The VIMOS Public Extragalactic Redshift Survey (VIPERS)

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

doi:10.1051/0004-6361/201630113

Cited by 47 publications

(80 citation statements)

References 123 publications

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“…Similar analysis of the properties of galaxies in large redshift surveys have shown this. For example, the VIMOS Public Extragalactic Redshift Survey (VIPERS) studied massive galaxies with intermediate redshifts and found a similar significant trend indicating that galaxies with higher masses are, on average, redder than the lower mass galaxies (Cucciati et al 2017).…”

Section: Color and Mass Versus Environmentmentioning

confidence: 95%

Large-scale Structure in CHILES Using DisPerSE

Luber

Gorkom

Hess

et al. 2019

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We demonstrate that the Discrete Persistent Source Extractor (DisPerSE) can be used with spectroscopic redshifts to define the cosmic web and its distance to galaxies in small area deepfields. Here we analyze the use of DisPerSE to identify structure in observational data. We apply DisPerSE to the distribution of galaxies in the COSMOS field and find the best parameters to identify filaments. We compile a catalog of 11500 spectroscopic redshifts from the Galaxy and Mass Assembly (GAMA) G10 data release. We analyze two-dimensional slices, extract filaments and calculate the distance for each galaxy to its nearest filament. We find that redder and more massive galaxies are closer to filaments. To study the growth of galaxies across cosmic time, and environment, we are carrying out an HI survey covering redshifts z = 0 -0.45, the COSMOS HI Large Extragalactic Survey (CHILES). In addition we present the predicted HI mass fraction as a function of distance to filaments for the spectroscopically known galaxies in CHILES. Lastly, we discuss the cold gas morphology of a few individual galaxies and their positions with respect to the cosmic web. The identification of the cosmic web, and the ability of CHILES to study the resolved neutral hydrogen morphologies and kinematics of galaxies, will allow future studies of the properties of neutral hydrogen in different cosmic web environments across the redshift range z = 0.1 -0.45.

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Section: Color and Mass Versus Environmentmentioning

confidence: 95%

Large-scale Structure in CHILES Using DisPerSE

Luber

Gorkom

Hess

et al. 2019

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“…Galaxy properties in clusters and groups have been studied thoroughly at different redshifts (e.g. Martínez & Muriel 2006;Martínez et al 2008;Wilman et al 2009;Kovač et al 2010;Presotto et al 2012;Cucciati et al 2017;Coenda et al 2018), however, the study of galaxies inhabiting the region between two groups/cluster (filament region) have not been as widely studied.…”

Section: Introductionmentioning

confidence: 99%

Filaments in VIPERS: galaxy quenching in the infalling regions of groups

Salerno

Martínez

Muriel

2019

Monthly Notices of the Royal Astronomical Society

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We study the quenching of galaxies in different environments and its evolution in the redshift range 0.43 z 0.89. For this purpose, we identify galaxies inhabiting in filaments, the isotropic infall region of groups, the field, and groups in the VIMOS Public Extragalactic Redshift Survey (VIPERS). We classify galaxies as quenched (passive), through their NUV − r vs. r − K colours. We study the fraction of quenched galaxies (F r ) as a function of stellar mass and environment at two redshift intervals. Our results confirm that stellar mass is the dominant factor determining galaxy quenching over the full redshift range explored. We find compelling evidence of evolution in the quenching of intermediate mass galaxies (9.3 log(M /M ) 10.5) for all environments. For this mass range, F r is largest for galaxies in groups, and smallest for galaxies in the field, while galaxies in filaments and in the isotropic infall regions appear to have intermediate values with the exception of the high redshift bin, where the latter show similar fraction of quenched galaxies as in the field. Galaxies in filaments are systematically more quenched than their counterparts infalling from other directions, in agreement to similar results found at low redshift. The least massive galaxies in our samples, do not show evidence of internal or environmental quenching.

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“…At higher redshift (z ∼ 1), samples from the VI-MOS Very Deep Survey (VVDS, Le Fèvre et al 2005Fèvre et al , 2013, the Deep Extragalactic Evolutionary Probe 2 (DEEP2, Davis et al 2003;Newman et al 2013), the zCOSMOS-Bright survey (Lilly et al 2007(Lilly et al , 2009, and the VIMOS Public Extragalactic Redshift Survey (VIPERS; Garilli et al 2014;Guzzo et al 2014) have been extensively studied to measure variations of f q . In such surveys, this quantity is typically proxied by the number of red galaxies relative to the total number of galaxies, as a function of redshift, stellar mass (or, somewhat equivalently, absolute magnitude), and environment (e.g., Cucciati et al 2006;Cooper et al 2007;Peng et al 2010;Kovač et al 2014;Cucciati et al 2017). However, the range of environments probed by each survey is typically limited to, at most, massive group environments, and the spectroscopic populations are typically skewed toward bluer galaxies.…”

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confidence: 99%

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

Lemaux

Tomczak

Lubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using ∼5000 spectroscopically-confirmed galaxies drawn from the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey we investigate the relationship between color and galaxy density for galaxy populations of various stellar masses in the redshift range 0.55 ≤ z ≤ 1.4. The fraction of galaxies with colors consistent with no ongoing star formation ( f q ) is broadly observed to increase with increasing stellar mass, increasing galaxy density, and decreasing redshift, with clear differences observed in f q between field and group/cluster galaxies at the highest redshifts studied. We use a semi-empirical model to generate a suite of mock group/cluster galaxies unaffected by environmentally-specific processes and compare these galaxies at fixed stellar mass and redshift to observed populations to constrain the efficiency of environmentally-driven quenching (Ψ convert ). High-density environments from 0.55 ≤ z ≤ 1.4 appear capable of efficiently quenching galaxies with log(M * /M ⊙ ) > 10.45. Lower stellar mass galaxies also appear efficiently quenched at the lowest redshifts studied here, but this quenching efficiency is seen to drop precipitously with increasing redshift. Quenching efficiencies, combined with simulated group/cluster accretion histories and results on the star formation rate-density relation from a companion ORELSE study, are used to constrain the average time from group/cluster accretion to quiescence and the elapsed time between accretion and the inception of the quenching event. These timescales were constrained to be t convert = 2.4 ± 0.3 and t delay = 1.3 ± 0.4 Gyr, respectively, for galaxies with log(M * /M ⊙ ) > 10.45 and t convert = 3.3 ± 0.3 and t delay = 2.2 ± 0.4 Gyr for lower stellar mass galaxies. These quenching efficiencies and associated timescales are used to rule out certain environmental mechanisms as being the primary processes responsible for transforming the star-formation properties of galaxies over this 4 Gyr window in cosmic time.

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The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Cited by 47 publications

References 123 publications

Large-scale Structure in CHILES Using DisPerSE

Large-scale Structure in CHILES Using DisPerSE

Filaments in VIPERS: galaxy quenching in the infalling regions of groups

Persistence of the colour–density relation and efficient environmental quenching to z ∼ 1.4

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