Probing Dark Energy with Baryonic Acoustic Oscillations from Future Large Galaxy Redshift Surveys

By H. Seo, Daniel J. Eisenstein. 2003

688 citations recorded by the source corpus.

We show that the measurement of the baryonic acoustic oscillations in large high-redshift galaxy surveys offers a precision route to the measurement of dark energy. The cosmic microwave background provides the scale of the oscillations as a standard ruler that can be measured in the clustering of galaxies, thereby yielding the Hubble parameter and angular diameter distance as a function of redshift. This, in turn, enables one to probe dark energy. We use a Fisher matrix formalism to study the statistical errors for redshift surveys up to z = 3 and report errors on cosmography while marginalizing over a large number of cosmological parameters, including a time-dependent equation of state. With redshift surveys combined with cosmic microwave background satellite data, we achieve errors of 0.037 on ΩX, 0.10 on w(z = 0.8), and 0.28 on dw(z)/dz for the cosmological constant model. Models with less negative w(z) permit tighter constraints. We test and discuss the dependence of performance on redshift, survey conditions, and the fiducial model. We find results that are competitive with the performance of future Type Ia supernova surveys. We conclude that redshift surveys offer a promising independent route to the measurement of dark energy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a54fd625f9a4315677dfd84ccdbeda973fbf4dbb

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Citations in the corpus

Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “, is reduced to two dimensions by symmetry [1075].”
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Improved Forecasts for the Baryon Acoustic Oscillations and Cosmological Distance Scale (2007, methodology): “We show that the full, 12 dimensional (for one redshift bin) Fisher matrix in Seo & Eisenstein (2003) can be contracted to a two-dimensional (2D) or even one-dimensional (1D) covariance matrix of DA and H with physically motivated approximations.”
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Observational probes of cosmic acceleration (2012, methodology): “In 2003, several papers appeared discussing the acoustic scale as a standard ruler for the measurement of dark energy in higher redshift galaxy surveys (Eisenstein, 2002; Blake and Glazebrook, 2003; Hu and Haiman, 2003; Linder, 2003; Seo and Eisenstein, 2003).”
Holographic dark energy (2016, methodology): “Different from the SNIa that provides a “standard candle” for astronomical observations, the BAO provides a “standard ruler”, which is the radius of the sound horizon at the drag epoch, to explore the expansion history of the universe [92, 93, 94].”
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A 2 per cent distance to $z$=0.35 by reconstructing baryon acoustic oscillations - I. Methods and application to the Sloan Digital Sky Survey (2012, background): “…a considerable literature quantitatively exploring these effects using both perturbative techniques and simulations (Meiksin, White & Peacock 1999; Seo & Eisenstein 2003; Jeong & Komatsu 2006; Eisenstein et al. 2007b; Guzik, Bernstein & Smith 2007; Huff et al. 2007; Angulo et al. 2008; Crocce &…”
THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: QUASAR TARGET SELECTION FOR DATA RELEASE NINE (2011, background): “The scale of these peaks, which is set by the sound horizon at last scattering (Eisenstein & Hu 1998; Blake & Glazebrook 2003; Seo & Eisenstein 2003), can be used as a cosmological standard ruler.”
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Cosmic distance-duality as a probe of exotic physics and acceleration (2003, background): “ciprocity relation should allow us to distinguish between the two possibilities. Further, large galaxy surveys such as the proposed KAOSexperiment, will provideaccurateestimates of dA(z) out to z = 3 [25], allowing us to test deviations from the reciprocity relation at the level of a few percent, im”
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THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III (2012, methodology): “A long-standing prediction of cosmological models (Sakharov 1966; Peebles & Yu 1970; Sunyaev & Zel’dovich 1970), BAO rose to prominence in recent years as a tool to measure the expansion history of the universe (Eisenstein et al. 1998; Blake & Glazebrook 2003; Seo & Eisenstein 2003).”
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