Observations by the WMAP experiment have identified an excess of microwave emission from the center of the Milky Way .
It has previously been shown that this “ WMAP Haze ” could be synchrotron emission from relativistic electrons and positrons produced in the annihilations of dark matter particles .
In particular , the intensity , spectrum and angular distribution of the WMAP Haze is consistent with an electroweak scale dark matter particle ( such as a supersymmetric neutralino or Kaluza-Klein dark matter in models with universal extra dimensions ) annihilating with a cross section on the order of \sigma v \sim 3 \times 10 ^ { -26 } cm ^ { 3 } /s and distributed with a cusped halo profile .
No further exotic astrophysical or annihilation boost factors are required .
If dark matter annihilations are in fact responsible for the observed Haze , then other annihilation products will also be produced , including gamma rays .
In this article , we study the prospects for the GLAST satellite to detect gamma rays from dark matter annihilations in the Galactic Center region in this scenario .
We find that by studying only the inner 0.1 ^ { \circ } around the Galactic Center , GLAST will be able to detect dark matter annihilating to heavy quarks or gauge bosons over astrophysical backgrounds with 5 \sigma ( 3 \sigma ) significance if they are lighter than approximately 320-500 GeV ( 500-750 GeV ) .
If the angular window is broadened to study the dark matter halo profile ’ s angular extension ( while simultaneously reducing the astrophysical backgrounds ) , WIMPs as heavy as several TeV can be identified by GLAST with high significance .
Only if the dark matter particles annihilate mostly to electrons or muons will GLAST be unable to identify the gamma ray spectrum associated with the WMAP Haze .