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

Abstract

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 $M_{\mathrm{halo}}\ge 10^{10.3}{h}^{-1}{\mathrm{M}}_{\odot }$, 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, $⟨N{⟩}_{\left[OII\right]cen}$, being far from the canonical step function. The $⟨N{⟩}_{\left[OII\right]cen}$ 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.

17 pages, 16 figures, MNRAS

References in corpus (18)

• The propagation of uncertainties in stellar population synthesis modeling I: The relevance of uncertain aspects of stellar evolution and the IMF to the derived physical properties of galaxies
• The DESI Experiment Part I: Science,Targeting, and Survey Design
• A primer on hierarchical galaxy formation: the semi-analytical approach
• Structure and star formation in galaxies out to z=3: evidence for surface density dependent evolution and upsizing
• Weak Gravitational Lensing with COSMOS: Galaxy Selection and Shape Measurements
• Ram pressure stripping the hot gaseous halos of galaxies in groups and clusters
• The DESI Experiment Part II: Instrument Design
• Environmental Effects on Satellite Galaxies: The Link Between Concentration, Size and Colour Profile
• The Luminosity Function and Star Formation Rate between Redshifts of 0.07 and 1.47 for Narrow-band Emitters in the Subaru Deep Field
• Evolution of the H$\beta$+[OIII] and [OII] luminosity functions and the [OII] star-formation history of the Universe up to $z$ ~ 5 from HiZELS
• SDSS IV MaNGA - The spatially resolved transition from star formation to quiescence
• The 0.1<z<1.65 evolution of the bright end of the [OII] luminosity function
• Project overview and update on WEAVE: the next generation wide-field spectroscopy facility for the William Herschel Telescope
• Testing the predictions of the cold dark matter model for the sizes, colours, morphologies and luminosities of galaxies with the SDSS
• The clustering of Ly-alpha emitters in a LambdaCDM Universe
• The evolution of the star forming sequence in hierarchical galaxy formation models
• The SDSS-IV eBOSS: emission line galaxy catalogues at z=0.8 and study of systematic errors in the angular clustering
• A new methodology to test galaxy formation models using the dependence of clustering on stellar mass

Cited by in corpus (5)

• Linear bias forecasts for emission line cosmological surveys
• The Mass-Metallicity Relation at $z\sim 0.8$: Redshift Evolution and Parameter Dependency
• The Completed SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: GLAM-QPM mock galaxy catalogs for the Emission Line Galaxy Sample
• Global analysis of luminosity- and colour-dependent galaxy clustering in the Sloan Digital Sky Survey
• A new approach to finding galaxy groups using Markov Clustering