to the center is not well motivated given the uncertainties in the the deduced pulsar distribution closer to the galactic center.

-   For local measurements at energies 5 GeV and higher, the dominant contribution to the flux should come from a few local sources and we cannot use a smooth source spatial distribution to describe this (given the large expected variance).

-   In the outer gap model for pulsars we use, the energy spectrum around a GeV and lower is very uncertain because of the cut-off, as discussed earlier. This is not a complicating factor for the haze because most of the contribution comes from approximately 5 GeV and higher, but it is an issue that must be addressed if one is normalizing to lower energy data. In addition, the low energy data is also affected by solar modulation.

-   In order to link the haze to local measurements, we need a better understanding of how the $e^+e^-$ flux is affected by changes in diffusion between the local and central parts of the galaxy.

Morphology
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The pulsar contribution to the haze is non-spherical, with the deviation from sphericity determined by a combination of factors including the diffusion coefficient, the 