TY - JOUR
T1 - Mass profile and dynamical status of the z ∼ 0.8 galaxy cluster LCDCS 0504
AU - Guennou, L.
AU - Biviano, A.
AU - Adami, C.
AU - Limousin, M.
AU - Lima Neto, G. B.
AU - Mamon, G. A.
AU - Ulmer, M. P.
AU - Gavazzi, R.
AU - Cypriano, E. S.
AU - Durret, F.
AU - Clowe, D.
AU - Lebrun, V.
AU - Allam, S.
AU - Basa, S.
AU - Benoist, C.
AU - Cappi, A.
AU - Halliday, C.
AU - Ilbert, O.
AU - Johnston, D.
AU - Jullo, E.
AU - Just, D.
AU - Kubo, J. M.
AU - Márquez, I.
AU - Marshall, P.
AU - Martinet, N.
AU - Maurogordato, S.
AU - Mazure, A.
AU - Murphy, K. J.
AU - Plana, H.
AU - Rostagni, F.
AU - Russeil, D.
AU - Schirmer, M.
AU - Schrabback, T.
AU - Slezak, E.
AU - Tucker, D.
AU - Zaritsky, D.
AU - Ziegler, B.
N1 - Funding Information:
We wish to express our sincere condolences and grief to the family of Alain Mazure, who unexpectedly passed away during the preparation of this paper. We wish to thank the anonymous referee for her/his suggestions. Based on XMM-Newton archive data and on data retrieved from the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Also based on observations made with the FORS2 multi-object spectrograph mounted on the Antu VLT telescope at ESO-Paranal Observatory (programme 175.A-0706(B)). Also based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnología e Inovación Productiva (Argentina). Finally, this research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. Also based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. Also based on visiting astronomer observations, at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, under contract with the National Science Foundation. This work has been carried out thanks to the support of the Labex OCEVU (ANR-11-LABX-0060) and the A*MIDEX (ANR-11-IDEX-0001-02) funded by the “Investments for the Future” French government program managed by the French National Research Agency (ANR). M.L. acknowledges the Centre National de la Recherche Scientifique (CNRS) for its support. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work has been conducted using facilities offered by CeSAM (Centre de donnéeS Astrophysique de Marseille – http://www.lam.fr/cesam/ ). F.D. acknowledges long-term support from CNES and CAPES/COFECUB program 711/11. A.B. acknowledges the hospitality of the Inst. d’Astroph. de Paris and of the Obs. de la Côte d’Azur. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. G.B.L.N. and ESC acknowledge the support of the Brazilian funding agencies FAPESP and CNPq. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). I.M. acknowledges financial support from the Spanish grant AYA2010-15169 and from the Junta de Andalucia through TIC-114 and the Excellence Project P08-TIC-03531.
PY - 2014/6
Y1 - 2014/6
N2 - Context. Constraints on the mass distribution in high-redshift clusters of galaxies are currently not very strong. Aims. We aim to constrain the mass profile, M(r), and dynamical status of the z ≃ 0.8 LCDCS 0504 cluster of galaxies that is characterized by prominent giant gravitational arcs near its center. Methods. Our analysis is based on deep X-ray, optical, and infrared imaging as well as optical spectroscopy, collected with various instruments, which we complemented with archival data. We modeled the mass distribution of the cluster with three different mass density profiles, whose parameters were constrained by the strong lensing features of the inner cluster region, by the X-ray emission from the intracluster medium, and by the kinematics of 71 cluster members. Results. We obtain consistent M(r) determinations from three methods based on kinematics (dispersion-kurtosis, caustics, and MAMPOSSt), out to the cluster virial radius, ≃ 1.3 Mpc and beyond. The mass profile inferred by the strong lensing analysis in the central cluster region is slightly higher than, but still consistent with, the kinematics estimate. On the other hand, the X-ray based M(r) is significantly lower than the kinematics and strong lensing estimates. Theoretical predictions from ΛCDM cosmology for the concentration-mass relation agree with our observational results, when taking into account the uncertainties in the observational and theoretical estimates. There appears to be a central deficit in the intracluster gas mass fraction compared with nearby clusters. Conclusions. Despite the relaxed appearance of this cluster, the determinations of its mass profile by different probes show substantial discrepancies, the origin of which remains to be determined. The extension of a dynamical analysis similar to that of other clusters of the DAFT/FADA survey with multiwavelength data of sufficient quality will allow shedding light on the possible systematics that affect the determination of mass profiles of high-z clusters, which is possibly related to our incomplete understanding of intracluster baryon physics.
AB - Context. Constraints on the mass distribution in high-redshift clusters of galaxies are currently not very strong. Aims. We aim to constrain the mass profile, M(r), and dynamical status of the z ≃ 0.8 LCDCS 0504 cluster of galaxies that is characterized by prominent giant gravitational arcs near its center. Methods. Our analysis is based on deep X-ray, optical, and infrared imaging as well as optical spectroscopy, collected with various instruments, which we complemented with archival data. We modeled the mass distribution of the cluster with three different mass density profiles, whose parameters were constrained by the strong lensing features of the inner cluster region, by the X-ray emission from the intracluster medium, and by the kinematics of 71 cluster members. Results. We obtain consistent M(r) determinations from three methods based on kinematics (dispersion-kurtosis, caustics, and MAMPOSSt), out to the cluster virial radius, ≃ 1.3 Mpc and beyond. The mass profile inferred by the strong lensing analysis in the central cluster region is slightly higher than, but still consistent with, the kinematics estimate. On the other hand, the X-ray based M(r) is significantly lower than the kinematics and strong lensing estimates. Theoretical predictions from ΛCDM cosmology for the concentration-mass relation agree with our observational results, when taking into account the uncertainties in the observational and theoretical estimates. There appears to be a central deficit in the intracluster gas mass fraction compared with nearby clusters. Conclusions. Despite the relaxed appearance of this cluster, the determinations of its mass profile by different probes show substantial discrepancies, the origin of which remains to be determined. The extension of a dynamical analysis similar to that of other clusters of the DAFT/FADA survey with multiwavelength data of sufficient quality will allow shedding light on the possible systematics that affect the determination of mass profiles of high-z clusters, which is possibly related to our incomplete understanding of intracluster baryon physics.
KW - Galaxies: clusters: general
KW - Galaxies: kinematics and dynamics
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U2 - 10.1051/0004-6361/201322447
DO - 10.1051/0004-6361/201322447
M3 - Article
AN - SCOPUS:84903287568
SN - 0004-6361
VL - 566
JO - Astronomy and astrophysics
JF - Astronomy and astrophysics
M1 - A149
ER -