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-20 -15 -10 -5 0 5 10 15 20 ecliptic latitude(degree)
Figure 2. The result of model fitting in case of i = 2°.2andfi = 53°. The six pairs from top to bottom are the profiles in the heliocentric longitude of A — Ae = 55°, 60°, 65°, 70°, 100° and 115°, respectively.
High spatial resolution distribution of the zodiacal light brightness S.M. Kwon,a S.S. Hongb and J.L. Weinberg0 *
aDept. of Science Education, Kangwon National University, Chunchon 200-701, KOREA bAstronomy Program, SEES, Seoul National University, Seoul 151-742, KOREA °Space Astronomy Laboratory, Snellville, GA 30039, U. S. A.
By adopting a semi-empirical method for correcting the atmospheric diffuse light and using an improved technique for subtracting the discrete starlight, we have isolated the zodiacal light (ZL) surface brightness in ground-based, photo-polarimetric observations of the night sky. Advantages of this new reduction methodology compared to previous schemes are pointed out. A two-dimensional distribution of the ZL is presented with a spatial resolution better than 2 degrees over most of the sky that can be observed from the ground. The symmetry plane is found to have an inclination i ~ 2° and longitude of ascending node fi ~ 80° by comparing the observed brightness distribution with that expected for a 3-dimensional cosine model.
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