Bistatic radar observations of the lunar surface conducted with Explorer 35 at 2.2 meters have been used to measure the average large-scale (tens to hundreds of meters) lunar slopes. Data obtained for the equatorial band between 70° east and west longitude show significant (3:1) regional variations. Unidirectional rms slopes of 2°, 3°, and 6° were obtained for Mare Fecunditatis and Oceanus Procellarum, the central highlands and terra surrounding the crater Alfraganus, and the Censorinus highlands, respectively. A comparison of the slope variations and visible surface structure suggests that the meter wavelength radar slopes are those of the visible surface measured on the set of scales given above.
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