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This document contains refereed supplementary information for the paper``Rapid planetesimal formation in turbulent circumstellar discs''. It contains15 sections (\S1.1 -- \S1.15) that address a number of subjects related to themain paper. We describe in detail the Poisson solver used to find theself-potential of the solid particles, including a linear and a non-linear testproblem (\S1.3). Dissipative collisions remove energy from the motion of theparticles by collisional cooling (\S1.4), an effect that allows gravitationalcollapse to occur in somewhat less massive discs (\S1.7). A resolution study ofthe gravitational collapse of the boulders is presented in \S1.6. We find thatgravitational collapse can occur in progressively less massive discs as thegrid resolution is increased, likely due to the decreased smoothing of theparticle-mesh self-gravity solver with increasing resolution. In \S1.10 we showthat it is in good agreement with the Goldreich & Ward (1973) stabilityanalysis to form several-hundred-km-sized bodies, when the analysis is appliedto 5 AU and to regions of increased boulder column density. \S11 is devoted tothe measurement of random speeds and collision speeds between boulders. We findgood agreement between our measurements and analytical theory for the randomspeeds, but the measured collision speeds are 3 times lower than expected fromanalytical theory. Higher resolution studies, and an improved analytical theoryof collision speeds that takes into account epicyclic motion, will be needed todetermine whether collision speeds have converged. In \S1.12 we present modelswith no magnetic fields. The boulder layer still exhibits strong clumping, dueto the streaming instability, if the global solids-to-gas ratio is increased bya factor 3. Gravitational collapse occurs as readily as in magnetised discs.

Supplementary Information for ``Rapid planetesimal formation in turbulent circumstellar discs''