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Can Third- and Fourth-order Multipoles plus Radial Variation of Isodensity Ellipses Explain the Observed Flux Ratios in B1422+231? YES, and a Lesson Learned from a TNG100 Lensing Galaxy Sample

  • Authors: Ruizhe Feng, Dandan Xu, Dominique Sluse, Giulia Despali, Anowar J. Shajib, Cai-Na Hao

Ruizhe Feng et al 2026 The Astrophysical Journal 1012 .

  • Provider: AAS Journals

Caption: Figure 11.

The left panel presents the distributions of the radial difference Δq2−6 kpc ≡ q6 kpc − q2 kpc for both the successful and failed cases when adopting EPL+γ in the presence of perturbation Qv alone (assuming σf = 10%, σp = 10 mas), and in the right panel are the distributions for Δϕq, 2−6 kpc ≡ ϕq, 6 kpc − ϕq, 2 kpc when adding perturbation PAv alone. The samples essentially correspond to the fourth row in Table 4.

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