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Ahuna Mons is the highest mountain on Ceres. A unique complex in terms of size, shape, and morphology, Ahuna is bordered by flanks of the talus around its summit. Recent work by Ruesch et al. ([Ruesch, O., 2016]) based on Dawn's Framing Camera images shed light on the possible origin of Ahuna Mons. According to Ruesch et al. (2016), Ahuna Mons is formed by a volcanic process involving the ascent of cryomagma and extrusion onto the surface followed by dome development and subsequent spreading. Here we analyzed in detail the composition of Ahuna Mons, using data acquired by the visible and infrared spectrometer aboard Dawn. The spectral analysis reveals a relatively high abundance of carbonates and a nonhomogeneous variation in carbonate composition and abundance along Ahuna's flanks, associated with a lower amount of the Ceres's ubiquitous NH4‐phyllosilicates over a large portion of the flanks. The grain size is coarser on the flanks than in the surrounding regions, suggesting the presence of fresher material, also compatible with a larger abundance of carbonates. Thermal variations are seen in Ahuna, supporting the evidence of different compactness of the surface regolith in specific locations. Results of the spectral analysis are consistent with a possible cryovolcanic origin which exposed fresher material that slid down on the flanks. Spectral analysis of Ahuna Mons reveals compositional variations that reflect multiple episodes of cryovolcanic extrusion on Ceres' surfaceSpectral parameter analysis of Ahuna Mons shows a gradient in the composition and abundance of carbonatesThermal variations observed in Ahuna Mons indicate different compactness of the surface regolith in specific locations

High-resolution near-infrared observations of the Occator bright areas on the dwarf planet Ceres suggest that the bright material is mostly made up of endogenous sodium carbonate.

The increasing number and complexity of planetary exploration space missions require new tools to access, visualize and analyse data to improve their scientific return.

Although water vapour is the main species observed in the coma of comet 67P/Churyumov–Gerasimenko and water is the major constituent of cometary nuclei, limited evidence for exposed water-ice regions on the surface of the nucleus has been found so far. The absence of large regions of exposed water ice seems a common finding on the surfaces of many of the comets observed so far. The nucleus of 67P/Churyumov–Gerasimenko appears to be fairly uniformly coated with dark, dehydrated, refractory and organic-rich material. Here we report the identification at infrared wavelengths of water ice on two debris falls in the Imhotep region of the nucleus. The ice has been exposed on the walls of elevated structures and at the base of the walls. A quantitative derivation of the abundance of ice in these regions indicates the presence of millimetre-sized pure water-ice grains, considerably larger than in all previous observations. Although micrometre-sized water-ice grains are the usual result of vapour recondensation in ice-free layers, the occurrence of millimetre-sized grains of pure ice as observed in the Imhotep debris falls is best explained by grain growth by vapour diffusion in ice-rich layers, or by sintering. As a consequence of these processes, the nucleus can develop an extended and complex coating in which the outer dehydrated crust is superimposed on layers enriched in water ice. The stratigraphy observed on 67P/Churyumov–Gerasimenko is therefore the result of evolutionary processes affecting the uppermost metres of the nucleus and does not necessarily require a global layering to have occurred at the time of the comet’s formation.

Studies of the dwarf planet (1) Ceres using ground-based and orbiting telescopes have concluded that its closest meteoritic analogues are the volatile-rich CI and CM carbonaceous chondrites. Water in clay minerals, ammoniated phyllosilicates, or a mixture of Mg(OH)2(brucite), Mg2CO3and iron-rich serpentine have all been proposed to exist on the surface. In particular, brucite has been suggested from analysis of the mid-infrared spectrum of Ceres. But the lack of spectral data across telluric absorption bands in the wavelength region 2.5 to 2.9 micrometres—where the OH stretching vibration and the H2O bending overtone are found—has precluded definitive identifications. In addition, water vapour around Ceres has recently been reported, possibly originating from localized sources. Here we report spectra of Ceres from 0.4 to 5 micrometres acquired at distances from ~82,000 to 4,300 kilometres from the surface. Our measurements indicate widespread ammoniated phyllosilicates across the surface, but no detectable water ice. Ammonia, accreted either as organic matter or as ice, may have reacted with phyllosilicates on Ceres during differentiation. This suggests that material from the outer Solar System was incorporated into Ceres, either during its formation at great heliocentric distance or by incorporation of material transported into the main asteroid belt.

The first ever regional thermal properties map of Vesta has been derived from the temperatures retrieved by infrared data by the mission Dawn. The low average value of thermal inertia, 30 ± 10 J m−2s−0.5K−1, indicates a surface covered by a fine regolith. A range of thermal inertia values suggesting terrains with different physical properties has been determined. The lower thermal inertia of the regions north of the equator suggests that they are covered by an older, more processed surface. A few specific areas have higher than average thermal inertia values, indicative of a more compact material. The highest thermal inertia value has been determined on the Marcia crater, known for its pitted terrain and the presence of hydroxyl in the ejecta. Our results suggest that this type of terrain can be the result of soil compaction following the degassing of a local subsurface reservoir of volatiles. A thermophysical map of Vesta has been derived from spatially resolved dataThe average thermal inertia of the surface of Vesta is 30 ± 10 Jm−2s−0.5K−1Pitted terrains in Marcia crater have the highest thermal inertia value

Abstract—The laboratory analyses of cosmic dust analogues—that in the context of this paper include interstellar, circumstellar as well as cometary dust—have a critical role in the study of circumstellar and cometary dust. The morphological, structural and chemical characterization of these analogues are critical for comparisons of their infrared and ultraviolet spectra with those obtained by astronomical observations, as well as for modeling purposes. Besides, the results from these laboratory studies are important to the success of space missions to comets when testing and calibrating the payload instruments. The interpretations of returned scientific data would benefit from the comparison with data recorded by the instruments in a laboratory setting for different classes of previously characterized analogues. We produced various types of condensed samples: (1) Mg,Fe‐silicates, (olivine, pyroxene), (2) carbon‐rich dust, and (3) mixed carbon‐silicate dust. The samples were prepared using different techniques, viz.(1) laser bombardment of solid targets in an Ar and O2atmosphere, (2) arc discharge in an Ar and H2atmosphere, and (3) grinding powders of natural minerals. We simulated various post‐condensation processes, such as thermal annealing, ultraviolet irradiation, ion bombardment and exposure to atomic hydrogen. These processes produced compound samples of a wide range of physico‐chemical properties. To identify their textures, morphologies, grain compositions and crystallographic properties we used electron microscopy and far‐ultraviolet to far‐infrared (millimeter range) spectroscopy.

We present the results of ISOCAM observations performed on Comets 2P/Encke and 103P/Hartley 2, on 31 October 1997 and 1 January 1998, respectively. Images were obtained in the broadband filters LW3 (centered at 15.00 μm) and LW10 (centered at 11.50 μm). Tail models have been applied to the images to analyze the evolution of the dust coma environment and to derive information about the velocity of the grains. The image of 2P/Encke presents a sunward spike interpreted as a Neck-Line. Thanks to the model, the time evolution of the comet dust environment during 3 months preceding the observation has been reconstructed. 2P/Encke presents a strong maximum in the dust velocity, a broad maximum of the dust mass loss rate, and a dip of the size distribution power index around perihelion. Model results indicate that the largest grains in the tail can reach sizes from centimeters to decimeters. This has important implications for the source of the Taurid meteoroids. For Comet 103P/Hartley 2 the numerical model suggests an anisotropic dust ejection with a tail composed of grains smaller than those in 2P/Encke. Both dust ejection velocity and dust mass loss rate reach a maximum about 2 weeks before perihelion. The power law best fitting the time-averaged size distribution of both comets has an index of about −3.2, indicating that the released dust is strongly dominated in mass by the largest ejected grains.

The Planetary Fourier Spectrometer (PFS) is a Fourier transform interferometer, operating in the range 1.2–45 μm. The instrument, previously included in the payload of the failed mission Mars ′96, is proposed for the future space mission Mars Express, under study by ESA. The present paper is aimed at presenting the radiometric performances of PFS. The two channels (LW and SW) forming PFS were analysed and characterised in terms of sensitivity and noise equivalent brightness. To cover the wide spectral range of PFS, different blackbodies were used for calibration. The built-in blackbodies, needed for the in-flight calibrations, were also characterised. The results show that the LW channel is comparable with IRIS Mariner 9 in terms of noise equivalent brightness. The SW channel performances, while satisfactorily, could be improved by lowering the sensor operative temperature. A simple model of the Mars radiance is used in order to calculate the signal-to-noise ratio on the spectra in typical observation conditions. The computed signal-to-noise ratio for the LW channel varies between 430 and 40, while for the SW channel it ranges from 150 to 30. The radiometric analyses confirm that PFS performances are compliant with the design requirements of the instrument. PFS is fully validated for future remote exploration of the atmosphere and the surface of Mars.

The signs that may arise after perinatal infection with human immunodeficiency virus type 1 (HIV-1) have been classified by the Centers for Disease Control, but the clinical usefulness of the classification system and the prognostic importance of each disease pattern have not been established. We sought to address these issues by analysing data from the Italian Register for HIV infection in children. We studied 1887 children born to HIV-1-seropositive mothers. 1045 were identified at birth and the others were registered later (median age 4·8 [range 0·4-72] months). HIV-1-associated signs developed in 433 (81·8%) of 529 seropositive infected children at a median age of 5 (0·03-84) months. These signs appeared significantly earlier in the 102 children who died of HIV-1-related illness than in those who are still alive (median 3 [0·03-55] vs6 [0·03-84] months; p<0·001). The cumulative proportion surviving at age 9 years was 49·5% (95% confidence interval 27-65%) and the median survival time was 96·2 months. Separate analysis of the 112 seropositive infected children followed from birth and older than 15 months gave similar results. Hepatomegaly, splenomegaly, lymphadenopathy, parotitis, skin diseases, and recurrent respiratory tract infections formed the mildest disease pattern. Lymphoid interstitial pneumonitis and thrombocytopenia were signs of intermediate disease. By contrast, in multivariate analysis specific secondary infectious diseases, severe bacterial infections, progressive neurological disease, anaemia, and fever were significant and independent negative predictors of survival. Growth failure, persistent oral candidosis, hepatitis, and cardiopathy were associated in univariate analysis with significantly shorter survival. Our findings suggest that the outlook for children with perinatal HIV-1 infection is better than previously thought and that a new clinical staging system of single disease patterns is needed. Lancet1992; 339:1249-53.

Reflectance spectroscopy in the infrared is a powerful tool to characterise the optical properties of analogue materials for Mars. In this work we present laboratory studies of four Martian analogues: calcite, montmordlonite, palagonite and andesite. Diffuse and specular reflectance and transmittance spectra in the IR are shown. The spectral effect produced by small grains clung to the larger ones is analysed for calcite. Significant variations in the diffuse reflectance spectrum, especially in the reststrahlen region, are observed. The diffuse reflectance spectra of the other materials show the shift of the reststrahlen features with Si content in the materials. Optical constants of andesite are retrieved, by using the Lorentz model, from the specular reflectance spectrum. These values are fundamental in performing modelling of the radiance coming from the planet Mars.

Thermal inertia is a key information to quantify the physical status of a planetary surface. We derive the thermal inertia of the surface of Ceres using spatially resolved data from the Dawn mission. For each location, this quantity can be constrained by comparing theoretical and observed diurnal temperature profiles from retrieved temperatures. We calculated Ceres's surface theoretical temperatures with a thermophysical model that provides temperature as a function of thermal conductivity and roughness, and we determined the values of those parameters for which the best fit with the observed data is obtained. Our results suggest that the area of crater Haulani displays thermal inertia values (up to 130–140 J·m−2·s−½·K−1) substantially higher than the very low to low values (from 1–15 to 50–60 J·m−2·s−½·K−1) derived for the overall surface of Ceres. The results are more ambiguous for the bright faculae located in the floor of crater Occator. We have calculated Ceres's surface temperatures and we have compared them with the observations. We have used new high‐resolution data provided by the Dawn/National Aeronautics and Space Administration mission, which was launched in 2007 with the aim of studying two of the largest bodies of the Main Belt: Vesta and Ceres. Our results suggest that the surface is made of fine‐grained material, according to previous analysis made by other authors by using other independent data and methods. We have also studied two particular areas of Ceres that shows peculiar properties (albedo and/or chemical/physical structure). The thermal inertia of the surface of Ceres has been derived using spatially resolved data from the Dawn missionThe Haulani crater appears to have a higher thermal inertia with respect to Ceres's averageThe average thermal inertia of the surface of Ceres appears to have low values (1–15 J·m−2·s−½·K−1)

The interest towards Mars is nowadays renewed as various satellites, already launched or foreseen for the future, will visit this planet, providing a new wealth of data. In particular, infrared spectroscopic observations need a parallel modelling effort for a proper interpretation of observations. The goal of our modelling is to evaluate the influence of a non negligible fraction of dust particles on intensity and profile of atmospheric Martian spectra. The joint effects of the atmosphere and the surface materials have been also accounted for. For the modelling, a version of the MODTRAN code, expressly modified for application to the Mars environment, has been used. As an example of the materials forming dust dispersed in the atmosphere and on the surface, we have considered andesite. Indices of refraction (nand k) of this material have been derived from laboratory measurements. The obtained results can have an important impact on the interpretation of infrared spectra that instruments such as TES (Thermal Emission Spectrometer), on board the Mars Global Surveyor, and PFS, in the Mars Express mission, will provide.