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Title:
Comparing Dark Energy Survey and HST-CLASH observations of the galaxy cluster RXC J2248.7-4431: implications for stellar mass versus dark matter
Authors:
Palmese, A.; Lahav, O.; Banerji, M.; Gruen, D.; Jouvel, S.; Melchior, P.; Aleksic, J.; Annis, J.; Diehl, H. T.; Hartley, W. G.; Jeltema, T.; Romer, A. K.; Rozo, E.; Rykoff, E. S.; Seitz, S.; Suchyta, E.; Zhang, Y.; Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Capozzi, D.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; Desai, S.; Dietrich, J. P.; Doel, P.; Estrada, J.; Evrard, A. E.; Flaugher, B.; Frieman, J.; Gerdes, D. W.; Goldstein, D. A.; Gruendl, R. A.; Gutierrez, G.; Honscheid, K.; James, D. J.; Kuehn, K.; Kuropatkin, N.; Li, T. S.; Lima, M.; Maia, M. A. G.; Marshall, J. L.; Miller, C. J.; Miquel, R.; Nord, B.; Ogando, R.; Plazas, A. A.; Roodman, A.; Sanchez, E.; Scarpine, V.; Sevilla-Noarbe, I.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; Tucker, D.; Vikram, V.
Affiliation:
AA(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK ), AB(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK), AC(Institute of Astronomy, University of Cambidge, Madingley Road, Cambridge CB3 0HA, UK), AD(SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA; Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA; University Observatory Munich, Scheinerstrasse 1, D-81679 Munich, Germany; Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, D-85748 Garching, Germany), AE(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK), AF(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), AG(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain), AH(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), AI(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), AJ(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK), AK(Department of Physics, University of California, Santa Cruz, CA 95064, USA), AL(Department of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton BN1 9QH, UK), AM(Department of Physics, University of Arizona, Tucson, AZ 85721, USA), AN(SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA; Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA), AO(University Observatory Munich, Scheinerstrasse 1, D-81679 Munich, Germany; Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, D-85748 Garching, Germany), AP(Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA), AQ(Physics Department, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USA), AR(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), AS(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK; Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown, 6140, South Africa), AT(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), AU(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK; CNRS, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France; Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France), AV(CNRS, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France; Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France), AW(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK), AX(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), AY(SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA; Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA), AZ(Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK), BA(Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil; Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil), BB(Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA; National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA), BC(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain; Institut de Ciències de l'Espai, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, E-08193 Bellaterra, Barcelona, Spain), BD(Institut de Ciències de l'Espai, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, E-08193 Bellaterra, Barcelona, Spain), BE(Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA), BF(Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK; School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK), BG(Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil; Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil), BH(Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany; Faculty of Physics, Ludwig-Maximilians University, Scheinerstr. 1, D-81679 Munich, Germany), BI(Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany; Faculty of Physics, Ludwig-Maximilians University, Scheinerstr. 1, D-81679 Munich, Germany), BJ(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK), BK(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), BL(Physics Department, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USA; Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA), BM(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), BN(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA; Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA), BO(Physics Department, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USA), BP(Department of Astronomy, University of California, Berkeley, 501 Campbell Hall, Berkeley, CA 94720, USA; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), BQ(Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA; National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA), BR(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), BS(Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA; Department of Physics, The Ohio State University, Columbus, OH 43210, USA), BT(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), BU(Australian Astronomical Observatory, North Ryde, NSW 2113, Australia), BV(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), BW(George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA), BX(Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil; Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, CEP 05314-970, São Paulo, SP, Brazil), BY(Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil; Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil), BZ(George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA), CA(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA; Physics Department, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USA), CB(Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain; Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain), CC(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), CD(Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil; Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil), CE(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA), CF(SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA; Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA), CG(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain), CH(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), CI(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain; Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA), CJ(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), CK(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), CL(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA; Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil), CM(National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA), CN(Physics Department, University of Michigan, 450 Church Street, Ann Arbor, MI 48109, USA), CO(Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK), CP(Fermi National Accelerator Laboratory, Batavia, IL 60510, USA), CQ(Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 463, Issue 2, p.1486-1499 (MNRAS Homepage)
Publication Date:
12/2016
Origin:
OUP
Astronomy Keywords:
galaxies: clusters: general, galaxies: evolution, galaxies: photometry, surveys
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stw2062
Bibliographic Code:
2016MNRAS.463.1486P

Abstract

We derive the stellar mass fraction in the galaxy cluster RXC J2248.7-4431 observed with the Dark Energy Survey (DES) during the Science Verification period. We compare the stellar mass results from DES (five filters) with those from the Hubble Space Telescope Cluster Lensing And Supernova Survey (CLASH; 17 filters). When the cluster spectroscopic redshift is assumed, we show that stellar masses from DES can be estimated within 25 per cent of CLASH values. We compute the stellar mass contribution coming from red and blue galaxies, and study the relation between stellar mass and the underlying dark matter using weak lensing studies with DES and CLASH. An analysis of the radial profiles of the DES total and stellar mass yields a stellar-to-total fraction of f* = (6.8 ± 1.7) × 10-3 within a radius of r200c ~= 2 Mpc. Our analysis also includes a comparison of photometric redshifts and star/galaxy separation efficiency for both data sets. We conclude that space-based small field imaging can be used to calibrate the galaxy properties in DES for the much wider field of view. The technique developed to derive the stellar mass fraction in galaxy clusters can be applied to the ˜100 000 clusters that will be observed within this survey and yield important information about galaxy evolution.
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