Optical constants of amorphous and crystalline H2O-ice in the near infrared from 1.1 to 2.6 μm

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

doi:10.1016/j.icarus.2008.04.008

Cited by 132 publications

(152 citation statements)

References 47 publications

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“…In the VIS-NIR range optical constants from Warren et al (1984) pertain to ice at -7 °C, whose temperature is too high if compared to Rhea's surface at 77 K (Pitman et al, 2010). However these values match reasonably well with the ones derived by Mastrapa et al (2008) at 120 K. Optical constants in the 3.2-5.1 µm range are from Clark et al (2011b) and have been computed starting from Mastrapa's values at the same wavelengths. The temperature difference between Rhea's surface and ice for which optical constants are determined introduces a tolerable error in our calculations, because it only minimally affects the results concerning grain size and contamination.…”

Section: Optical Constantsmentioning

confidence: 68%

“…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%

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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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Section: Optical Constantsmentioning

confidence: 68%

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 minimization is applied outside the telluric absorption bands, which can affect the results. Best models are based on an intimate mixture of crystalline water ice (optical constants at 50 K from Grundy & Schmitt 1998), ammoniahydrate (with only 1% of ammonia diluted in water, Brown et al 1988), amorphous carbon (Zubko et al 1996), and amorphous water ice (at low temperature, Mastrapa et al 2008). The model applied to both spectra returns very similar results for the A46, page 5 of 7 compounds abundances, with almost 85% of crystalline water ice (4 µm grain size), 8% of ammonia hydrate (35 µm), 5% of amorphous carbon (10 µm), 2% of amorphous water ice (100 µm), and an asymmetry parameter comprised between 0.86 and 0.90.…”

Section: Results For Intimate Mixturesmentioning

confidence: 99%

Near-infrared spectroscopy of Miranda

Gourgeot¹,

Dumas²,

Merlin³

et al. 2014

A&A

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Aims. We present new near-infrared spectra of the leading and trailing hemispheres of Uranus's icy satellite Miranda. This body is probably the most remarkable of all the satellites of Uranus, because it displays series of surface features such as faults, craters, and large-scale upwelling, a remnant of a geologically very active past. Methods. The observations were obtained with PHARO at Palomar and SpeX at the IRTF Observatory. We performed spectral modelings to further constrain the nature and the chemical and physical states of the compounds possibly present on the surface of Miranda. Results. Water ice signatures are clearly visible in the H and K bands, and it appears to be found in its crystalline state over most of the satellite's surface. Unlike what has been found for Uranus's outer moons, we did not find any significative differences in the abundances of ices covering the leading and trailing hemispheres of Miranda. The signature of carbon dioxide cannot be seen in our spectra, which could still account for the presence of ammonia hydrate, though in small amounts.

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“…IR interference fringes dominate over NH 3 absorptions in this spectral zone and are affected by scattering, incoherence, and double reflections, which prevents us from using them for spectral reproduction. We took a different approach, inspired by Mastrapa et al (2008), to determine the NIR optical constants of H 2 O. We focused on the two spectral regions where NH 3 has absorption, i.e., the 6800-5900 cm −1 and 5200-4100 cm −1 intervals.…”

Section: Optical Constants Calculationmentioning

confidence: 99%

OPTICAL CONSTANTS OF NH₃AND NH₃:N₂AMORPHOUS ICES IN THE NEAR-INFRARED AND MID-INFRARED REGIONS

Zanchet

Rodrı́guez-Lazcano

Gálvez

et al. 2013

ApJ

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Ammonia ice has been detected on different astrophysical media ranging from interstellar medium (ISM) particles to the surface of various icy bodies of our solar system, where nitrogen is also present. We have carried out a detailed study of amorphous NH 3 ice and NH 3 :N 2 ice mixtures, based on infrared (IR) spectra in the mid-IR (MIR) and near-IR (NIR) regions, supported by theoretical quantum chemical calculations. Spectra of varying ice thicknesses were obtained and optical constants were calculated for amorphous NH 3 at 15 K and 30 K and for a NH 3 :N 2 mixture at 15 K over a 500-7000 cm −1 spectral range. These spectra have improved accuracy over previous data, where available. Moreover, we also obtained absolute values for the band strengths of the more prominent IR features in both spectral regions. Our results indicate that the estimated NH 3 concentration in ISM ices should be scaled upward by ∼30%.

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Optical constants of amorphous and crystalline H2O-ice in the near infrared from 1.1 to 2.6 μm

Cited by 132 publications

References 47 publications

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

Near-infrared spectroscopy of Miranda

OPTICAL CONSTANTS OF NH₃AND NH₃:N₂AMORPHOUS ICES IN THE NEAR-INFRARED AND MID-INFRARED REGIONS

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Optical constants of amorphous and crystalline H2O-ice in the near infrared from 1.1 to 2.6 μm

Cited by 132 publications

References 47 publications

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

Near-infrared spectroscopy of Miranda

OPTICAL CONSTANTS OF NH3AND NH3:N2AMORPHOUS ICES IN THE NEAR-INFRARED AND MID-INFRARED REGIONS

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OPTICAL CONSTANTS OF NH₃AND NH₃:N₂AMORPHOUS ICES IN THE NEAR-INFRARED AND MID-INFRARED REGIONS