Models of the Strongly Lensed Quasar DES J0408-5354
Models of the Strongly Lensed Quasar DES J0408-5354
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DOI：
10.1093/mnras/stx2242
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发表时间：
2017-02
影响因子：
4.8
通讯作者：
A. Agnello;Huan Lin;L. Buckley-Geer;T. Treu;V. Bonvin;F. Courbin;C. Lemon;T. Morishita;A. Amara;M. Auger;S. Birrer;J. Chan;T. Collett;A. More;C. Fassnacht;J. Frieman;P. Marshall;R. McMahon;G. Meylan;S. Suyu;F.Castander;D. Finley;A.Howell;C. Kochanek;M. Makler;P. Martini;N. Morgan;B.Nord;F. Ostrovski;P. Schechter;D. Tucker;Risa Wechsler;T. Abbott;F. Abdalla;S. Allam;A. Benoit-Lévy;E. Bertin;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;M. Crocce;C. Cunha;C. D'Andrea;L. Costa;S. Desa;J. Dietrich;T. Eifler;B. Flaugher;P. Fosalba;J. Garc'ia-Bellido;E. Gaztañaga;D. Goldstein;D. Gruen;R. Gruendl;J. Gschwend;G. Gutiérrez;K. Honscheid;D. James;K. Kuehn;N. Kuropatkin;T. Li;M. Lima;M. Maia;M. March;J. Marshall;Peter Melchior;F. Menanteau;R. Miquel;R. Ogando;A. Plazas;A. Romer;E. Sánchez;R. Schindler;M. Schubnell;I. Sevilla-Noarbe;M. Smith;R. C. Smith;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;A. Walker
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作者：
A. Agnello;Huan Lin;L. Buckley-Geer;T. Treu;V. Bonvin;F. Courbin;C. Lemon;T. Morishita;A. Amara;M. Auger;S. Birrer;J. Chan;T. Collett;A. More;C. Fassnacht;J. Frieman;P. Marshall;R. McMahon;G. Meylan;S. Suyu;F.Castander;D. Finley;A.Howell;C. Kochanek;M. Makler;P. Martini;N. Morgan;B.Nord;F. Ostrovski;P. Schechter;D. Tucker;Risa Wechsler;T. Abbott;F. Abdalla;S. Allam;A. Benoit-Lévy;E. Bertin;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;M. Crocce;C. Cunha;C. D'Andrea;L. Costa;S. Desa;J. Dietrich;T. Eifler;B. Flaugher;P. Fosalba;J. Garc'ia-Bellido;E. Gaztañaga;D. Goldstein;D. Gruen;R. Gruendl;J. Gschwend;G. Gutiérrez;K. Honscheid;D. James;K. Kuehn;N. Kuropatkin;T. Li;M. Lima;M. Maia;M. March;J. Marshall;Peter Melchior;F. Menanteau;R. Miquel;R. Ogando;A. Plazas;A. Romer;E. Sánchez;R. Schindler;M. Schubnell;I. Sevilla-Noarbe;M. Smith;R. C. Smith;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;D. Thomas;A. Walker
我们对最近发现的四倍透镜类星体J0408−5354进行了详细的建模，目的是解释其显着的结构：除了围绕主偏转器（G1）的三个类星体图像（A，B，D）外，第四张图像(C)被暗能量调查成像数据中未检测到的摄动器（G2）显着变红和变暗。从包含（尘埃校正）通量比的透镜模型中，我们发现了一个摄动点爱因斯坦半径0.04 arcsec≤RE, G2≤0.2 arcsec，封闭质量Mp(RE, G2)≤1.0 × 1010 M⊙。主偏转器的恒星质量log10(M - - - /M⊙)=11.49+0.46−0.32，在其爱因斯坦半径RE内的投影质量Mp(RE, G1)≈6 × 1011 M⊙,G1 =(1.85±0.15)arcsec，预测速度色散267-280 km s−1。来自一个同伴监测活动的后续图像显示了额外的成分，包括类星体和G1之间红移的候选第二源。还探讨了具有自由摄动器的模型，以及尘埃校正和延迟校正的通量比。预测的时延(ΔtAB =（135.0±12.6)d， ΔtBD =(21.0±3.5)d）与实测值大致一致，但需要更好的成像才能进行适当的建模和比较。我们还讨论了J0408−5354在透镜类星体寻找策略上的一些经验教训，这是由于它的色度和形态。
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.