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arxiv: 1711.03971 · v1 · pith:KDPA4FBVnew · submitted 2017-11-10 · 🌌 astro-ph.CO · astro-ph.GA

DES meets Gaia: discovery of strongly lensed quasars from a multiplet search

A. Agnello , H. Lin , N. Kuropatkin , E. Buckley-Geer , T. Anguita , P.L. Schechter , T. Morishita , V. Motta
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K. Rojas T. Treu A. Amara M.W. Auger F. Courbin C.D. Fassnacht J. Frieman A. More P.J. Marshall R.G. McMahon G. Meylan S.H. Suyu K. Glazebrook N. Morgan B. Nord T. M. C. Abbott F. B. Abdalla J. Annis K. Bechtol A. Benoit-L\'evy E. Bertin R. A. Bernstein D. Brooks D. L. Burke A. Carnero Rosell J. Carretero C. E. Cunha C. B. D'Andrea L. N. da Costa S. Desai A. Drlica-Wagner T. F. Eifler B. Flaughe J. Garc\'ia-Bellido E. Gaztanaga D. W. Gerdes D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez K. Honscheid D. J. James K. Kuehn O. Lahav M. Lima M. A. G. Maia M. March F. Menanteau R. Miquel R. L. C. Ogando A. A. Plazas E. Sanchez V. Scarpine R. Schindler M. Schubnel I. Sevilla-Noarbe M. Smith M. Soares-Santos F. Sobreira E. Suchyta M. E. C. Swanson G. Tarle D. Tucker R. Wechsler
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classification 🌌 astro-ph.CO astro-ph.GA
keywords primedeflectordiscoveryeinsteinfirstgaialenslensed
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We report the discovery, spectroscopic confirmation and first lens models of the first two, strongly lensed quasars from a combined search in WISE and Gaia over the DES footprint. The four-image lensWGD2038-4008 (r.a.=20:38:02.65, dec.=-40:08:14.64) has source- and lens-redshifts $z_{s}=0.777 \pm 0.001$ and $z_l = 0.230 \pm 0.002$ respectively. Its deflector has effective radius $R_{\rm eff} \approx 3.4^{\prime\prime}$, stellar mass $\log(M_{\star}/M_{\odot}) = 11.64^{+0.20}_{-0.43}$, and shows extended isophotal shape variation. Simple lens models yield Einstein radii $R_{\rm E}=(1.30\pm0.04)^{\prime\prime},$ axis ratio $q=0.75\pm0.1$ (compatible with that of the starlight) and considerable shear-ellipticity degeneracies. The two-image lensWGD2021-4115 (r.a.=20:21:39.45, dec.=--41:15:57.11) has $z_{s}=1.390\pm0.001$ and $z_l = 0.335 \pm 0.002$, and Einstein radius $R_{\rm E} = (1.1\pm0.1)^{\prime\prime},$ but higher-resolution imaging is needed to accurately separate the deflector and faint quasar image. We also show high-rank candidate doubles selected this way, some of which have been independently identified with different techniques, and discuss a DES+WISE quasar multiplet selection.

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