We have derived the brightness distribution of the smooth zodiacal light based on our observation by a cooled CCD camera at Mauna Kea in December 1998 in the sky region of 55° < A - A0 < 115° and -20° < (3 < 20°. As a result of the model fitting procedure, we have found that the brightness distribution of our observation can be explained reasonably by the zodiacal cloud model with a symmetry plane of i = 2°.2 and ft = 53°. Figure 2 shows the results of model fitting, where the observed data (the dots) fit well to the curve of model calculation at almost all cases of A — Ae, but some disagreement appears around the ecliptic latitude of (3 = 0° in A - A0 = 55°. This may arise from a fact that the dust band components around the ecliptic plane are removed too much from the original photometric data. This disagreement causes, however, no serious effect in a determination of i and ft.
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