New Measurements of the Motion of the Zodiacal Dust

Abstract

Using the Wisconsin Hα Mapper (WHAM), we have measured at high spectral resolution and high signal-to-noise ratio the profile of the scattered solar Mg I λ5184 Fraunhofer line in the zodiacal light. The observations were carried out toward 49 directions that sampled the ecliptic equator from solar elongations of 48° (evening sky) to 334° (morning sky) plus observations near +47° and +90° ecliptic latitude. The spectra show a clear prograde kinematic signature that is inconsistent with dust confined to the ecliptic plane and in circular orbits influenced only by the Sun's gravity. In particular, the broadened widths of the profiles, together with large amplitude variations in the centroid velocity with elongation angle, indicate that a significant population of dust is on eccentric orbits. In addition, the wide, flat-bottomed line profile toward the ecliptic pole indicates a broad distribution of orbital inclinations extending up to about 30°-40° with respect to the ecliptic plane. The absence of pronounced asymmetries in the shape of the profiles limits the retrograde population to less than 10% of the prograde population, and also places constraints on the scattering phase function of the particles. These results do not show the radial outflow or evening-morning velocity amplitude asymmetry reported in some earlier investigations. The reduction of the spectra included the discovery and removal of extremely faint, unidentified terrestrial emission lines that contaminate and distort the underlying Mg I profile. This atmospheric emission is too weak to have been seen in earlier, lower signal-to-noise ratio observations, but it probably affected the line centroid measurements of previous investigations.