Luminosity function of [OII] emission-line galaxies in the MassiveBlack-II simulation

Abstract

We examine the luminosity function (LF) of [OII] emission-line galaxies in the high-resolution cosmological simulation MassiveBlack-II (MBII). From the spectral energy distribution of each galaxy, we select a sub-sample of star-forming galaxies at $0.06\le z\le 3.0$ using the [OII] emission line luminosity L([OII]). We confirm that the specific star formation rate matches that in the GAMA survey. We show that the [OII] LF at z=1.0 from the MBII shows a good agreement with the LFs from several surveys below L([OII])=$10^{43.0}$ erg/s while the low redshifts ($z\le 0.3$) show an excess in the prediction of bright [OII] galaxies, but still displaying a good match with observations below L([OII])=$10^{41.6}$ erg/s. Based on the validity in reproducing the properties of [OII] galaxies at low redshift ($z\le 1$), we forecast the evolution of the [OII] LF at high redshift ($z\le 3$), which can be tested by upcoming surveys such as the HETDEX and DESI. The slopes of the LFs at bright and faint ends range from -3 to -2 showing minima at z=2. The slope of the bright end evolves approximately as 1/(z+1) at z=2 while the faint end evolves as ~3/(z+1) at $0.6\le z\le 2$. In addition, a similar analysis is applied for the evolution of [OIII] LFs, which is to be explored in the forthcoming survey WFIRST-AFTA. Finally, we show that the auto-correlation function of [OII] and [OIII] emitting galaxies shows a rapid evolution from z=2 to 1.

12 pages, 13 figures, 3 tables, accepted for publication in MNRAS

References in corpus (16)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• The Cosmic Evolution Survey (COSMOS) -- Overview
• A Highly Consistent Framework for the Evolution of the Star-Forming "Main Sequence" from z~0-6
• Properties of galaxies reproduced by a hydrodynamic simulation
• Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report
• A unified model for AGN feedback in cosmological simulations of structure formation
• Formation of Supermassive Black Holes by Direct Collapse in Pregalactic Halos
• Direct cosmological simulations of the growth of black holes and galaxies
• Formation of z ~ 6 quasars from hierarchical galaxy mergers
• Quasars at z=6: the survival of the fittest
• The BlueTides Simulation: First Galaxies and Reionization
• 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
• The 0.1<z<1.65 evolution of the bright end of the [OII] luminosity function
• BigBOSS: The Ground-Based Stage IV Dark Energy Experiment
• Supermassive Black Holes and Their Environments

Cited by in corpus (12)

• A massive, quiescent galaxy at redshift of z=3.717
• First Light: exploring the Spectra of High-Redshift Galaxies in the Renaissance Simulations
• The first Super Massive Black Holes: indications from models for future observations
• The HETDEX Survey: Emission Line Exploration and Source Classification
• HOD modelling of high redshift galaxies using the BLUETIDES simulation
• First Light II: Emission Line Extinction, Population III Stars, and X-ray Binaries
• Massive Quiescent Galaxies at z>3 in The Millennium Simulation Populated by A Semi-analytic Galaxy Formation Model
• Clustering of emission line galaxies with IllustrisTNG I.: fundamental properties and halo occupation distribution
• The OTELO survey: Faint end of the luminosity function of [OII] emitters at <z>= 1.43
• X-ray Selected Narrow-Line Active Galactic Nuclei in the COSMOS Field: Nature of Optically Dull Active Galactic Nuclei
• Universal conditional distribution function of [OII] luminosity of galaxies, and prediction for the [OII] luminosity function at redshift $z<3$
• Cloudy-Maraston: Integrating nebular continuum and line emission with the Maraston stellar population synthesis models