Solutions to the hydrostatic equilibrium equation at a radius of 6 kpc. The left, middle, and right panels present density solutions for stars, molecular, and atomic gas, respectively. The solid lines in each panel represent solutions when the hydrostatic equations were solved with the iterative method using CALIFA IFU data. The dashed lines represent the solutions with the analytically calculated stellar velocity dispersion described by Eq. (9). The choice of stellar velocity dispersion greatly influences the density solutions in all three baryonic disks.