Power-spectrum analysis of three-dimensional redshift surveys

Feldman, Hume A.; Kaiser, Nick; Peacock, J. A.

doi:10.1086/174036

Cited by 920 publications

(1,212 citation statements)

References 22 publications

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“…Tegmark et al (2006) analyzed the DR4 LRG and main galaxy samples with a quadratic estimator for the power spectrum and redshiftspace distortion. Hütsi (2006) analyzed the monopole of the power spectrum of the LRG data set with the Feldman et al (1994) (FKP) method. Percival et al (2007) applied the FKP method to the combined DR5 LRG and main galaxy samples, along with the 2dFGRS sample, to measure the acoustic scale at two different redshifts (z = 0.20 and 0.35).…”

Section: The Current State Of Playmentioning

confidence: 99%

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%

Observational probes of cosmic acceleration

et al. 2013

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“…Here we will summarise these measurements but refer to the above mentioned references for more details. The first three non-zero power spectrum multipoles can be calculated as (Feldman, Kaiser & Peacock 1994) …”

Section: Boss Measurements and Uncertaintiesmentioning

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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“…The fact that we have to estimate the mean density of galaxies from the sample itself means that the k = 0 mode is artificially set to zero, equivalent to subtracting a single Dirac delta function from the centre of the un-convolved power. The equivalent correction for correlation function estimates is commonly know as the "Integral constraint" The comoving power spectrum, as measured from the Data Release 9 (DR9) BOSS data, using the Feldman et al (1994) technique is shown in Fig. 3.…”

Section: Measuring the Power Spectrummentioning

confidence: 99%