For α = 0 the solutions are not real for 0 < ρ < b and therefore we should exclude this region from the spacetime. For this purpose we introduce the new radial coordinate r as With this new coordinate, the above metric becomes where the coordinates r assumes the values 0 ≤ r < ∞ , and N $^{2}$( r ), f $^{2}$( r ), Φ( r ) and R $^{2}$( r ) are now given as It is notable to mention that these solutions are valid for all values of α . When ( α = 0 = γ ), these solutions describe the ( n +1)-dimensional asymptotically AdS Reissner-Nordstrom black branes. For b = 0 (Γ = 1), the charge parameter q and the scalar field Φ( r ) vanish and our solutions reduce to the solutions of Einstein gravity in the presence of cosmological constant. Here we should discuss singularity(ies). After some algebraic manipulation, one can show that the Kretschmann and the Ricci scalars in ( n + 1)-dimensions are finite for r = 0, but in the vicinity of r = 0, we have and thus they diverge at r = 0 ( ρ = b ). Thus, r = 0 is a curvature singularity. It is worthwhile to note that the scalar field Φ( r ) and the electromagnetic field F$_{tρ}$ become zero 6 R$_{µνλκ}$R µνλκ ∝ r − 4( n − 2) [ 1+ ( α $^{2}$+ n − 2 ) − $^{1}$]$_{,}$ R ∝ r − 2( n − 2) [ 1+ ( α $^{2}$+ n − 2 ) − $^{1}$]$_{,}$ N $^{2}$( r ) = Γ − γ ( n − $^{3)}$, (16) f $^{2}$( r ) = r 2 + b 2 l 2 Γ ( n − 2) γ + [ k − ( c √$_{r}$ 2 + b 2 ) n − 2 ] Γ 1 − $^{γ}$, (17) Φ( r ) = n − 1 4 √ γ (2 + 2 γ − nγ ) ln Γ , (18) R $^{2}$( r ) = Γ $^{γ}$, (19) Γ = 1 − ( b √$_{r}$ 2 + b 2 ) n − 2 . A. Properties of the solutions: ds 2 = − N $^{2}$( r ) f $^{2}$( r ) dt 2 + r $^{2}$dr2 ( r 2 + b $^{2}$) f $^{2}$( r ) + ( r 2 + b $^{2}$) R $^{2}$( r ) d Ω 2 n − $_{1}$, (15) r 2 = ρ 2 − b 2 ⇒ dρ 2 = r 2 r 2 + b $_{2}$dr$^{2}$. (14)