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dc.contributor.authorCucciati, O.
dc.contributor.authorDavidzon, I.
dc.contributor.authorBolzonella, M.
dc.contributor.authorGranett, B. R.
dc.contributor.authorDe Lucia, G.
dc.contributor.authorBranchini, E.
dc.contributor.authorZamorani, G.
dc.contributor.authorIovino, A.
dc.contributor.authorGarilli, B.
dc.contributor.authorGuzzo, L.
dc.contributor.authorScodeggio, M.
dc.contributor.authorde la Torre, S.
dc.contributor.authorAbbas, U.
dc.contributor.authorAdami, C.
dc.contributor.authorArnouts, S.
dc.contributor.authorBottini, D.
dc.contributor.authorCappi, A.
dc.contributor.authorFranzetti, P.
dc.contributor.authorFritz, A.
dc.contributor.authorKrywult, J.
dc.contributor.authorLe Brun, V.
dc.contributor.authorLe Fèvre, O.
dc.contributor.authorMaccagni, D.
dc.contributor.authorMałek, K.
dc.contributor.authorMarulli, F.
dc.contributor.authorMoutard, T.
dc.contributor.authorPolletta, M.
dc.contributor.authorPollo, A.
dc.contributor.authorTasca, L. A. M.
dc.contributor.authorTojeiro, R.
dc.contributor.authorVergani, D.
dc.contributor.authorZanichelli, A.
dc.contributor.authorBel, J.
dc.contributor.authorBlaizot, J.
dc.contributor.authorCoupon, J.
dc.contributor.authorHawken, A.
dc.contributor.authorIlbert, O.
dc.contributor.authorMoscardini, L.
dc.contributor.authorPeacock, J. A.
dc.contributor.authorGargiulo, A.
dc.date.accessioned2017-06-21T12:30:12Z
dc.date.available2017-06-21T12:30:12Z
dc.date.issued2017-06-01
dc.identifier.citationCucciati , O , Davidzon , I , Bolzonella , M , Granett , B R , De Lucia , G , Branchini , E , Zamorani , G , Iovino , A , Garilli , B , Guzzo , L , Scodeggio , M , de la Torre , S , Abbas , U , Adami , C , Arnouts , S , Bottini , D , Cappi , A , Franzetti , P , Fritz , A , Krywult , J , Le Brun , V , Le Fèvre , O , Maccagni , D , Małek , K , Marulli , F , Moutard , T , Polletta , M , Pollo , A , Tasca , L A M , Tojeiro , R , Vergani , D , Zanichelli , A , Bel , J , Blaizot , J , Coupon , J , Hawken , A , Ilbert , O , Moscardini , L , Peacock , J A & Gargiulo , A 2017 , ' The VIMOS Public Extragalactic Redshift Survey (VIPERS) : The decline of cosmic star formation: quenching, mass, and environment connections ' , Astronomy & Astrophysics , vol. 602 , A15 . https://doi.org/10.1051/0004-6361/201630113en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 250289431
dc.identifier.otherPURE UUID: 258543c5-11c5-468b-b05f-00e4603ab929
dc.identifier.otherScopus: 85019742168
dc.identifier.otherWOS: 000404648300074
dc.identifier.urihttps://hdl.handle.net/10023/11043
dc.descriptionRT acknowledges financial support from the European Research Council through grant n. 202686.en
dc.description.abstractWe 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, fap, as a function of environment at fixed stellar mass. fap 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 fap 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 fap 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.
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2017. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/201630113en
dc.subjectCosmology: observationsen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: high-redshiften
dc.subjectGalaxies: statisticsen
dc.subjectLarge-scale structure of Universeen
dc.subjectQB Astronomyen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.titleThe VIMOS Public Extragalactic Redshift Survey (VIPERS) : The decline of cosmic star formation: quenching, mass, and environment connectionsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201630113
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1611.07049en


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