The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Pezzotta, Andrea; Torre, S. de la; Bel, J.; Granett, B. R.; Guzzo, L.; Peacock, J. A.; Garilli, B.; Scodeggio, M.; Bolzonella, M.; Abbas, U.; Adami, C.; Bottini, D.; Cappi, A.; Cucciati, O.; Davidzon, I.; Franzetti, P.; Fritz, A.; Iovino, A.; Krywult, J.; Brun, V. Le; Fèvre, O. Le; Maccagni, D.; Małek, K.; Marulli, F.; Polletta, M.; Pollo, A.; Tasca, L.; Tojeiro, Rita; Vergani, D.; Zanichelli, A.; Arnouts, S.; Branchini, E.; Coupon, J.; Lucia, G. De; Koda, Jun; Ilbert, O.; Mohammad, Faizan G.; Moutard, T.; Moscardini, L.

doi:10.1051/0004-6361/201630295

Cited by 172 publications

(179 citation statements)

References 71 publications

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“…The random sample we used to estimate the 2PCF of the VIPERS galaxies was constructed as in Marulli et al (2013), with 30 times more objects than galaxies. The weighting scheme we adopted has been described by Pezzotta et al (2017) and de la Torre et al (2017). The errors on the VIPERS 2PCF were estimated with the bootstrap method in the same way as for the mock catalogs.…”

Section: Clusteringmentioning

confidence: 99%

The stellar-to-halo mass relation over the past 12 Gyr

Girelli

Pozzetti²,

Bolzonella³

et al. 2020

A&A

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116

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Aims. Understanding the link between the galaxy properties and the dark matter halos they reside in and their coevolution is a powerful tool for constraining the processes related to galaxy formation. In particular, the stellar-to-halo mass relation (SHMR) and its evolution throughout the history of the Universe provides insights on galaxy formation models and allows us to assign galaxy masses to halos in N-body dark matter simulations. To address these questions, we determine the SHMR throughout the entire cosmic history from z ∼ 4 to the present. Methods. We used a statistical approach to link the observed galaxy stellar mass functions on the COSMOS field to dark matter halo mass functions up to z ∼ 4 from the ΛCDM DUSTGRAIN-pathfinder simulation, which is complete for M h > 10 12.5 M , and extended this to lower masses with a theoretical parameterization. We propose an empirical model to describe the evolution of the SHMR as a function of redshift (either in the presence or absence of a scatter in stellar mass at fixed halo mass), and compare the results with several literature works and semianalytic models of galaxy formation. We also tested the reliability of our results by comparing them to observed galaxy stellar mass functions and to clustering measurements. Results. We derive the SHMR from z = 0 to z = 4, and model its empirical evolution with redshift. We find that M * /M h is always lower than ∼ 0.05 and depends both on redshift and halo mass, with a bell shape that peaks at M h ∼ 10 12 M . Assuming a constant cosmic baryon fraction, we calculate the star-formation efficiency of galaxies and find that it is generally low; its peak increases with cosmic time from ∼ 30% at z ∼ 4 to ∼ 35% at z ∼ 0. Moreover, the star formation efficiency increases for increasing redshifts at masses higher than the peak of the SHMR, while the trend is reversed for masses lower than the peak. This indicates that massive galaxies (i.e., galaxies hosted at halo masses higher than the SHMR peak) formed with a higher efficiency at higher redshifts (i.e., downsizing effect) and vice versa for low-mass halos. We find a large scatter in results from semianalytic models, with a difference of up to a factor ∼ 8 compared to our results, and an opposite evolutionary trend at high halo masses. By comparing our results with those in the literature, we find that while at z ∼ 0 all results agree well (within a factor of ∼ 3), at z > 0 many differences emerge. This suggests that observational and theoretical work still needs to be done. Our results agree well (within ∼ 10%) with observed stellar mass functions (out to z = 4) and observed clustering of massive galaxies (M * > 10 11 M from z ∼ 0.5 to z ∼ 1.1) in the two-halo regime.

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Section: Clusteringmentioning

confidence: 99%

The stellar-to-halo mass relation over the past 12 Gyr

Girelli

Pozzetti²,

Bolzonella³

et al. 2020

A&A

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116

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“…In VIPERS, the first effect suppresses angular clustering below a scale of 5 arcsec, producing a scale-dependent damping of the observed clustering below 1 h −1 Mpc; the second is instead responsible for a nearly scale-independent reduction of the two-point correlation function amplitude above this scale. These effects and their correction are discussed in detail in the parallel paper by Pezzotta et al (2017). The method builds upon the original approach of de la Torre et al (2013, by up-weighting galaxies on the basis of the target sampling rate (TSR), namely…”

Section: Target Sampling Ratementioning

confidence: 99%

“…This is finally integrated around the position of each observed galaxy within a rectangular aperture with size 60 × 100 arcsec 2 to obtain the local values of δ s i and δ p i . It can be shown (Pezzotta et al 2017) that a rectangular aperture more efficiently accounts for the angular anisotropy in the distribution of targets within a quadrant introduced by the shadowing effect of the MOS slits.…”

Section: Target Sampling Ratementioning

confidence: 99%

“…An accurate knowledge of the typical redshift measurement uncertainty is clearly important for the scientific analysis of the VIPERS sample, in particular when modelling the observed shape of the power spectrum or the effect of Redshift Space Distortions (see the parallel papers by Rota et al 2017;de la Torre et al 2017;Pezzotta et al 2017;Wilson et al, in prep.). It is also important to probe the possible redshift dependence of this uncertainty.…”

Section: Updated Estimate Of Redshift Errorsmentioning

confidence: 99%

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The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Scodeggio

Guzzo

Garilli

et al. 2018

A&A

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We present the full public data release (PDR-2) of the VIMOS Public Extragalactic Redshift Survey (VIPERS), performed at the ESO VLT. We release redshifts, spectra, CFHTLS magnitudes and ancillary information (as masks and weights) for a complete sample of 86 775 galaxies (plus 4732 other objects, including stars and serendipitous galaxies); we also include their full photometrically-selected parent catalogue. The sample is magnitude limited to i AB ≤ 22.5, with an additional colour-colour pre-selection devised as to exclude galaxies at z < 0.5. This practically doubles the effective sampling of the VIMOS spectrograph over the range 0.5 < z < 1.2 (reaching 47% on average), yielding a final median local galaxy density close to 5 × 10 −3 h 3 Mpc −3 . The total area spanned by the final data set is 23.5 deg 2 , corresponding to 288 VIMOS fields with marginal overlaps, split over two regions within the CFHTLS-Wide W1 and W4 equatorial fields (at RA 2 and 22 h, respectively). Spectra were observed at a resolution R = 220, covering a wavelength range 5500−9500 Å. Data reduction and redshift measurements were performed through a fully automated pipeline; all redshift determinations were then visually validated and assigned a quality flag. Measurements with a quality flag ≥2 are shown to have a confidence level of 96% or larger and make up 88% of all measured galaxy redshifts (76 552 out of 86 775), constituting the VIPERS prime catalogue for statistical investigations. For this sample the rms redshift error, estimated using repeated measurements of about 3000 galaxies, is found to be σ z = 0.00054(1 + z). All data are available at http://vipers.inaf.it and on the ESO Archive.

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“…In particular, the so-called redshift-space distortions (RSD) in the tracer clustering function (Jackson 1972;Kaiser 1987;Hamilton 1998;Scoccimarro 2004) have been effectively exploited to test the gravity theory on cosmological scales, providing robust constraints on the linear growth rate of cosmic structure, using different techniques in both configuration space (e.g. Guzzo et al 2000;Reid et al 2012;Beutler et al 2012;Samushia et al 2012;Chuang & Wang 2013;Chuang et al 2013;de la Torre et al 2013;Samushia et al 2014;Howlett et al 2015;Okumura et al 2016;Chuang et al 2016;Pezzotta et al 2017;Mohammad et al 2018) and Fourier space (e.g. Tojeiro et al 2012;Blake et al 2012Blake et al , 2013Beutler et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Validating the methodology for constraining the linear growth rate from clustering anisotropies

García-Farieta

Marulli

Moscardini

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Redshift-space clustering distortions provide one of the most powerful probes to test the gravity theory on the largest cosmological scales. In this paper we perform a systematic validation study of the state-of-the-art statistical methods currently used to constrain the linear growth rate from redshift-space distortions in the galaxy two-point correlation function. The numerical pipelines are tested on mock halo catalogues extracted from large N-body simulations of the standard cosmological framework, in the redshift range 0.5 z 2. We consider both the monopole and quadrupole multipole moments of the redshift-space two-point correlation function, as well as the radial and transverse clustering wedges, in the comoving scale range 10 < r[h −1 Mpc] < 55. Moreover, we investigate the impact of redshift measurement errors, up to δz ∼ 0.5%, which introduce spurious clustering anisotropies. We quantify the systematic uncertainties on the growth rate and linear bias measurements due to the assumptions in the redshiftspace distortion model. Considering both the dispersion model and two widely-used models based on perturbation theory, that is the Scoccimarro (2004) model and the Taruya et al. (2010) model, we find that the linear growth rate is underestimated by about 5 − 10% at z < 1, while limiting the analysis at larger scales, r > 30 h −1 Mpc, the discrepancy is reduced below 5%. At higher redshifts, we find instead an overall good agreement between measurements and model predictions. The Taruya et al. (2010) model is the one which performs better, with growth rate uncertainties below about 3%. The effect of redshift errors is degenerate with the one of small-scale random motions, and can be marginalised over in the statistical analysis, not introducing any statistically significant bias in the linear growth constraints, especially at z ≥ 1.

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The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Cited by 172 publications

References 71 publications

The stellar-to-halo mass relation over the past 12 Gyr

The stellar-to-halo mass relation over the past 12 Gyr

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Validating the methodology for constraining the linear growth rate from clustering anisotropies

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