Models of the strongly lensed quasar DES J0408−5354

Agnello, A and Lin, H and Buckley Geer, L and Treu, T and Bonvin, V and Courbin, F and Lemon, C and Morishita, T and Amara, A and Auger, M W and Birrer, S and Chan, J and Collett, T E and More, A and Fassnacht, C D and Frieman, J and Marshall, P J and McMahon, R G and Meylan, G and Suyu, S H and Castander, F J and Finley, D A and Howell, A and Kochanek, C and Makler, M and Martini, P and Morgan, N and Nord, B and Ostrovski, F and Schechter, P and Tucker, D L and Wechsler, R H and Abbott, T M C and Abdalla, F B and Allam, S and Benoit-Lévy, A and Bertin, E and Brooks, D and Burke, D L and Rosell, A Carnero and Kind, M Carrasco and Carretero, J and Crocce, M and Cunha, C E and D’Andrea, C B and da Costa, L N and Desai, Shantanu (2017) Models of the strongly lensed quasar DES J0408−5354. Monthly Notices of the Royal Astronomical Society, 472 (4). pp. 4038-4050. ISSN 0035-8711

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Abstract

We present detailed modelling of the recently discovered, quadruply lensed quasar J0408−5354, with the aim of interpreting its remarkable configuration: besides three quasar images (A,B,D) around the main deflector (G1), a fourth image (C) is significantly reddened and dimmed by a perturber (G2) which is not detected in the Dark Energy Survey imaging data. From lens models incorporating (dust-corrected) flux ratios, we find a perturber Einstein radius 0.04 arcsec ≲ RE, G2 ≲ 0.2 arcsec and enclosed mass Mp(RE, G2) ≲ 1.0 × 1010 M⊙. The main deflector has stellar mass log10(M⋆/M⊙)=11.49+0.46−0.32 , a projected mass Mp(RE, G1) ≈ 6 × 1011 M⊙ within its Einstein radius RE, G1 = (1.85 ± 0.15) arcsec and predicted velocity dispersion 267–280 km s−1. Follow-up images from a companion monitoring campaign show additional components, including a candidate second source at a redshift between the quasar and G1. Models with free perturbers, and dust-corrected and delay-corrected flux ratios, are also explored. The predicted time-delays (ΔtAB = (135.0 ± 12.6) d, ΔtBD = (21.0 ± 3.5) d) roughly agree with those measured, but better imaging is required for proper modelling and comparison. We also discuss some lessons learnt from J0408−5354 on lensed quasar finding strategies, due to its chromaticity and morphology.

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