Statistical properties of the two Maxwellian electron densities and temperatures characterizing the differential suprathermal electron fluxes measured by the Pioneer-Venus Lockheed-IPW retarding potential analyzer in the Venus umbra between approximately 1000 and 2000 km altitude and nightward of 130¿ solar zenith angle are reported. We find that the median density n2 and temperature T2 of the principal Maxwellian component are 3 cm-3 and 14 eV, respectively, and do not exhibit an altitude or solar zenith angle dependence within the umbra region studied. Two thirds of the measured values of n2 and T2 typically fall within plus or minus a factor of 2 of the median values. The second suprathermal component density n3 is less well defined but has a median density of 0.06 cm-3 and similarly exhibits no clear altitude or solar zentih angle dependence. Two thirds of the n3 values fall within plus or minus a factor of 2 of the median value. The temperature T3 of the second component is assumed constant and equal to 200 eV. The median integral flux measured in this study between 15 and 45 eV energy is consistent with that reported earlier for the Venus nightside ionosphere by Spenner et al. (1981) at altitudes below 1000 km. The integral flux measured by the Pioneer-Venus retarding potential analyzer appears to be larger than the Venera measured median flux by a factor of approximately 2 in the energy range of the Pioneer-Venus retarding potential analyzer.