Inverse Compton emission from millisecond pulsars in the Galactic bulge
  Analyses of Fermi Gamma-Ray Space Telescope data have revealed a source of
excess diffuse gamma rays towards the Galactic center that extends up to
roughly $\pm$20 degrees in latitude. The leading theory postulates that this
GeV excess is the aggregate emission from a large number of faint millisecond
pulsars (MSPs). The electrons and positrons ($e^\pm$) injected by this
population could produce detectable inverse-Compton (IC) emissions by
up-scattering ambient photons to gamma-ray energies. In this work, we calculate
such IC emissions using GALPROP. A triaxial three-dimensional model of the
bulge stars obtained from a fit to infrared data is used as a tracer of the
putative MSP population. This model is compared against one in which the MSPs
are spatially distributed as a Navarro-Frenk-White squared profile. We show
that the resulting spectra for both models are indistinguishable, but that
their spatial morphologies have salient recognizable features. The IC component
above $\sim$TeV energies carries information on the spatial morphology of the
injected $e^\pm$. Such differences could potentially be used by future
high-energy gamma-ray detectors such as the Cherenkov Telescope Array to
provide a viable multiwavelength handle for the MSP origin of the GeV excess.
