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Compositional Maps of Saturn's Moon Phoebe from Imaging Spectroscopy

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Compositional Maps of Saturn's Moon Phoebe from Imaging Spectroscopy letters to nature .............................................................. features may be caused by cyanide and organic compounds. Compositional maps of Saturn’s The composition of Phoebe should reflect the composition of the region in the solar nebula where it accreted. If Phoebe originated in moon Phoebe from imaging the region of the asteroid main belt (,3 AU), it should consist largely of volatile-poor mafic minerals. Alternatively, it could have accreted spectroscopy in the volatile-rich outer solar nebula where the Kuiper belt objects (KBOs) originated. Dynamical scattering inward from an accretion Roger N. Clark1, Robert H. Brown2, Ralf Jaumann3, Dale P. Cruikshank4, site among the KBOs is more likely than scattering outward from Robert M. Nelson5, Bonnie J. Buratti5, Thomas B. McCord6, J. Lunine2, the asteroid belt5. For example, inward scattering may have occurred K. H. Baines5, G. Bellucci7, J.-P. Bibring8, F. Capaccioni7, P. Cerroni7, during events that are thought to have forced the KBOs outward by A. Coradini7, V. Formisano7, Y. Langevin8, D. L. Matson5, V. Mennella7, the outward migration of Neptune6. P. D. Nicholson9, B. Sicardy10, C. Sotin11, Todd M. Hoefen1, With a diameter of 220 km, Phoebe is comparable in size to most 1 13 12 3 John M. Curchin , Gary Hansen , Karl Hibbits & K.-D. Matz of the nearly 800 known KBOs. Other physical properties that 1 Phoebe shares with KBOs include the presence of H2O ice and an US Geological Survey, MS964, Box 25046, Federal Center, Denver, Colorado overall low surface albedo7. KBOs exhibit a wide range of colour8, 80225, USA 9 2Lunar and Planetary Laboratory and Stewart Observatory, University of including the neutral colour characteristic of Phoebe .Ithas Arizona, Tucson, Arizona 85721, USA been postulated that material from Phoebe (for example, ejected by 3German Aerospace Center (DLR), Institute of Space Sensor Technology and impacts) may coat the leading surface of Saturn’s moon Iapetus10,so Planetary Exploration, Rutherfordstrasse 2, D-12489 Berlin, Germany this material might be found elsewhere in the Saturn system. 4 NASA Ames Research Center, Moffett Field, California 94035, USA Mapping results from VIMS indicate that H2O ice is distributed 5 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, over most of Phoebe’s observed surface, but generally shows California 91109, USA stronger spectral signatures toward the southern polar region 6University of Hawaii at Manoa, HIGP/SOEST, 1680 East-West Road, Honolulu, (Fig. 1b, h). In the highest spatial resolution data, crater interiors Hawaii 96822, USA 7Istituto di Fisica dello Spazio Interplanetario, CNR, Rome 00133, Italy display less exposed ice than the surrounding terrain (arrows in 8Institut d’Astrophysique Spatiale, Universite´ de Paris-Sud, F-91405 Orsay Cedex Fig. 1b). In the jovian system, cratering tends to expose fresh ice in France the subsurface11. The highest resolution VIMS data for Phoebe also 9Cornell University, Astronomy Department, Ithaca, New York 14853, USA indicate an ice-rich layer exposed in crater walls just below Phoebe’s 10Observatoire de Paris, 92195 Meudon, France surface (Fig. 1b). Therefore, it is likely that ice is less abundant in the 11 Laboratoire de Plane´tologie et Ge´odynamique, UMR CNRS 6112, Universite´ de deeper subsurface, at least in the region of highest resolution data Nantes, 44322 Nantes, France 12 (near longitude 08, latitude 08). Planetary Science Institute NW, Corporate Center Pasadena, 255 S. Lake 2þ Avenue, Suite 300, Pasadena, California 91101, USA The Fe absorption is quite broad (Fig. 2b, feature f1), unlike 13Department of Earth and Space Sciences, University of Seattle, Washington that in pyroxenes, but similar to that in olivines and phyllo- 12 2 98195-1310, USA silicates . If phyllosilicates were present, (OH) absorptions ............................................................................................................................................................................. might be expected, but would be relatively weak owing to the low The origin of Phoebe, which is the outermost large satellite of reflectance. Indeed, weak 2.2- and 2.3-mm absorptions (f10, f23) are Saturn, is of particular interest because its inclined, retrograde orbit suggests that it was gravitationally captured by Saturn, having accreted outside the region of the solar nebula in which Saturn formed1. By contrast, Saturn’s regular satellites (with Table 1 Observed spectral features prograde, low-inclination, circular orbits) probably accreted Feature Wavelength (mm) Width (mm) Origin ............................................................................................................................................................................. 2 within the sub-nebula in which Saturn itself formed . Here f1 1.0 1.1 Probable Fe2þ we report imaging spectroscopy of Phoebe resulting from the f2 1.04 ,0.05 H2O ice overtone Cassini–Huygens spacecraft encounter on 11 June 2004. We f3 1.2 ,0.02 OH stretch, CH combination, or calibration artefact mapped ferrous-iron-bearing minerals, bound water, trapped f4 1.3 ,0.02 OH stretch, CH combination, or CO2, probable phyllosilicates, organics, nitriles and cyanide calibration artefact compounds. Detection of these compounds on Phoebe makes it f5 1.4 ,0.02 OH stretch, CH combination, or calibration artefact one of the most compositionally diverse objects yet observed in f6 1.5 ,0.2 H2O ice overtone our Solar System. It is likely that Phoebe’s surface contains f7 1.7 Variable CH stretch overtone primitive materials from the outer Solar System, indicating a f8 1.95 ,0.1 Bound H2O f9 2.02 ,0.2 H2O ice combination surface of cometary origin. f10 2.16 ,0.03 Probable metal-OH combination, for example, We report the identification and possible origins of the surface phyllosilicates f11 2.42 ,0.07 Probable CN combination materials on Phoebe by compositional mapping with the Visible f12 2.95 ,0.7 H O ice and/or bound H O 3 2 2 and Infrared Mapping Spectrometer (VIMS) on board Cassini. f13 3.1 ,0.05 H2O ice Fresnel peak Cassini VIMS spatially resolved the surface of Phoebe, and data f14 3.2–3.3 Variable CH stretch fundamentals , have been registered and projected into simple cylindrical maps: f15 3.55 0.06 Probable CH f16 3.9 ,0.2 Perhaps CH, CN or H2O low to medium resolution with near hemispheric coverage, and f17 4.26 ,0.03 Trapped CO2 (gaseous or fluid inclusion) high resolution of a small area (Fig. 1). Spectra of Phoebe indicate f18 4.50 ,0.03 CN in a nitrile f19 4.8–5.0 ,0.05 Probable CN fundamental a low albedo surface, from ,1% to 6% reflectance (Fig. 2), with a f20 .5.1 ND ND variety of absorption features. These features are due to materials f21 4.3 0.7 H2O ice and/or bound water f22 2.05 ,0.17 H2Oice (Table 1) that occur with variable abundances and/or grain sizes f23 2.3 ,0.08 Probable metal-OH combination, for example, in different locations on the body. They include: previously phyllosilicates 4 f24 2.72 ,0.05 OH stretch fundamental, common in identified water ice , bound water, and trapped CO2 (maps, phyllosilicates Fig. 1; spectra, Fig. 2). A broad 1-mm feature, attributed to , 2þ f25 1.25 0.1 H2Oice Fe -bearing minerals, is present in almost all regions but f26 3.62 ,0.07 Probable CH or CN f27 2.54 ,0.016 Probable CH stronger in equatorial areas. Bound water and hydroxyl absorp- ............................................................................................................................................................................. tions indicate the presence of phyllosilicates. Other weak spectral ND, not determined. 66 NATURE | VOL 435 | 5 MAY 2005 | www.nature.com/nature © 2005 Nature Publishing Group letters to nature seen in some spectra, indicating a probable metal-OH absorption structures of variable CO2 abundances, showing structures only (Fig. 2b). Hydrated mineral absorptions are also consistent with seen in composition maps (Fig. 1g) and not observed in reflectance phyllosilicates. We attribute the 1.5- and 1.95-mm absorptions (Fig. 1a). (Fig. 2b, spectrum S2, f6, f8) to hydrated mineral absorptions, but The absorption feature at 2.42 mm (Fig. 2a, c, e, f11) has not been these features are not diagnostic of specific mineralogy and indicate reported on any Solar System body before Cassini. Searches of only the presence of bound water. available spectral libraries12,13 and scientific papers that show OH- CO2 is ubiquitous on Phoebe. The wavelength and shape of the bearing minerals with an absorption at this position also have other CO2 absorption, 4.26 mm (Fig. 2a, c, d, f17), is similar to that of the absorptions nearby that are not seen in Phoebe spectra. Cyanide 11 trapped CO2 found on Jupiter’s satellites Callisto and Ganymede . compounds, however, have unique absorptions in this region, and a CO2 is more spatially variable than water ice in the areas where it spectrum of potassium ferrocyanide trihydrate, K4Fe(CN)6·3H2O, maps on Phoebe’s surface (Fig. 1g). The highest spatial resolution closely matches Phoebe’s absorption position and shape (Fig. 2e). data indicate a linear structure of lower CO2 that is at least 60 km in Spatially, the 2.42-mm absorption maps mainly in the equatorial length (Fig. 1g). Medium resolution data indicate other linear regions (Fig. 1e). The same 2.42-mm absorption has been observed Figure 1 VIMS data, x and y axes show longitude and latitude, respectively, in degrees. high resolution image. b–h, The continuum-removed absorption band depth is shown for a–h, Compositional maps of Phoebe in simple cylindrical projection, VIMS obtained each material, as defined in ref. 21. b, The 2-mm ice absorption strength. Note that two spatially resolved hyperspectral images of Phoebe at 352 wavelengths (0.4–5 mm) from craters (arrows) have no ice in the floors. The crater on the right shows enhanced ice 8:47 UT June 11, 2004 at an initial range of 245,833 km and phase angle of 84.98,to strength near the top of the crater (bright arc). Other materials map in the floors of the two 2þ 10:22 UT June 12, 2004 at a final range of 338,401 km and phase angle of 92.28.
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