... (lowered

The mean velocity of clouds in the central plane of the torus is lower than the virial velocity there.

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... way

Note that integrating the mass density for an $\alpha$-model (see Eq. (18)) of a quasi-isothermal stellar cluster gives an enclosed mass of $M(r) \sim 4 \pi \rho_{\star,\rm c}~ R_{\rm c}^3 (r/R_{\rm c})^{(3-\alpha)}$ within a radius $r = R\sqrt{1 + x^2}$ larger than the core radius $R_{\rm c}$. The contribution to the potential $\Psi$ is $\Psi_{{\rm cluster}} = (\alpha-2) G M(r)/r$. The factor  $(\alpha-2)$, which is often negative, indicates that it is not simply the total enclosed mass which must be inserted in Eq. (14) for the potential. This is in contrast with calculating the gravitational force where the enclosed mass is sufficient.

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