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The XXL Survey

Arya FarahiDepartment of Physics and Michigan Center for Theoretical Physics, University of Michigan, Ann Arbor, MI 48109, USAValentina GuglielmoAix Marseille Univ., CNRS, CNES, LAM, Marseille, FranceAugust E. EvrardDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USABianca M. PoggiantiINAF–Osservatorio astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, ItalyChristophe AdamiAix Marseille Univ., CNRS, CNES, LAM, Marseille, FranceStefano EttoriINAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, ItalyFabio GastaldelloIstituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milan, ItalyPaul A. GilesSchool of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol, BS8 1TL, UKBen J. MaughanSchool of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol, BS8 1TL, UKDavid RapettiCenter for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Science, University of Colorado, Boulder, CO 80309, USAMauro SerenoDipartimento di Fisica e Astronomia, Università di Bologna, viale Berti Pichat 6/2, 40127 Bologna, ItalyBruno AltieriHerschel Science Centre, European Space Astronomy Centre, ESA, 28691 Villanueva de la Cañada, SpainIvan BaldryAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKMark BirkinshawSchool of Physics, HH Wills Physics Laboratory, Tyndall Avenue, Bristol, BS8 1TL, UKMicol BolzonellaINAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, ItalyAngela BongiornoINAF–Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monte Porzio Catone (Rome), ItalyMichael J. I. BrownSchool of Physics, Monash University, Clayton, Victoria 3800, AustraliaLucio 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, AustraliaAndrii ElyivDipartimento di Fisica e Astronomia, Università di Bologna, viale Berti Pichat 6/2, 40127 Bologna, ItalyBianca GarilliIstituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milan, ItalyLoïc GuennouAstrophysics and Cosmology Research Unit, University of KwaZulu-Natal, 4041 Durban, South AfricaAndrew HopkinsAustralian Astronomical Observatory, Box 915, North Ryde 1670, AustraliaAngela IovinoINAF, Osservatorio Astronomico di Brera, via Brera 28, 20159 Milano, ItalyElias KoulouridisAIM, CEA, CNRS, Univ. Paris-Saclay, Univ. Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, FranceJochen LiskeUniversität Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, GermanySophie MaurogordatoLaboratoire Lagrange, UMR 7293, Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, 06304 Nice, FranceMatthew OwersDepartment of Physics and Astronomy, Macquarie University, NSW 2109, Australia and Australian Astronomical Observatory PO Box 915, North Ryde NSW 1670, AustraliaFlorian PacaudArgelander Institut für Astronomie, Universität Bonn, Auf dem Huegel 71, 53121 Bonn, GermanyMarguerite PierreAIM, CEA, CNRS, Univ. Paris-Saclay, Univ. Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, FranceManolis PlionisAristotle University of Thessaloniki, Physics Department, 54124 Thessaloniki, GreeceTrevor PonmanSchool of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UKAaron RobothamInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, M468, 35 Stirling Highway, Crawley, WA 6009, AustraliaTatyana SadibekovaAIM, CEA, CNRS, Univ. Paris-Saclay, Univ. Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, FranceMarco ScodeggioIstituto di Astrofisica Spaziale e Fisica Cosmica Milano, via Bassini 15, 20133 Milan, ItalyRichard TuffsMax-Planck Institut füer Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, GermanyIvan ValtchanovHerschel Science Centre, European Space Astronomy Centre, ESA, 28691 Villanueva de la Cañada, Spain

Astronomy and Astrophysicsjournal2017en

ABI

Аннотация

Context. An X-ray survey with the XMM-Newton telescope, XMM-XXL, has identified hundreds of galaxy groups and clusters in two 25 deg 2 fields. Combining spectroscopic and X-ray observations in one field, we determine how the kinetic energy of galaxies scales with hot gas temperature and also, by imposing prior constraints on the relative energies of galaxies and dark matter, infer a power-law scaling of total mass with temperature. Aims. Our goals are: i) to determine parameters of the scaling between galaxy velocity dispersion and X-ray temperature, T 300 kpc , for the halos hosting XXL-selected clusters, and; ii) to infer the log-mean scaling of total halo mass with temperature, ⟨ln M 200 | T 300 kpc , z ⟩. Methods. We applied an ensemble velocity likelihood to a sample of >1500 spectroscopic redshifts within 132 spectroscopically confirmed clusters with redshifts z < 0.6 to model, ⟨ln σ gal | T 300 kpc , z ⟩, where σ gal is the velocity dispersion of XXL cluster member galaxies and T 300 kpc is a 300 kpc aperture temperature. To infer total halo mass we used a precise virial relation for massive halos calibrated by N -body simulations along with a single degree of freedom summarising galaxy velocity bias with respect to dark matter. Results. For the XXL-N cluster sample, we find σ gal ∝ T 300 kpc 0.63±0.05 , a slope significantly steeper than the self-similar expectation of 0.5. Assuming scale-independent galaxy velocity bias, we infer a mean logarithmic mass at a given X-ray temperature and redshift, 〈ln( E ( z ) M 200 /10 14 M ⊙ )|T 300 kpc, z 〉 = π T + α T ln ( T 300 kpc/ T p ) + β T ln ( E ( z )/ E ( z p )) using pivot values kT p = 2.2 keV and z p = 0.25, with normalization π T = 0.45 ± 0.24 and slope α T = 1.89 ± 0.15. We obtain only weak constraints on redshift evolution, β T = −1.29 ± 1.14. Conclusions. The ratio of specific energies in hot gas and galaxies is scale dependent. Ensemble spectroscopic analysis is a viable method to infer mean scaling relations, particularly for the numerous low mass systems with small numbers of spectroscopic members per system. Galaxy velocity bias is the dominant systematic uncertainty in dynamical mass estimates.

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Мавзулар

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

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DOI: 10.1051/0004-6361/201731321

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