TY - JOUR
T1 - Cosmological constraints from the clustering of the Sloan Digital Sky Survey DR7 luminous red galaxies
AU - Reid, Beth A.
AU - Percival, Will J.
AU - Eisenstein, Daniel J.
AU - Verde, Licia
AU - Spergel, David N.
AU - Skibba, Ramin A.
AU - Bahcall, Neta A.
AU - Budavari, Tamas
AU - Frieman, Joshua A.
AU - Fukugita, Masataka
AU - Gott, J. Richard
AU - Gunn, James E.
AU - Ivezic, Zeljko
AU - Knapp, Gillian R.
AU - Kron, Richard G.
AU - Lupton, Robert H.
AU - McKay, Timothy A.
AU - Meiksin, Avery
AU - Nichol, Robert C.
AU - Pope, Adrian C.
AU - Schlegel, David J.
AU - Schneider, Donald P.
AU - Stoughton, Chris
AU - Strauss, Michael A.
AU - Szalay, Alexander S.
AU - Tegmark, Max
AU - Vogeley, Michael S.
AU - Weinberg, David H.
AU - York, Donald G.
AU - Zehavi, Idit
PY - 2010/5/1
Y1 - 2010/5/1
N2 - We present the power spectrum of the reconstructed halo density field derived from a sample of luminous red galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS) Seventh Data Release (DR7). The halo power spectrum has a direct connection to the underlying dark matter power for k <= 0.2 h Mpc(-1), well into the quasi-linear regime. This enables us to use a factor of similar to 8 more modes in the cosmological analysis than an analysis with k(max) = 0.1 h Mpc(-1), as was adopted in the SDSS team analysis of the DR4 LRG sample. The observed halo power spectrum for 0.02< k < 0.2 h Mpc(-1) is well fitted by our model: chi(2) = 39.6 for 40 degrees of freedom for the best-fitting Lambda cold dark matter (Lambda CDM) model. We find Omega(m)h(2)(n(s)/0.96)(1.2) = 0.141(-0.012+)(0.010) for a power-law primordial power spectrum with spectral index ns and Omega(b)h(2) = 0.022 65 fixed, consistent with cosmic microwave background measurements. The halo power spectrum also constrains the ratio of the comoving sound horizon at the baryon-drag epoch to an effective distance to z = 0.35: r(s)/DV(0.35) = 0.1097(-0.0042)(+0.0039). Combining the halo power spectrum measurement with the Wilkinson Microwave Anisotropy Probe (WMAP) 5 year results, for the flat Lambda CDM model we find Omega(m) = 0.289 +/- 0.019 and H-0 = 69.4 +/- 1.6 kms(-1) Mpc(-1). Allowing for massive neutrinos in Lambda CDM, we find Sigma m(nu) < 0.62 eV at the 95 per cent confidence level. If we instead consider the effective number of relativistic species N-eff as a free parameter, we find N-eff = 4.8(-1.7)(+1.8). Combining also with the Kowalski et al. supernova sample, we find Omega(tot) = 1.011 +/- 0.009 and w = -0.99 +/- 0.11 for an open cosmology with constant dark energy equation of state w. The power spectrum and a module to calculate the likelihoods are publicly available at http://lambda.gsfc.nasa.gov/toolbox/lrgdr/.
AB - We present the power spectrum of the reconstructed halo density field derived from a sample of luminous red galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS) Seventh Data Release (DR7). The halo power spectrum has a direct connection to the underlying dark matter power for k <= 0.2 h Mpc(-1), well into the quasi-linear regime. This enables us to use a factor of similar to 8 more modes in the cosmological analysis than an analysis with k(max) = 0.1 h Mpc(-1), as was adopted in the SDSS team analysis of the DR4 LRG sample. The observed halo power spectrum for 0.02< k < 0.2 h Mpc(-1) is well fitted by our model: chi(2) = 39.6 for 40 degrees of freedom for the best-fitting Lambda cold dark matter (Lambda CDM) model. We find Omega(m)h(2)(n(s)/0.96)(1.2) = 0.141(-0.012+)(0.010) for a power-law primordial power spectrum with spectral index ns and Omega(b)h(2) = 0.022 65 fixed, consistent with cosmic microwave background measurements. The halo power spectrum also constrains the ratio of the comoving sound horizon at the baryon-drag epoch to an effective distance to z = 0.35: r(s)/DV(0.35) = 0.1097(-0.0042)(+0.0039). Combining the halo power spectrum measurement with the Wilkinson Microwave Anisotropy Probe (WMAP) 5 year results, for the flat Lambda CDM model we find Omega(m) = 0.289 +/- 0.019 and H-0 = 69.4 +/- 1.6 kms(-1) Mpc(-1). Allowing for massive neutrinos in Lambda CDM, we find Sigma m(nu) < 0.62 eV at the 95 per cent confidence level. If we instead consider the effective number of relativistic species N-eff as a free parameter, we find N-eff = 4.8(-1.7)(+1.8). Combining also with the Kowalski et al. supernova sample, we find Omega(tot) = 1.011 +/- 0.009 and w = -0.99 +/- 0.11 for an open cosmology with constant dark energy equation of state w. The power spectrum and a module to calculate the likelihoods are publicly available at http://lambda.gsfc.nasa.gov/toolbox/lrgdr/.
UR - http://www.scopus.com/inward/record.url?scp=77954074610&partnerID=8YFLogxK
U2 - 10.1111/j.1365-2966.2010.16276.x
DO - 10.1111/j.1365-2966.2010.16276.x
M3 - Article
VL - 404
SP - 60
EP - 85
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -