Treu, T.Agnello, A.Baumer, M.A.Birrer, S.Buckley-Geer, E.J.Courbin, F.Kim, Y.J.Lin, H.Marshall, P.J.Nord, B.Schechter, P.L.Sivakumar, P.R.Abramson, L.E.Anguita, T.Apostolovski, Y.Auger, M.W.Chan, J.Chen, G.Collett, T.E.Fassnacht, C.D.Hsueh, J.-W.Lemon, C.McMahon, R.G.Motta, V.Ostrovski, F.Rojas, K.Rusu, C.E.Williams, P.Frieman, J.Meylan, G.Suyu, S.H.Abbott, T.M.C.Abdalla, F.B.Allam, S.Annis, J.Avila, S.Banerji, M.Brooks, D.Rosell, A.C.Carrasco Kind, M.Carretero, J.Castander, F.J.D'Andrea, C.B.da Costa, L.N.De Vicente, J.Doel, P.Eifler, T.F.Flaugher, B.Fosalba, P.García-Bellido, J.Goldstein, D.A.Gruen, D.Gruendl, R.A.Gutierrez, G.Hartley, W.G.Hollowood, D.Honscheid, K.James, D.J.Kuehn, K.Kuropatkin, N.Lima, M.Maia, M.A.G.Martini, P.Menanteau, F.Miquel, R.Plazas, A.A.Romer, A.K.Sanchez, E.Scarpine, V.Schindler, R.Schubnell, M.Sevilla-Noarbe, I.Smith, M.Smith, R.C.Soares-Santos, M.Sobreira, F.Suchyta, E.Swanson, M.E.C.Tarle, G.Thomas, D.Tucker, D.L.Walker, A.R.2019-12-102019-12-102018-11Monthly Notices of the Royal Astronomical Society, 481(1), pp. 1041-1054.0035-8711DOI: 10.1093/MNRAS/STY2329http://repositorio.unab.cl/xmlui/handle/ria/11362Indexación: Scopus.The authors thank the referee for a constructive report that helped improved the paper. TT thanks Masamune Oguri for several useful conversations on finding lensed quasars and on SQLS. TT and VM acknowledge support by the David and Lucille Packard Foundation through a Packard Research Fellowship to TT. TT acknowledges support by the National Science Foundation through grants AST-1450141 and AST-1714953. CDF and GCFC acknowledge support from the National Science Foundation through grants AST-1312329 and AST-1715611. TA and YA acknowledge support by proyecto FONDECYT11130630 and by the Ministry for the Economy, Development, and Tourism’s Programa Inicativa Científica Milenio through grant IC 12009, awarded to The Millennium Institute of Astrophysics (MAS). FC, VB, and JC acknowledge support from the Swiss National Science Foundation. SHS thanks the Max Planck Society for support through the Max Planck Research Group.Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desen-volvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovac¸ão, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey.The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambi-entales y Tecnológicas-Madrid, the University of Chicago, Univer- sity College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Univer-sität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium.Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-88861, FPA2015-68048, SEV-2012-0234, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Frame-work Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. (Some of) The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership amongst the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tec-nologia, Inovac¸ãos e Comunicac¸ãoes (MCTIC) do Brasil, the US National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Based in part 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), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tec-nologia e Inovac¸ão (Brazil). Based in part on observations made with ESO Telescopes at the La Silla Paranal Observatory. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.The primary goals of the STRong lensing Insights into the Dark Energy Survey (STRIDES) collaboration are to measure the dark energy equation of state parameter and the free streaming length of dark matter. To this aim, STRIDES is discovering strongly lensed quasars in the imaging data of the Dark Energy Survey and following them up to measure time delays, high resolution imaging, and spectroscopy sufficient to construct accurate lens models. In this paper, we first present forecasts for STRIDES. Then, we describe the STRIDES classification scheme, and give an overview of the Fall 2016 follow-up campaign. We continue by detailing the results of two selection methods, the outlier selection technique and a morphological algorithm, and presenting lens models of a system that could possibly be a lensed quasar in an unusual configuration. We conclude with the summary statistics of the Fall 2016 campaign. Including searches presented in companion papers (Anguita et al.; Ostrovski et al.), STRIDES followed up 117 targets identifying 7 new strongly lensed systems, and 7 nearly identical quasars, which could be confirmed as lenses by the detection of the lens galaxy. 76 candidates were rejected and 27 remain otherwise inconclusive, for a success rate in the range of 6-35 per cent. This rate is comparable to that of previous searches like SDSS Quasar Lens Search even though the parent data set of STRIDES is purely photometric and our selection of candidates cannot rely on spectroscopic information. © 2018 The Author(s).enCataloguesGravitational lensing: strongMethods: statisticalArtículo