  Inverse Compton scattering by relativistic electrons produces a major
component of the diffuse emission from the Galaxy. The photon fields involved
are the cosmic microwave background and the interstellar radiation field from
stars and dust. Calculations of the inverse Compton distribution have usually
assumed a smooth ISRF, but in fact a large part of the Galactic luminosity
comes from the most luminous stars which are rare. Therefore we expect the
ISRF, and hence the inverse Compton emission, to be clumpy at some level which
could be detectable by instruments such as GLAST. Even individual nearby
luminous stars could be detectable assuming just the normal cosmic-ray electron
spectrum. We present the basic formalism required and give possible candidate
stars to be detected, and make predictions for GLAST. Then we apply the
formalism to OB associations and the Sun, showing that the IC emission produced
is not negligible compared to the sensitivity of current or coming detectors.
We estimate that the gamma-ray flux from the halo around the Sun contributes to
the diffuse background emission at about the few percent level.
