The inner rings of β Pictoris

We present Keck images of the dust disk around β Pictoris at λ = 17.9 μm that reveal new structure in its morphology. Within 1Prime; (19 AU) of the star, the long axis of the dust emission is rotated by more than 10° with respect to that of the overall disk. This angular offset is more pronounced than the warp detected at 3Prime;.5 by the Hubble Space Telescope (HST) and is in the opposite direction. By contrast, the long axis of the emission contours ∼1Prime;.5 from the star is aligned with the HST warp. Emission peaks between 1Prime;.5 and 4Prime; from the star hint at the presence of rings similar to those observed in the outer disk at ∼25″ with the HST Space Telescope Imaging Spectrograph. A deconvolved image strongly suggests that the newly detected features arise from a system of four noncoplanar rings. Bayesian estimates based on the primary image lead to ring radii of 14 ± 1, 28 ± 3, 52 ± 2, and 82 ± 2 AU, with orbital inclinations that alternate in orientation relative to the overall disk and decrease in magnitude with increasing radius. We believe these new results make a strong case for the existence of a nascent planetary system around β Pic.