•A solar modulation model is compared to observations from Voyager 1 and PAMELA.•A heliopause spectrum is subsequently calculated from 1MeV to 50GeV.•A spectral break is found for this spectrum between ∼800MeV and ∼2GeV.•Below ∼1GeV it exhibits a power-law E−(1.55±0.05) with E kinetic energy.•Above ∼5GeV a different power law is found, with E−(3.15±0.05). A heliopause spectrum at 122AU from the Sun is presented for galactic electrons over an energy range from 1MeV to 50GeV that can be considered the lowest possible local interstellar spectrum (LIS). The focus of this work is on the spectral shape of the LIS below ∼1.0GeV. The study is done by using a comprehensive numerical model for solar modulation in comparison with Voyager 1 observations at ∼112AU from the Sun and PAMELA data at Earth. Below ∼1.0GeV, this LIS exhibits a power law with E−(1.55±0.05), where E is the kinetic energy of these electrons. However, reproducing the PAMELA electron spectrum averaged for 2009, requires a LIS with a different power law of the form E−(3.15±0.05) above ∼5GeV. Combining the two power laws with a smooth transition from low to high energies yields a LIS over the full energy range that is relevant and applicable to the modulation of cosmic ray electrons in the heliosphere. The break occurs between ∼800MeV and ∼2GeV as a characteristic feature of this LIS. The power-law form below ∼1GeV produces a challenge to the origin of these low energy galactic electrons. On the other hand, the results of this study can be used as a gauge for astrophysical modeling of the local interstellar spectrum for electrons.