The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Davidzon, I.; Cucciati, O.; Bolzonella, M.; Lucia, G. De; Zamorani, G.; Arnouts, S.; Moutard, T.; Ilbert, O.; Garilli, B.; Scodeggio, M.; Guzzo, L.; Abbas, U.; Adami, C.; Bel, J.; Bottini, D.; Branchini, E.; Cappi, A.; Coupon, J.; Torre, S. de la; Porto, C. Di; Fritz, A.; Franzetti, P.; Fumana, M.; Granett, B. R.; Guennou, L.; Iovino, A.; Krywult, J.; Brun, V. Le; Fèvre, O. Le; Maccagni, D.; Małek, K.; Marulli, F.; McCracken, H. J.; Mellier, Y.; Moscardini, L.; Polletta, M.; Pollo, A.; Tasca, L.; Tojeiro, Rita; Vergani, D.; Zanichelli, A.

doi:10.1051/0004-6361/201527129

Cited by 87 publications

(146 citation statements)

References 145 publications

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“…Our results are in very good agreement with other works performed with the VIPERS sample, that is, with the study of the galaxy stellar mass function per environment (Davidzon et al 2016, based on a previous VIPERS release) and the study of galaxy properties with relation to distance from filaments describing the VIPERS large-scale structure (Malavasi et al 2017, based on the same VIPERS release as this work, but with a different definition of environment). It is difficult to perform a quantitative comparison of our results with similar works in the literature because of the different environment definitions (or the same definition, but different tracer samples) and the different galaxy-type classification.…”

Section: Discussionsupporting

confidence: 91%

“…We remark that this cosmology is outdated, with for instance σ 8 based on the first-year results of the Wilkinson Microwave Anisotropy Probe (WMAP1, Spergel et al 2003) being larger than more recent measurements such as WMAP7 (Komatsu et al 2011) and WMAP9 (Hinshaw et al 2013), where they find σ 8 to be of the order of 0.8. Davidzon et al (2016) showed that the density distribution is slightly different in two simulations based on the cosmologies from WMAP1 and WMAP3, but WMAP3 had a very low σ 8 (σ 8 = 0.7). Given that σ 8 (and also other cosmological parameters) from WMAP7 and WMAP9 is closer to that of WMAP1, we do not expect a large difference between simulations based on WMAP1 or WMAP7 and WMAP9, as also shown in Guo et al (2013).…”

Section: Mock Samplesmentioning

confidence: 95%

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The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Cucciati

Davidzon

Bolzonella

et al. 2017

A&A

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We use the final data of the VIMOS Public Extragalactic Redshift Survey (VIPERS) to investigate the effect of the environment on the evolution of galaxies between z = 0.5 and z = 0.9. We characterise local environment in terms of the density contrast smoothed over a cylindrical kernel, the scale of which is defined by the distance to the fifth nearest neighbour. This is performed by using a volume-limited sub-sample of galaxies complete up to z = 0.9, but allows us to attach a value of local density to all galaxies in the full VIPERS magnitude-limited sample to i < 22.5. We use this information to estimate how the distribution of galaxy stellar masses depends on environment. More massive galaxies tend to reside in higher-density environments over the full redshift range explored. Defining star-forming and passive galaxies through their (NUV−r) vs. (r − K) colours, we then quantify the fraction of star-forming over passive galaxies, f ap , as a function of environment at fixed stellar mass. f ap is higher in low-density regions for galaxies with masses ranging from log(M/M ) = 10.38 (the lowest value explored) to at least log(M/M ) ∼ 11.3, although with decreasing significance going from lower to higher masses. This is the first time that environmental effects on high-mass galaxies are clearly detected at redshifts as high as z ∼ 0.9. We compared these results to VIPERS-like galaxy mock catalogues based on a widely used galaxy formation model. The model correctly reproduces f ap in low-density environments, but underpredicts it at high densities. The discrepancy is particularly strong for the lowest-mass bins. We find that this discrepancy is driven by an excess of low-mass passive satellite galaxies in the model. In high-density regions, we obtain a better (although not perfect) agreement of the model f ap with observations by studying the accretion history of these model galaxies (that is, the times when they become satellites), by assuming either that a non-negligible fraction of satellites is destroyed, or that their quenching timescale is longer than ∼2 Gyr.

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Section: Discussionsupporting

confidence: 91%

Section: Mock Samplesmentioning

confidence: 95%

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Cucciati

Davidzon

Bolzonella

et al. 2017

A&A

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“…The photometric multi-wavelength coverage combines improved ugriz-bands photometry based on the T0007 release of the CFHTLS 1 and K s-band observations from the VIPERS Multi-Lambda Survey (VIPERS-MLS 2 , Moutard et al 2016a) or, when available, from the VISTA Deep Extragalactic Observations (VIDEO; Jarvis et al 2013) survey (more details in Davidzon et al 2013Davidzon et al , 2016Moutard et al 2016b). …”

Section: Physical and Structural Parameters Of Vipers Galaxiesmentioning

confidence: 99%

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Gargiulo

Bolzonella

Scodeggio

et al. 2017

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We use the final data from the VIPERS redshift survey to extract an unparalleled sample of more than 2000 massive M ≥1011 M ⊙ passive galaxies (MPGs) at redshift 0.5 ≤ z ≤ 1.0, based on their NUVrK colours. This enables us to investigate how the population of these objects was built up over cosmic time. We find that the evolution of the number density depends on the galaxy mean surface stellar mass density, Σ. In particular, dense (Σ ≥ 2000 M ⊙ pc −2 ) MPGs show a constant comoving number density over this redshift range, whilst this increases by a factor ∼ 4 for the least dense objects, defined as having Σ < 1000 M ⊙ pc −2 . We estimate stellar ages for the MPG population both fitting the Spectral Energy Distribution (SED) and through the D4000 n index, obtaining results in good agreement. Our findings are consistent with passive ageing of the stellar content of dense MPGs. We show that at any redshift the less dense MPGs are younger than dense ones and that their stellar populations evolve at a slower rate than predicted by passive evolution. This points to a scenario in which the overall population of MPGs was built up over the cosmic time by continuous addition of less dense galaxies: on top of an initial population of dense objects that passively evolves, new, larger, and younger MPGs continuously join the population at later epochs. Finally, we demonstrate that the observed increase in the number density of MPGs is totally accounted for by the observed decrease in the number density of correspondingly massive star forming galaxies (i.e. all the nonpassive M ≥10 11 M ⊙ objects). Such systems observed at z ≃ 1 in VIPERS, therefore, represent the most plausible progenitors of the subsequent emerging class of larger MPGs.

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“…In contrast, when considering local density estimates, the GSMF seems to depend on environment, being steeper in less dense environments (e.g. Baldry et al 2006;Bolzonella et al 2010;Vulcani et al 2012;Davidzon et al 2016;Etherington et al 2016).…”

Section: Introductionmentioning

confidence: 99%

“…Balogh et al 2001;Yang et al 2009;Calvi et al 2013;Vulcani et al 2011Vulcani et al , 2012Vulcani et al , 2013Vulcani et al , 2014bDavidzon et al 2016;Muzzin et al 2013;van der Burg et al 2015;Nantais et al 2016). Its shape has been described by a Schechter or a double Schechter function (Schechter 1976).…”

Section: Introductionmentioning

confidence: 99%

The XXL Survey

Guglielmo

Poggianti

Vulcani

et al. 2018

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Context. The fraction of galaxies bound in groups in the nearby Universe is high (50% at z ∼ 0). Systematic studies of galaxy properties in groups are important in order to improve our understanding of the evolution of galaxies and of the physical phenomena occurring within this environment. Aims. We have built a complete spectrophotometric sample of galaxies within X-ray detected, optically spectroscopically confirmed groups and clusters (G&C), covering a wide range of halo masses at z ≤ 0.6. Methods. In the context of the XXL survey, we analyse a sample of 164 G&C in the XXL-North region (XXL-N), at z ≤ 0.6, with a wide range of virial masses (1.24 × 10 13 ≤ M 500 (M ) ≤ 6.63 × 10 14 ) and X-ray luminosities (2.27 × 10 41 ≤ L XXL 500 (erg s −1 ) ≤ 2.15 × 10 44 ). The G&C are X-ray selected and spectroscopically confirmed. We describe the membership assignment and the spectroscopic completeness analysis, and compute stellar masses. As a first scientific exploitation of the sample, we study the dependence of the galaxy stellar mass function (GSMF) on global environment.Results. We present a spectrophotometric characterisation of the G&C and their galaxies. The final sample contains 132 G&C, 22111 field galaxies and 2225 G&C galaxies with r-band magnitude < 20. Of the G&C, 95% have at least three spectroscopic members, and 70% at least ten. The shape of the GSMF seems not to depend on environment (field versus G&C) or X-ray luminosity ( used as a proxy for the virial mass of the system). These results are confirmed by the study of the correlation between mean stellar mass of G&C members and L XXL 500 .We release the spectrophotometric catalogue of galaxies with all the quantities computed in this work. Conclusions. As a first homogeneous census of galaxies within X-ray spectroscopically confirmed G&C at these redshifts, this sample will allow environmental studies of the evolution of galaxy properties.

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The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Cited by 87 publications

References 145 publications

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

The XXL Survey

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