Final stellar surface abundances of the elements heavier than Fe for the 3, 4, and 5 M_⊙ ATON stars (top, middle, and bottom panel, respectively), post-processed with SNUPPAT with three different convective overshoot parameters, ω. The elements marked in red are those most sensitive to the neutron density. The breaks in the abundance distribution are due to the unstable isotopes Tc (Z = 43) and Pm (Z = 61).