Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since<i>z</i>  ~  1.2

Coupon, J.; Kilbinger, M.; McCracken, H. J.; Ilbert, O.; Arnouts, S.; Mellier, Y.; Abbas, U.; Torre, S. de la; Goranova, Y.; Hudelot, P.; Kneib, Jean-Paul; Fèvre, O. Le

doi:10.1051/0004-6361/201117625

Cited by 172 publications

(290 citation statements)

References 93 publications

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“…The VIPERS sample allows us to constraint these parameters with an unprecedented accuracy over the redshift range 0.5 < z < 1.1. Our results are consistent with previous measurements, in particular with the DEEP2 (Zheng et al 2007) and CFHTLS (Coupon et al 2012) analyses. Our HOD analysis is aimed at modelling the global clustering properties in VIPERS, but we refer the reader to Marulli et al (2013) and de la Torre et al (in prep.…”

Section: Real-space Clusteringsupporting

confidence: 93%

“…The parameter M 0 is generally poorly constrained and we decided in this analysis to fix M 0 = M min (see also White et al 2011;de la Torre & Guzzo 2012). In the halo model formalism, the galaxy power spectrum or two-point correlation function can be written as the sum of two The VIPERS results are compared to the pervious measurements performed in the DEEP2 (Zheng et al 2007), BOSS , and CFHTLS (Coupon et al 2012) surveys.…”

Section: Real-space Clusteringmentioning

confidence: 99%

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The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Torre¹,

Guzzo²,

Peacock³

et al. 2013

A&A

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288

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We present the general real-and redshift-space clustering properties of galaxies as measured in the first data release of the VIPERS survey. VIPERS is a large redshift survey designed to probe in detail the distant Universe and its large-scale structure at 0.5 < z < 1.2. We describe in this analysis the global properties of the sample and discuss the survey completeness and associated corrections. This sample allows us to measure the galaxy clustering with an unprecedented accuracy at these redshifts. From the redshift-space distortions observed in the galaxy clustering pattern we provide a first measurement of the growth rate of structure at z = 0.8: f σ 8 = 0.47 ± 0.08. This is completely consistent with the predictions of standard cosmological models based on Einstein gravity, although this measurement alone does not discriminate between different gravity models.

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Section: Real-space Clusteringsupporting

confidence: 93%

Section: Real-space Clusteringmentioning

confidence: 99%

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Torre¹,

Guzzo²,

Peacock³

et al. 2013

A&A

Self Cite

288

117

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“…However, through the Bayesian framework, the joint analysis becomes natural. We may further add constraints given by the density reconstructions in the gaps by the ZADE algorithm (Cucciati et al 2014) or photometric redshift samples from the full CFHTLS Wide fields (Granett et al 2012;Coupon et al 2012). Sheer measurements in these fields can provide additional constraints on the underlying matter density providing a powerful probe in combination (Coupon et al 2015).…”

Section: Discussionmentioning

confidence: 99%

The VIMOS Public Extragalactic Redshift Survey

Granett

Branchini

Guzzo

et al. 2015

A&A

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Aims. Using the VIMOS Public Extragalactic Redshift Survey (VIPERS) we aim to jointly estimate the key parameters that describe the galaxy density field and its spatial correlations in redshift space. Methods. We use the Bayesian formalism to jointly reconstruct the redshift-space galaxy density field, power spectrum, galaxy bias and galaxy luminosity function given the observations and survey selection function. The high-dimensional posterior distribution is explored using the Wiener filter within a Gibbs sampler. We validate the analysis using simulated catalogues and apply it to VIPERS data taking into consideration the inhomogeneous selection function. Results. We present joint constraints on the anisotropic power spectrum, and the bias and number density of red and blue galaxy classes in luminosity and redshift bins as well as the measurement covariances of these quantities. We find that the inferred galaxy bias and number density parameters are strongly correlated although they are only weakly correlated with the galaxy power spectrum. The power spectrum and redshiftspace distortion parameters are in agreement with previous VIPERS results with the value of the growth rate f σ 8 = 0.38 with 18% uncertainty at redshift 0.7.

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“…(15). The bias of a particular population is usually measured from the analysis of the correlation function and is well established in that the bias increases with luminosity and stellar mass (see Zehavi et al 2011;Coupon et al 2012;Marulli et al 2013;Arnalte-Mur et al 2013, and references therein). The estimation of the bias is a laborious task, so we decided to use the redshift and the number density n of the population under study instead of the bias to characterise the cosmic variance.…”

Section: Theoretical Backgroundmentioning

confidence: 99%

The ALHAMBRA survey: An empirical estimation of the cosmic variance for merger fraction studies based on close pairs

López-Sanjuan¹,

Cenarro²,

Hernández-Monteagudo³

et al. 2014

A&A

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Aims. Our goal is to estimate empirically the cosmic variance that affects merger fraction studies based on close pairs for the first time. Methods. We compute the merger fraction from photometric redshift close pairs with 10 h −1 kpc ≤ r p ≤ 50 h −1 kpc and Δv ≤ 500 km s −1 and measure it in the 48 sub-fields of the ALHAMBRA survey. We study the distribution of the measured merger fractions that follow a log-normal function and estimate the cosmic variance σ v as the intrinsic dispersion of the observed distribution. We develop a maximum likelihood estimator to measure a reliable σ v and avoid the dispersion due to the observational errors (including the Poisson shot noise term). Results. The cosmic variance σ v of the merger fraction depends mainly on (i) the number density of the populations under study for both the principal (n 1 ) and the companion (n 2 ) galaxy in the close pair and (ii) the probed cosmic volume V c . We do not find a significant dependence on either the search radius used to define close companions, the redshift, or the physical selection (luminosity or stellar mass) of the samples. Conclusions. We have estimated the cosmic variance that affects the measurement of the merger fraction by close pairs from observations. We provide a parametrisation of the cosmic variance with n 1 , n 2 , and V c , σ v ∝ n −0.54(n 2 /n 1 ) −0.37 . Thanks to this prescription, future merger fraction studies based on close pairs could properly account for the cosmic variance on their results.

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Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Cited by 172 publications

References 93 publications

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

The VIMOS Public Extragalactic Redshift Survey

The ALHAMBRA survey: An empirical estimation of the cosmic variance for merger fraction studies based on close pairs

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