Agnello, A.Lin, H.Kuropatkin, N.Buckley-Geer, E.Anguita, T.Schechter, P.L.Morishita, T.Motta, V.Rojas, K.Treu, T.Amara, A.Auger, M.W.Courbin, F.Fassnacht, C.D.Frieman, J.More, A.Marshall, P.J.McMahon, R.G.Meylan, G.Suyu, S.H.Glazebrook, K.Morgan, N.Nord, B.Abbott, T.M.C.Abdalla, F.B.Annis, J.Bechtol, K.Benoit-Lévy, K.Bertin, E.Bernstein, R.A.Brooks, D.Burke, D.L.Carnero Rosell, A.Carretero, J.Cunha, C.E.D'Andrea, C.B.da Costa, L.N.Desai, S.Drlica-Wagner, A.Eifler, T.F.Flaugher, B.García-Bellido, J.Gaztanaga, E.Gerdes, D.W.Gruen, D.Gruendl, R.A.Gschwend, J.Gutierrez, G.Honscheid, K.James, D.J.Kuehn, K.Lahav, O.Lima, M.Maia, M.A.G.March, M.Menanteau, F.Miquel, R.Ogando, R.L.C.Plazas, A.A.Sanchez, E.Scarpine, V.Schindler, R.Schubnell, M.Sevilla-Noarbe, I.Smith, M.Soares-Santos, M.Sobreira, F.Suchyta, E.Swanson, M.E.C.Tarle, G.Tucker, D.Wechsler, R.2019-11-282019-11-282018-10Monthly Notices of the Royal Astronomical Society, 479(4), pp. 4345-4354.0035-8711DOI: 10.1093/mnras/sty1419http://repositorio.unab.cl/xmlui/handle/ria/10865Indexación: Scopus.This paper was written as part of the STRong lensing Insights into the Dark Energy Survey (STRIDES) collaboration, a broad external collaboration of the Dark Energy Survey, http://strides.as tro.ucla.edu TT acknowledges support from NSF through grant AST-1450141, and from the Packard Foundation through a Packard Research Fellowship. CDF acknowledges support from the U.S. National Science Foundation through grant number AST-1312329.Funding for the DES Projects has been provided by the DOE and NSF (USA), MISE (Spain), STFC (UK), HEFCE (UK), NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA (Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), MINECO (Spain), DFG (Germany), and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Zürich, Fermilab, University of Illinois, ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU München and the associated Excellence Cluster Universe, University of Michigan, NOAO, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford University, University of Sussex, and Texas A&M University. The DES Data Management System is supported by the NSF under grant number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelen-cia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the ERC under the EU’s 7th Framework Programme including grants ERC 240672, 291329, and 306478.This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.i nt/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web /gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.This work is based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovac¸ão (MCTI) da República Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).We report the discovery, spectroscopic confirmation, and first lens models of the first, strongly lensed quasars from a combined search in WISE and Gaia-DR1 over the DES footprint. Their Einstein radii span a range between ≈2.0 arcsec and ≈0.4 arcsec. Two of these (WGD2038-4008, RA = 20:38:02.65, Dec.=-40:08:14.64; WGD2021-4115, RA = 20:21:39.45, Dec. = -41:15:57.11) also have confirmed deflector redshifts. The four-image lens WGD2038-4008, with source and deflector redshifts s = 0.777 ± 0.001 and zl = 0.230 ± 0.002, respectively, has a deflector with radius Reff ≈ 3.4 arcsec, stellar mass log(M*/M⊙) = 11.64+0.20 -0.43, and extended isophotal shape variation. Simple lens models yield Einstein radii RE = (1.30 ± 0.04) arcsec, axis ratio q = 0.75 ± 0.1 (compatible with that of the starlight) and considerable shear-ellipticity degeneracies. The two-image lens WGD2021-4115 has zs = 1.390 ± 0.001 and zl = 0.335 ± 0.002, and Einstein radius RE = (1.1 ± 0.1) arcsec, but higher-resolution imaging is needed to accurately separate the deflector and faint quasar image. Analogous lens model degeneracies hold for the other six lenses (J0146-1133, J0150-4041, J0235-2433, J0245-0556, J0259-2338, and J0508-2748) shown in this paper. © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.enGravitational lensing: strongMethods: statisticalSurveysTechniques: image processingArtículo