  Previous investigations have revealed that eccentric super-Earths represent a
class of planets which are particularly effective at transporting minor bodies
towards white dwarfs and subsequently polluting their atmospheres with
observable chemical signatures. However, the lack of discoveries of these
planets beyond a few astronomical units from their host stars prompts a better
understanding of their orbital architectures from their nascent birth cluster.
Here, we perform stellar cluster simulations of 3-planet and 7-planet systems
containing super-Earths on initially circular, coplanar orbits. We adopt the
typical stellar masses of main-sequence progenitors of white dwarfs
($1.5\,\mathrm{M}_{\odot}$-$2.5\,\mathrm{M}_{\odot}$) as host stars and include
8,000 main-sequence stars following a Kroupa initial mass function in our
clusters. Our results reveal that about 30 per cent of the simulated planets
generate eccentricities of at least 0.1 by the time of cluster dissolution,
which would aid white dwarf pollution. We provide our output parameters to the
community for potential use as initial conditions for subsequent evolution
simulations.
