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We use the Copernicus Complexio (COCO) high resolution $N$-body simulationsto investigate differences in the properties of small-scale structures in thestandard cold dark matter (CDM) model and in a model with a cutoff in theinitial power spectrum of density fluctuations consistent with both a thermallyproduced warm dark matter (WDM) particle or a sterile neutrino with mass 7 keVand leptogenesis parameter $L_6=8.7$. The latter corresponds to the "coldest"model with this sterile neutrino mass compatible with the identification of therecently detected 3.5 keV X-ray line as resulting from particle decay. CDM andWDM predict very different number densities of subhaloes with mass $\leq10^9\,h^{-1}\,M_\odot$ although they predict similar, nearly universal,normalised subhalo radial density distributions. Haloes and subhaloes in bothmodels have cuspy NFW profiles, but WDM subhaloes below the cutoff scale in thepower spectrum (corresponding to maximum circular velocities$V_{\mathrm{max}}^{z=0} \leq50~\mathrm{kms}^{-1}$) are less concentrated thantheir CDM counterparts. We make predictions for observable properties using theGALFORM semi-analytic model of galaxy formation. Both models predict Milky Waysatellite luminosity functions consistent with observations, although the WDMmodel predicts fewer very faint satellites. This model, however, predictsslightly more UV bright galaxies at redshift $z>7$ than CDM, but both areconsistent with observations. Gravitational lensing offers the best prospect ofdistinguishing between the models.

Substructure and galaxy formation in the Copernicus Complexio warm dark matter simulations