Dark matter distribution in the very inner region of our Galaxy is still debated. In N-body simulations, a cuspy dark matter halo density profile is favored. Several dissipative baryonic processes, however, are found to be able to significantly flatten dark matter distribution, and a cored dark matter halo density profile is possible. Baryons dominate the gravitational potential in the inner Galaxy, hence a direct constraint on the abundance of dark matter particles is rather challenging. Recently, a few groups have identified a tentative 130 GeV line signal in the Galactic center, which could be interpreted as the signal of dark matter annihilation. Using current 130 GeV line data and adopting the generalized Navarro-Frenk-White profile of the dark matter halo—local dark matter density ρ₀ = 0.4 GeV cm^-3 and r _s = 20 kpc—we obtain a 95% confidence level lower (upper) limit on the inner slope of dark matter density distribution, α = 1.06 (the cross section of dark matter annihilation into γ-rays langσvrang_{χχ → γγ} = 1.3 × 10^-27 cm³ s^-1). Such a slope is consistent with the results of some N-body simulations and, if the signal is due to dark matter, suggests that baryonic processes may be unimportant.