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Table A.1

Definition of all the dynamical populations use here as a function of their semimajor axis, eccentricity, perihelion, and aphelion (using the definitions in Carry et al. 2016; Gladman et al. 2008).

Class Semimajor axis (au) Eccentricity Perihelion (au) Aphelion (au)
min. max. min. max. min. max. min. max.

NEA 1.300
Atira a q
Aten a q
Apollo a 4.600 Q
Amor a 4.600 Q 1.300
MC 1.300 4.600 1.300 Q
MBA Q 4.600 Q
Hungaria J4:1 Q
IMB J4:1 J3:1 Q
MMB J3:1 J5:2 Q
OMB J5:2 J2:1 Q
Cybele J2:1 J5:3 Q
Hilda J5:3 4.600 Q
Trojan 4.600 5.500
Centaur 5.500 a
SDO a 37.037
Detached a 0.24 37.037
ICB 37.037 N2:3 0.24 37.037
MCB N2:3 N1:2 0.24 37.037
OCB N1:2 0.24 37.037

Notes. See Fig. A.1 for the distribution of these populations in the semimajor axis – eccentricity orbital element space. The numerical value of the semimajor axes a, perihelion q, aphelion Q, and mean-motion resonances (indices i:j) are for the Earth a, q, and Q at 1.0, 0.983, and 1.017 AU; for Mars Q at 1.666 AU; for Jupiter J4:1, J3:1, J5:2, J2:1, and J5:3 at 2.06, 2.5, 2.87, 3.27, 3.7 AU; and for Neptune a, N2:3, and N1:2 at 30.07, 47.7, and 39.4 AU. The somewhat arbitrary limit of 37.037 AU corresponds to the innermost perihelion that is accessible to detached KBOs (semimajor axis of N1:2 and eccentricity of 0.24).

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