon And The Spectral Lag Behavior Of The Non-thermal Emission Xrf 060218/sn2006aj: Thermal Emission From A Hot Cocoon And The Spectral Lag Behavior Of The Non-thermal Emission

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1349l&link_type=abstract

American Astronomical Society, HEAD meeting #9, #13.49; Bulletin of the American Astronomical Society, Vol. 38, p.374

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The nearby, sub-energetic XRF060218/SN2006aj is a peculiar event. We perform detailed analysis of the Swift data and discover a new thermal emission component (high-T component) accompanying the prompt X-ray emission of XRF 060218, with temperature kTH=1.21+0.22-0.24 keV and effective blackbody radius RH 5*109 cm. This high-T component co-exists with another low-T thermal component as reported by Campana et al. (2006) for at least 2700 seconds, but evolves independently with respect to the low- T component by tracing the lightcurve of the non-thermal component. We identify this high- T thermal component as the emission from a hot cocoon surrounding the relativistic jet, as expected from the theoretical models. In addition, we investigate the duration and spectral lag for the non-thermal emission and find that these time scales are energy-dependent, and more interestingly, the spectral lag of this burst is consistent with the relation of isotropic luminosity vs. lag. This result, together with the fact that XRF060218 follows the Amati-relation, suggests that XRFs and GRBs have similar underlying radiation physics. The extremely long timescales and soft spectra of XRF060218 are probably due to its low bulk Lorentz factor.

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