The 2dF Galaxy Redshift Survey: the power spectrum and the matter content of the Universe

Percival, Will J.; Baugh, C. M.; Bland-Hawthorn, Joss; Bridges, Terry J.; Cannon, R. D.; Cole, Shaun; Colless, Matthew; Collins, Chris; Couch, Warrick J.; Dalton, Gavin; Propris, Roberto De; Driver, Simon P.; Efstathiou, G.; Ellis, Richard S.; Frenk, Carlos S.; Glazebrook, Karl; Jackson, C. A.; Lahav, O.; Lewis, Ian; Lumsden, S. L.; Maddox, S.; Moody, Stephen J.; Norberg, Peder; Peacock, J. A.; Peterson, Bruce A.; Sutherland, William J.; Taylor, Keith

doi:10.1046/j.1365-8711.2001.04827.x

Cited by 742 publications

(440 citation statements)

References 24 publications

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“…Early results from the 2dF Galaxy Redshift Survey (2dFGRS) (Percival et al, 2001;Efstathiou et al, 2002;Percival et al, 2002) and the Abell/ACO cluster sample (Miller et al, 1999) gave hints of the acoustic feature in the power spectrum. However, the first convincing detections of BAO came in 2005 from the SDSS Data Release 3 (DR3) and final 2dFGRS samples Cole et al, 2005).…”

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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“…A sample of the size of the 2dFGRS survey allows large-scale structure statistics to be measured with very small random errors. An initial estimate of the convolved, redshift-space power spectrum of the 2dFGRS has been determined [36] based on a sample of 140 000 redshifts. On scales 0.02 < k < 0.15h Mpc −1 the data are robust and the shape of the power spectrum is not affected by redshift-space or nonlinear effects, though the amplitude is increased by redshift-space distortions.…”

Section: The 2df Galaxy Redshift Surveymentioning

confidence: 99%

“…On scales 0.02 < k < 0.15h Mpc −1 the data are robust and the shape of the power spectrum is not affected by redshift-space or nonlinear effects, though the amplitude is increased by redshift-space distortions. One should bear in mind that what is measured is the convolution of the true galaxy power spectrum with the window function of the survey [36,37],…”

Section: The 2df Galaxy Redshift Surveymentioning

confidence: 99%

“…It is seen from figure 3 that the error bars on the power spectrum data points are correlated, as discussed in [36], and this is taken into account throughout this paper by using the full covariance matrix of the data when computing likelihoods. For the 32 data points, the Ω ν = 0-model had χ 2 = 32.9, Ω ν = 0.01 gives χ 2 = 33.4,whereas the model with Ω ν = 0.05 provides a poor fit to the data with χ 2 = 92.2.…”

Section: The 2df Galaxy Redshift Surveymentioning

confidence: 99%

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Upper limits on neutrino masses from the 2dFGRS and WMAP: the role of priors

Elgarøy¹,

Lahav²

2003

J. Cosmol. Astropart. Phys.

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Abstract. Solar, atmospheric, and reactor neutrino experiments have confirmed neutrino oscillations, implying that neutrinos have non-zero mass, but without pinning down their absolute masses. While it is established that the effect of neutrinos on the evolution of cosmic structure is small, the upper limits derived from large-scale structure could help significantly to constrain the absolute scale of the neutrino masses. In a recent paper the 2dF Galaxy Redshift Survey (2dFGRS) team provided an upper limit m ν,tot < 2.2 eV , i.e. approximately 0.7 eV for each of the three neutrino flavours, or phrased in terms of their contribution to the matter density, Ω ν /Ω m < 0.16. Here we discuss this analysis in greater detail, considering issues of assumed 'priors' like the matter density Ω m and the bias of the galaxy distribution with respect to the dark matter distribution. As the suppression of the power spectrum depends on the ratio Ω ν /Ω m , we find that the out-of-fashion Mixed Dark Matter model, with Ω ν = 0.2, Ω m = 1 and no cosmological constant, fits both the 2dFGRS power spectrum and the CMB data reasonably well, but only for a Hubble constant H 0 < 50 km s −1 Mpc −1 . As a consequence, excluding low values of the Hubble constant, e.g. with the HST Key Project, is important in order to get a strong upper limit on the neutrino masses. We also comment on the improved limit obtained by the WMAP team, and point out that the main neutrino signature comes from the 2dFGRS and the Lyman α forest.PACS numbers: 95.35.+d, 14.60.Pq, 98.62.Py, 98.80.Es Upper limits on neutrino masses from the 2dFGRS and WMAP: the role of priors 2

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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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The 2dF Galaxy Redshift Survey: the power spectrum and the matter content of the Universe

Cited by 742 publications

References 24 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Upper limits on neutrino masses from the 2dFGRS and WMAP: the role of priors

Constraining the relative velocity effect using the Baryon Oscillation Spectroscopic Survey

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