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