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tokens: host mass and distance is shown in Figure 7 , as well as the limits on θ E , π E , and the lens flux. We infer that the host is a dwarf, likely in the Galactic bulge at kpc. Using the mass ratio and scaled instantaneous projected separation from the model, we find that the planet mass is , and it orbits its host beyond the snowline at a projected separation of au. The estimated physical properties are summarized in Table 2 . Figure 7. Posterior probability distributions of the host mass and distance derived from the Bayesian analysis. Also shown are the limits on the lens flux (blue), on θ E for either bulge or far disk sources (red), and on the microlens parallax for a bulge source (green). Table 2 Physical Properties One of the main uncertainties in our Galactic model is the source distance. However, we note the the posterior probability for the lens mass (and thus the planet mass) is weakly dependent on the source distance. For a source at 8 kpc the mass is only 10% lower than for a source at 15 kpc, well within the range of our uncertainty. The lens distance, and consequently the projected separation between the planet and its host, is more sensitive to the source distance, with a difference of 45% between a bulge source and a far disk source. Future observations can resolve this and give a better estimation of the source distance, as we discuss below in Section 7 . 6. Extinction Law Recent studies of dust properties in the inner bulge suggest deviations from the standard extinction law (Nataf et al. 2016 ; Alonso-García et al. 2017 ). The extinction coefficient measured in our field, , is lower than the value of 1.37 from Nishiyama et al. ( 2009 ). This offset is a disconcertingly large ∼0.4 mag in K S . The offset relative to the value of predicted by Fitzpatrick ( 1999 ) is even larger—about 1.4 mag in K s . The magnitude of the RC can also be predicted in the YJ bands by assuming the color–color relations from Nataf et al. ( 2016 ) and the extinction coefficients from Fitzpatrick ( 1999 ). These are Y RC ≈ 14.63 + 1.63 + (7.35–3.12) ≈ 20.49 and J RC ≈ 14.63 + 1.63 + (5.44–3.12) ≈ 18.58, where we add the corresponding intrinsic color offsets and reddening offsets, respectively, to the observed clump H -band magnitude. Given that the limiting magnitudes for the DECam and VVV data sets are, respectively, Y ∼ 21.2 and J ∼ 19.4 (see Section 4.2 above), the RC should be clearly detected in each of these bandpasses by a wide margin of 0.7–0.8 mag, respectively. However, the photometry in both cases barely covers the RC. Figure 8 shows the HK s CMD of our field (gray points), with the sources detected in Y shown as yellow circles in the left panel, and the points detected in J shown as purple in the right panel. We conclude that the extinction toward this field is steeper than standard (as defined by Fitzpatrick 1999 ). Figure 8. Detection limits of DECam Y -band data (left) and VVV J -band data (right). These limits are brighter than