Bessel functions J_1 and J_0 are crucial for solving integrals related to galaxy rotation modeling, but simplifying them for numerical integration poses challenges. The discussion highlights the need for Hankel transforms to compute integrals S(k) and V(R), with the latter becoming complex when using a truncated linear density profile. Replacing the exponential density function with a linear one significantly alters convergence, complicating the analytical solutions. The conclusion suggests avoiding truncated laws for simplicity, recommending numerical integration if truncation is necessary. Overall, the discussion emphasizes the complexities of integrating Bessel functions in astrophysical contexts.