Cosmological parameters from eigenmode analysis of sloan digital sky survey galaxy redshifts

Adrian C. Pope; Takahiko Matsubara; Alexander S. Szalay; Michael R. Blanton; Daniel J. Eisenstein; Jim Gray; Bhuvnesh Jain; Neta A. Bahcall; Jon Brinkmann; Tamas Budavari; Andrew J. Connolly; Joshua A. Frieman; James E. Gunn; David Johnston; Stephen M. Kent; Robert H. Lupton; Avery Meiksin; Robert C. Nichol; Donald P. Schneider; Ryan Scranton; Michael A. Strauss; Istvan Szapudi; Max Tegmark; Michael S. Vogeley; David H. Weinberg; Idit Zehavi

doi:10.1086/383533

Cosmological parameters from eigenmode analysis of sloan digital sky survey galaxy redshifts

Adrian C. Pope, Takahiko Matsubara, Alexander S. Szalay, Michael R. Blanton, Daniel J. Eisenstein, Jim Gray, Bhuvnesh Jain, Neta A. Bahcall, Jon Brinkmann, Tamas Budavari, Andrew J. Connolly, Joshua A. Frieman, James E. Gunn, David Johnston, Stephen M. Kent, Robert H. Lupton, Avery Meiksin, Robert C. Nichol, Donald P. Schneider, Ryan ScrantonMichael A. Strauss, Istvan Szapudi, Max Tegmark, Michael S. Vogeley, David H. Weinberg, Idit Zehavi

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Abstract

We present estimates of cosmological parameters from the application of the Karhunen-Loève transform to the analysis of the three-dimensional power spectrum of density fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use Ω_mh and f_b = Ω_b/ Ω_m to describe the shape of the power spectrum, σ_8g^L for the (linearly extrapolated) normalization, and β to parameterize linear theory redshift-space distortions. On scales k ≲ 0.16 h Mpc^-1, our maximum likelihood values are Ω_mh = 0.264 ± 0.043, f_b = 0.286 ± 0.065, σ_8g^L = 0.966 ± 0.048, and β= 0.45 ± 0.12. When we take a prior on Ω_b from the Wilkinson Micro-wave Anisotropy Probe (WMAP), we find Ω_mh = 0.207 ± 0.030, which is in excellent agreement with WMAP and the Two-Degree Field. This indicates that we have reasonably measured the gross shape of the power spectrum, but we have difficulty breaking the degeneracy between Ω_mh and f_b, because the baryon oscillations are not resolved in the current spectroscopic survey window function.

Original language	English (US)
Pages (from-to)	655-660
Number of pages	6
Journal	Astrophysical Journal
Volume	607
Issue number	2 I
DOIs	https://doi.org/10.1086/383533
State	Published - Jun 1 2004

Keywords

Cosmological parameters
Cosmology: theory
Galaxies: distances and redshifts
Large-scale structure of universe
Methods: statistical

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/383533

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Pope, A. C., Matsubara, T., Szalay, A. S., Blanton, M. R., Eisenstein, D. J., Gray, J., Jain, B., Bahcall, N. A., Brinkmann, J., Budavari, T., Connolly, A. J., Frieman, J. A., Gunn, J. E., Johnston, D., Kent, S. M., Lupton, R. H., Meiksin, A., Nichol, R. C., Schneider, D. P., ... Zehavi, I. (2004). Cosmological parameters from eigenmode analysis of sloan digital sky survey galaxy redshifts. Astrophysical Journal, 607(2 I), 655-660. https://doi.org/10.1086/383533

Pope, AC, Matsubara, T, Szalay, AS, Blanton, MR, Eisenstein, DJ, Gray, J, Jain, B, Bahcall, NA, Brinkmann, J, Budavari, T, Connolly, AJ, Frieman, JA, Gunn, JE, Johnston, D, Kent, SM, Lupton, RH, Meiksin, A, Nichol, RC, Schneider, DP, Scranton, R, Strauss, MA, Szapudi, I, Tegmark, M, Vogeley, MS, Weinberg, DH & Zehavi, I 2004, 'Cosmological parameters from eigenmode analysis of sloan digital sky survey galaxy redshifts', Astrophysical Journal, vol. 607, no. 2 I, pp. 655-660. https://doi.org/10.1086/383533

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title = "Cosmological parameters from eigenmode analysis of sloan digital sky survey galaxy redshifts",

abstract = "We present estimates of cosmological parameters from the application of the Karhunen-Lo{\`e}ve transform to the analysis of the three-dimensional power spectrum of density fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use Ωmh and fb = Ωb/ Ωm to describe the shape of the power spectrum, σ8gL for the (linearly extrapolated) normalization, and β to parameterize linear theory redshift-space distortions. On scales k ≲ 0.16 h Mpc-1, our maximum likelihood values are Ωmh = 0.264 ± 0.043, fb = 0.286 ± 0.065, σ8gL = 0.966 ± 0.048, and β= 0.45 ± 0.12. When we take a prior on Ωb from the Wilkinson Micro-wave Anisotropy Probe (WMAP), we find Ωmh = 0.207 ± 0.030, which is in excellent agreement with WMAP and the Two-Degree Field. This indicates that we have reasonably measured the gross shape of the power spectrum, but we have difficulty breaking the degeneracy between Ωmh and fb, because the baryon oscillations are not resolved in the current spectroscopic survey window function.",

keywords = "Cosmological parameters, Cosmology: theory, Galaxies: distances and redshifts, Large-scale structure of universe, Methods: statistical",

author = "Pope, {Adrian C.} and Takahiko Matsubara and Szalay, {Alexander S.} and Blanton, {Michael R.} and Eisenstein, {Daniel J.} and Jim Gray and Bhuvnesh Jain and Bahcall, {Neta A.} and Jon Brinkmann and Tamas Budavari and Connolly, {Andrew J.} and Frieman, {Joshua A.} and Gunn, {James E.} and David Johnston and Kent, {Stephen M.} and Lupton, {Robert H.} and Avery Meiksin and Nichol, {Robert C.} and Schneider, {Donald P.} and Ryan Scranton and Strauss, {Michael A.} and Istvan Szapudi and Max Tegmark and Vogeley, {Michael S.} and Weinberg, {David H.} and Idit Zehavi",

year = "2004",

month = jun,

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doi = "10.1086/383533",

language = "English (US)",

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journal = "Astrophysical Journal",

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T1 - Cosmological parameters from eigenmode analysis of sloan digital sky survey galaxy redshifts

AU - Pope, Adrian C.

AU - Matsubara, Takahiko

AU - Szalay, Alexander S.

AU - Blanton, Michael R.

AU - Eisenstein, Daniel J.

AU - Gray, Jim

AU - Jain, Bhuvnesh

AU - Bahcall, Neta A.

AU - Brinkmann, Jon

AU - Budavari, Tamas

AU - Connolly, Andrew J.

AU - Frieman, Joshua A.

AU - Gunn, James E.

AU - Johnston, David

AU - Kent, Stephen M.

AU - Lupton, Robert H.

AU - Meiksin, Avery

AU - Nichol, Robert C.

AU - Schneider, Donald P.

AU - Scranton, Ryan

AU - Strauss, Michael A.

AU - Szapudi, Istvan

AU - Tegmark, Max

AU - Vogeley, Michael S.

AU - Weinberg, David H.

AU - Zehavi, Idit

PY - 2004/6/1

Y1 - 2004/6/1

N2 - We present estimates of cosmological parameters from the application of the Karhunen-Loève transform to the analysis of the three-dimensional power spectrum of density fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use Ωmh and fb = Ωb/ Ωm to describe the shape of the power spectrum, σ8gL for the (linearly extrapolated) normalization, and β to parameterize linear theory redshift-space distortions. On scales k ≲ 0.16 h Mpc-1, our maximum likelihood values are Ωmh = 0.264 ± 0.043, fb = 0.286 ± 0.065, σ8gL = 0.966 ± 0.048, and β= 0.45 ± 0.12. When we take a prior on Ωb from the Wilkinson Micro-wave Anisotropy Probe (WMAP), we find Ωmh = 0.207 ± 0.030, which is in excellent agreement with WMAP and the Two-Degree Field. This indicates that we have reasonably measured the gross shape of the power spectrum, but we have difficulty breaking the degeneracy between Ωmh and fb, because the baryon oscillations are not resolved in the current spectroscopic survey window function.

AB - We present estimates of cosmological parameters from the application of the Karhunen-Loève transform to the analysis of the three-dimensional power spectrum of density fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use Ωmh and fb = Ωb/ Ωm to describe the shape of the power spectrum, σ8gL for the (linearly extrapolated) normalization, and β to parameterize linear theory redshift-space distortions. On scales k ≲ 0.16 h Mpc-1, our maximum likelihood values are Ωmh = 0.264 ± 0.043, fb = 0.286 ± 0.065, σ8gL = 0.966 ± 0.048, and β= 0.45 ± 0.12. When we take a prior on Ωb from the Wilkinson Micro-wave Anisotropy Probe (WMAP), we find Ωmh = 0.207 ± 0.030, which is in excellent agreement with WMAP and the Two-Degree Field. This indicates that we have reasonably measured the gross shape of the power spectrum, but we have difficulty breaking the degeneracy between Ωmh and fb, because the baryon oscillations are not resolved in the current spectroscopic survey window function.

KW - Cosmological parameters

KW - Cosmology: theory

KW - Galaxies: distances and redshifts

KW - Large-scale structure of universe

KW - Methods: statistical

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U2 - 10.1086/383533

DO - 10.1086/383533

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SN - 0004-637X

VL - 607

SP - 655

EP - 660

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 I

ER -

Cosmological parameters from eigenmode analysis of sloan digital sky survey galaxy redshifts

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