gravitational lensing: strong; galaxies: groups: general; quasars: individual: HE 0435-1223
Abstract :
[en] Galaxies located in the environment or along the line of sight towards gravitational lenses can significantly affect lensing observables, and can lead to systematic errors on the measurement of H[SUB]0[/SUB] from the time-delay technique. We present the results of a systematic spectroscopic identification of the galaxies in the field of view of the lensed quasar HE 0435-1223 using the W. M. Keck, Gemini and ESO-Very Large telescopes. Our new catalogue triples the number of known galaxy redshifts in the direct vicinity of the lens, expanding to 102 the number of measured redshifts for galaxies separated by less than 3 arcmin from the lens. We complement our catalogue with literature data to gather redshifts up to 15 arcmin from the lens, and search for galaxy groups or clusters projected towards HE 0435-1223. We confirm that the lens is a member of a small group that includes at least 12 galaxies, and find 8 other group candidates near the line of sight of the lens. The flexion shift, namely the shift of lensed images produced by high-order perturbation of the lens potential, is calculated for each galaxy/group and used to identify which objects produce the largest perturbation of the lens potential. This analysis demonstrates that (i) at most three of the five brightest galaxies projected within 12 arcsec of the lens need to be explicitly used in the lens models, and (ii) the groups can be treated in the lens model as an external tidal field (shear) contribution.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Sluse, Dominique ; Université de Liège > Département d'astrophys., géophysique et océanographie (AGO) > Département d'astrophys., géophysique et océanographie (AGO)
Sonnenfeld, A.; Physics Department, University of California, Santa Barbara, CA 93106, USA ; Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA ; Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
Rumbaugh, N.; Department of Physics, University of California, Davis, CA 95616, USA
Rusu, C. E.; Department of Physics, University of California, Davis, CA 95616, USA
Fassnacht, C. D.; Department of Physics, University of California, Davis, CA 95616, USA
Treu, T.; Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA
Suyu, S. H.; Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, D-85740 Garching, Germany ; Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan ; Physik Department, Technische Universität München, James-Franck-Straße 1, D-85748 Garching, Germany
Wong, K. C.; Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan ; National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Auger, M. W.; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
Bonvin, V.; Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland
Collett, T.; Institute of Cosmology and Gravitation, University of Portsmouth, Burnaby Rd, Portsmouth PO1 3FX, UK
Courbin, F.; Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland
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