Results for stellar distribution in the three-component, gravitationally coupled stars plus HI plus H₂ disk, two-component stars plus HI disk, and stars-alone case at R = 4.5 kpc. Panel a: stellar vertical density distribution, ρ(z) vs. z is shown for stars-alone case (solid curve), gravitationally coupled stars plus HI case (dashed curve), and stars plus HI plus H₂ case (dash-dotted curve). The gas gravity constrains the distribution of stars towards the mid-plane by raising its mid-plane density and reducing its scale height value. This constraining effect is highest in the three-component case. At the same time, the relative contribution of H₂ is higher than that of HI as the surface density of H₂ is higher than HI at R = 4.5 kpc. Panel b: vertical force per unit mass, i.e. |K_z| vs. z, acting on stars is shown due to the self-gravity of stars (solid curve), due to the force from the gravitationally coupled stars plus HI disk (dashed curve), and due to the force from the coupled stars plus HI plus H₂ disk (dash-dotted curve). The force at any z is highest in the three-component case. Panel c: work done (E_z) to raise a unit test mass from the mid-plane to any vertical height as a function of z (shown up to z = 1 kpc here) for stars against its self-gravity (solid curve), against the gravitational force from the coupled stars plus HI disk (dashed curve), and against the gravitational force from the coupled stars plus HI plus H₂ disk (dash-dotted curve). The work done in the three-component case is highest. This shows that stellar distribution in a three-component system is more strongly bound to the mid-plane than in a two-component system.