Disk fraction in the remnant galaxy at 1 Gyr after the merger as a function of the three angles. The columns from left to right are $⟨{\theta }_{{\mathbf{L}}_{\text{main}},{\mathbf{L}}_{\text{orbit}}}^{\mathrm{\prime }}⟩,⟨{\theta }_{{\mathbf{L}}_{\text{sat}},{\mathbf{L}}_{\text{orbit}}}^{\mathrm{\prime }}⟩$, and ⟨θ_{r, v}⟩. The rows from the second top to the bottom corresponds to mergers with mass ratio of 1/2–2, 1/3–1/2, and 1/5–1/3, respectively. Each dot represents one merger pair colored by Δf_disk, with red dots denoting a decrease in the disk fraction and blue dots denoting an increase in the disk fraction compared to the main progenitor galaxy at 1 Gyr before the merger. In each panel, the black solid line represents the running median of f_{disk,+1 Gyr} and the gray shadow regions indicate the ± 1σ scatter. The correlation coefficients between f_{disk,+1 Gyr} and angles are shown in each panel. The top row illustrates the probability density function (PDF) of the angles. The red, green, and blue lines represent mass ratio between 1/2 and 2, 1/3 and 1/2, 1/5, and 1/3, respectively, all smoothed using Gaussian kernel density estimation (KDE). The black line represents the PDF expected from an isotropic model.