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We report on interferometric observations of a face-on accretion systemaround the High-Mass young stellar object, G353.273+0.641. The innermostaccretion system of 100 au radius was resolved in a 45 GHz continuum imagetaken with the Jansky-Very Large Array. Our spectral energy distributionanalysis indicated that the continuum could be explained by optically thickdust emission. The total mass of the dusty system is $\sim$ 0.2 $M_{\sun}$ atminimum and up to a few $M_{\sun}$ depending on the dust parameters. 6.7 GHzCH$_{3}$OH masers associated with the same system were also observed with theAustralia Telescope Compact Array. The masers showed a spiral-like,non-axisymmetric distribution with a systematic velocity gradient. Theline-of-sight velocity field is explained by an infall motion along a parabolicstreamline that falls onto the equatorial plane of the face-on system. Thestreamline is quasi-radial and reaches the equatorial plane at a radius of 16au. This is clearly smaller than that of typical accretion disks in High-Massstar formation, indicating that the initial angular momentum was very small, orthe CH$_{3}$OH masers selectively trace accreting material that has smallangular momentum. In the former case, the initial specific angular momentum isestimated to be 8 $\times$ 10$^{20}$ ($M_{*}$$/$10 $M_{\sun}$)$^{0.5}$ cm$^{2}$s$^{-1}$, or a significant fraction of the initial angular momentum was removedoutside of 100 au. The physical origin of such a streamline is still an openquestion and will be constrained by the higher-resolution ($\sim$ 10 mas)thermal continuum and line observations with ALMA long baselines.

A Face-on Accretion System in High-Mass Star-Formation: Possible Dusty Infall Streams within 100 AU