Measuring the matter density using baryon oscillations in the SDSS

Will J. Percival; Robert C. Nichol; Daniel J. Eisenstein; David H. Weinberg; Masataka Fukugita; Adrian C. Pope; Donald P. Schneider; Alex S. Szalay; Michael S. Vogeley; Idit Zehavi; Neta A. Bahcall; Jon Brinkmann; Andrew J. Connolly; Jon Loveday; Avery Meiksin

doi:10.1086/510772

Measuring the matter density using baryon oscillations in the SDSS

Will J. Percival, Robert C. Nichol, Daniel J. Eisenstein, David H. Weinberg, Masataka Fukugita, Adrian C. Pope, Donald P. Schneider, Alex S. Szalay, Michael S. Vogeley, Idit Zehavi, Neta A. Bahcall, Jon Brinkmann, Andrew J. Connolly, Jon Loveday, Avery Meiksin

Astrophysical Sciences

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133 Scopus citations

Abstract

We measure the cosmological matter density by observing the positions of baryon acoustic oscillations in the clustering of galaxies in the Sloan Digital Sky Survey (SDSS). We jointly analyze the main galaxies and LRGs in the SDSS DR5 sample, using over half a million galaxies in total. The oscillations are detected with 99.74% confidence (3.0 σ assuming Gaussianity) compared to a smooth power spectrum. When combined with the observed scale of the peaks within the CMB, we find a best-fit value of Ω_M = 0.256 _-0.029^+0.029 (68% confidence interval) for a flat A cosmology when marginalizing over the Hubble parameter and the baryon density. This value of the matter density is derived from the locations of the baryon oscillations in the galaxy power spectrum and in the CMB, and does not include any information from the overall shape of the power spectra. This is an extremely clean cosmological measurement, as the physics of the baryon acoustic oscillation production is well understood, and the positions of the oscillations are expected to be independent of systematics such as galaxy bias.

Original language	English (US)
Pages (from-to)	51-55
Number of pages	5
Journal	Astrophysical Journal
Volume	657
Issue number	1 I
DOIs	https://doi.org/10.1086/510772
State	Published - Mar 1 2007

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Cosmological parameters
Large-scale structure of universe

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10.1086/510772

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Percival, W. J., Nichol, R. C., Eisenstein, D. J., Weinberg, D. H., Fukugita, M., Pope, A. C., Schneider, D. P., Szalay, A. S., Vogeley, M. S., Zehavi, I., Bahcall, N. A., Brinkmann, J., Connolly, A. J., Loveday, J., & Meiksin, A. (2007). Measuring the matter density using baryon oscillations in the SDSS. Astrophysical Journal, 657(1 I), 51-55. https://doi.org/10.1086/510772

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title = "Measuring the matter density using baryon oscillations in the SDSS",

abstract = "We measure the cosmological matter density by observing the positions of baryon acoustic oscillations in the clustering of galaxies in the Sloan Digital Sky Survey (SDSS). We jointly analyze the main galaxies and LRGs in the SDSS DR5 sample, using over half a million galaxies in total. The oscillations are detected with 99.74% confidence (3.0 σ assuming Gaussianity) compared to a smooth power spectrum. When combined with the observed scale of the peaks within the CMB, we find a best-fit value of ΩM = 0.256 -0.029+0.029 (68% confidence interval) for a flat A cosmology when marginalizing over the Hubble parameter and the baryon density. This value of the matter density is derived from the locations of the baryon oscillations in the galaxy power spectrum and in the CMB, and does not include any information from the overall shape of the power spectra. This is an extremely clean cosmological measurement, as the physics of the baryon acoustic oscillation production is well understood, and the positions of the oscillations are expected to be independent of systematics such as galaxy bias.",

keywords = "Cosmological parameters, Large-scale structure of universe",

author = "Percival, {Will J.} and Nichol, {Robert C.} and Eisenstein, {Daniel J.} and Weinberg, {David H.} and Masataka Fukugita and Pope, {Adrian C.} and Schneider, {Donald P.} and Szalay, {Alex S.} and Vogeley, {Michael S.} and Idit Zehavi and Bahcall, {Neta A.} and Jon Brinkmann and Connolly, {Andrew J.} and Jon Loveday and Avery Meiksin",

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doi = "10.1086/510772",

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T1 - Measuring the matter density using baryon oscillations in the SDSS

AU - Percival, Will J.

AU - Nichol, Robert C.

AU - Eisenstein, Daniel J.

AU - Weinberg, David H.

AU - Fukugita, Masataka

AU - Pope, Adrian C.

AU - Schneider, Donald P.

AU - Szalay, Alex S.

AU - Vogeley, Michael S.

AU - Zehavi, Idit

AU - Bahcall, Neta A.

AU - Brinkmann, Jon

AU - Connolly, Andrew J.

AU - Loveday, Jon

AU - Meiksin, Avery

PY - 2007/3/1

Y1 - 2007/3/1

N2 - We measure the cosmological matter density by observing the positions of baryon acoustic oscillations in the clustering of galaxies in the Sloan Digital Sky Survey (SDSS). We jointly analyze the main galaxies and LRGs in the SDSS DR5 sample, using over half a million galaxies in total. The oscillations are detected with 99.74% confidence (3.0 σ assuming Gaussianity) compared to a smooth power spectrum. When combined with the observed scale of the peaks within the CMB, we find a best-fit value of ΩM = 0.256 -0.029+0.029 (68% confidence interval) for a flat A cosmology when marginalizing over the Hubble parameter and the baryon density. This value of the matter density is derived from the locations of the baryon oscillations in the galaxy power spectrum and in the CMB, and does not include any information from the overall shape of the power spectra. This is an extremely clean cosmological measurement, as the physics of the baryon acoustic oscillation production is well understood, and the positions of the oscillations are expected to be independent of systematics such as galaxy bias.

AB - We measure the cosmological matter density by observing the positions of baryon acoustic oscillations in the clustering of galaxies in the Sloan Digital Sky Survey (SDSS). We jointly analyze the main galaxies and LRGs in the SDSS DR5 sample, using over half a million galaxies in total. The oscillations are detected with 99.74% confidence (3.0 σ assuming Gaussianity) compared to a smooth power spectrum. When combined with the observed scale of the peaks within the CMB, we find a best-fit value of ΩM = 0.256 -0.029+0.029 (68% confidence interval) for a flat A cosmology when marginalizing over the Hubble parameter and the baryon density. This value of the matter density is derived from the locations of the baryon oscillations in the galaxy power spectrum and in the CMB, and does not include any information from the overall shape of the power spectra. This is an extremely clean cosmological measurement, as the physics of the baryon acoustic oscillation production is well understood, and the positions of the oscillations are expected to be independent of systematics such as galaxy bias.

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KW - Large-scale structure of universe

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ER -

Measuring the matter density using baryon oscillations in the SDSS

Abstract

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