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We investigate the dust distribution in the crescent disk around HD 142527based on the continuum emission at $890 \mathrm{\ \mu m}$ obtained by ALMACycle 0. The map is divided into $18$ azimuthal sectors, and the radialintensity profile in each sector is reproduced with a 2D disk model. Our modeltakes account of scattering and inclination of the disk as well as theazimuthal dependence in intensity. When the dust is assumed to have theconventional composition and maximum size of $1\ \mathrm{mm}$, the northwesternregion ($PA=329^{\circ}-29^{\circ}$) cannot be reproduced. This is because themodel intensity gets insensitive to the increase in surface density due toheavy self-scattering, reaching its ceiling much lower than the observedintensity. The ceiling depends on the position angle. When the scatteringopacity is reduced by a factor of $10$, the intensity distribution isreproduced successfully in all the sectors including those in the northwesternregion. The best fit model parameters depend little on the scattering opacityin the southern region where the disk is optically thin. The contrast of dustsurface density along $PA$ is derived to be about $40$, much smaller than thevalue for the cases of conventional opacities ($70-130$). These resultsstrongly suggest that the albedo is lower than considered by some reasons atleast in the northwestern region.

Detailed modeling of dust distribution in the disk of HD 142527