The dead-zone inner edge is a preferential site of rocky planetesimal formation via the dust-pileup followed by the streaming instability. We performed simulations of one-dimensional dust and gas disk evolution to investigate the properties of a dust-pileup at the dead-zone inner edge. We show that a strong dust-pileup at the dead-zone inner edge occurs only for conditions where the dimensionless stopping time of dust is much larger than the turbulence parameter alpha in the dead-zone. We found that if the critical fragmentation velocity of silicate dust is 1 m/s, alpha value in the dead-zone should be lower than 0.0003 to operate the dust-pileup. Using the dust distribution obtained above, we performed the radiative transfer simulations with RADMC-3D to construct models of the inner region of disks including the effect of the dust-pileup. We found that if dust concentrates on the dead-zone inner edge, the dust-pileup casts a shadow behind it, which could be extended to ~ 10 au. The shadow would be a useful tracer of the dust-pileup and we can constrain the turbulence strength through it. In this poster, I would like to discuss the observability of the shadow based on our results.