Comprehensive study of WIMP models explaining the F e r m i -LAT Galactic Center excess

The Galactic Center excess (GCE) of GeV γ rays may hint at dark matter (DM), yet its origin remains debated. Motivated by this, we survey weakly interacting massive particle (WIMP) models that can fit the GCE while satisfying relic-density, direct-detection (DD), and indirect-detection (ID) bounds. We group candidates into (Higgs portals; simplified scalar/vector mediators), [ U ( 1 ) L i − L j ], and [ U ( 1 ) B − L , Z -portal] classes. Across all cases, present DD and dwarf-spheroidal γ -ray limits exclude wide regions, leaving mainly narrow with m DM ≃ m med / 2 and portal couplings ≪ 1 . In hadronic setups, scalar and vector Higgs portals survive only in a thin strip near m h / 2 ≃ 62.5 GeV with portal couplings ∼ 10 − 4 , while the Dirac Higgs and Z portals are essentially excluded. The UV-complete vector Higgs portal retains resonant bands whose viable portal strength depends on the mixing angle. Simplified scalars allow small windows for complex-scalar or vector DM; Dirac DM is strongly disfavored, whereas a pseudoscalar with Dirac DM remains viable over a broader parameter range. For a simplified Z ′ mediator, a pure vector coupling leaves only a marginal region, while pure axial is excluded by DD/ID bounds. In leptonic scenarios, inverse-Compton emission is essential: L μ − L e (and, to a lesser extent, B − L ) fits the GCE with near-thermal cross sections, while L μ − L τ is disfavored. Overall, viable WIMP explanations are , with leptophilic vectors and pseudoscalar portals emerging as the most robust options.