Mass fraction of different orbital components in the remnant galaxy at 1 Gyr after the merger as a function of ⟨θ_{r, v}⟩. Columns from left to right: disk, warm component, bulge, and hot inner stellar halo. Rows from top to bottom: mergers with mass ratios of 1/2–2, 1/3–1/2, and 1/5–1/3, respectively. In each panel, the colors indicate the change in the mass fraction of each component compared to that in the main progenitor galaxy at 1 Gyr before the merger, as illustrated by the colorbar. The solid black line represents the running median and the gray shadow region denotes the 1 ± σ scatter. The correlation coefficient $\mathcal{R}$ is calculated and labeled in each panel.