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

V. Gonzalez-Perez, J. Comparat, P. Norberg, C. M. Baugh, S. Contreras, C. Lacey, N. McCullagh, A. Orsi, J. Helly, J. Humphries

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Emission line galaxies (ELGs) are used in several ongoing and upcoming surveys as tracers of the dark matter distribution. Using a new galaxy formation model, we explore the characteristics of [O II] emitters, which dominate optical ELG selections at z ≃ 1. Model [O II] emitters at 0.5 < z < 1.5 are selected to mimic the DEEP2, VVDS, eBOSS and DESI surveys. The luminosity functions of model [O II] emitters are in reasonable agreement with observations. The selected [O II] emitters are hosted by haloes with Mhalo≥1010.3h−1M, with ∼90% of them being central star-forming galaxies. The predicted mean halo occupation distributions of [O II] emitters has a shape typical of that inferred for star-forming galaxies, with the contribution from central galaxies, ⟨N⟩[O II],cen, being far from the canonical step function. The ⟨N⟩[O II],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 [O II] emitters have a clustering bias close to unity, which is below the expectations for eBOSS and DESI ELGs. At z∼1, a comparison with observed g-band selected galaxy, which are expected to be dominated by [O II] emitters, indicates that our model produces too few [O II] emitters that are satellite galaxies. This suggests the need to revise our modelling of hot gas stripping in satellite galaxies.
Original languageEnglish
Pages (from-to)4024-4038
Number of pages15
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Early online date30 Oct 2017
Publication statusPublished - 1 Mar 2018


  • astro-ph.GA
  • astro-ph.CO
  • RCUK
  • STFC
  • ST/L00075X/1
  • ST/K00042X/1
  • ST/H008519/1
  • ST/K00087X/1
  • ST/K003267/1
  • methods: analytical
  • methods: numerical
  • galaxies: evolution
  • galaxies: formation
  • cosmology: theory


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