Second-order matter fluctuations via higher order galaxy correlators

Bel, J.; Marinoni, C.

doi:10.1111/j.1365-2966.2012.21257.x

Cited by 12 publications

(33 citation statements)

References 64 publications

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“…Since it has been shown (Fry and Gaztanaga 1993;Bel and Marinoni 2012) that the local non-linear bias model conserves the hierarchical properties of both, cumulants and correlators of matter, one can express such quantities for any biased tracers (haloes or galaxies) with respect to the linear and quadratic bias coefficients…”

Section: Non-linear Biasmentioning

confidence: 99%

“…This is done by the countin-cell estimators for the discrete S3,N and C12,N , which are described in Bel and Marinoni (2012) and used in this analysis. We correct these estimations from shot noise by assuming the local Poisson process approximation (Layser 1956).…”

Section: Non-linear Biasmentioning

confidence: 99%

“…Following an orginal idea of Szapudi (1998), Bel and Marinoni (2012) worked out the explicit expressions of the bias coefficients up to fourth order. Since in the present paper we focus on the quadratic biasing model we recall the expressions they obtained at second order.…”

Section: Non-linear Biasmentioning

confidence: 99%

“…σ8) and depends only on the shape of the linear power spectrum. This has been shown by several authors using the the skewness S3 (Gaztanaga 1994;Gaztanaga and Frieman 1994), the bispectrum (Fry 1994;Gaztanaga and Frieman 1994;Scoccimarro 1998;Feldman et al 2001; Verde et al 2002), the three-point correlation function Q, Gaztañaga and Scoccimarro 2005;Pan and Szapudi 2005;Marín 2011;McBride et al 2011;Marín et al 2013), and the two-point cumulants C12 (Bernardeau 1996;Szapudi 1998;Gaztañaga et al 2002;Bel and Marinoni 2012).…”

Section: Introductionmentioning

confidence: 99%

“…Recently, Bel and Marinoni (2012) demonstrated that it is possible to use these higher-order correlations to constrain bias and fundamental properties of the underlying matter field using a combination of S3 and C12, which they call τ = 3C12 − 2S3.…”

Section: Introductionmentioning

confidence: 99%

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Measuring the growth of matter fluctuations with third-order galaxy correlations

Hoffmann

Bel

Gaztañaga

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Measurements of the linear growth factor D at different redshifts z are key to distinguish among cosmological models. One can estimate the derivative dD(z)/d ln(1 + z) from redshift space measurements of the 3D anisotropic galaxy two-point correlation ξ(z), but the degeneracy of its transverse (or projected) component with galaxy bias, introduces large errors in the growth measurement.Here we present a comparison between two methods which break this degeneracy by combining second-and third-order statistics. One uses the shape of the reduced three-point correlation and the other a combination of third-order one-and two-point cumulants. These methods use the fact that, for Gaussian initial conditions and scales larger than 20 h −1 Mpc, the reduced third-order matter correlations are independent of redshift (and therefore of the growth factor) while the third-order galaxy correlations depend on b. We use matter and halo catalogs from the MICE-GC simulation to test how well we can recover b(z) and therefore D(z) with these methods in 3D real space. We also present a new approach, which enables us to measure D directly from the redshift evolution of second-and third-order galaxy correlations without the need of modelling matter correlations.For haloes with masses lower than 10 14 h −1 M ⊙ , we find 10% deviations between the different estimates of D, which are comparable to current observational errors. At higher masses we find larger differences that can probably be attributed to the breakdown of the bias model and non-Poissonian shot noise.

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Section: Non-linear Biasmentioning

confidence: 99%

Section: Non-linear Biasmentioning

confidence: 99%

Section: Non-linear Biasmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Measuring the growth of matter fluctuations with third-order galaxy correlations

Hoffmann

Bel

Gaztañaga

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Large-scale galaxy bias

2018

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Determination of the abundance of cosmic matter via the cell count moments of the galaxy distribution

Bel¹,

Marinoni²

2014

A&A

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We demonstrate that accurate and precise information about the matter content of the universe can be retrieved via a simple cell count analysis of the 3D spatial distribution of galaxies. A new clustering statistic, the galaxy clustering ratio η, is the key to this process. This is defined as the ratio between one-and two-point second-order moments of the smoothed galaxy density distribution. The distinguishing feature of this statistic is its universality: on large cosmic scales both galaxies (in redshift space) and mass (in real space) display the same η amplitude. This quantity, in addition, does not evolve as a function of redshift. As a consequence, the η statistic provides insight into characteristic parameters of the real-space power spectrum of mass density fluctuations without the need to specify the galaxy biasing function, neither a model for galaxy redshift distortions, nor the growing mode of density ripples. We demonstrate the method with the luminous red galaxy (LRG) sample extracted from the spectroscopic Sloan Digital Sky Survey (SDSS) data release 7 (DR7) catalogue. Taking weak (flat) priors of the curvature of the universe (Ω k ) and of the constant value of the dark energy equation of state (w), and strong (Gaussian) priors of the physical baryon density Ω b h 2 , of the Hubble constant H 0 , and of the spectral index of primordial density perturbations n s , we estimate the abundance of matter with a relative error of 8% (Ω m = 0.283 ± 0.023). We expect that this approach will be instrumental in searching for evidence of new physics beyond the standard model of cosmology and in planning future redshift surveys, such as BigBOSS or EUCLID.

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Second-order matter fluctuations via higher order galaxy correlators

Abstract: International audienc

Cited by 12 publications

References 64 publications

Measuring the growth of matter fluctuations with third-order galaxy correlations

Measuring the growth of matter fluctuations with third-order galaxy correlations

Large-scale galaxy bias

Determination of the abundance of cosmic matter via the cell count moments of the galaxy distribution

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