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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 10.

Distributions of the best (successful) macromodel parameters, s, q, ϕq, γ, and ϕγ − ϕq, for all seven kinds of perturbations, each added to EPL+γ to fit to image positions only (assuming σp = 2 mas, essentially the last row in Table 3). We deliberately omit the y-axis ticks in each panel so that panels in the same row can share a common y-axis.

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