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In this paper we compare galactic electron spectra measured up to TeVenergies by AMS2 and CALET and that measured by Voyager at the lowest energiesdown to 1 MeV with that calculated using a Monte Carlo diffusion model forelectron propagation in the galaxy. The observations and calculations at bothends of the electron spectrum, differing by a factor ~10^6 in energy, can bematched to within a few percent with a minimal set of assumptions. Thisincludes an electron spectrum which has an index increasing from ~2.1 at thelowest energies to 2.4 at ~1 TeV, along with a diffusion coefficient thatremains essentially constant below ~1.5 GV above which it becomes P^0.45. TheMonte Carlo calculations indicate that the lowest and highest energy electronsoriginate within a local region near the galactic plane of size, less than Lwhere L is the thickness of the trapping region. The remarkable agreement towithin a few percent between the calculations and measurements from 20 GeV upto ~1 TeV also indicates that there are no individual sources greater than10-20 percent of the Monte Carlo calculated background that are contributing tothe observed electron intensity in this energy range.

Fitting the Galactic Electron Spectrum Measured by Voyager at Low  Energies and also by CALET/AMS-2 at High Energies Using a Monte Carlo  Diffusion Model for Electron Propagation - One Spectrum Fits All