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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 6.

Relations between multipole strengths from total mass maps and velocity dispersion. Left: a3/a versus σv; right: a4/a versus σv. For comparison, the multipole strengths are averaged within two different annuli (as the right panel of Figure 4): 0.8–1.2 Rein (gray points and shaded histogram) and 0.5–2.0 Rein (blue points and histogram).

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