as $r\rightarrow\infty$, has a unique solution in the region where $2A>rA'$. In this region, using a suitable scalar field distribution, we can simulate some spherically symmetric geometry with a given metric function $A(r)$, and therefore the corresponding effective potential of a test particle for arbitrary specific angular momentum and energy. The condition $2A>rA'$ holds for naked singularities with any physically reasonable gravitating matter and it holds for black holes outside the photon sphere. The effective potential alone does not uniquely determine all the parameters of a bound orbit but only the pericentre and apocentre radii; in addition, we can approximately reconstruct the shape of the orbit by simultaneous varying the angular momentum and energy. In this paper we are mainly interested in just the shape of orbits because the angle of precession cumulates from revolution to revolution. However, there are other important observational parameters, namely, the period of an oscillation, the orbital (tangential) velocity $v_o$ in pericentre, and the radial velocity $v_r$ of a test particle, which can be expressed from (\[int-motion\]) in the form $$\label{}
T_{\scriptscriptstyle osc}=2E\!\int \limits_{\,r_{\!\scriptscriptstyle min}}^{\:r_{\!\scriptscriptstyle max}}\! \frac{\,\mathrm{e}^{\Phi}} {\,A\sqrt{E^2-V_{\!\scriptscriptstyle eff}\,}}\,dr\,,
\nonumber$$ $$\label{}
v_o=\frac{J}{E}\frac{\,A(r_{min})}{\,r}, \qquad
v_r=\frac{dr}{dt}= \frac{1}{E}\! \sqrt{fA\left(E^2- {V\vphantom{\underline{A}}}_{\!\!eff}\right)\,}\,.
\nonumber$$ Given an orbit around a SFNS and 