Journal Article 1 Mention
Detection of the Baryon Acoustic Peak in the Large‐Scale Correlation Function of SDSS Luminous Red Galaxies
Daniel J. Eisenstein2005
Idit ZehaviDavid W. Hogg
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4,620 citations · Astronomy and Astrophysics
Open AccessCharacterization of tungsten carbide synthesized by controlled template method

TLDR

A huge galaxy map revealed a faint, predictable spacing pattern left by sound waves in the young universe. This pattern supports the standard picture of cosmic growth and helps measure how the universe has expanded.

Summary

1 Study Aim

The authors aim to detect baryon acoustic oscillations (BAO), a spacing pattern created by sound waves in the early universe, within nearby galaxy clustering. They test whether the pattern matches standard cosmological theory and can measure cosmic distances. The study also examines matter density, dark energy, and spatial curvature. The research asks whether an ancient spacing pattern can confirm how the universe grew and expanded.

2 Study Design

The study analyzes 46,748 luminous red galaxies from the Sloan Digital Sky Survey (SDSS), a large map of galaxies, covering 0.72 cubic gigaparsecs and redshifts from 0.16 to 0.47. The authors calculate the two-point correlation function, which measures how often galaxies occur at given separations. They use the Landy–Szalay estimator, a method for correcting survey geometry and uneven sampling. They compare the measurements with theoretical models, including corrections for nonlinear growth, galaxy bias, and redshift distortions. They estimate uncertainties from 1,278 simulated survey catalogs and ten jackknife tests. The researchers compared a very large galaxy sample with predictions and simulations.

3 Findings

The research detects a clear correlation peak near 100 h⁻¹ megaparsecs, matching the predicted BAO feature. The authors report a 3.4-sigma preference for a baryonic model over a pure cold-dark-matter model without the peak. They measure the distance to redshift 0.35 with 5% accuracy and its ratio to the cosmic microwave background (CMB), leftover light from the early universe, with 4% accuracy. The study finds Ωₘh² = 0.130 ± 0.011, agreeing with CMB estimates. The authors infer Ωₘ = 0.273 ± 0.025, with additional dependence on dark-energy behavior and curvature. Assuming a cosmological constant, they find spatial curvature Ωₖ = −0.010 ± 0.009. They argue that the peak supports linear growth, meaning large structures grew gradually under gravity, and provides geometric evidence for dark energy. They recommend larger surveys at redshifts above 0.5 for stronger expansion-history measurements. The galaxy pattern matches theory, supports dark energy, and gives a reliable way to measure cosmic expansion.

Abstract

We present the large-scale correlation function measured from a spectroscopic sample of 46,748 luminous red galaxies from the Sloan Digital Sky Survey. The survey region covers 0.72 h -3 Gpc 3 over 3816 deg 2 and 0.16 < z < 0.47, making it the best sample yet for the study of large-scale structure. We find a well-detected peak in the correlation function at 100 h -1 Mpc separation that is an excellent match to the predicted shape and location of the imprint of the recombination-epoch acoustic oscillations on the low-redshift clustering of matter. This detection demonstrates the linear growth of structure by gravitational instability between z ≈ 1000 and the present and confirms a firm prediction of the standard cosmological theory. The acoustic peak provides a standard ruler by which we can measure the ratio of the distances to z = 0.35 and z = 1089 to 4% fractional accuracy and the absolute distance to z = 0.35 to 5% accuracy. From the overall shape of the correlation function, we measure the matter density Ω m h 2 to 8% and find agreement with the value from cosmic microwave background (CMB) anisotropies. Independent of the constraints provided by the CMB acoustic scale, we find Ω m = 0.273 ± 0.025 + 0.123(1 + w 0 ) + 0.137Ω K . Including the CMB acoustic scale, we find that the spatial curvature is Ω K = -0.010 ± 0.009 if the dark energy is a cosmological constant. More generally, our results provide a measurement of cosmological distance, and hence an argument for dark energy, based on a geometric method with the same simple physics as the microwave background anisotropies. The standard cosmological model convincingly passes these new and robust tests of its fundamental properties.

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