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Sylvia is a triple asteroid system located in the main belt. We report newadaptive optics observations of this system that extend the baseline ofexisting astrometric observations to a decade. We present the first fullydynamical 3-body model for this system by fitting to all available astrometricmeasurements. This model simultaneously fits for individual masses, orbits, andprimary oblateness. We find that Sylvia is composed of a dominant central masssurrounded by two satellites orbiting at 706.5 +/- 2.5 km and 1357 +/- 4.0 km,i.e., about 5 and nearly 10 primary radii. We derive individual masses of 1.484-0.014/+0.016 x 10^19 kg for the primary (corresponding to a density of 1.29+/- 0.39 g cm^-3), 7.33 -2.3/+4.7 x 10^14 kg for the inner satellite, and 9.32-8.3/+20.7 x 10^14 kg for the outer satellite. The oblateness of the primaryinduces substantial precession and the J_2 value can be constrained to therange of 0.0985-0.1. The orbits of the satellites are relatively circular witheccentricities less than 0.04. The spin axis of the primary body and theorbital poles of both satellites are all aligned within about two degrees ofeach other, indicating a nearly coplanar configuration and suggestive ofsatellite formation in or near the equatorial plane of the primary. We alsoinvestigate the past orbital evolution of the system by simulating the effectsof a recent passage through 3:1 mean-motion eccentricity-type resonances. Insome scenarios this allow us to place constraints on interior structure andpast eccentricities.

Orbits, masses, and evolution of main belt triple (87) Sylvia