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dc.contributor.authorLawler, S. M.
dc.contributor.authorShankman, C.
dc.contributor.authorKavelaars, J. J.
dc.contributor.authorAlexandersen, M.
dc.contributor.authorBannister, M. T.
dc.contributor.authorChen, Ying-Tung
dc.contributor.authorGladman, B.
dc.contributor.authorFraser, W. C.
dc.contributor.authorGwyn, S.
dc.contributor.authorKaib, N.
dc.contributor.authorPetit, J.-M.
dc.contributor.authorVolk, K.
dc.date.accessioned2018-05-23T15:42:57Z
dc.date.available2018-05-23T15:42:57Z
dc.date.issued2018-05
dc.identifier.citationS. M. Lawler et al 2018 AJ 155 197en_US
dc.identifier.issn1538-3881
dc.identifier.doi10.3847/1538-3881/aab8ff
dc.identifier.urihttp://hdl.handle.net/10150/627754
dc.description.abstractThe scattering trans-Neptunian Objects (TNOs) can be measured to smaller sizes than any other distant small-body population. We use the largest sample yet obtained, 68 discoveries, primarily by the Outer Solar System Origins Survey (OSSOS), to constrain the slope of its luminosity distribution, with sensitivity to much fainter absolute H-magnitudes than previous work. Using the analysis technique in Shankman et al., we confirm that a single slope for the H-distribution is not an accurate representation of the scattering TNOs and Centaurs, and that a break in the distribution is required, in support of previous conclusions. A bright-end slope of alpha(b) = 0.9 transitioning to a faint-end slope alpha(f) of 0.4-0.5 with a differential number contrast c from 1 (a knee) to 10 (a divot) provides an acceptable match to our data. We find that break magnitudes H-b of 7.7 and 8.3, values both previously suggested for dynamically hot Kuiper Belt populations, are equally non-rejectable for a range of alpha(f) and c in our statistical analysis. Our preferred divot H-distribution transitions to alpha(f) = 0.5 with a divot of contrast c = 3 at H-b = 8.3, while our preferred knee H-distribution transitions to alpha(f) = 0.4 at H-b = 7.7. The intrinsic population of scattering TNOs required to match the OSSOS detections is 3 x 10(6) for H-r < 12, and 9 x 10(4) for H-r < 8.66 (D greater than or similar to 100 km), with Centaurs having an intrinsic population two orders of magnitude smaller.en_US
dc.description.sponsorshipNRC-Canada Plaskett Fellowship; UK STFC [ST/L000709/1]; Science and Technology Facilities Council [ST/P0003094/1]; National Science and Engineering Research Council; National Research Council of Canadaen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/1538-3881/155/i=5/a=197?key=crossref.a4a2f22c5981ecb306f967b91c8effe0en_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.subjectKuiper belt: generalen_US
dc.titleOSSOS. VIII. The Transition between Two Size Distribution Slopes in the Scattering Disken_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.identifier.journalASTRONOMICAL JOURNALen_US
dc.description.collectioninformationThis 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 repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astronomical Journal
dc.source.volume155
dc.source.issue5
dc.source.beginpage197
refterms.dateFOA2018-05-23T15:42:58Z


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