info:eu-repo/semantics/article
Clustering properties of g-selected galaxies at z ~ 0.8
Fecha
2016-10Registro en:
Favole, Ginevra; Comparat, Johan; Prada, Francisco; Yepes, Gustavo; Jullo, Eric; et al.; Clustering properties of g-selected galaxies at z ~ 0.8; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 461; 4; 10-2016; 3421-3431
0035-8711
CONICET Digital
CONICET
Autor
Favole, Ginevra
Comparat, Johan
Prada, Francisco
Yepes, Gustavo
Jullo, Eric
Niemiec, Anna
Kneib, Jean-Paul
Rodriguez Torres, Sergio A.
Klypin, Anatoly
Skibba, Ramin A.
McBride, Cameron K.
Eisenstein, Daniel J.
Schlegel, David J.
Nuza, Sebastian Ernesto
Chuang, Chia-Hsun
Delubac, Timotheé
Yèche, Christophe
Schneider, Donald P.
Schneider, Donald P.
Resumen
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) × 10 12 h -1 M⊙ 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.