Unbiased Inclination Distributions for Objects in the Kuiper Belt
Name
Elliot_Unbiased inclination.pdf
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2.91 MB
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Author(s)
Gulbis, Amanda A. S.
Elliot, James L.
Adams, Elisabeth Rose
Benecchi, Susan D.
Buie, Marc W.
Trilling, David E.
Wasserman, L. H.
Date Issued
July 2009
Journal
Astronomical Journal
Publisher
IOP Publishing
Citation
Gulbis, A. A. S. et al. “Unbiased Inclination Distributions for Objects in the Kuiper Belt.” The Astronomical Journal 140.2 (2010): 350–369.
Version
Author's final manuscript
Abstract
Using data from the Deep Ecliptic Survey (DES), we investigate the inclination distributions of objects in the Kuiper Belt. We present a derivation for observational bias removal and use this procedure to generate unbiased inclination distributions for Kuiper Belt objects (KBOs) of different DES dynamical classes, with respect to the Kuiper Belt plane. Consistent with previous results, we find that the inclination distribution for all DES KBOs is well fit by the sum of two Gaussians, or a Gaussian plus a generalized Lorentzian, multiplied by sin i. Approximately 80% of KBOs are in the high-inclination grouping. We find that Classical object inclinations are well fit by sin i multiplied by the sum of two Gaussians, with roughly even distribution between Gaussians of widths 2.0[superscript +0.6] [subscript –0.5°] and 8.1[superscript +2.6] [subscript –2.1°]. Objects in different resonances exhibit different inclination distributions. The inclinations of Scattered objects are best matched by sin i multiplied by a single Gaussian that is centered at 19.1[superscript +3.9] [subscript –3.6°] with a width of 6.9[superscript +4.1] [subscript –2.7°]. Centaur inclinations peak just below 20°, with one exceptionally high-inclination object near 80°. The currently observed inclination distribution of the Centaurs is not dissimilar to that of the Scattered Extended KBOs and Jupiter-family comets, but is significantly different from the Classical and Resonant KBOs. While the sample sizes of some dynamical classes are still small, these results should begin to serve as a critical diagnostic for models of solar system evolution.
MIT Department
Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences
Massachusetts Institute of Technology. Department of Physics
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DOI of Published Version
https://doi.org/10.1088/0004-6256/140/2/350
