2004/08/31 by Kevork Abazajian, Zheng Zheng, Idit Zehavi +8
Physics and Astronomy · #Astronomy and Astrophysical Research #Cosmic microwave background #Cosmology #Cosmology and Gravitation Theories #Galactic halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Halo #Planck #Redshift #Satellite galaxy #Sky #astro-ph
paper · pdf · doi:10.1086/429685
published as Astrophys.J.625:613-620,2005 · v2: includes an expanded modeling discussion, a test for halo spatial bias model dependence, and a small but non-negligible contribution from sample variance
arxiv created 2005/01/18 · openalex publication_date 2005/05/27 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We use the projected correlation function w p ( r p ) of a volume-limited subsample of the Sloan Digital Sky Survey (SDSS) main galaxy-redshift catalog to measure the halo occupation distribution (HOD) of the galaxies of the sample. Simultaneously, we allow the cosmology to vary within cosmological constraints imposed by cosmic microwave background experiments in a ΛCDM model. We find that combining w p ( r p ) for this sample alone with observations by the Wilkinson Microwave Anisotropy Probe ( WMAP ), Arcminute Cosmology Bolometer Array Receiver (ACBAR), Cosmic Background Imager (CBI), and Very Small Array (VSA) can provide one of the most precise techniques available to measure cosmological parameters. For a minimal, flat, six-parameter ΛCDM model with an HOD with three free parameters, we find Ω m = 0.278 , σ 8 = 0.812 , and H 0 = 69.8 km s -1 Mpc -1 ; these errors are significantly smaller than from cosmic microwave background (CMB) alone and similar to those obtained by combining CMB with the large-scale galaxy power spectrum assuming scale-independent bias. The corresponding HOD parameters describing the minimum halo mass and the normalization and cutoff of the satellite mean occupation are M min = (3.03 ) × 10 12 h -1 M ☉ , M 1 = (4.58 ) × 10 13 h -1 M ☉ , and κ = 4.44 . These HOD parameters thus have small fractional uncertainty when cosmological parameters are allowed to vary within the range permitted by the data. When more parameters are added to the HOD model, the error bars on the HOD parameters increase because of degeneracies, but the error bars on the cosmological parameters do not increase greatly. Similar modeling for other galaxy samples could reduce the statistical errors on these results, while more thorough investigations of the cosmology dependence of nonlinear halo bias and halo mass functions are needed to eliminate remaining systematic uncertainties, which may be comparable to statistical uncertainties.