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Dust continuum observation is one of the best methods to constrain theproperties of protoplanetary disks. Recent theoretical studies have suggestedthat the dust scattering at the millimeter wavelength potentially reduces theobserved intensity, which results in an underestimate in the dust mass. Weinvestigate whether the dust scattering indeed reduces the observed continuumintensity by comparing the ALMA archival data of the TW Hya disk at Band 3, 4,6, 7 and 9 to models obtained by radiative transfer simulations. We find thatthe model with scattering by 300 ${\rm \mu m}$-sized grains well reproduces theobserved SED of the central part of the TW Hya disk while the model withoutscattering is also consistent within the errors of the absolute fluxes. Toexplain the intensity at Band 3, the dust surface density needs to be $\sim$ 10${\rm g\,cm^{-2}}$ at 10 au in the model with scattering, which is 26 timesmore massive than previously predicted. The model without scattering needs 2.3times higher dust mass than the model with scattering because it needs lowertemperature. At Band 7, scattering reduces the intensity by $\sim$ 35% whichmakes the disk looks optically thin even though it is optically thick. Ourstudy suggests the TW Hya disk is still capable of forming cores of giantplanets at where the current solar system planets exist.

Scattering-induced intensity reduction: large mass content with small grains in the inner region of the TW Hya disk