GALPROP obtained LIS using modulated spectra from HelMod
The local interstellar spectra (LIS) are input cosmic ray intensities for any modulation models. Fluxes are assumed isotropically distributed at heliosphere boundary, in a steadystate configuration. The LIS is usually computed using numerical model accounting for the propagation in galaxy. The heliosphere modulation is the added using, e.g.,the modulation module available here for on line use or download.
Recently, Della Torre et al. 2017, Boschini et al 2017b deduced LIS's for protons, helium and antiprotons using the most recent experimental results combined with GALPROP model for propagation in galaxy and HelMod for the propagation in heliosphere.
HelMod and GALPROP were combined to provide a single framework and run to reproduce a comprehensive set of observations of CR species collected in different time periods, from 1997 up to 2015.
The numerical table of computed LIS is available as supplementary material of Boschini et al 2017b.
In Della Torre et al. 2017, Boschini et al 2017a,b authors proposed an analytical expression for proton and helium nuclei LIS's as a function of the rigidity:
\begin{equation}
J_{LIS}(P)\times P^{2.7} =\left\{
\begin{array}{ll}
\sum_{i=0}^5 a_i P^{i}, &P\le1\ {\rm GV},\\
b + \frac{c}{P} + \frac{d_1}{d_2+P} + \frac{e_1}{e_2+P} + \frac{f_1}{f_2+P} + g P, & P>1 \ {\rm GV},
\end{array}
\right.
\end{equation}
where \(a_i, b, c, d_i, e_i, f_i, g\) are the numerical coefficients summarized as follow:
The accuracy of the lowenergy expression is 2% in the range \(0.2 \) GV\( < R < 1\) GV for the proton LIS. The highenergy part reproduces the numerical proton LIS calculated with GALPROP with an accuracy of \(\sim\)9\% for \(0.45\) GV \( < R < 1\) GV (i.e., \(E_{\rm kin}>0.11\) GeV), where the constraints from Voyager 1 are wider than 10%, and of \(2\)% for \(R>1\) GV. The discrepancies with respect to AMS02 data at higher energies expressed in standard deviations are virtually zero, with \(0.5\sigma\) around \(12\) GV at most. In the case of Helium, the lowenergy expression is valid in the range of \(0.15\ {\rm GV} < R < 2 \) GV, i.e., approximately between 3 MeV/nucleon and 450 MeV/nucleon. At higher rigidities \(1.5\) GV\( < R < 2\times 10^{4}\) GV (i.e., \(>0.3\) GeV/nucleon), it reproduces the He LIS calculated with GALPROP with an accuracy of 2%.
The derived expressions are virtually identical, to \(<12\)%, to numerical solutions in over 5 orders of magnitude energy interval including the spectral flattening at high energies, and are based on Voyager 1, AMS02, and CREAMI data.
In addition to the Proton and Helium nuclei LIS, Boschini et al 2017a,b provides analytical fits to the derived LIS. The fit to the antiproton LIS provides an accuracy of 23% for 3 GV \(<R<1000\) GV and 10% for 1.5 GV \(<R<3\) GV:
\begin{equation}
F(R)\times R^{2.7} = \frac{168}{31.1+R^{2}} +\frac{13600}{22200+R^{2}}, \quad R>1\ {\rm GV},
\end{equation}
while the average accuracy of AMS02 data is about 10%20%.
Bibliography
Boschini, M.J., Della Torre, S., Gervasi, M., La Vacca, G. and Rancoita, P. G. (2017a) Propagation of Cosmic Rays in Heliosphere: the HelMod Model Submitted to Advances in Space Research. 

Boschini, M.J., Della Torre, S., Gervasi, M., Grandi, D., Johannesson, G., Kachelriess, M., La Vacca, G., Masi, N., Moskalenko, I. V., Orlando, E., Ostapchenko, S.S., Pensotti, S., Porter, T. A., Quadrani, L., Rancoita, P. G., Rozza, D. and Tacconi, M. (2017b) Solution of Heliospheric Propagation: Unveiling the Local Interstellar Spectrum of Cosmic Rays Species Submitted to Astrophysical Journal  
Della Torre, S., Gervasi, M., Grandi, D., Johannesson, G., La Vacca, G., Masi, N., Moskalenko, I. V., Orlando, E., Porter, T. A., Quadrani, L., Rancoita, P. G. and Rozza, D. (2017). From Observations near the Earth to the Local Interstellar Spectra. In Proceedings of the 25th European Cosmic Rays Symposyum (ECRS2016) eConf C160904.3, Septembers 49,2016 (Torino, Italy) arXiv: 1701.02363.. 
