  Context. Small binary asteroid systems and pairs are thought to form through
fission induced by spin up via the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP)
effect. This process is expected to depend on their structural strength, hence
composition. Aims. We aim to determine how taxonomic classes, used as a proxy
for composition, distribute amongst binary asteroids and asteroid pairs
compared to the general population. Methods. We compare the distribution of
taxonomic classes of binary systems and pairs with that of a reference sample
of asteroids. We build this sample by selecting asteroids to reproduce the
orbital and size distribution of the binaries and pairs to minimize potential
biases between samples. Results. A strong deficit of primitive compositions (C,
B, P, D types) among binary asteroids and asteroid pairs is identified, as well
as a strong excess of asteroids with mafic-silicate rich surface compositions
(S, Q, V, A types). Conclusions. Amongst low mass, rapidly rotating asteroids,
those with mafic-silicate rich compositions are more likely to form multiple
asteroid systems than their primitive counterparts.
