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Fig. 7.

image

Distributions for the effective source velocity and mean microlens mass. Left panel: probability density for the effective velocity (in Einstein units ⟨M*/M1/2 km s−1) across the source plane from the ensemble of Monte Carlo fits to the observed light curves (heavy black curve). The lighter black curve is our prior on the true effective velocity of source (in physical units km s−1) generated from a model of the effective velocity of source, lens, observer and the velocity dispersion of lens galaxy stars. Right panel: probability density for the mean mass of a lens galaxy star ⟨M*⟩ derived by convolving the probability density for the effective velocity with our model for the true effective velocity (see left panel). Since , the distribution is broad. The expectation value for is lower than the predictions of standard IMF models, but our results for the accretion disc size are consistent when we assume a more physical uniform prior 0.1 ≤ ⟨M*/M⟩ ≤ 1.0 (see the right panel of Fig. 8).

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