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Binzel Et Al MITHNEOS Icarus Cite as Binzel et al. Icarus 324 (2019) 41–76 https://doi.org/10.1016/j.icarus.2018.12.035 Compositional distributions and evolutionary processes for the near-Earth object population: Results from the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS) R.P. Binzela,1,⁎, F.E. DeMeoa, E.V. Turtelbooma, S.J. Busb, A. Tokunagab, T.H. Burbinec, C. Lantzd, D. Polishooke, B. Carryf, A. Morbidellif, M. Birlang, P. Vernazzah, B.J. Burti, N. Moskovitzi, S.M. Slivanj, C.A. Thomask, A.S. Rivkinl, M.D. Hicksm, T. Dunnn, V. Reddyo, J.A. Sanchezp, M. Granvikq, T. Kohoutr a Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, United States b University of Hawaii, United States c Mount Holyoke College, United States d Institut d'Astrophysique Spatiale, CNRS/Université Paris Saclay, France e Weizmann Institute, Israel f Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Lagrange, France g IMCCE, Paris Observatory and Astronomical Institute of Romanian Academy, Bucharest, Romania h LAM–CNRS/AMU, Marseille, France i Lowell Observatory, United States j Wellesley College, United States k Northern Arizona University, United States l Johns Hopkins University Applied Physics Laboratory, United States m Jet Propulsion Laboratory, United States n Colby College, United States o University of Arizona, United States p Planetary Science Institute, United States q University of Helsinki and Luleå University of Technology, Kiruna, Sweden r University of Helsinki, Finland ⁎ Corresponding author. 1 Chercheur Associé, IMCCE-Observatoire de Paris, France. A B S T R A C T Advancing technology in near-infrared instrumentation and dedicated planetary telescope facilities have enabled nearly two decades of reconnoitering the spectral properties for near-Earth objects (NEOs). We report measured spectral properties for more than 1000 NEOs, representing>5% of the currently discovered population. Thermal flux detected below 2.5 μm allows us to make albedo estimates for nearly 50 objects, including two comets. Additional spectral data are reported for more than 350 Mars-crossing asteroids. Most of these measurements were achieved through a collaboration between researchers at the Massachusetts Institute of Technology and the University of Hawaii, with full cooperation of the NASA Infrared Telescope Facility (IRTF) on Mauna Kea. We call this project the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS; myth-neos). While MITHNEOS has continuously released all spectral data for immediate use by the scientific community, our objectives for this paper are to: (1) detail the methods and limits of the survey data, (2) formally present a compilation of results including their taxonomic classification within a single internally consistent framework, (3) perform a preliminary analysis on the overall population characteristics with a concentration toward deducing key physical processes and identifying their source region for escaping the main belt. Augmenting our newly published measurements are the previously published results from the broad NEO community, including many results graciously shared by colleagues prior to formal publication. With this collective data set, we find the near-Earth population matches the diversity of the main-belt, with all main-belt taxonomic classes represented in our sample. Potentially hazardous asteroids (PHAs) as well as the subset of mission accessible asteroids (ΔV≤7 km/s) both appear to be a representative mix of the overall NEO population, consistent with strong dynamical mixing for the population that interacts most closely with Earth. Mars crossers, however, are less diverse and appear to more closely match the inner belt population from where they have more recently diffused. The fractional distributions of major taxonomic classes (60% S, 20% C, 20% other) appear remarkably constant over two orders of magnitude in size (10 km to 100 m), which is eight orders of magnitude in mass, though we note unaccounted bias effects enter into our statistics below about 500 m. Given the range of surface ages, including possible refreshment by planetary encounters, we are able to identify a very specific space weathering vector tracing the transition from Q- to Sq- to S-types that follows the natural dispersion for asteroid spectra mapped into principal component space. We also are able to interpret a shock darkening vector that may account for some objects having featureless spectra. Space weathering effects for C-types are complex; these results are described separately by Lantz, Binzel, DeMeo. (2018, Icarus 302, 10–17). Independent correlation of dynamical models with taxonomic classes map the escape zones for NEOs to main-belt regions consistent with well established heliocentric compositional gradients. We push beyond taxonomy to interpret our visible plus near-infrared spectra in terms of the olivine and pyroxene mineralogy consistent with the H, L, and LL classes of ordinary chondrites meteorites. Correlating meteorite interpretations with dynamical escape region models shows a preference for LL chondrites to arrive from the ν6 resonance and H chondrites to have a preferential signature from the mid-belt region (3:1 resonance). L chondrites show some preference toward the outer belt, but not at a significant level. We define a Space Weathering Parameter as a continuous variable and find evidence for step-wise changes in space weathering properties across different planet crossing zones in the inner solar system. Overall we hypothesize the relative roles of planetary encounters, YORP spin-up, and thermal cycling across the inner solar system. © 2018 Elsevier Inc. All rights reserved. This manuscript version is made available under the CC-BY-NC-ND 4.0 license http://creativecommons.org/licenses/by-nc-nd/4.0/ 1. Introduction Near-Earth objects (NEOs) are our planet's closest neighbors in space, simultaneously providing tantalizing opportunities for advancing scientific knowledge of our solar system, beckoning as exploration and resource utilization destinations, while at the same time threatening civilization by their potential for catastrophic impacts. Telescopic characterization is a key component for advancing all aspects of NEO understanding for both science and planetary protection. In this work we concentrate on the spectral (color) characterization of NEOs as a step toward interpreting their compositions and origins, exploration potential, and hazard assessment. We present the results of a long-term collaborative partnership that we call the MIT-Hawaii Near- Earth Object Spectroscopic Survey (abbreviated MITHNEOS; myth-neos). Researchers Fig. 1. Inner solar system position of all MITHNEOS targets at the time of their spectral measurement (geocentric X, Y coordinates in astronomical units [AU]). Each panel shows a factor of 10 closer view near Earth's location at the axes origin. Circle size depicts the estimated diameter of each object according to the scale at left for each panel. Shading scale indicates measured or inferred albedo according to taxonomic class. at the Massachusetts Institute of Technology (MIT) served as the 750 objects are contributed by this study, where Fig. 1 depicts their organizational leaders with the University of Hawaii supporting the staffing geocentric viewing geometry on their date of measurement. The majority of and operations for the NASA Infrared Telescope Facility on Mauna Kea. While these new spectral data were obtained using the instrument “SpeX” (Rayner immediate release of the spectral measurements for open use by the scientific et al., 2003) on the 3-meter NASA Infrared Telescope Facility (IRTF) located community has been a central tenet of the survey's operation since inception, on Mauna Kea, Hawaii. As has been long documented (e.g. Gaffey et al., formal systematic classification and interpretive analysis of the data set en 1993), the capability to reveal and measure spectral characteristics of masse has been forestalled pending accumulation of a sizeable sample for absorption bands present near 1and 2-microns provides a highly diagnostic statistically robust investigation. tool for distinguishing taxonomic classes and for enabling follow-on steps of We begin with a discussion of the definitions we use for describing the NEO compositional interpretation. We operated the SpeX instrument in its low population. In Section 2 we describe the survey methods for our observations resolution mode allowing the simultaneous collection of photons spanning and outline our tabulation of results. We also describe how complementary the wavelength range of 0.8–2.5 µm. About fifty of the new measurements data sets from the literature have been incorporated as an augmentation to covering the same near-infrared wavelength range were obtained with the the tabulation, noting our indebtedness to members of the planetary 6.5 m Baade Telescope at the Magellan Observatory in Las Campanas, Chile, using the FIRE (Folded-port InfraRed Echellette) instrument described by astronomy community who very generously made available in digital form Simcoe et al. (2013). Magellan observing and reductions are detailed by published (and in some cases unpublished) measurements supporting the Binzel et al. (2015), noting that we employed essentially identical completeness of this analysis. Our tabulation in Section 3 and Appendix II observation and reduction techniques for the two telescopic systems. endeavors to fully attribute all of these sources.
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