Top panel: Retained mass (relative to the initial one) as a function of time for clumps of different masses in circular orbits at 1 kpc from the centre of the system. The residual mass is computed within 4r_s, where r_s is the initial Plummer scale radius. In this case, the clumps orbit in a Sparkler-like spherical potential representing the total mass, defined in Sect. 4.1. Masses go from log(M_*/M_⊙) = 6 to log(M_*/M_⊙) = 7.8 with a step of 0.3 dex (the arrow points from the smallest to the highest mass). Bottom panel: Same as the left panel but for clumps in quasi-circular orbit at 1 kpc from the centre of the system including a stellar disc component (modelled as in Sect. 5.2). The clump orbital plane is inclined of 30 degrees with respect to the plane of the disc.