OPTICAL CONSTANTS OF AMORPHOUS AND CRYSTALLINE H2O-ICE: 2.5-22 μm (4000-455 cm–1) OPTICAL CONSTANTS OF H2O-ICE

Mastrapa, Rachel M. E.; Sandford, Scott A.; Roush, T. L.; Cruikshank, D. P.; Ore, C. M. Dalle

doi:10.1088/0004-637x/701/2/1347

Cited by 176 publications

(189 citation statements)

References 26 publications

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“…However, the wavelength shift of the 3.7 μm peak to longer wavelengths in the chaos regions cannot be attributed to grain size. This peak wavelength shift does occur with changing temperature in pure water ice (e.g., Mastrapa et al 2009;Clark et al 2012), though pure water ice likely cannot produce the magnitude of this shift (∼0.1 μm) or the absolute wavelength. For example, Figure 2 shows spectra of water ice at 90 K and 130 K, which is a reasonable dayside temperature range (e.g., Moore et al 2009).…”

Section: Resultsmentioning

confidence: 97%

“…NaCl is an irradiated evaporite and KCl is irradiated anhydrous grains at 100 K from K. P. Hand et al (2016, in preparation). Water ice spectra at 90 and 130 K are derived using optical constants from Mastrapa et al (2009) and the spectral modeling approach of Hapke (1981) with agrain size of 20 μm. For comparison, blödite is shown scaled by a factor of 0.4, and blödite and epsomite are shifted vertically by 0.05 and 0.044. only non-water ice feature at the resolution and S/N of our observations is at 3.5 μm, attributed to peroxide (Carlson et al 1999) and localized to the leading hemisphere ).…”

Section: Resultsmentioning

confidence: 99%

“…We also note that the selection in Figure 2 represents the limited number of laboratory spectra available, although many spectra from the USGS and ASTER spectral libraries are clearly inconsistent with the observed spectra and are not shown. Though cryogenic optical constants are available for water ice (Mastrapa et al 2009), we are aware of no other optical constants for candidate materials at these wavelengths, low temperatures, and necessary precision to justify a detailed spectral modeling investigation.…”

Section: Resultsmentioning

confidence: 99%

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SPATIALLY RESOLVED SPECTROSCOPY OF EUROPA’S LARGE-SCALE COMPOSITIONAL UNITS AT 3–4 μm WITH KECK NIRSPEC

Fischer

Brown

Trumbo

et al. 2016

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We present spatially resolved spectroscopic observations of Europa's surface at 3-4 μm obtained with the nearinfrared spectrograph and adaptive optics system on the Keck II telescope. These are the highest quality spatially resolved reflectance spectra of Europa's surface at 3-4 μm. The observations spatially resolve Europa's large-scale compositional units at a resolution of several hundred kilometers. The spectra show distinct features and geographic variations associated with known compositional units; in particular, large-scale leading hemisphere chaos shows a characteristic longward shift in peak reflectance near 3.7 μm compared to icy regions. These observations complement previous spectra of large-scale chaos, and can aid efforts to identify the endogenous nonice species.

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Section: Resultsmentioning

confidence: 97%

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

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SPATIALLY RESOLVED SPECTROSCOPY OF EUROPA’S LARGE-SCALE COMPOSITIONAL UNITS AT 3–4 μm WITH KECK NIRSPEC

Fischer

Brown

Trumbo

et al. 2016

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“…The dark grains have optical constants chosen to match the albedo level of the continuum and the ice is a fine-grained frost with a volume fraction of 1.1% (chosen to match the depth of the absorption) coating the dark grains. Water ice optical constants are obtained from Mastrapa et al (2009). The spectral fit to the 3.1 μm band is quite good (Figure 6).…”

Section: Spectral Modelingmentioning

confidence: 92%

THE 3–4 μm SPECTRA OF JUPITER TROJAN ASTEROIDS

Brown

2016

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To date, reflectance spectra of Jupiter Trojan asteroids have revealed no distinctive absorption features. For this reason, the surface composition of these objects remains a subject of speculation. Spectra have revealed, however, that the Jupiter Trojan asteroids consist of two distinct sub-populations that differ in the optical to near-infrared colors. The origins and compositional differences between the two sub-populations remain unclear. Here, we report the results from a 2.2-3.8 μm spectral survey of a collection of 16 Jupiter Trojan asteroids, divided equally between the two sub-populations. We find clear spectral absorption features centered around 3.1 μm in the less-red population. Additional absorption consistent with that expected from organic materials might also be present. No such features are see in the red population. A strong correlation exists between the strength of the 3.1 μm absorption feature and the optical to near-infrared color of the objects. While, traditionally, absorptions such as these in dark asteroids are modeled as being due to fine-grain water frost, we find it physically implausible that the special circumstances required to create such fine-grained frost would exist on a substantial fraction of the Jupiter Trojan asteroids. We suggest, instead, that the 3.1 μm absorption on Trojans and other dark asteroids could be due to N-H stretch features. Additionally, we point out that reflectivities derived from WISE observations show a strong absorption beyond 4 μm for both populations. The continuum of 3.1 μm features and the common absorption beyond 4 μm might suggest that both sub-populations of Jupiter Trojan asteroids formed in the same general region of the early solar system.

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“…We used separately tholin from Khare et al (1993), Triton tholin (McDonald et al, 1994; optical constants from Cruikshank, personal communication), Titan tholin (McDonald et al, 1994;Khare et al, 1984; optical constants from Cruikshank, personal communication) and hydrogenated amorphous carbon (ACH2) from Zubko et al (1996). Optical constants for crystalline water ice are those derived by Warren (1984) (0.35-1.25 µm, 266.15 K), Mastrapa et al (2008) (1.25-2.5 µm, 120 K), Mastrapa et al. (2009) (2.5-3.20 µm, 120 K) and Clark et al (20110b) (3.20-5.12 µm, 120 K).…”

Section: Spectral Fitmentioning

confidence: 99%

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

Ciarniello

Capaccioni

Filacchione

et al. 2011

Icarus

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The surface properties of the icy bodies in the saturnian system have been investigated by means of the CASSINI-VIMS (Visual Infrared Mapping Spectrometer) hyperspectral imager which operates in the 0.35-5.1 m wavelength range. In particular, we have analyzed 111 full disk hyperspectral images of Rhea ranging in solar phase between 0.08° and 109.8°. These data have been previously analyzed by Filacchione et al. (2007Filacchione et al. ( , 2010 to study, adopting various "spectral indicators" (such as spectral slopes, band depth, continuum level, etc.), the relations among various saturnian satellites.As a further step we proceed in this paper to a quantitative evaluation of the physical parameters determining the spectrophotometric properties of Rhea's surface. To do this we have applied Hapke (1993) IMSA model (Isotropic Multiple Scattering Approximation) which allow us to model the phase function at VIS-IR (visible-infrared) wavelengths as well as the spectra taking into account various types of mixtures of surface materials. Thanks to this method we have been able to constrain the size of water ice particles covering the surface, the amount of organic contaminants, the large scale surface roughness and the opposition effect surge. From our analysis it appears that wavelength dependent parameters, e.g. opposition surge width (h) and single-particle phase function parameters (b,v), are strongly correlated to the estimated single-scattering albedo of particles. For Rhea the best fit solution is obtained by assuming:1) an intraparticle mixture of crystalline water ice and a small amount (0.4%) of Triton tholin; 2) a monodisperse grain size distribution having a particle diameter a m = 38 µm; and 3) a surface roughness parameter value of 33°. The study of phase function shows that both Shadow Hiding and Coherent Backscattering contribute to the opposition surge. This study represents the first attempt, in the case of Rhea, to join the spectral and the photometric analysis. The surface model we derived gives a good quantitative description of both spectrum and phase curve of the satellite. The same approach and model, with appropriate modifications, shall be applied to VIMS data of the other icy satellites of Saturn, in order to reveal similarities and differences in the surface characteristics to understand how these bodies interact with their environment.

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OPTICAL CONSTANTS OF AMORPHOUS AND CRYSTALLINE H₂O-ICE: 2.5-22 μm (4000-455 cm^–1) OPTICAL CONSTANTS OF H₂O-ICE

Cited by 176 publications

References 26 publications

SPATIALLY RESOLVED SPECTROSCOPY OF EUROPA’S LARGE-SCALE COMPOSITIONAL UNITS AT 3–4 μm WITH KECK NIRSPEC

SPATIALLY RESOLVED SPECTROSCOPY OF EUROPA’S LARGE-SCALE COMPOSITIONAL UNITS AT 3–4 μm WITH KECK NIRSPEC

THE 3–4 μm SPECTRA OF JUPITER TROJAN ASTEROIDS

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

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