Notes. ^(a)Spatial resolution obtained from 1.22λ/D, where λ is the central wavelength, and D is the telescope pupil size seen by the instrument. ^(b)In the H and K bands, two stellar flux images were acquired on separate nights. The mean flux in the K band was computed based on the two observed values, with preference given to the flux from the second night, accounting for seeing conditions. We calculated the standard deviation with two flux values the H and K band considering a potential stellar brightness variation. We also computed as the photonic noise following a Poisson distribution. For instance, in the case of observations in the H2 band, the photonic noise was computed as . The overall errors in stellar flux were determined by combining the photonic noise and the standard deviation with two night flux values. ^(c) Average disk surface brightness for the unconvolved models. The error was calculated by the Markov chain of the corresponding disk parameters obtained in the process of forward modeling.^(d) Average disk surface brightness for an observation with throughput correction in the major axis. The error was calculated based on the residual image in the region outside of the disk.^(e) Average disk surface brightness for an observation with the throughput correction out of the major axis. Considering the low inclination of the disk, the scatter angle of the region is nearly 90°. ^(ƒ)The average polarized disk surface brightness for the unconvolved disk model.