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

Seo, Hee-Jong; Eisenstein, Daniel J.

doi:10.1086/379122

Cited by 771 publications

(1,142 citation statements)

References 98 publications

(109 reference statements)

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“…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). Compelling detections in 2005 intensified these plans (Cole et al, 2005;Eisenstein et al, 2005), with several observational surveys proposed and numerous theoretical investigations.…”

Section: The Current State Of Playmentioning

confidence: 99%

“…However, any realistic bias relation must be at least somewhat non-linear, which alters the relative weighting of overdense and underdense regions and should shift the acoustic scale at second order. Early work attempted to measure this shift in simulations (Seo and Eisenstein, 2003;Angulo et al, 2008), but the volume of the simulations was insufficient to get a conclusive detection of the effect. More recently, explored galaxy bias as the ratio of the second-order to first-order bias term, finding shifts of a few tenths of a percent for reasonable bias cases.…”

Section: Non-linear Evolution and Galaxy Clustering Biasmentioning

confidence: 99%

“…This has been done with Fisher matrix analyses (Seo and Eisenstein, 2003;Seo and Eisenstein, 2007) or with Monte Carlo approaches (Blake and Glazebrook, 2003;Glazebrook and Blake, 2005;Blake et al, 2006). Several analyses have focused on the anisotropy of the power spectrum in order to measure H(z) and D A (z) separately.…”

Section: Statistical Errorsmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: The Current State Of Playmentioning

confidence: 99%

Section: Non-linear Evolution and Galaxy Clustering Biasmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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“…Measurements of the baryon acoustic scale in the distribution of galaxies have established themselves as one of the most powerful tools for precision cosmology (Eisenstein, Hu & Tegmark 1998;Percival et al 2001;Blake & Glazebrook 2003;Hu & Haiman 2003;Seo & Eisenstein 2003;Linder 2003;Eisenstein et al 2005;Cole et al 2005;Beutler et al 2011;Blake et al 2011;Alam et al 2016). With the most recent measurements of the BAO scale in the BOSS survey we have now reached 1% precision in two redshift bins (Alam et al 2016;Beutler et al 2016a;Ross et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Constraining the relative velocity effect using the Baryon Oscillation Spectroscopic Survey

Beutler

Seljak

Vlah

2017

Monthly Notices of the Royal Astronomical Society

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We analyse the power spectrum of the Baryon Oscillation Spectroscopic Survey (BOSS), Data Release 12 (DR12) to constrain the relative velocity effect, which represents a potential systematic for measurements of the Baryon Acoustic Oscillation (BAO) scale. The relative velocity effect is sourced by the different evolution of baryon and cold dark matter perturbations before decoupling. Our power spectrum model includes all 1-loop redshift-space terms corresponding to v bc parameterised by the bias parameter b v 2 . We also include the linear terms proportional to the relative density, δ bc , and relative velocity dispersion, θ bc , which we parameterise with the bias parameters b bc δ and b bc θ . Our data does not support a detection of the relative velocity effect in any of these parameters. Combining the low and high redshift bins of BOSS, we find limits of b v 2 = 0.012 ± 0.015 (±0.031), b bc δ = −1.0 ± 2.5 (±6.2) and b bc θ = −114 ± 55 (±175) with 68% (95%) confidence levels. These constraints restrict the potential systematic shift in D A (z), H(z) and f σ 8 , due to the relative velocity, to 1%, 0.8% and 2%, respectively. Given the current uncertainties on the BAO measurements of BOSS these shifts correspond to 0.53σ, 0.5σ and 0.22σ for D A (z), H(z) and f σ 8 , respectively.

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“…Considering impacts of early dark energy to the matter power spectrum, we estimated possible changes to the Baryon Acoustic Peak measurement of Eisenstein et al We found that these changes are roughly a factor of two smaller than the experimental errors on the A-parameter measured by Eisenstein et al Put another way, allowing for an dark energy contribution at last scattering slightly increases the systematic uncertainty in A. Whilst current BAO measurements are a useful probe for cosmological parameters of the late universe [16,17], they turn out to be less stringent for the early universe.…”

Section: Discussionmentioning

confidence: 90%