Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:1805.12151)
· On-line Data
· References in the article
· Citations to the Article (5) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The STRong lensing Insights into the Dark Energy Survey (STRIDES) 2016 follow-up campaign - II. New quasar lenses from double component fitting
Authors:
Anguita, T.; Schechter, P. L.; Kuropatkin, N.; Morgan, N. D.; Ostrovski, F.; Abramson, L. E.; Agnello, A.; Apostolovski, Y.; Fassnacht, C. D.; Hsueh, J. W.; Motta, V.; Rojas, K.; Rusu, C. E.; Treu, T.; Williams, P.; Auger, M.; Buckley-Geer, E.; Lin, H.; McMahon, R.; Abbott, T. M. C.; Allam, S.; Annis, J.; Bernstein, R. A.; Bertin, E.; Brooks, D.; Burke, D. L.; Carnero Rosell, A.; Carrasco-Kind, M.; Carretero, J.; Cunha, C. E.; D'Andrea, C. B.; De Vicente, J.; DePoy, D. L.; Desai, S.; Diehl, H. T.; Doel, P.; Flaugher, B.; García-Bellido, J.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Hartley, W. G.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Kuehn, K.; Lima, M.; Maia, M. A. G.; Miquel, R.; Plazas, A. A.; Sanchez, E.; Scarpine, V.; Smith, M.; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Tarle, G.; Walker, A. R.
Affiliation:
AA(Departamento de Ciencias Fisicas, Universidad Andres Bello Fernandez Concha 700, 7591538 Las Condes, Santiago, Chile; Millennium Institute of Astrophysics, Monseñor Nuncio Sotero Sanz 100, Oficina 104, 7500011 Providencia, Santiago, Chile 0000-0003-0930-5815), AB(MIT Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139, USA), AC(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), AD(Staples High School, Westport, CT 06880, USA), AE(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK; CAPES Foundation, Ministry of Education of Brazil, Brasilia, DF 70040-020, Brazil), AF(Department of Physics and Astronomy, PAB, 430 Portola Plaza, Box 951547, Los Angeles, CA 90095-1547, USA 0000-0002-8860-1032), AG(European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, DE, Germany), AH(Departamento de Ciencias Fisicas, Universidad Andres Bello Fernandez Concha 700, 7591538 Las Condes, Santiago, Chile), AI(Department of Physics, University of California Davis, 1 Shields Avenue, Davis, CA 95616, USA), AJ(Department of Physics, University of California Davis, 1 Shields Avenue, Davis, CA 95616, USA), AK(Instituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretaña 1111, Playa Ancha, Valparaíso 2360102, Chile), AL(Instituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretaña 1111, Playa Ancha, Valparaíso 2360102, Chile), AM(Subaru Telescope, National Astronomical Observatory of Japan, 650 N Aohoku Pl, Hilo, HI 96720, USA), AN(Department of Physics and Astronomy, PAB, 430 Portola Plaza, Box 951547, Los Angeles, CA 90095-1547, USA), AO(Department of Physics and Astronomy, PAB, 430 Portola Plaza, Box 951547, Los Angeles, CA 90095-1547, USA 0000-0002-4645-6578), AP(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK), AQ(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), AR(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), AS(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK), AT(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile), AU(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), AV(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), AW(Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St, Pasadena, CA 91101, USA), AX(CNRS, UMR 7095, Institut d'Astrophysique de Paris, F-75014 Paris, France; Institut d'Astrophysique de Paris, Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, F-75014 Paris, France), AY(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK), AZ(Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA; SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA), 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 at Urbana-Champaign, 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), BD(Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA), BE(Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA), BF(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain), BG(Department of Physics and Astronomy, George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA), BH(Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India), BI(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), BJ(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK), BK(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), BL(Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-28049 Madrid, Spain), BM(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA; Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA), BN(Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA; SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA 0000-0003-3270-7644), BO(Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USA; National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA), BP(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), BQ(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK; Department of Physics, ETH Zurich, Wolfgang-Pauli-Strasse 16, CH-8093 Zurich, Switzerland), BR(Santa Cruz Institute for Particle Physics, Santa Cruz, CA 95064, 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(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), BU(Australian Astronomical Observatory, North Ryde, NSW 2113, Australia), BV(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, São Paulo, SP 05314-970, Brazil), BW(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), BX(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), BY(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA), BZ(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain), CA(Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA), CB(School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK), CC(Physics Department, Brandeis University, 415 South Street, Waltham, MA 02453, USA 0000-0001-6082-8529), CD(Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil; Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, Campinas, SP 13083-859, Brazil), CE(Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA 0000-0002-7047-9358), CF(Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA), CG(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 480, Issue 4, p.5017-5028 (MNRAS Homepage)
Publication Date:
11/2018
Origin:
OUP
Astronomy Keywords:
gravitational lensing: strong, techniques: image processing, surveys, quasars: general
Abstract Copyright:
2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/sty2172
Bibliographic Code:
2018MNRAS.480.5017A

Abstract

We report upon the follow-up of 34 candidate lensed quasars found in the Dark Energy Survey using NTT EFOSC, Magellan-IMACS, KECK-ESI, and SOAR-SAMI. These candidates were selected by a combination of double component fitting, morphological assessment, and colour analysis. Most systems followed up are indeed composed of at least one quasar image and 13 with two or more quasar images: two lenses, four projected binaries, and seven nearly identical quasar pairs (NIQs). The two systems confirmed as genuine gravitationally lensed quasars are one quadruple at zs = 1.713 and one double at zs = 1.515. Lens modelling of these two systems reveals that both systems require very little contribution from the environment to reproduce the image configuration. Nevertheless, small flux anomalies can be observed in one of the images of the quad. Further observations of nine inconclusive systems (including seven NIQs) will allow to confirm (or not) their gravitational lens nature.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints