Two-site observations of interplanetary scintillation using the EISCAT facility can provide measurements of solar wind velocity at any point in the heliosphere between 15 and 120 solar radii (R). In this paper we discuss a series of observations made as part of the Whole Sun Month campaign (August 10 to September 8 1996) and compare the results with coronal data and in-situ measurements made during the campaign. The results of the comparison revealed extremely good agreement between solar wind speeds measured by IPS at 16--73 R and in situ measurements at 213 R and beyond, both in the general morphology of the solar wind and in the absolute velocities observed. These results confirm that structures in the solar wind, originating in the corona, preserve their form out to 910 R or more. Observations of fast solar wind were always associated with coronal holes and slow wind with the bright corona. Velocities intermediate between normal fast and slow flow speeds are associated with interaction regions between fast and slow flow and are also found above the boundaries of coronal holes. ¿ 1999 American Geophysical Union