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28 results on '"Dalle Ore, Cristina M."'

2. Cryovolcanic flooding in Viking Terra on Pluto

Author

Cruikshank, Dale P., Dalle Ore, Cristina M., Scipioni, Francesca, Beyer, Ross A., White, Oliver L., Moore, Jeffrey M., Grundy, William M., Schmitt, Bernard, Runyon, Kirby D., Keane, James T., Robbins, Stuart J., Stern, S. Alan, Bertrand, Tanguy, Beddingfield, Chloe B., Olkin, Catherine B., Young, Leslie A., Weaver, Harold A., and Ennico, Kimberly

Published
2021
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3. The distribution of H2O, CH3OH, and hydrocarbon-ices on Pluto: Analysis of New Horizons spectral images

Author

Cook, Jason C., Dalle Ore, Cristina M., Protopapa, Silvia, Binzel, Richard P., Cruikshank, Dale P., Earle, Alissa, Grundy, William M., Ennico, Kimberly, Howett, Carly, Jennings, Donald E., Lunsford, Allen W., Olkin, Catherine B., Parker, Alex H., Philippe, Sylvain, Reuter, Dennis, Schmitt, Bernard, Singer, Kelsi, Stansberry, John A., Stern, S. Alan, Verbiscer, Anne, Weaver, Harold A., Young, Leslie A., Hanley, Jennifer, Alketbi, Fatima, Thompson, Garrett L., Pearce, Logan A., Lindberg, Gerrick E., and Tegler, Stephen C.

Published
2019
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4. Recent cryovolcanism in Virgil Fossae on Pluto

Author

Cruikshank, Dale P., Umurhan, Orkan M., Beyer, Ross A., Schmitt, Bernard, Keane, James T., Runyon, Kirby D., Atri, Dimitra, White, Oliver L., Matsuyama, Isamu, Moore, Jeffrey M., McKinnon, William B., Sandford, Scott A., Singer, Kelsi N., Grundy, William M., Dalle Ore, Cristina M., Cook, Jason C., Bertrand, Tanguy, Stern, S. Alan, Olkin, Catherine B., Weaver, Harold A., Young, Leslie A., Spencer, John R., Lisse, Carey M., Binzel, Richard P., Earle, Alissa M., Robbins, Stuart J., Gladstone, G. Randall, Cartwright, Richard J., and Ennico, Kimberly

Published
2019
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7. Analysis of Charon’s spectrum at 2.21-μm from New Horizons/LEISA and Earth-based observations

Author

Cook, Jason C., primary, Protopapa, Silvia, additional, Dalle Ore, Cristina M., additional, Cruikshank, Dale P., additional, Grundy, William M., additional, Lisse, Carey M., additional, Schmitt, Bernard, additional, Verbiscer, Anne, additional, Singer, Kelsi N., additional, Spencer, John, additional, Stern, S. Alan, additional, and Weaver, Harold A., additional

Published
2023
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9. Pluto: Fluidized Transport of Tholins by Heating of the Subsurface

Author

Cruikshank, Dale P, Spohrer, Steven, Grundy, William M, Moore, Jeffrey M, Umurhan, Orkan M, White, Oliver L, Beyer, Ross A, Dalle Ore, Cristina M, Stern, S. A, Young, Leslie, Weaver, Harold A, Olkin, Catherine, and Ennico, Kimberly

Subjects
Lunar And Planetary Science And Exploration
Abstract

New Horizons images of Pluto show evidence of the transport of the colored non-ice component across the surface, with substantial accumulations in some areas of low elevation. The non-ice component is presumed to be tholin produced in the atmosphere as a precipitating aerosol, in the surface ices by photolysis or radiolysis, or both. We model the surface layer of N2 ice with varying amounts of incorporated tholin particles to explore the heating within the ice that occurs by the solid-state greenhouse effect. We find that in plausible models of the contaminated N2 surface ice the triple point temperature (63.15K) is reached at a depth of approximately less than 1m. At that depth the confining pressure of the ice column is much less than the triple point pressure (12.52 kPa), so N2 should convert to the gas phase, exerting pressure on the overburden. When the gas pressure exceeds the strength of the confining ice, a breakout on the surface will occur, fluidizing fragments of ice and its contaminants that are then free to flow downhill, rafted on entrained gas, similar in some ways to the pyroclastic volcanic phenomenon known as nuée ardente. The digital elevation map of Pluto made from stereo images shows some surface regions that may have been stripped of the N2 layer, exposing H2O ice (presumed to be bedrock) below, with a corresponding accumulation of dark material that was that was the previously entrained particulate tholin. Accumulations of tholin are found associated with some of the fossae, and some cover preexisting topography to depths of up to a few hundred meters.

Published
2017

10. Organic Molecules On the Surfaces of Iapetus and Phoebe

Author

Pendleton, Yvonne J, Dalle Ore, Cristina M, Clark, Roger N, and Cruikshank, Dale P

Subjects
Instrumentation And Photography, Lunar And Planetary Science And Exploration
Abstract

Absorption bands of both aliphatic and aromatic organic molecules are found in the reflectance spectra of Saturn satellites Iapetus, Phoebe, and Hyperion obtained with the Cassini Visible-Infrared Mapping Spectrometer (VIMS). The VIMS data do not fully resolve the individual bands of C-H functional groups specific to particular molecules, but instead show absorption envelopes representing blended clusters of the bands of aromatic (approximately 3.28 microns) and aliphatic (approximately 3.4 microns) hydrocarbons known in spectra of interstellar dust. In Cruikshank et al. (2014), we matched components of the unresolved hydrocarbon band envelopes with clusters of bands of a range of functional groups in specific types of organic compounds (e.g., normal and N-substituted polycyclic aromatic hydrocarbons, olefins, cycloalkanes, and molecules with lone-pair interactions of N and O with CH3+). In the work reported here, we revisit the spectra of Iapetus and Phoebe using VIMS data processed with improved radiometric and wavelength calibration (denoted RC19). The band envelopes of both aromatic and aliphatic hydrocarbons are now more clearly defined, corroborating the provisional assignment of specific classes of molecules in Cruikshank et al. 2014, but permitting a more reliable quantitative assessment of the relative contributions of those classes, and a revision to the earlier estimate of the ratio of the abundances of aromatic to aliphatic molecules.

Published
2017

11. Amorphous and Crystalline H20 Ice at Rhea's Inktomi Crater

Author

Lewis, Emma M, Dalle Ore, Cristina M, Cruikshank, Dale P, and White, Oliver L

Subjects
Lunar And Planetary Science And Exploration
Abstract

We present the analysis of Cassini spectral data from spectral mapping of Saturnian icy moons Dione and Rhea, to investigate possible effects of impact crater formation on the relative abundances of crystalline and amorphous water ice in the moons' ice crusts. Both moons display morphologically young ray craters as well as older craters. Possible changes in ice properties due to crater formation are conjectured to be more visible in younger craters, and as such Rhea's well imaged ray crater Inktomi is analysed, as are older craters for comparison. We used data from Cassini's Visual and Infrared Mapping Spectrometer (VIMS). For each pixel in the VIMS maps, spectral data were extracted in the near-infrared range (1.75 micrometers less than lambda less than 2.45 micrometers). Analysis was begun by fitting a single Gaussian to the peak in absorption at 2.0 micrometers, which was then subtracted from the data, leaving residuals with a minimum on either side of the original 2.0-micrometers band. The spectra of the individual spatial pixels were then clustered by the differences between these minima, which are sensitive to changes in both ice grain size and crystallinity. This yielded preliminary maps which approximated the physical characteristics of the landscape and were used to identify candidates for further analysis. Spectra were then clustered by the properties of the 1.5-micrometers band, to divide the map into regions based on inferred grain size. For each region, the predicted differences in minima from the Gaussian residuals, over a range of crystallinities, were calculated based on the found grain sizes. This model was used to find the crystallinity of each pixel via grain size and characteristics of the residual function. Preliminary results show a greater degree of crystallization of young crater interiors, particularly in Rhea's ray crater Inktomi, where ice showed crystalline ice abundances between 33 percent and 61 percent. These patterns in ice crystallization are possibly attributable to increased heat generated during crater formation.

Published
2014

12. Dione’s Wispy Terrain: A Cryovolcanic Story?

Author

Dalle Ore, Cristina M., primary, Long, Christopher J., additional, Nichols-Fleming, Fiona, additional, Scipioni, Francesca, additional, Rivera Valentín, Edgard G., additional, Lopez Oquendo, Andy J., additional, and Cruikshank, Dale P., additional

Published
2021
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14. Search for the 3.4-[micro]m C-H spectral bands on low-albedo asteroids

Author

Cruikshank, Dale P., Geballe, Thomas R., Owen, Tobias C., Dalle Ore, Cristina M., Roush, Ted L., Brown, Robert H., and Lewis, John H.

Subjects
Asteroids -- Analysis, Astronomical research -- Evaluation, Astronomical spectroscopy -- Usage, Infrared spectroscopy -- Usage, Chemistry, Organic -- Usage, Hydrocarbons -- Observations, Astronomy, Earth sciences
Abstract

A report of the detection of the C-H hydrocarbon band complex at 3.4/[micro]m in an asteroid spectrum, by D. P. Cruikshank and R. H. Brown (1987, Science 238, 183-184) is not confirmed by recent data of higher quality. Spectra of the same asteroid and six other low-albedo asteroids do not show this feature, which if present would indicate the presence of hydrocarbons and might link these asteroids with certain classes of carbonaceous meteorites. Key Words: asteroid composition; infrared observations; organic chemistry; spectroscopy; asteroid surfaces.

Published
2002

15. Constraints on the composition of Trojan asteroid 624 Hektor

Author

Cruikshank, Dale P., Dalle Ore, Cristina M., Roush, Ted L., Geballe, Thomas R., Owen, Tobias C., de Bergh, Catherine, Cash, Michele D., and Hartmann, William K.

Subjects
Asteroids -- Models, Astrogeology -- Research, Astronomy, Earth sciences
Abstract

We present a composite spectrum of Trojan asteroid 624 Hektor, 0.3-3.6 [micro]m, and models computed for the full wavelength range with the Hapke scattering theory. The data show that there is no discernible 3-[micro]m absorption band. Such a band would indicate the presence of OH- or [H.sub.2]O-bearing silicate minerals, or macromolecular carbon-rich organic material of the kind seen on the low-albedo hemisphere of Saturn's satellite Iapetus. The absence of spectral structure is itself indicative of the absence of the nitrogen-rich tholins (which show a distinctive absorption band attributed to N-H). The successful models in this study all incorporate magnesium-rich pyroxene (Mg, Fe Si[O.sub.3]), which satisfactorily matches the red color of Hektor. Pyroxene is a mafic mineral common in terrestrial and lunar lavas, and is also identified in Main Belt asteroid spectra. An upper limit to the amount of crystalline [H.sub.2]O ice (30-[micro]m grains) in the surface layer of Hektor accessible to near-infrared remote sensing observations is 3 wt%. The upper limit for serpentine, as a representative of hydrous silicates, is much less stringent, at 40%, based on the shape of the spectral region around 3 [micro]m. Thus, the spectrum at 3 [micro]m does not preclude the presence of a few weight percent of volatile material in the uppermost surface layer of Hektor. Below this 'optical' surface that our observations probe, any amount of [H.sub.2]O ice and other volatile-rich materials might exist. All of the models we calculated require a very low-albedo, neutral color material to achieve the low geometric albedo that matches Hektor; we use elemental carbon. If elemental carbon is present on Hektor, it could be of organic or inorganic origin. By analogy, other D-type asteroids could achieve their red color, low albedo, and apparent absence of phyllosilicates from compositions similar to the models

Published
2001

16. Disk-resolved Photometric Properties of Pluto and the Coloring Materials across its Surface

Author

Protopapa, Silvia, primary, Olkin, Cathy B., additional, Grundy, Will M., additional, Li, Jian-Yang, additional, Verbiscer, Anne, additional, Cruikshank, Dale P., additional, Gautier, Thomas, additional, Quirico, Eric, additional, Cook, Jason C., additional, Reuter, Dennis, additional, Howett, Carly J. A., additional, Stern, Alan, additional, Beyer, Ross A., additional, Porter, Simon, additional, Young, Leslie A., additional, Weaver, Hal A., additional, Ennico, Kim, additional, Dalle Ore, Cristina M., additional, Scipioni, Francesca, additional, and Singer, Kelsi, additional

Published
2020
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17. Geologic Landforms and Chronostratigraphic History of Charon as Revealed by a Hemispheric Geologic Map

Author

Robbins, Stuart J., primary, Beyer, Ross A., additional, Spencer, John R., additional, Grundy, William M., additional, White, Oliver L., additional, Singer, Kelsi N., additional, Moore, Jeffrey M., additional, Dalle Ore, Cristina M., additional, McKinnon, William B., additional, Lisse, Carey M., additional, Runyon, Kirby, additional, Beddingfield, Chloe B., additional, Schenk, Paul, additional, Umurhan, Orkan M., additional, Cruikshank, Dale P., additional, Lauer, Tod R., additional, Bray, Veronica J., additional, Binzel, Richard P., additional, Buie, Marc W., additional, Buratti, Bonnie J., additional, Cheng, Andrew F., additional, Linscott, Ivan R., additional, Reuter, Dennis C., additional, Showalter, Mark R., additional, Young, Leslie A., additional, Olkin, Catherine B., additional, Ennico, Kimberly S., additional, Weaver, Harold A., additional, and Stern, S. Alan, additional

Published
2019
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18. Water Ice on Triton

Author

Cruikshank, Dale P., Schmitt, Bernard, Roush, Ted L., Owen, Tobias C., Quirico, Eric, Geballe, Thomas R., de Bergh, Catherine, Bartholomew, Mary Jane, Dalle Ore, Cristina M., Douté, Sylvain, and Meier, Roland

Published
2000
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19. Methanol On The Extra-red Tnos And Centaurs

Author

Barucci, Maria Antonella, Dalle Ore, Cristina M., Emery, Joshua P., Merlin, Frédéric, Cruikshank, Dale P., Perna, Davide, de Bergh, Catherine, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2012

20. (90377) Sedna: Heterogeneous Surface Composition

Author

Dalle Ore, Cristina M., Barucci, Maria Antonella, Alvarez-Candal, Alvaro, de Bergh, Catherine, Merlin, Frédéric, Dumas, Christophe, Cruikshank, Dale P., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2010

21. Composition of KBO (50000) Quaoar

Author

Dalle Ore, Cristina M., Barucci, Maria Antonella, Emery, Joshua P., Cruikshank, Dale P., Dalle Ore, L. V., Merlin, Frédéric, Alvarez-Candal, Alvaro, de Bergh, Catherine, Perna, Davide, Fornasier, Sonia, Mastrapa, Rachel M. E., Dotto, Elisabetta, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2009

22. Nitrogen and Methane Ices on the Surface of Sedna ?

Author

Barucci, Maria Antonella, Cruikshank, Dale P., Dotto, Elisabetta, Merlin, Frédéric, Poulet, François, Dalle Ore, Cristina M., Fornasier, Sonia, de Bergh, Catherine, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2005

23. A spectroscopic study of the surfaces of Saturn's large satellites: H2O ice, tholins, and minor constituents

Author

Cruikshank, Dale P., Owen, Tobias C., Dalle Ore, Cristina M., Geballe, Thomas R., Roush, Ted L., de Bergh, Catherine, Sandford, Scott A., Poulet, François, Benedix, Gretchen K., Emery, Joshua P., SETI Institute, NASA Ames Research Center, Moffett Field, Institute for Astronomy, University of Hawaii, Gemini Observatory, Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Department of Earth and Planetary Sciences, Washington University, and Washington University in Saint Louis (WUSTL)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; We present spectra of Saturn's icy satellites Mimas, Enceladus, Tethys, Dione, Rhea, and Hyperion, 1.0-2.5 mum, with data extending to shorter (Mimas and Enceladus) and longer (Rhea and Dione) wavelengths for certain objects. The spectral resolution ( R=lambda/Deltalambda) of the data shown here is in the range 800-1000, depending on the specific instrument and configuration used; this is higher than the resolution ( R=225 at 3 mum) afforded by the Visual-Infrared Mapping Spectrometer on the Cassini spacecraft. All of the spectra are dominated by water ice absorption bands and no other features are clearly identified. Spectra of all of these satellites show the characteristic signature of hexagonal H 2O ice at 1.65 mum. We model the leading hemisphere of Rhea in the wavelength range 0.3-3.6 mum with the Hapke and the Shkuratov radiative transfer codes and discuss the relative merits of the two approaches to fitting the spectrum. In calculations with both codes, the only components used are H 2O ice, which is the dominant constituent, and a small amount of tholin (Ice Tholin II). Tholin in small quantities (few percent, depending on the mixing mechanism) appears to be an essential component to give the basic red color of the satellite in the region 0.3-1.0 mum. The quantity and mode of mixing of tholin that can produce the intense coloration of Rhea and other icy satellites has bearing on its likely presence in many other icy bodies of the outer Solar System, both of high and low geometric albedos. Using the modeling codes, we also establish detection limits for the ices of CO 2 (a few weight percent, depending on particle size and mixing), CH 4 (same), and NH 4OH (0.5 weight percent) in our globally averaged spectra of Rhea's leading hemisphere. New laboratory spectral data for NH 4OH are presented for the purpose of detection on icy bodies. These limits for CO 2, CH 4, and NH 4OH on Rhea are also applicable to the other icy satellites for which spectra are presented here. The reflectance spectrum of Hyperion shows evidence for a broad, unidentified absorption band centered at 1.75 mum.

Published
2005

28. Search for the 3.4-μm C–H Spectral Bands on Low-Albedo Asteroids

Author

Cruikshank, Dale P., Geballe, Thomas R., Owen, Tobias C., Dalle Ore, Cristina M., Roush, Ted L., Brown, Robert H., and Lewis, John H.

Subjects
*ASTEROIDS, *ALBEDO, *HYDROCARBONS
Abstract

A report of the detection of the C–H hydrocarbon band complex at 3.4 μm in an asteroid spectrum, by D. P. Cruikshank and R. H. Brown (1987, Science238, 183–184) is not confirmed by recent data of higher quality. Spectra of the same asteroid and six other low-albedo asteroids do not show this feature, which if present would indicate the presence of hydrocarbons and might link these asteroids with certain classes of carbonaceous meteorites. [Copyright &y& Elsevier]

Published
2002
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