TY - JOUR

T1 - Cosmology and the halo occupation distribution from small-scale galaxy clustering in the sloan digital sky survey

AU - Abazajian, Kevork

AU - Zheng, Zheng

AU - Zehavi, Idit

AU - Weinberg, David H.

AU - Frieman, Joshua A.

AU - Berlind, Andreas A.

AU - Blanton, Michael R.

AU - Bahcall, Neta A.

AU - Brinkmann, J.

AU - Schneider, Donald P.

AU - Tegmark, Max

N1 - Copyright:
Copyright 2015 Elsevier B.V., All rights reserved.

PY - 2005/6/1

Y1 - 2005/6/1

N2 - We use the projected correlation function wp(rp) 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 ACDM model. We find that combining wp(rp) 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 ACDM model with an HOD with three free parameters, we find Ωm = 0.278-0.027+0.027, σ8 = 0.812 -0.027+0.028, and H0 = 69.8-2.6 +2.6 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 Mmin = (3.03-0.36 +0.36)x 1012 h-lM⊙, M1 = (4.58 -0.60+0.60)xl013 h-l M⊙, and k = 4.44-0.69+0.51. 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.

AB - We use the projected correlation function wp(rp) 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 ACDM model. We find that combining wp(rp) 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 ACDM model with an HOD with three free parameters, we find Ωm = 0.278-0.027+0.027, σ8 = 0.812 -0.027+0.028, and H0 = 69.8-2.6 +2.6 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 Mmin = (3.03-0.36 +0.36)x 1012 h-lM⊙, M1 = (4.58 -0.60+0.60)xl013 h-l M⊙, and k = 4.44-0.69+0.51. 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.

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U2 - 10.1086/429685

DO - 10.1086/429685

M3 - Review article

AN - SCOPUS:22544440013

VL - 625

SP - 613

EP - 620

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 I

ER -