  AGB stars are, together with supernovae, the main contributors of stellar
dust to the interstellar medium (ISM). Dust grains formed by AGB stars are
thought to be large. However, as dust nucleation and growth within their
outflows are still not understood, the dust-grain size distribution (GSD) is
unknown. This is an important uncertainty regarding our knowledge of the
chemical and physical history of interstellar dust, as AGB dust forms $\sim$
70% of the starting point of its evolution. We expand on our chemical kinetics
model, which uniquely includes a comprehensive dust-gas chemistry. The GSD is
now allowed to deviate from the commonly assumed canonical Mathis et al. (1977)
distribution. We find that the specific GSD can significantly influence the
dust-gas chemistry within the outflow. Our results show that the level of
depletion of gas-phase species depends on the average grain surface area of the
GSD. Gas-phase abundance profiles and their possible depletions can be
retrieved from observations of molecular emission lines when using a range of
transitions. Due to degeneracies within the prescription of GSD, specific
parameters cannot be retrieved, only (a lower limit to) the average grain
surface area. Nonetheless, this can discriminate between dust composed of
predominantly large or small grains. We show that when combined with other
observables such as the spectral energy distribution and polarised light,
depletion levels from molecular gas-phase abundance profiles can constrain the
elusive GSD of the dust delivered to the ISM by AGB outflows.
