  High energy cosmic ray electrons and positrons, during propagation in the
Galaxy, mainly lose energy through either the inverse Compton scattering (ICS)
off of the interstellar radiation field (ISRF) or emitting synchrotron
radiation in the Galactic magnetic field (GMF). Emitted photons by these two
main energy loss mechanisms contribute to, respectively, diffuse Galactic gamma
rays and radio waves. The variation of the distribution of the ISRF and the GMF
has a sizable impact on the spectrum of cosmic ray electrons and positrons
throughout the Galaxy. This impact is revealed both locally through measuring
the local flux of cosmic ray electrons and positrons and globally by observing
the spectra and morphology of diffuse gamma rays and radio waves. In this
paper, we quantify this impact and conclude that recent data from AMS-02,
\textit{Fermi} and H.E.S.S experiments are powerful enough to be alternatively
applied for constraining properties of the ISRF and the GMF.
