Maqola

The XXL Survey

V. GuglielmoDepartment of Physics and Astronomy, University of Padova, Vicolo Osservatorio 3, 35122 Padova, ItalyBianca M. PoggiantiINAF–Osservatorio astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, ItalyBenedetta VulcaniSchool of Physics, University of Melbourne, VIC 3010, AustraliaC. AdamiAix Marseille Univ., CNRS, CNES, LAM, Marseille FranceF. GastaldelloIstituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milan, ItalyS. EttoriINAF, Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, ItalyS. FotoupoulouDepartment of Astronomy, University of Geneva, ch. d'Ecogia 16, 1290 Versoix, SwitzerlandE. KoulouridisIRFU, CEA, Universit Paris-Saclay, Universit Paris Diderot, AIM,M. E. Ramos-CejaArgelander Institut fr Astronomie, Universitt Bonn, Auf dem Huegel 71, 53121 Bonn, GermanyPaul GilesSchool of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol, BS8 1TL, UKSean McGeeSchool of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UKB. AltieriHerschel Science Centre, European Space Astronomy Centre, ESA, 28691 Villanueva de la Caada, SpainI. K. BaldryAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool, L3 5RF, UKM. BirkinshawSchool of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol, BS8 1TL, UKM. BolzonellaINAF, Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, ItalyA. BongiornoOsservatorio Astronomico di Roma (INAF), via Frascati 33, 00078 Monte Porzio Catone (Rome), ItalyM. J. I. BrownSchool of Physics and Astronomy, Monash University, Clayton, Victoria 3800, AustraliaL. ChiappettiIstituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milan, ItalySimon P. DriverInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, M468, 35 Stirling Highway, Crawley, WA 6009, AustraliaA. ElyivDipartimento di Fisica e Astronomia, Alma Mater Studiorum -Universit di Bologna, viale Berti Pichat 6/2, 40127 Bologna, ItalyA. E. EvrardDepartment of Physics and Michigan Center for Theoretical Physics, University of Michigan, Ann Arbor, MI Us-48109, USAB. GarilliIstituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milan, ItalyMeiert W. GrootesESA/ESTEC, Noordwijk 2201 AZ, The NetherlandsL. GuennouAstrophysics and Cosmology Research Unit, University of KwaZulu-Natal, ZA-4041 Durban, South AfricaAndrew HopkinsAustralian Astronomical Observatory, PO Box 915, North Ryde 1670, AustraliaC. HorellouChalmers University of Technology Onsala Space Observatory, 439 92 Onsala, SwedenA. IovinoINAF-Osservatorio Astronomico di Brera, via Brera, 28, 20159 Milano, ItalyC. LidmanAustralian Astronomical Observatory, PO Box 915, North Ryde 1670, AustraliaJ. LiskeUniversitt Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, GermanyS. MaurogordatoLaboratoire Lagrange, UMR 7293, Universit de Nice Sophia Antipolis, CNRS, Observatoire de la Cte d'Azur, 06304 Nice, FranceM. S. OwersDepartment of Physics and Astronomy, Macquarie University, NSW 2109; Australian Astronomical Observatory PO Box 915, North Ryde NSW 1670, AustraliaF. PacaudArgelander Institut fr Astronomie, Universitt Bonn, Auf dem Huegel 71, 53121 Bonn, GermanyS. PaltaniDepartment of Astronomy, University of Geneva, ch. d'Ecogia 16, 1290 Versoix, SwitzerlandM. PierreIRFU, CEA, Universit Paris-Saclay, Universit Paris Diderot, AIM,M. PlionisInstituto Nacional de Astrofísica Óptica y Electrónica, AP 51 y 216, 72000 Puebla, MexicoT. J. PonmanSchool of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UKA. S. G. RobothamInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, M468, 35 Stirling Highway, Crawley, WA 6009, AustraliaT. SadibekovaIRFU, CEA, Université Paris-Saclay, Université Paris Diderot, AIM, Sorbonne Paris Cité, CEA, CNRS, 91191 Gif-sur-Yvette, FranceM. ScodeggioIstituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milan, ItalyM. SerenoDipartimento di Fisica e Astronomia, Alma Mater Studiorum -Universit di Bologna, viale Berti Pichat 6/2, 40127 Bologna, ItalyV. SmolčićDepartment of Physics, University of Zagreb, Bijenicka cesta 32, 10000 Zagreb, CroatiaR. TuffsESA/ESTEC, Noordwijk 2201 AZ, The NetherlandsI. ValtchanovHerschel Science Centre, European Space Astronomy Centre, ESA, 28691 Villanueva de la Caada, SpainC. VignaliDipartimento di Fisica e Astronomia, Alma Mater Studiorum -Universit di Bologna, viale Berti Pichat 6/2, 40127 Bologna, ItalyJ. P. WillisDepartment of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Victoria, BC, Canada

Astronomy and Astrophysicsjournal2017en

ABI

Annotatsiya

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, scal ( M ⊙ ) ≤ 6.63 × 10 14 ) and X-ray luminosities ((2.27 × 10 41 ≤ L 500,scal XXL (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, 22 111 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 500,scal XXL . 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.

Mavzular

Galaxies: Formation, Evolution, Phenomena Astronomy and Astrophysical Research Scientific Research and Discoveries

Identifikatorlar

DOI: 10.1051/0004-6361/201730709

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