Composition of the northern regions of Vesta analyzed by the Dawn mission

Combe, Jean-Philippe; McCord, T. B.; McFadden, L. A.; Ieva, S.; Tosi, F.; Longobardo, A.; Frigeri, Alessandro; Sanctis, M. C. De; Ammannito, E.; Ruesch, O.; Palomba, E.; Fulchignoni, M.; Raymond, C. A.; Russell, C. T.

doi:10.1016/j.icarus.2015.04.026

Cited by 25 publications

(13 citation statements)

References 77 publications

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“…) or mixtures of low‐ and high‐Ca pyroxene (Combe et al. ), abuts a region of higher topography to its north, which may be the source of more coherent material exposed in its crater walls.…”

Section: Observations Of Crater Wallsmentioning

confidence: 99%

Global variations in regolith properties on asteroid Vesta from Dawn's low‐altitude mapping orbit

Denevi

Beck

Coman

et al. 2016

Meteorit & Planetary Scien

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We investigate the depth, variability, and history of regolith on asteroid Vesta using data from the Dawn spacecraft. High‐resolution (15–20 m pixel−1) Framing Camera images are used to assess the presence of morphologic indicators of a shallow regolith, including the presence of blocks in crater ejecta, spur‐and‐gully–type features in crater walls, and the retention of small (<300 m) impact craters. Such features reveal that the broad, regional heterogeneities observed on Vesta in terms of albedo and surface composition extend to the physical properties of the upper ~1 km of the surface. Regions of thin regolith are found within the Rheasilvia basin and at equatorial latitudes from ~0–90°E and ~260–360°E. Craters in these areas that appear to excavate material from beneath the regolith have more diogenitic (Rheasilvia, 0–90°E) and cumulate eucrite (260–360°E) compositions. A region of especially thick regolith, where depths generally exceed 1 km, is found from ~100–240°E and corresponds to heavily cratered, low‐albedo surface with a basaltic eucrite composition enriched in carbonaceous chondrite material. The presence of a thick regolith in this area supports the idea that this is an ancient terrain that has accumulated a larger component of exogenic debris. We find evidence for the gardening of crater ejecta toward more howarditic compositions, consistent with regolith mixing being the dominant form of “weathering” on Vesta.

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Section: Observations Of Crater Wallsmentioning

confidence: 99%

Global variations in regolith properties on asteroid Vesta from Dawn's low‐altitude mapping orbit

Denevi

Beck

Coman

et al. 2016

Meteorit & Planetary Scien

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“…This region was chosen because Olivine, a mineral indicative of deep magmatic processes, was first detected in this area [55]. This mineral is never found alone in meteorites coming from Vesta-4 [56], [57], implying the use of an algorithm able to decompose spectra as a combination of mixtures of materials.…”

Section: Discussionmentioning

confidence: 99%

Joint Anomaly Detection and Spectral Unmixing for Planetary Hyperspectral Images

Nakhostin

Clénet

Corpetti

et al. 2016

IEEE Trans. Geosci. Remote Sensing

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Abstract-Hyperspectral images are commonly used in the context of planetary exploration, especially for the analysis of the composition of planets. As several instruments have been sent throughout the Solar System, a huge quantity of data is getting available for the research community. Among classical problems in the analysis of hyperspectral images, a crucial one is unsupervised non-linear spectral unmixing, which aims at estimating the spectral signatures of elementary materials and determining their relative contribution at a sub-pixel level. While the unmixing problem is well studied for earth observation, some of the traditional problems encountered with earth images are somehow magnified in planetary exploration. Among them, large image sizes, strong non-linearities in the mixing (often different from those found in the earth images) and presence of anomalies are usually impairing the unmixing algorithms. This paper presents a new method that scales favorably with the problem posed by this analysis. It performs an unsupervised unmixing jointly with anomaly detection capacities, and has a global linear complexity. Non linearities are handled by decomposing the hyperspectral data on an overcomplete set of spectra, combined with a specific sparse projection, which guarantees the interpretability of the analysis. A theoretical study is proposed on synthetic datasets, and results are presented over the challenging 4-Vesta asteroid dataset.

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“…This type of modeling is applicable to surfaces both in the inner and the outer solar system and it is of high relevance to studies related to formation and evolutionary processes over a wide range of distances from the Sun (e.g., [56][57][58][59]).…”

Section: Modeling Of Planetary Surfacesmentioning

confidence: 99%

Planetary Spectrum Generator: An accurate online radiative transfer suite for atmospheres, comets, small bodies and exoplanets

Villanueva

Smith

Protopapa

et al. 2018

Journal of Quantitative Spectroscopy and Radiative Transfer

232

218

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We have developed an online radiative-transfer suite (https://psg.gsfc.nasa.gov) applicable to a broad range of planetary objects (e.g., planets, moons, comets, asteroids, TNOs, KBOs, exoplanets). The Planetary Spectrum Generator (PSG) can synthesize planetary spectra (atmospheres and surfaces) for a broad range of wavelengths (UV/Vis/near-IR/IR/far-IR/THz/submm/Radio) from any observatory (e.g., JWST, ALMA, Keck, SOFIA), any orbiter (e.g., ExoMars, Juno), or any lander (e.g., MSL). This is achieved by combining several state-of-the-art radiative transfer models, spectroscopic databases and planetary databases (i.e., climatological and orbital).PSG has a 3D (three-dimensional) orbital calculator for most bodies in the solar system, and all confirmed exoplanets, while the radiative-transfer models can ingest billions of spectral signatures for hundreds of species from several spectroscopic repositories. It integrates the latest radiativetransfer and scattering methods in order to compute high resolution spectra via line-by-line calculations, and utilizes the efficient correlated-k method at moderate resolutions, while for computing cometary spectra, PSG handles non-LTE and LTE excitation processes. PSG includes a realistic noise calculator that integrates several telescope / instrument configurations (e.g., interferometry, coronagraphs) and detector technologies (e.g., CCD, heterodyne detectors, bolometers). Such an integration of advanced spectroscopic methods into an online tool can greatly serve the planetary community, ultimately enabling the retrieval of planetary parameters from remote sensing data, efficient mission planning strategies, interpretation of current and future planetary data, calibration of spectroscopic data, and development of new instrument/spacecraft concepts. Number of species: 52 Number of isotopologues: 118 JPL Molecular Spectroscopy [16] Wavelength range: 2.65 µm to radio Number of lines: 888,113 Number of species: 383 CDMS Cologne Database for Molecular Spectroscopy [17] Wavelength range: 1.81 µm to radio Number of lines: 1,612,154 Number of species: 792 Exo-Transmit Opacities database [33] Wavelength range: 0.1 to 170 µm Number of spectral points: 7454 Number of temperatures: 30 (100 to 3000 K) Number of pressures: 13 (1E-9 to 1000 bar) Number of species: 30 The MPI-Mainz UV/VIS Spectral Atlas [34] UV cross-sections for O3 [35] UV cross-sections for CO2 [36] Wavelength range: 0.01 to 1 um Number of cross-sections: 70 Number of species: 22 (e.g., H2O, CH4, CO2, N2O, O3)

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Composition of the northern regions of Vesta analyzed by the Dawn mission

Cited by 25 publications

References 77 publications

Global variations in regolith properties on asteroid Vesta from Dawn's low‐altitude mapping orbit

Global variations in regolith properties on asteroid Vesta from Dawn's low‐altitude mapping orbit

Joint Anomaly Detection and Spectral Unmixing for Planetary Hyperspectral Images

Planetary Spectrum Generator: An accurate online radiative transfer suite for atmospheres, comets, small bodies and exoplanets

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