Col-OSSOS: Color and Inclination Are Correlated throughout the Kuiper Belt
Fraser, Wesley C.
Pike, Rosemary E.
Bannister, Michele T.
Schwamb, Megan E.
Kavelaars, J. J.
Gladman, Brett J.
Gwyn, Stephen D. J.
Lehner, Matthew J.
AffiliationUniv Arizona, Lunar & Planetary Lab
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationMichaël Marsset et al 2019 AJ 157 94
Rights© 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractBoth physical and dynamical properties must be considered to constrain the origins of the dynamically excited distant solar system populations. We present high-precision (g-r) colors for 25 small (H-r > 5) dynamically excited trans-Neptunian objects (TNOs) and centaurs acquired as part of the Colours of the Outer Solar System Origins Survey. We combine our data set with previously published measurements and consider a set of 229 colors of outer solar system objects on dynamically excited orbits. The overall color distribution is bimodal and can be decomposed into two distinct classes, termed gray and red, that each has a normal color distribution. The two color classes have different inclination distributions: red objects have lower inclinations than the gray ones. This trend holds for all dynamically excited TNO populations. Even in the worst-case scenario, biases in the discovery surveys cannot account for this trend; it is intrinsic to the TNO population. Considering that TNOs are the precursors of centaurs, and that their inclinations are roughly preserved as they become centaurs, our finding solves the conundrum of centaurs being the only outer solar system population identified so far to exhibit this property. The different orbital distributions of the gray and red dynamically excited TNOs provide strong evidence that their colors are due to different formation locations in a disk of planetesimals with a compositional gradient.
VersionFinal published version
SponsorsCol-OSSOS program; CanadianSpace Agency; UK STFC [ST/L000709/1]; Gemini Observatory; NASA [NNX14AG93G, NNX15AH59G]; Portuguese FCT-Foundation for Science and Technology [SFRH/BGCT/113686/2015]; FCT-Foundation for Science and Technology [UID/Multi/00611/2013]; FEDER-European Regional Development Fund through COMPETE 2020-Operational Programme Competitiveness and Internationalisation [POCI-01-0145-FEDER-006922]