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               <dc:title>Nine lensed quasars and quasar pairs discovered through spatially extended variability in Pan-STARRS</dc:title>
               <dc:creator>Dux, F.</dc:creator>
               <dc:creator>Lemon, C.</dc:creator>
               <dc:creator>Courbin, Frédéric</dc:creator>
               <dc:creator>Neira, Favio</dc:creator>
               <dc:creator>Anguita, Timo</dc:creator>
               <dc:creator>Galan, A.</dc:creator>
               <dc:creator>Kim, Sam</dc:creator>
               <dc:creator>Hempel, Maren</dc:creator>
               <dc:creator>Hempel, Angela</dc:creator>
               <dc:creator>Lachaume, Régis</dc:creator>
               <dc:subject>Gravitació</dc:subject>
               <dc:subject>Quàsars</dc:subject>
               <dc:subject>Gravitation</dc:subject>
               <dc:subject>Quasars</dc:subject>
               <dc:description>We present the proof of concept of a method for finding strongly lensed quasars using their spatially extended photometric variability through difference imaging in cadenced imaging survey data. We applied the method to Pan-STARRS, starting with an initial selection of 14 107 Gaia multiplets with quasar-like infrared colours from WISE. We identified 229 candidates showing notable spatially extended variability during the Pan-STARRS survey period. These include 20 known lenses and an additional 12 promising candidates for which we obtained long-slit spectroscopy follow-up. This process resulted in the confirmation of four doubly lensed quasars, four unclassified quasar pairs, and one projected quasar pair. Only three are pairs of stars or quasar+star projections. The false-positive rate accordingly is 25%. The lens separations are between 0.8100 and 1.2400, and the source redshifts lie between z = 1.47 and z = 2.46. Three of the unclassified quasar pairs are promising dual-quasar candidates with separations ranging from 6.6 to 9.3 kpc. We expect that this technique is a particularly efficient way to select lensed variables in the upcoming Rubin-LSST, which will be crucial given the expected limitations for spectroscopic follow-up.</dc:description>
               <dc:date>2025-05-23T20:30:57Z</dc:date>
               <dc:date>2025-05-23T20:30:57Z</dc:date>
               <dc:date>2025-05-20T06:43:12Z</dc:date>
               <dc:date>2025-05-20T06:43:12Z</dc:date>
               <dc:date>2024-01-31</dc:date>
               <dc:date>2025-05-20T06:43:13Z</dc:date>
               <dc:type>info:eu-repo/semantics/article</dc:type>
               <dc:type>info:eu-repo/semantics/publishedVersion</dc:type>
               <dc:identifier>http://hdl.handle.net/2445/221124</dc:identifier>
               <dc:relation>Reproducció del document publicat a: https://doi.org/10.1051/0004-6361/202347598</dc:relation>
               <dc:relation>Astronomy &amp; Astrophysics, 2024, vol. 682</dc:relation>
               <dc:relation>https://doi.org/10.1051/0004-6361/202347598</dc:relation>
               <dc:rights>cc-by (c) Dux, F. et al., 2024</dc:rights>
               <dc:rights>http://creativecommons.org/licenses/by/3.0/es/</dc:rights>
               <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
               <dc:publisher>EDP Sciences</dc:publisher>
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