Infrared spectroscopic characterization of the low-albedo materials on Iapetus

Ore, C. M. Dalle; Cruikshank, D. P.; Clark, R. N.

doi:10.1016/j.icarus.2012.09.010

Cited by 22 publications

(4 citation statements)

References 32 publications

(52 reference statements)

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“…In addition, the relative geographic information of each spectrum is maintained in the process, and the resulting clusters can be correlated with high‐resolution geological maps previously described. This approach has been already applied for compositional interpretations of different solar system objects, for example, Mars, Iapetus, and Phobos (Dalle Ore et al, ; Marzo et al, , ; Pajola et al, ; Pinilla‐Alonso et al, ). This technique is agnostic of the physical meaning of the clusters; hence, scientific interpretation is required as part of the subsequent evaluation of the results.…”

Section: Data Set and Methodsmentioning

confidence: 99%

Mercury Hollows as Remnants of Original Bedrock Materials and Devolatilization Processes: A Spectral Clustering and Geomorphological Analysis

et al. 2018

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We perform a detailed geomorphological and compositional analysis on three craters hosting hollows located in the Victoria and Kuiper Quadrangles of Mercury. Based on Mercury Dual Imaging System data, high‐resolution detailed geomorphological mapping is provided in order to fully characterize the geological framework where hollows formed. In addition, we apply an unsupervised spectral clustering, based on a K‐mean algorithm, to separate in clusters our data sets. The comparison between the spectral and the well‐defined geomorphological units reveals a spatially coherent distribution. In particular, all hollows are uniquely identified by a well‐defined spectrum showing a wide absorption band between 0.558 and 0.828, with a possible hint of absorption toward 1 μm. Our analysis suggests that the composition of hollows may be characterized by a mixture of different minerals contributing to the absorptions found in our spectra. Indeed, sulfides alone (CaS, MnS, and MgS) cannot explain the spectrum behavior of hollows, even if the mechanism forming hollows likely involves the loss of volatiles from the surface. Hence, we have to consider bedrock‐forming material as partial responsible of the absorptions. For the studied hollows we suggest that the bedrock‐forming minerals are pyroxenes presenting transitional elements, like Cr, Ti, and Ni in substitution of Mg and/or Fe. Therefore, we suggest that the spectral characteristics of hollows are related to both remnant material produced by devolatilization process and to bedrock in which the hollows formed.

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Section: Data Set and Methodsmentioning

confidence: 99%

Mercury Hollows as Remnants of Original Bedrock Materials and Devolatilization Processes: A Spectral Clustering and Geomorphological Analysis

et al. 2018

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“…Spitzer's discovery of the Phoebe ring explained the origin of Iapetus' unusual appearance and thereby solved one of planetary science's long-standing mysteries 46 . Further cementing this link, hydrocarbons have been found in the near-infrared spectra of both Phoebe and the leading hemisphere of Iapetus, drawing a compositional connection between the two bodies 47,48 .…”

Section: Dust and Rings In The Solar Systemmentioning

confidence: 88%

Spitzer’s Solar System studies of asteroids, planets and the zodiacal cloud

et al. 2020

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In its 16 years of scientific measurements, the Spitzer Space Telescope performed a number of ground-breaking infrared measurements of Solar System objects. In this second of two papers, we describe results from Spitzer observations of asteroids, dust rings, and planets that provide new insight into the formation and evolution of our Solar System. The key Spitzer results presented here can be grouped into three broad classes: characterizing the physical properties of asteroids, notably including a large survey of Near Earth Objects; detection and characterization of several dust/debris disks in the Solar System; and comprehensive characterization of ice giant (Uranus, Neptune) atmospheres. Many of these observations provide critical foundations for future infrared space-based observations.

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“…The Saturnian moon Iapetus has a dark leading hemisphere that is coated by dust grains originating on Phoebe and Saturn's other irregular satellites (e.g., Soter 1974;Burns et al 1979;Verbiscer et al 2009;Tamayo et al 2011Tamayo et al , 2014. Analysis of data collected by the Visual and Infrared Mapping Spectrometer (VIMS) on the Cassini spacecraft demonstrated that a broad feature centered near 3.29 μm is present in pixels covering Iapetus' dark leading hemisphere, consistent with a C-H stretching mode in polycyclic aromatic hydrocarbon (PAH) molecules (e.g., Clark et al 2005Clark et al , 2012Dalle Ore et al 2012;Cruikshank et al 2014) that are possibly delivered in dust grains from Phoebe. Determining whether organic-related spectral features between 3.2 and 3.5 μm are present on Umbriel is a key goal of upcoming observations by the James Webb Space Telescope (Cartwright et al 2021a).…”

Section: Implications For Umbriel's Surface Chemistry and Geochemistrymentioning

confidence: 99%

Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?

Cartwright¹,

DeColibus²,

Castillo‐Rogez³

et al. 2023

Planet. Sci. J.

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Near-infrared spectra of Umbriel and the other classical Uranian moons exhibit 2.2 μm absorption bands that could result from ammonia (NH3) bearing species, possibly exposed in the geologically recent past. However, Umbriel has an ancient surface with minimal evidence for recent endogenic activity, raising the possibility that more refractory species are present, and/or that NH3 is retained over long timescales. We analyzed 33 spectra of Umbriel to investigate its 2.2 μm band, along with three other absorption features we identified near 2.14, 2.22, and 2.24 μm. We assessed the subobserver longitudinal distributions of these four bands, finding that they are present across Umbriel and may be spatially associated with geologic features such as craters and large basins. We compared the bands to 15 candidate constituents. We found that Umbriel’s 2.14 μm and 2.22 μm bands are most consistent with the spectral signature of organics, its 2.24 μm band is best matched by NH3 ice, and its 2.2 μm band is consistent with the signatures of NH3–H2O mixtures, aluminum-bearing phyllosilicates, and sodium-bearing carbonates. However, some of these candidate constituents do not match Umbriel’s spectral properties in other wavelength regions, highlighting the gaps in our understanding of the Uranian moons’ surface compositions. Umbriel’s 2.14 μm band may alternatively result from a 2ν 3 overtone mode of CO2 ice. If present on Umbriel, these candidate constituents could have formed in contact with an internal ocean and were subsequently exposed during Umbriel’s early history. Alternatively, these constituents might have originated in an undifferentiated crust or were delivered by impactors.

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Infrared spectroscopic characterization of the low-albedo materials on Iapetus

Cited by 22 publications

References 32 publications

Mercury Hollows as Remnants of Original Bedrock Materials and Devolatilization Processes: A Spectral Clustering and Geomorphological Analysis

Mercury Hollows as Remnants of Original Bedrock Materials and Devolatilization Processes: A Spectral Clustering and Geomorphological Analysis

Spitzer’s Solar System studies of asteroids, planets and the zodiacal cloud

Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?

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