The host dark matter halos of [OII] emitters at 0.5< z< 1.5
  Emission line galaxies (ELGs) are used in several ongoing and upcoming
surveys (SDSS-IV/eBOSS, DESI) as tracers of the dark matter distribution. Using
a 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. The
luminosity functions of model [OII] emitters are in reasonable agreement with
observations. The selected [OII] emitters are hosted by haloes with $M_{\rm
halo}\geq 10^{10.3}h^{-1}{\rm M}_{\odot}$, with ~90% of them being central
star-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 of
an asymmetric Gaussian for disks and a step function for spheroids, which
plateaus below unity. The model [OII] emitters have a clustering bias close to
unity, which is below the expectations for eBOSS and DESI ELGs. At $z\sim 1$, a
comparison with observed g-band selected galaxy, which are expected to be
dominated by [OII] emitters, indicates that our model produces too few [OII]
emitters that are satellite galaxies. This suggests the need to revise our
modelling of hot gas stripping in satellite galaxies.
