### Abstract

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 ~8 more modes in the cosmological analysis than an analysis with k_{max} = 0.1 h Mpc^{-1},aswas 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: χ^{2} = 39.6 for 40 degrees of freedom for the best-fitting Δ cold dark matter (ΔCDM) model. We find Ω_{m}h^{2}(n_{s}/0.96)^{1.2} = 0.141^{+0.010}_{-0.012} for a power-law primordial power spectrum with spectral index n_{s} and Ω_{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}/D_{V}(0.35) = 0.1097^{+0.0039}_{-0.0042}. Combining the halo power spectrum measurement with the Wilkinson Microwave Anisotropy Probe (WMAP) 5 year results, for the flat ΔCDM model we find Ω_{m} = 0.289 ± 0.019 and H_{0} = 69.4 ± 1.6 km s^{-1} Mpc^{-1}. Allowing ∑ for massive neutrinos in ΔCDM, we find σm_{ν} < 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^{+1.8}_{-1.7}. Combining also with the Kowalski et al. supernova sample, we find Ω_{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/.

Original language | English (US) |
---|---|

Pages (from-to) | 60-85 |

Number of pages | 26 |

Journal | Monthly Notices of the Royal Astronomical Society |

Volume | 404 |

Issue number | 1 |

DOIs | |

State | Published - May 1 2010 |

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### All Science Journal Classification (ASJC) codes

- Astronomy and Astrophysics
- Space and Planetary Science

### Cite this

*Monthly Notices of the Royal Astronomical Society*,

*404*(1), 60-85. https://doi.org/10.1111/j.1365-2966.2010.16276.x

}

*Monthly Notices of the Royal Astronomical Society*, vol. 404, no. 1, pp. 60-85. https://doi.org/10.1111/j.1365-2966.2010.16276.x

**Cosmological constraints from the clustering of the Sloan Digital Sky Survey DR7 luminous red galaxies.** / Reid, Beth A.; Percival, Will J.; Eisenstein, Daniel J.; Verde, Licia; Spergel, David N.; Skibba, Ramin A.; Bahcall, Neta A.; Budavari, Tamas; Frieman, Joshua A.; Fukugita, Masataka; Gott, J. Richard; Gunn, James E.; Ivezić, Željko; Knapp, Gillian R.; Kron, Richard G.; Lupton, Robert H.; McKay, Timothy A.; Meiksin, Avery; Nichol, Robert C.; Pope, Adrian C.; Schlegel, David J.; Schneider, Donald P.; Stoughton, Chris; Strauss, Michael A.; Szalay, Alexander S.; Tegmark, Max; Vogeley, Michael S.; Weinberg, David H.; York, Donald G.; Zehavi, Idit.

Research output: Contribution to journal › Article

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 - Ivezić, Željko

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 ~8 more modes in the cosmological analysis than an analysis with kmax = 0.1 h Mpc-1,aswas adopted in the SDSS team analysis of the DR4 LRG sample. The observed halo power spectrum for 0.02 -1 is well fitted by our model: χ2 = 39.6 for 40 degrees of freedom for the best-fitting Δ cold dark matter (ΔCDM) model. We find Ωmh2(ns/0.96)1.2 = 0.141+0.010-0.012 for a power-law primordial power spectrum with spectral index ns and Ωbh2 = 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: rs/DV(0.35) = 0.1097+0.0039-0.0042. Combining the halo power spectrum measurement with the Wilkinson Microwave Anisotropy Probe (WMAP) 5 year results, for the flat ΔCDM model we find Ωm = 0.289 ± 0.019 and H0 = 69.4 ± 1.6 km s-1 Mpc-1. Allowing ∑ for massive neutrinos in ΔCDM, we find σmν < 0.62 eV at the 95 per cent confidence level. If we instead consider the effective number of relativistic species Neff as a free parameter, we find Neff = 4.8+1.8-1.7. Combining also with the Kowalski et al. supernova sample, we find Ωtot = 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 ~8 more modes in the cosmological analysis than an analysis with kmax = 0.1 h Mpc-1,aswas adopted in the SDSS team analysis of the DR4 LRG sample. The observed halo power spectrum for 0.02 -1 is well fitted by our model: χ2 = 39.6 for 40 degrees of freedom for the best-fitting Δ cold dark matter (ΔCDM) model. We find Ωmh2(ns/0.96)1.2 = 0.141+0.010-0.012 for a power-law primordial power spectrum with spectral index ns and Ωbh2 = 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: rs/DV(0.35) = 0.1097+0.0039-0.0042. Combining the halo power spectrum measurement with the Wilkinson Microwave Anisotropy Probe (WMAP) 5 year results, for the flat ΔCDM model we find Ωm = 0.289 ± 0.019 and H0 = 69.4 ± 1.6 km s-1 Mpc-1. Allowing ∑ for massive neutrinos in ΔCDM, we find σmν < 0.62 eV at the 95 per cent confidence level. If we instead consider the effective number of relativistic species Neff as a free parameter, we find Neff = 4.8+1.8-1.7. Combining also with the Kowalski et al. supernova sample, we find Ωtot = 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/.

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U2 - 10.1111/j.1365-2966.2010.16276.x

DO - 10.1111/j.1365-2966.2010.16276.x

M3 - Article

AN - SCOPUS:77954074610

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 -