Microlensing and the Surface Brightness Profile of the Afterglow Image of Gamma‐Ray Burst 000301C

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Abstract
The optical afterglow of gamma-ray burst (GRB) 000301C exhibited a significant, short timescale deviation from the power-law flux decline expected in the standard synchrotron shock model. Garnavich, Loeb, & Stanek found that this deviation was well fitted by an ad hoc model in which a thin ring of emission is microlensed by an intervening star. We revisit the microlensing interpretation of this variability, first by testing whether microlensing of afterglow images with realistic surface brightness profiles (SBPs) can fit the data, and second by directly inverting the observed light curve to obtain a nonparametric measurement of the SBP. We find that microlensing of realistic SBPs can reproduce the observed deviation, provided that the optical emission arises from frequencies above the cooling break. Conversely, if the variability is indeed caused by microlensing, the SBP must be significantly limb-brightened. Specifically, ≥60% of the flux must originate from the outer 25% of the area of the afterglow image. The latter requirement is satisfied by the best-fit theoretical SBP. The underlying optical/infrared afterglow light curve is consistent with a model in which a jet is propagating into a uniform medium with the cooling break frequency below the optical band.