Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 474, Issue 3, Pages 4024-4038Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx2807
Keywords
methods: analytical; methods: numerical; galaxies: evolution; galaxies: formation; cosmology: theory
Categories
Funding
- University of Portsmouth
- European Research Council Starting Grant [DEGAS-259586]
- Royal Astronomical Society Grant
- Science and Technology Facilities Council [ST/L00075X/1]
- Royal Society through the award of a University Research Fellowship
- European Research Council [DEGAS-259586]
- BIS National E-infrastructure capital grant [ST/K00042X/1]
- STFC [ST/H008519/1, ST/K00087X/1]
- STFC DiRAC Operations grant [ST/K003267/1]
- Durham University
- STFC [ST/P006299/1, ST/I00162X/1, ST/H008519/1, ST/P00556X/1, ST/R000832/1, ST/L00075X/1, ST/K00042X/1, ST/M007006/1, ST/P002293/1, ST/P000541/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/I00162X/1, ST/H008519/1, ST/P000541/1, ST/P002293/1, ST/R000832/1, ST/P00556X/1, ST/P006299/1, ST/M007006/1, ST/K00042X/1, ST/L00075X/1] Funding Source: researchfish
- UK Space Agency [ST/I002960/1] Funding Source: researchfish
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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 [O II] emitters, which dominate optical ELG selections at z similar or equal to 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 M-halo >= 10(10.3) h(-1)M(circle dot), with similar to 90 per cent of them being central star-forming galaxies. The predicted mean halo occupation distributions of [O II] emitters have 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 discs and a step function for spheroids, which plateau 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 similar to 1, a comparison with observed g-band-selected galaxy, which is 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.
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