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Fig. 6


Same as Fig. 4 for the remnants M0 (top two rows) and M3 (bottom two rows). From top to bottom: mass distribution log Σ and mock line-of-sight velocity maps for different stellar populations in the remnant. From left to right: the first column shows all the stars of the merger remnant (“All stars”), the second column shows only the particles that initially belonged to the disk of the progenitor that was inclined by 90° with respect to the orbital plane (“Polar Pr. disk”) and show strong prolate rotation in the remnant. The third column shows the same for the particles that initially formed the disk of the progenitor that was aligned with the orbital plane (“Aligned Pr. disk”), while the last column shows the remaining stellar particles of the remnant that initially formed the progenitor bulges (“Pr. bulges”). The mass fraction of each component with respect to the total stellar mass of the remnant is denoted in the top right corner.

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