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dc.contributor.authorNoonan, John W.
dc.contributor.authorReddy, Vishnu
dc.contributor.authorHarris, Walter M.
dc.contributor.authorBottke, William F.
dc.contributor.authorSanchez, Juan A.
dc.contributor.authorFurfaro, Roberto
dc.contributor.authorBrown, Zarah
dc.contributor.authorFernandes, Rachel
dc.contributor.authorKareta, Theodore
dc.contributor.authorLejoly, Cassandra
dc.contributor.authorNallapu, Ravi Teja
dc.contributor.authorNiazi, Haris Khan
dc.contributor.authorSlick, Lindsay R.
dc.contributor.authorSchatz, Lauren
dc.contributor.authorSharkey, Benjamin N. L.
dc.contributor.authorSpringmann, Alessondra
dc.contributor.authorAngle, Geoff
dc.contributor.authorBailey, Leandra
dc.contributor.authorAcuna, Derian D.
dc.contributor.authorLewin, Collin
dc.contributor.authorMarchese, Katherina
dc.contributor.authorMeshel, Max
dc.contributor.authorQuintero, Natalie
dc.contributor.authorTatum, Kyle
dc.contributor.authorWilburn, Greg
dc.date.accessioned2019-12-13T00:39:12Z
dc.date.available2019-12-13T00:39:12Z
dc.date.issued2019-11-01
dc.identifier.citationJohn W. Noonan et al 2019 AJ 158 213en_US
dc.identifier.issn0004-6256
dc.identifier.doi10.3847/1538-3881/ab4813
dc.identifier.urihttp://hdl.handle.net/10150/636363
dc.description.abstractLinking meteorites to source regions in the main asteroid belt is important for understanding the conditions under which their parent bodies formed. Ordinary chondrites are the most abundant class of meteorites on Earth, totaling 86% of all collected samples. Some S-type asteroids/families have been proposed as sources for the three different (H, L, and LL) types of ordinary chondrites with Hebe, Agnia, Merxia, and Koronis families being the source for H chondrites, Gefion for H/L chondrites, and Flora family for LL chondrites. However, the composition and meteorite affinity of several large S-type main belt asteroids remains unconstrained leaving the possibility of additional source regions for ordinary chondrite meteorites. Here we investigate the surface composition of three large S-type asteroids, (3) Juno, (7) Iris, and (25) Phocaea, using their near-infrared spectra (0.7–2.55 μm) to identify the parent body of the H chondrites. We use a Bayesian inference model to confirm the meteorite analogs of the three asteroids. Based on our Bayes classifier we find the following analogs and probabilities: Juno is likely H chondrite (89%), Iris is likely LL chondrite (97.5%), and Phocaea is likely H chondrite (98.6%). While Phocaea has the highest probability of being an H chondrite, it is dynamically unlikely to deliver material to near-Earth space. While Juno has spectral properties similar to H chondrites, its family is unlikely to produce sizeable H-chondrite-type near-Earth objects (NEOs). If Juno is the primary source of H chondrite meteorites, it suggests that an additional source is needed to explain the H-chondrite-type NEOs.en_US
dc.description.sponsorshipNASA Near-Earth Object Observations (NEOO) program grant [NNXAL06G]; state of Arizona Technology Research Initiative Fund (TRIF)en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2019. The American Astronomical Society. All rights reserved.en_US
dc.subjectinfrared: planetary systemsen_US
dc.subjectminor planetsen_US
dc.subjectasteroids: individual (Juno, Iris, Phocaea)en_US
dc.subjecttechniques: spectroscopicen_US
dc.titleSearch for the H Chondrite Parent Body among the Three Largest S-type Asteroids: (3) Juno, (7) Iris, and (25) Phocaeaen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.contributor.departmentUniv Arizona, Dept Syst & Ind Engnen_US
dc.contributor.departmentUniv Arizona, Coll Opt Scien_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.volume158
dc.source.issue5
dc.source.beginpage213
refterms.dateFOA2019-12-13T00:39:12Z


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