Dust surface density maps in polar coordinates for model fid_dres without dust feedback (left hand side) and p1m6fb_dres with dust feedback after 500 orbits at 48 au for four different initial Stokes numbers and dust sizes. A dust agglomeration around the location of the trailing Lagrange point L5 is present for all Stokes numbers. Unlike the nonfeedback case, the right panels show that dust is trapped more efficiently in the leading Lagrange point L4 for smaller Stokes numbers. For St ≲ 3.6 × 10⁻², the L4 feature is more pronounced than the dust over density around L5. Dust feedback leads to an instability at the L5 point and fragments the asymmetric feature. Dust densities are normalized to the peak value of ring 1.