Logo
ScienceStack
Table of Contents
Fetching ...
Sign In

The VIMOS Public Extragalactic Redshift Survey (VIPERS). Galaxy clustering and redshift-space distortions at z=0.8 in the first data release

S. de la Torre, L. Guzzo, J. A. Peacock, E. Branchini, A. Iovino, B. R. Granett, U. Abbas, C. Adami, S. Arnouts, J. Bel, M. Bolzonella, D. Bottini, A. Cappi, J. Coupon, O. Cucciati, I. Davidzon, G. De Lucia, A. Fritz, P. Franzetti, M. Fumana, B. Garilli, O. Ilbert, J. Krywult, V. Le Brun, O. Le Fevre, D. Maccagni, K. Malek, F. Marulli, H. J. McCracken, L. Moscardini, L. Paioro, W. J. Percival, M. Polletta, A. Pollo, H. Schlagenhaufer, M. Scodeggio, L. A. M. Tasca, R. Tojeiro, D. Vergani, A. Zanichelli, A. Burden, C. Di Porto, A. Marchetti, C. Marinoni, Y. Mellier, P. Monaco, R. C. Nichol, S. Phleps, M. Wolk, G. Zamorani

TL;DR

The paper analyzes real- and redshift-space galaxy clustering in the VIPERS first data release to measure the growth rate of structure at $z\approx0.8$. It combines detailed survey characterisation, mock-based validation, and Halo Occupation Distribution modelling to extract unbiased clustering signals and robust $f\sigma_8$ constraints, using a multipole approach to redshift-space distortions. The key result is $f\sigma_8(z=0.8)=0.47\pm0.08$, consistent with General Relativity in a $\Lambda$CDM framework and with Planck-based mass power spectra, demonstrating VIPERS' capability to test gravity at intermediate redshift. The work establishes a foundation for future, tighter constraints from the full VIPERS dataset and provides realistic mocks for interpreting high-z galaxy clustering.

Abstract

We present in this paper 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 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: fσ_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.

The VIMOS Public Extragalactic Redshift Survey (VIPERS). Galaxy clustering and redshift-space distortions at z=0.8 in the first data release

TL;DR

The paper analyzes real- and redshift-space galaxy clustering in the VIPERS first data release to measure the growth rate of structure at . It combines detailed survey characterisation, mock-based validation, and Halo Occupation Distribution modelling to extract unbiased clustering signals and robust constraints, using a multipole approach to redshift-space distortions. The key result is , consistent with General Relativity in a CDM framework and with Planck-based mass power spectra, demonstrating VIPERS' capability to test gravity at intermediate redshift. The work establishes a foundation for future, tighter constraints from the full VIPERS dataset and provides realistic mocks for interpreting high-z galaxy clustering.

Abstract

We present in this paper 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 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: fσ_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.

Paper Structure

This paper contains 22 sections, 34 equations, 19 figures.

Table of Contents

  1. Introduction
  2. Data
  3. Angular completeness
  4. Slit assignment and footprint
  5. Small-scale incompleteness
  6. Large-scale incompleteneness
  7. Clustering estimation
  8. Tests of the clustering estimation
  9. Simulation data
  10. Effects of systematics on the correlation function
  11. Effects related to the radial selection function
  12. Effects related to the angular selection function
  13. Impact of possible residual zero-point uncertainties in the photometry
  14. Real-space clustering
  15. Redshift-space distortions
  16. ...and 7 more sections

Figures (19)

  • Figure 1: Redshift distribution of the combined W1+W4 galaxy sample when including only reliable redshifts (filled histogram) and that corrected for the full survey completeness (empty histogram) scaled down by 40% (see text). The curve shows the best-fitting template redshift distribution given by Eq. \ref{['eq:nz']} applied to the uncorrected observed distribution.
  • Figure 2: Illustration of the slit assignment in pointing W1P082. The slits are shown in red and associated rectangles represent the typical dispersion of the spectra. All objects meeting the survey selection criteria (potential spectroscopic targets) are represented by black circles.
  • Figure 3: Completeness fraction of angular galaxy pairs due to the slit-spectroscopy strategy in the W1 and W4 fields for all galaxies at $0.5<z<1.0$. This has been obtained from the parent and spectroscopic sample angular correlation function.
  • Figure 4: Variations of the target success rate (${TSR}$) with quadrants. The ${TSR}$ quantifies our ability of obtaining spectra from the potential targets meeting the survey selection in the parent photometric sample. The quadrants filled in black correspond to failed observations where no spectroscopy has been taken.
  • Figure 5: Variations of the spectroscopic success rate (${SSR}$) with quadrants. The ${SSR}$ quantifies our ability of determining galaxy redshifts from observed spectra. The quadrants filled in black correspond to failed observations where no spectroscopy has been taken.
  • ...and 14 more figures