The dark matter distribution in the very inner region of our Galaxy is still in debate . In the 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 . The baryons dominate the gravitational potential in the inner Galaxy , hence a direct constrain on the abundance of the 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 the dark matter annihilation . With current 130 GeV line data and adopting the generalized Navarro-Frenk-White profile of the dark matter halo , for local dark matter density \rho _ { 0 } = 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 \alpha = 1.06 ( the cross section of dark matter annihilation into gamma-rays \langle \sigma v \rangle _ { \chi \chi \rightarrow \gamma \gamma } = 1.3 \times 10 ^ { -27 } ~ { } % { cm ^ { 3 } ~ { } 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 .