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We investigate the origins of the photometrically Very Red and Less RedTrans-Neptunian Objects. We first reanalyse the dataset of Marsset et al. 2019and find that, in addition to the known color-inclination correlation in hotTNOs, a similar trend exists for color-eccentricity. We show that VR TNOs aresharply constrained to eccentricities < 0.42 and inclinations < 21 deg, leadingto a paucity of VR scattered disk and distant MMR objects. We then interpretthese findings using N-body simulations accounting for Neptune's outwardmigration into a massless particles disk, and find that these observations arebest reproduced with a LR-to-VR color transition line between 38 and 42 AU inthe primordial disk, separating the objects' formation locations. For aninitial surface density profile $\Sigma \propto 1/r^2$, a color transitionaround 38 AU is needed to explain the high abundance of VR plutinos but createstoo many VR scattered disk objects, while a transition line around 42 AU seemsto better reproduces the scattered disk colors but creates virtually no VRplutinos. Our simulations furthermore show that the rarity of VR particles athigh eccentricity is possibly due to the absence of sweeping higher order MMRs,and secular resonances, beyond 42 AU. Inspecting individual populations, weshow that the majority of VR SDOs originate as objects trapped in Neptune'ssecond and third order MMRs. These then evolve due to diffusion, scattering,Kozai-Lidov cycles, and secular resonances into their current orbits. Futureunbiased color surveys are crucial to better constrain the TNOs dynamicalorigins.

The rarity of very red TNOs in the scattered disk