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Emission line galaxies (ELGs) are used in several ongoing and upcomingsurveys (SDSS-IV/eBOSS, DESI) as tracers of the dark matter distribution. Usinga new galaxy formation model, we explore the characteristics of [OII] emitters,which dominate optical ELG selections at $z\simeq 1$. Model [OII] emitters at$0.5<z<1.5$ are selected to mimic the DEEP2, VVDS, eBOSS and DESI surveys. Theluminosity functions of model [OII] emitters are in reasonable agreement withobservations. The selected [OII] emitters are hosted by haloes with $M_{\rmhalo}\geq 10^{10.3}h^{-1}{\rm M}_{\odot}$, with ~90% of them being centralstar-forming galaxies. The predicted mean halo occupation distributions of[OII] emitters has a shape typical of that inferred for star-forming galaxies,with the contribution from central galaxies, $\langle N\rangle_{\left[OII\right]\, cen}$, being far from the canonical step function.The $\langle N \rangle_{\left[OII\right]\, cen}$ can be described as the sum ofan asymmetric Gaussian for disks and a step function for spheroids, whichplateaus below unity. The model [OII] emitters have a clustering bias close tounity, which is below the expectations for eBOSS and DESI ELGs. At $z\sim 1$, acomparison with observed g-band selected galaxy, which are expected to bedominated by [OII] emitters, indicates that our model produces too few [OII]emitters that are satellite galaxies. This suggests the need to revise ourmodelling of hot gas stripping in satellite galaxies.

The host dark matter halos of [OII] emitters at 0.5< z< 1.5