References

1. C. Leinert, M. Hanner, and I. Richter, Astron. Astrophys. 80 (1980) 328.

2. S.S. Hong and S.M. Kwon in Origin and Evlution of Interplanetary Dust, (eds. A.C. Levasseur-Regourd and H. Hasegawa) Kluwer, Dordrecht (1991) 147.

3. R. Dumont and A.C. Levasseur-Regourd, Astron. Astrophys. 64 (1978) 9.

4. T. Mukai and M. Ishiguro, this volume.

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9. T. Kelsall, J.L. Weiland, B.A. Franz, W.T. Reach, R.G. Arendt, E. Dwek, H.T. Freudenreich, M.G. Hauser, S.H. Moseley, N.P. Odegard, R.F. Silverberg and E.L. Wright, Astrophys. J. 508 (1998) 44.

-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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