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Open Access Publications from the University of California

Clustering properties ofg-selected galaxies atz∼ 0.8

  • Author(s): 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
  • et al.

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© 2016 The Authors. 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.

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