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BENNU from OSIRIS-Rex APPROACH and PRELIMINARY SURVEY OBSERVATIONS 50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1956.pdf VNIR AND TIR SPECTRAL CHARACTERISTICS OF (101955) BENNU FROM OSIRIS-REx APPROACH AND PRELIMINARY SURVEY OBSERVATIONS. V. E. Hamilton1, A. A. Simon2, P. R. Christensen3, D. C. Reuter2, D. N. Della Giustina4, J. P. Emery5, R. D. Hanna6, E. Howell4, H. H. Kaplan1, B. E. Clark7, B. Rizk4, D. S. Lauretta4, and the OSIRIS-REx Team, 1Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302 ([email protected]), 2NASA Goddard Space Flight Center, Greenbelt, MD, 3School of Earth & Space Ex- ploration, Arizona State University, Tempe, AZ 85287, 4Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, 5Dept. Earth & Planetary Science, University of Tennessee, Knoxville, TN 37996, 6University of Texas, Austin, TX, 78712, 7Dept. Physics & Astronomy, Ithaca College, Ithaca, NY 14850. Introduction: Visible to near infrared (VNIR) and generation and application of a photometric model, thermal infrared (TIR) spectrometers onboard the Ori- production of bolometric Bond albedo, reflectance gins, Spectral Interpretation, Resource Identification, factor spectra, and the calculation of spectral indices. Security–Regolith Explorer (OSIRIS-REx) spacecraft For OTES, this includes deriving emissivity spectra have revealed evidence of hydrated phases across the and temperature information with emissivity being an surface of asteroid (101955) Bennu. Here we describe input into a linear least squares mixing model and a spectral features identified in data collected during the spectral parameter representing the presence of surface Approach and Preliminary Survey phases of the mis- dust. sion, from 2 November 2018 to 17 December 2018. Observation sequences: Unlike either a true or- Background: The primary objective of the biter or fly-by mission, OSIRIS-REx has many differ- OSIRIS-REx mission is to collect and return to Earth a ent mission phases that incorporate different observing pristine sample of carbonaceous material from the strategies to best characterize Bennu and aid in the near-Earth (and potentially hazardous) asteroid Bennu selection of a sample site. [1]. To aid in asteroid characterization and sample site Spectroscopy in the Approach phase. Early Ap- selection, OSIRIS-REx carries a camera suite proach phase observations (2 to 9 November 2018) (OCAMS), a laser altimeter (OLA), and two hyper- were aimed at collecting disk-integrated spectral data, spectral spectrometers (see next section), along with a both to obtain an initial view of Bennu’s composition student-led x-ray imaging spectrometer (REXIS). and for comparison with ground-based data. Spectra OSIRIS-REx spectrometers. The OSIRIS-REx Visi- were acquired over multiple days, with two days being ble and Infrared Spectrometer (OVIRS) is a point spec- optimized for the OVIRS FOV and pointing (2 to 3 trometer covering the wavelength range from 0.4 to 4.3 November), and two later days being optimized for the µm with a 4-mrad field of view (FOV) and a spectral OTES FOV and pointing (5 and 9 November). A set of sampling of 2 nm from 0.392 to 2.4 µm, and 5 nm contingency observations was also acquired on 8 No- from 2.4 to 4.3 µm [2, 3]. OVIRS is a derivative of the vember. Both spectrometers acquired data on all ob- New Horizons Ralph instrument. The OSIRIS-REx servation days. On 2 December, during late Approach, Thermal Emission Spectrometer (OTES) is a point both spectrometers acquired “ride-along” data during a spectrometer that measures from ~100 to 1650 cm-1 sequence optimized for OCAMS imaging. (~5.5 to 100 µm), with an 8-mrad FOV and a spectral Spectroscopy during Preliminary Survey. OSIRIS- sampling of 8.66 cm-1 [4]. The OTES instrument is a REx arrived at Bennu on 3 December 2018, marking derivative of the Mars Exploration Rovers Mini-TES the end of the Approach phase and the beginning of the and Mars Global Surveyor TES. Although the OVIRS Preliminary Survey phase. All spectral observations FOV is within that of OTES, the two are not precisely obtained during Preliminary Survey were acquired as co-boresighted. part of imaging sequences aimed at characterizing Data processing: The OSIRIS-REx science team is Bennu’s polar and equatorial regions prior to orbit in- organized around science theme working groups, and sertion (which occurred 31 December 2018). As such, the Spectral Analysis Working Group (SAWG) is re- these observations were not tailored for spectroscopy sponsible for analyzing and integrating the results from in terms of the acquisition of calibration data, instru- OVIRS and OTES. To that end, the SAWG has devel- ment pointing, or local time. Spectral data were ac- oped an automated data processing pipeline to produce quired by OTES on all days, and by OVIRS on a sub- quicklook science (Level 3) products that are generated set of days, between 4 and 17 December. immediately after the data are downlinked and con- Preliminary Results: Approach and Preliminary verted to calibrated radiance. For OVIRS data in all Survey data have been invaluable for giving the mission phases, this includes removal of the thermal OVIRS and OTES teams a wide range of observing tail and conversion to I/F, and for mapping phases, sequences that allow for improvements to the calibra- 50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1956.pdf tion of both data sets and for revealing exciting in- with a range of particle sizes that do not vary spatially sights about Bennu early in the mission. at scales down to 80 m. Analysis of Bennu’s surface OVIRS results. OVIRS disk-integrated Approach geological characteristics indicates that it is a rubble data from 2 November 2018 reveal a visible to near- pile that has experienced recent dynamical processes infrared spectrum that is remarkably similar to the [8]. Redistribution of material [e.g., 9] may help ex- ground-based data of [5], having a blue (negative) plain the apparent spatial uniformity of the spectral/ slope and no visible features above the level of the compositional signatures at the scales observed thus noise. A 0.55-µm feature observed in OCAMS data [6] far, even as smaller-scale variability in albedo and geo- is not observed, but this is likely attributable to the logic features are observed [6]. Key questions that will whole-disk nature of the OVIRS observations, where be addressed with these future observations include the the FOV was only ~40% filled as compared to the spa- heterogeneity of surface compositions at higher spatial tially resolved OCAMS imagery. OVIRS data that will scales and the degree of aqueous alteration experienced be acquired during the Detailed Survey mission phase by Bennu’s parent body based on details of mineral may have sufficient spatial resolution (~40 m/spot) and distribution, abundance, and composition (e.g., Mg/Fe signal-to-noise to detect this feature. At longer wave- proportions in phyllosilicates and abundance of mag- lengths, an unambiguous 2.74-µm band is present, netite). consistent with the presence of hydrated silicates, in- Acknowledgements: This material is based upon cluding those contained in petrologic type 1, 1/2, and 2 work supported by NASA under Contract NN- carbonaceous chondrites. There is no apparent rota- M10AA11C issued through the New Frontiers Pro- tional variation in the OVIRS whole-disk spectra. gram. OTES results. OTES disk-integrated spectra require References: [1] Lauretta, D. S. et al. (2017) SSR, special calibration due to the FOV of the instrument 212, 925-984. [2] Reuter, D. C. et al. (2018) SSR, 214, not being fully filled. However, spatially resolved 54. [3] Simon A. A. et al. (2018) Remote Sens., 10, spectra (~80 m/spot) acquired during one of the Pre- 1486. [4] Christensen, P. R. et al. (2018), SSR, 214, 87. liminary Survey equatorial passes on 13 December [5] Clark, B. E. et al. (2011) Icarus, 216, 462-475. [6] 2018 reveal a spectrum with low contrast (2%) and a Rizk, B. et al. (2019) LPS L, Abstract #1717. [7] spectral shape that is broadly consistent with carbona- Hamilton, V. E. et al. (2018) LPS XLIX, Abstract ceous chondrites in the CI/CM groups, which fall into #1753, 2018. [8] Walsh, K. et al. (2019) LPS L, Ab- petrologic types 1, 1/2, and 2, indicating aqueous alter- stract #1898. [9] Scheeres, D. et al. (2019) LPS L, Ab- ation. A single spectral feature at 440 cm-1 (~22.7 µm) stract #1496. is particularly consistent with a volumetrically domi- nant phyllosilicate component in carbonaceous chon- drites [7]. The OTES spectra do not show evidence of abundant pyroxene or olivine, but features at 555 and 346 cm-1 are attributable to magnetite. This detection may support the proposed detection of a feature tenta- tively attributed to magnetite at ~0.55 µm in one of the darkest regions of the asteroid [6]. Derivation of modal mineralogy and the refinement of the degree of alter- ation. A relatively broad silicate stretching band(s) as compared to whole-rock spectra, combined with a lack of strong transparency features at >1110 cm-1 (<9 µm), is potentially consistent with a mixture of relatively fine (<125 µm) and coarse (>125 µm) particles, includ- ing cobbles and rocks. There is no discernible variation in the OTES spectra at these spatial scales. Summary and Ongoing Analysis: Spectroscopic results from visible through thermal infrared wave- lengths are highly complementary and reveal that the surface of Bennu not only exhibits evidence of hydrat- ed silicates, but appears to be dominated volumetrical- ly by such minerals and is consistent with a composi- tion similar to aqueously altered CI and CM carbona- ceous chondrites. The spectral datasets are consistent .
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