The primary cosmic ray electron flux has boon measured with a system composed of a cerenkov telescope and a scintillation detector separated by lead absorber. The sensitive energy range of the instrument was between 25 and 800 Mev.. A preliminary measurement with a modified detector has investigated the differential energy spectrum of the primary electrons. The results are taken from high altitude balloon flights which achieved a maximum altitude in excess of 5 gm/cm2. of residual atmosphere. Flights were made from Kiruna, Sweden (geomagnetic latitude 65°N) and Cardington, England (geomagnetic latitude 50°N) between 1964 and 1966. The flights at the lower latitude were used to correct those at the higher latitude for the influence of atmospheric secondary electrons. The Kiruna flights were also corrected independently using a theoretical estimate of the secondary flux.