The host dark matter haloes of O II emitters at 0.5 < z < 1.5

Emission line galaxies (ELGs) are used in several ongoing and upcoming surveys (SDSSIV/eBOSS, ) as tracers of the dark matter distribution. Using a new galaxy formation, we explore the characteristics of O II emitters, which dominate optical ELG selections z 1. Model O II emitters at 0. 5 < z < 1. 5 are selected to mimic the DEEP2, , eBOSS and DESI surveys. The luminosity functions of model O II emitters are in agreement with observations. The selected O II emitters are hosted by haloes with ≥ 1010. 3h−1M, with ∼90 per cent of them being central star-forming galaxies. The mean halo occupation distributions of O II emitters have a shape typical of that for star-forming galaxies, with the contribution from central galaxies, NO II cen, far from the canonical step function. The NO II cen can be described as the sum of an Gaussian for discs and a step function for spheroids, which plateau below unity. model O II emitters have a clustering bias close to unity, which is below the expectations eBOSS and DESI ELGs. At z ∼ 1, a comparison with observed g-band-selected galaxy, is expected to be dominated by O II emitters, indicates that our model produces too O II emitters that are satellite galaxies. This suggests the need to revise our modelling of gas stripping in satellite galaxies.