  The local interstellar spectra (LIS's) for galactic cosmic rays (CR's) cannot
be directly observed at the Earth below certain energies, because of solar
modulation in the heliosphere. With Voyager 1 crossing the heliopause in 2012,
in situ experimental LIS data below 100 MeV/nuc can now constrain computed
galactic CR spectra. Using galactic propagation models, galactic electron,
proton and light nuclei spectra can be computed, now more reliably as very
LIS's. Using the Voyager 1 observations made beyond the heliopause, and the
observations made by the PAMELA experiment in Earth orbit for the 2009 solar
minimum, as experimental constraints, we simultaneously reproduced the CR
electron, proton, Helium and Carbon observations by implementing the GALPROP
code. Below about 30 GeV/nuc solar modulation has a significant effect and a
comprehensive three-dimensional (3D) numerical modulation model is used to
compare the computed spectra with the observed PAMELA spectra possible at these
energies. Subsequently the computed LIS's can be compared over as wide a range
of energies as possible. The simultaneous calculation CR spectra with a single
propagation model allows the LIS's for positrons, Boron and Oxygen to also be
inferred. This implementation of the most comprehensive galactic propagation
model (GALPROP), alongside a sophisticated solar modulation model to compute CR
spectra for comparison with both Voyager 1 and PAMELA observations over a wide
energy range, allows us to present new self-consistent very LIS's (and
expressions) for electrons, positrons, protons, Helium, Carbon, Boron and
Oxygen for the energy range of 3 MeV/nuc to 100 GeV/nuc.
