The NEO (175706) 1996 FG3 in the 2–4μm spectral region: Evidence for an aqueously altered surface

Rivkin, A. S.; Howell, E. S.; Vervack, R. J.; Magri, C.; Nolan, M. C.; Fernández, Y. R.; Cheng, A. F.; Barucci, Maria Antonietta; Michel, Patrick

doi:10.1016/j.icarus.2012.12.016

Cited by 19 publications

(23 citation statements)

References 38 publications

(36 reference statements)

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“…Moreover, nonterrestrial L-proteinogenic amino acid excesses have been detected in this meteorite, strengthening the hypothesis that primitive minor bodies could have delivered enantiomerically enriched amino acids to the early Earth that could have triggered the emergence of life (Glavin et al 2012). If confirmed, a link with the Tagish Lake meteorite would be fascinating, and would confirm the very primitive nature of 1996 FG3, in agreement with the results by Rivkin et al (2013).…”

Section: Spectral Analysis and Discussionsupporting

confidence: 84%

“…4), in the form of pressed powder (grain size <125 µm). This association is strengthened by the recent detection of the 3 µm feature in the spectrum of 1996 FG3 (Rivkin et al 2013). Indeed, though deeper and different in shape, a 3 µm absorption band is present also in the spectrum of the Tagish Lake meteorite (Hiroi et al 2001).…”

Section: Spectral Analysis and Discussionmentioning

confidence: 86%

“…Nearinfrared spectra obtained by several authors (de León et al 2011;Binzel et al 2012;Walsh et al 2012a) are still consistent within the C-complex, but exhibit significant differences in the spectral slope. Observations in the 3 µm spectral region (Rivkin et al 2013) showed an absorption band of ∼5-10%, a diagnostic for hydrated/hydroxylated minerals on the surface. This indicates that the thermal heating was not intense enough to reach dehydrating temperatures, and that relatively fresh areas exist on the surface of 1996 FG3.…”

Section: +31mentioning

confidence: 99%

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Ultraviolet to near-infrared spectroscopy of the potentially hazardous, low delta-V asteroid (175706) 1996 FG3

Perna

Dotto

Barucci

et al. 2013

A&A

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Context. Primitive near-Earth asteroids (NEAs) are important subjects of study for current planetary research. Their investigation can provide crucial information on topics such as the formation of the solar system, the emergence of life, and the mitigation of the risk of asteroid impact. Sample return missions from primitive asteroids have been scheduled or are being studied by space agencies, including the MarcoPolo-R mission selected for the assessment study phase of ESA M3 missions. Aims. We want to improve our knowledge of the surface composition and physical nature of the potentially hazardous, low delta-V asteroid (175706) 1996 FG3, backup target of MarcoPolo-R. This intriguing object shows an as-yet unexplained spectral variability. Methods. We performed spectroscopic observations of 1996 FG3 using the visible spectrograph DOLORES at the Telescopio Nazionale Galileo (TNG), and the UV-to-NIR X-Shooter instrument at the ESO Very Large Telescope (VLT). Results. We find featureless spectra and we classify 1996 FG3 as a primitive Xc-type in the Bus-DeMeo taxonomy. Based on literature comparison, we confirm the spectral variability of this object at near-infrared (NIR) wavelengths, and find that spectral variations exist also for the visible spectral region. Phase reddening cannot explain such variations. Obtained with the same observational conditions for the whole 0.3-2.2 µm range, our X-Shooter spectrum allowed a proper comparison with the RELAB meteorite database. A very good fit is obtained with the very primitive C2 Tagish Lake carbonaceous chondrite (pressed powder), confirming 1996 FG3 as a suitable target for a sample return mission from primitive NEAs. Conclusions. We hypothesize a compacted/cemented surface for 1996 FG3, like that observed by the Hayabusa mission on (25143) Itokawa, with the possible presence of regions showing different degrees of surface roughness. This variegation could be related to the binary nature of 1996 FG3, but to check this hypothesis further observations are necessary.

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Section: Spectral Analysis and Discussionsupporting

confidence: 84%

Section: Spectral Analysis and Discussionmentioning

confidence: 86%

Section: +31mentioning

confidence: 99%

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Ultraviolet to near-infrared spectroscopy of the potentially hazardous, low delta-V asteroid (175706) 1996 FG3

Perna

Dotto

Barucci

et al. 2013

A&A

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“…However, absorptions have been found on two NEOs, 1992 UY4 (Volquardsen et al, 2007) and 1996 FG3 (Rivkin et al, 2013a). The band shapes for these objects are not as well-measured as those of brighter asteroids, but 1996 FG3 appears to have a Pallas-type/sharp band.…”

Section: 4mentioning

confidence: 95%

“…While beyond the scope of this chapter, details of these models can be found in Lebofsky and Spencer (1989) and Harris et al (2002), and Delbo et al in this volume. Thermal flux can also, in some circumstances, "fill in" an absorption band. Because these circumstances can arise in the 3-µm spectral region, of particular interest for hydrated asteroid studies, here we discuss those circumstances and the consequences for astronomical observations following the logic presented by Rivkin et al (2013a) and Clark (1979). In an absorption band, the emissivity increases relative to that outside the band because the reflectance decreases in the band.…”

Section: 2mentioning

confidence: 98%

Astronomical Observations of Volatiles on Asteroids

Rivkin¹,

Campins²,

Emery³

et al. 2015

Asteroids IV

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We have long known that water and hydroxyl are important components in meteorites and asteroids. However, in the time since the publication of Asteroids III, evolution of astronomical instrumentation, laboratory capabilities, and theoretical models have led to great advances in our understanding of H 2 O/OH on small bodies, and spacecraft observations of the Moon and Vesta have important implications for our interpretations of the asteroidal population. We begin this chapter with the importance of water/OH in asteroids, after which we will discuss their spectral features throughout the visible and near-infrared. We continue with an overview of the findings in meteorites and asteroids, closing with a discussion of future opportunities, the results from which we can anticipate finding in Asteroids V. Because this topic is of broad importance to asteroids, we also point to relevant in-depth discussions elsewhere in this volume.1 Water ice sublimation and processes that create, incorporate, or deliver volatiles to the asteroid belt Accretion/Solar system formation 1.1The concept of the "snow line" (also known as "water-frost line") is often used in discussing the water inventory of small bodies in our solar system. The snow line is the heliocentric distance at which water ice is stable enough to be accreted into planetesimals. The placement of the snow line has varied in different models. A location just inside Jupiter helps explain the greater mass of the giant planets as they accrete a larger fraction of the mass in the solar nebula. Although the location of the snow line before and during planet formation is uncertain, some studies show it may have fallen within the asteroid belt (Lunine, 2006). The location of the snow line in our solar system coinciding with the asteroid belt is consistent with observations of disks around other stars (e.g., Su et al., 2013), where planetesimal rings tend to coincide with the snow line around those stars. However, it seems the relatively simple concept of a static snow line requires revisions in light of new results on several fronts. For instance, the snow line likely moved with time as the Sun's luminosity changed early in solar system history (e.g., Martin and Livio, 2012). Even though there is no agreement on the details of planetesimal formation and growth, some models favor the growth of ~100 km-scale planetesimals directly from cm-scale pieces Cuzzi et al., 2010; for a dissenting view see Weidenschilling, 2011). Hence, the timing of those assemblies as conditions change could have a strong influence on the amount of radioactive elements present in a planetesimal's interior and on its rock-to-ice ratio, further complicating the concept of a snow line. Recent observations also point to a more complex picture. For example, the concept of an asteroid-comet continuum, where there is no clear boundary between primitive asteroids and cometary nuclei (e.g., Gounelle, 2011) is gaining support and is consistent with the intermittent cometary behavior of some main belt and near-E...

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Water in the Martian regolith from OMEGA/Mars Express

Audouard

Poulet

Vincendon

et al. 2014

J. Geophys. Res. Planets

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Here we discuss one of the current reservoirs of water on Mars, the regolith and rocks exposed at the surface. This reservoir is characterized by the presence of H 2 O-and OH-bearing phases that produce a broad absorption at a wavelength of~3 μm in near-infrared (NIR) reflectance spectra. This absorption is present in every ice-free spectrum of the Martian surface obtained thus far by orbital NIR spectrometers. We present a quantitative analysis of the global distribution of the 3 μm absorption using the Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité (OMEGA) imaging spectrometer that has been mapping the surface of Mars at kilometer scale for more than 10 years. Based on laboratory reflectance spectra of a wide range of hydrous minerals and phases, we estimate a model-dependent water content of 4 ± 1 wt % in the equatorial and midlatitudes. Surface hydration increases with latitude, with an asymmetry in water content between the Northern and Southern Hemispheres. The surface hydration is compared to various parameters (albedo, dust, geological units, time, relative humidity, atmospheric water pressure, and in situ measurements performed by Phoenix and Curiosity) to constrain the nature of the reservoir. We conclude that the nature of the surface hydration of the Martian low latitudes is not adsorbed water but rather more tightly bound water molecules and hydroxyl groups in the structure of the materials of the near-top surface. A frost-related process best explains the implementation of water into and onto the first microns of the high-latitude Martian regolith.

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The NEO (175706) 1996 FG3 in the 2–4μm spectral region: Evidence for an aqueously altered surface

Cited by 19 publications

References 38 publications

Ultraviolet to near-infrared spectroscopy of the potentially hazardous, low delta-V asteroid (175706) 1996 FG3

Ultraviolet to near-infrared spectroscopy of the potentially hazardous, low delta-V asteroid (175706) 1996 FG3

Astronomical Observations of Volatiles on Asteroids

Water in the Martian regolith from OMEGA/Mars Express

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