Clustering properties of g-selected galaxies at z ∼ 0.8
- Favole, Ginevra;
- Comparat, Johan;
- Prada, Francisco;
- Yepes, Gustavo;
- Jullo, Eric;
- Niemiec, Anna;
- Kneib, Jean-Paul;
- Rodríguez-Torres, Sergio A;
- Klypin, Anatoly;
- Skibba, Ramin A;
- McBride, Cameron K;
- Eisenstein, Daniel J;
- Schlegel, David J;
- Nuza, Sebastián E;
- Chuang, Chia-Hsun;
- Delubac, Timothée;
- Yèche, Christophe;
- Schneider, Donald P
Abstract
Current and future large redshift surveys, as the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey (SDSS-IV/eBOSS) or the Dark Energy Spectroscopic Instrument (DESI), will use emission-line galaxies (ELGs) to probe cosmological models by mapping the large-scale structure of the Universe in the redshift range 0.6 < z < 1.7. With current data, we explore the halo-galaxy connection by measuring three clustering properties of g-selected ELGs as matter tracers in the redshift range 0.6 < z < 1: (i) the redshift-space two-point correlation function using spectroscopic redshifts from the BOSS ELG sample and VIPERS; (ii) the angular two-point correlation function on the footprint of the CFHT-LS; (iii) the galaxy-galaxy lensing signal around the ELGs using the CFHTLenS. We interpret these observations by mapping them on to the latest high-resolution MultiDark Planck N-body simulation, using a novel (Sub)Halo-Abundance Matching technique that accounts for the ELG incompleteness. ELGs at z ~ 0.8 live in haloes of (1 ± 0.5) × 1012 h-1M⊙ and 22.5 ± 2.5 per cent of them are satellites belonging to a larger halo. The halo occupation distribution of ELGs indicates that we are sampling the galaxies in which stars form in the most efficient way, according to their stellar-to-halo mass ratio.