Allowed configurations for a possible inner planet in the (a_c, m_c ) plane for increasing values of initial eccentricity, e_c, under the constraint that the simulated disk reproduces the observed inner edge at 23 au. The plotting conventions are the same as in Fig. 2. The red line marks the upper mass limit set by observations and, when applicable, by the additional requirement that the outer planet TWA 7 b remains dynamically cold enough to support stable horseshoe-like co-orbitals (Sect. 2). The red dot indicates the intersection point where, for a given eccentricity, all solutions above this limit are excluded. As e_c increases, this constraint becomes increasingly restrictive, eventually ruling out all configurations compatible with the observed disk morphology.