ALBERT

Description: JUNGFRAU (adJUstiNg Gain detector FoR the Aramis User station) is a two-dimensional hybrid pixel detector for photon science applications in free electron lasers, particularly SwissFEL, and synchrotron light sources. JUNGFRAU is an automatic gain switching, charge-integrating detector which covers a dynamic range of more than 10 4 photons of an energy of 12 keV with a good linearity, uniformity of response, and spatial resolving power. The JUNGFRAU 1.0 application-specific integrated circuit (ASIC) features a 256 × 256 pixel matrix of 75 × 75 μ m 2 pixels and is bump-bonded to a 320 μ m thick Si sensor. Modules of 2 × 4 chips cover an area of about 4 × 8 cm 2 . Readout rates in excess of 2 kHz enable linear count rate capabilities of 20 MHz (at 12 keV) and 50 MHz (at 5 keV). The tolerance of JUNGFRAU to radiation is a key issue to guarantee several years of operation at free electron lasers and synchrotrons. The radiation hardness of JUNGFRAU 1.0 is tested with synchrotron radiation up to 10 MGy of delivered dose. The effect of radiation-induced changes on the noise, baseline, gain, and gain switching is evaluated post-irradiation for both the ASIC and the hybridized assembly. The bare JUNGFRAU 1.0 chip can withstand doses as high as 10 MGy with minor changes to its noise and a reduction in the preamplifier gain. The hybridized assembly, in particular the sensor, is affected by the photon irradiation which mainly shows as an increase in the leakage current. Self-healing of the system is investigated during a period of 11 weeks after the delivery of the radiation dose. Annealing radiation-induced changes by bake-out at 100 °C is investigated. It is concluded that the JUNGFRAU 1.0 pixel is sufficiently radiation-hard for its envisioned applications at SwissFEL and synchrotron beam lines.

Description: Developing countries that implement the Reducing emissions from deforestation and forest degradation (REDD+) mechanism under the United Nations Framework Convention on Climate Change are required to ensure the effective participation of all stakeholders including indigenous peoples and local communities. Community-based monitoring (CBM) of REDD+ projects could contribute to meeting REDD+ monitoring, reporting, and verification requirements and to ensuring effective community participation. The Democratic Republic of Congo (DRC) is the most advanced country in REDD+ implementation in the Congo Basin region, but the role of forest communities in REDD+ monitoring has not been adequately defined. Based on a Delphi survey, this study aimed to explore the factors that are crucial in achieving effective community participation in the monitoring of REDD+ projects. Out of 65 experts with in-depth knowledge of REDD+ and CBM in the DRC and elsewhere, 35 agreed to participate in the study. In three rounds, 19 feedbacks were received from the first round, 17 from the second and 14 from the third. Data were analyzed in a qualitative (MAXQDA) and quantitative (Microsoft Excel) manner. There was consensus among experts that, per definition, effective participation of communities in the monitoring of REDD+ projects must be a process characterized by a free and prior informed consent (FPIC), recognition of traditional knowledge and community rights, and involvement of communities in all steps of the monitoring process. In practice, the latter point poses several challenges as it requires capacity building, careful selection of indicators, adequate local institutional arrangements and a benefit-sharing system. Ideally, local CBM systems should be nested within the national forest monitoring system, but this will require more strategic efforts at the national level in the DRC, including a framework concept for the role of communities and CBM in REDD+ that can be further adapted to particular circumstances on the ground.

Description: X-ray phase contrast imaging enables the measurement of the electron density of a sample with high sensitivity compared to the conventional absorption contrast. This is advantageous for the study of dose-sensitive samples, in particular, for biological and medical investigations. Recent developments relaxed the requirement for the beam coherence, such that conventional X-ray sources can be used for phase contrast imaging and thus clinical applications become possible. One of the prominent phase contrast imaging methods, Talbot-Lau grating interferometry, is limited by the manufacturing, alignment, and photon absorption of the analyzer grating, which is placed in the beam path in front of the detector. We propose an alternative improved method based on direct conversion charge integrating detectors, which enables a grating interferometer to be operated without an analyzer grating. Algorithms are introduced, which resolve interference fringes with a periodicity of 4.7  μ m recorded with a 25  μ m pitch Si microstrip detector (GOTTHARD). The feasibility of the proposed approach is demonstrated by an experiment at the TOMCAT beamline of the Swiss Light Source on a polyethylene sample.

Description: The setup and first results from commissioning of a fast online photon energy spectrometer for the vacuum ultraviolet free electron laser at Hamburg (FLASH) at DESY are presented. With the use of the latest advances in detector development, the presented spectrometer reaches readout frequencies up to 1 MHz. In this paper, we demonstrate the ability to record online photon energy spectra on a shot-to-shot base in the multi-bunch mode of FLASH. Clearly resolved shifts in the mean wavelength over the pulse train as well as shot-to-shot wavelength fluctuations arising from the statistical nature of the photon generating self-amplified spontaneous emission process have been observed. In addition to an online tool for beam calibration and photon diagnostics, the spectrometer enables the determination and selection of spectral data taken with a transparent experiment up front over the photon energy of every shot. This leads to higher spectral resolutions without the loss of efficiency or photon flux by using single-bunch mode or monochromators.

Description: The VIRTIS (Visible, Infrared and Thermal Imaging Spectrometer) instrument on board the Rosetta spacecraft has provided evidence of carbon-bearing compounds on the nucleus of the comet 67P/Churyumov-Gerasimenko. The very low reflectance of the nucleus (normal albedo of 0.060 +/- 0.003 at 0.55 micrometers), the spectral slopes in visible and infrared ranges (5 to 25 and 1.5 to 5% kA(-1)), and the broad absorption feature in the 2.9-to-3.6-micrometer range present across the entire illuminated surface are compatible with opaque minerals associated with nonvolatile organic macromolecular materials: a complex mixture of various types of carbon-hydrogen and/or oxygen-hydrogen chemical groups, with little contribution of nitrogen-hydrogen groups. In active areas, the changes in spectral slope and absorption feature width may suggest small amounts of water-ice. However, no ice-rich patches are observed, indicating a generally dehydrated nature for the surface currently illuminated by the Sun.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Capaccioni, F -- Coradini, A -- Filacchione, G -- Erard, S -- Arnold, G -- Drossart, P -- De Sanctis, M C -- Bockelee-Morvan, D -- Capria, M T -- Tosi, F -- Leyrat, C -- Schmitt, B -- Quirico, E -- Cerroni, P -- Mennella, V -- Raponi, A -- Ciarniello, M -- McCord, T -- Moroz, L -- Palomba, E -- Ammannito, E -- Barucci, M A -- Bellucci, G -- Benkhoff, J -- Bibring, J P -- Blanco, A -- Blecka, M -- Carlson, R -- Carsenty, U -- Colangeli, L -- Combes, M -- Combi, M -- Crovisier, J -- Encrenaz, T -- Federico, C -- Fink, U -- Fonti, S -- Ip, W H -- Irwin, P -- Jaumann, R -- Kuehrt, E -- Langevin, Y -- Magni, G -- Mottola, S -- Orofino, V -- Palumbo, P -- Piccioni, G -- Schade, U -- Taylor, F -- Tiphene, D -- Tozzi, G P -- Beck, P -- Biver, N -- Bonal, L -- Combe, J-Ph -- Despan, D -- Flamini, E -- Fornasier, S -- Frigeri, A -- Grassi, D -- Gudipati, M -- Longobardo, A -- Markus, K -- Merlin, F -- Orosei, R -- Rinaldi, G -- Stephan, K -- Cartacci, M -- Cicchetti, A -- Giuppi, S -- Hello, Y -- Henry, F -- Jacquinod, S -- Noschese, R -- Peter, G -- Politi, R -- Reess, J M -- Semery, A -- New York, N.Y. -- Science. 2015 Jan 23;347(6220):aaa0628. doi: 10.1126/science.aaa0628.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy. fabrizio.capaccioni@iaps.inaf.it. ; Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy. ; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Universite Pierre et Marie Curie[acute accent over last letter in "Universite"]/Universite Paris-Diderot, Meudon, France. ; Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Berlin, Germany. ; Universite Grenoble Alpes, CNRS, Institut de Planetologie et d'Astrophysique de Grenoble, Grenoble, France. ; Osservatorio di Capodimonte, INAF, Napoli, Italy. ; Bear Fight Institute, Winthrop, WA 98862, USA. ; University of California, Los Angeles, Los Angeles, CA 90095, USA. ; European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Noordwijk, Netherlands. ; Institut d'Astrophysique Spatial, CNRS, Orsay, France. ; Dipartimento di Matematica e Fisica "Ennio De Giorgi," Universita del Salento, Italy. ; Space Research Centre, Polish Academy of Sciences, Warsaw, Poland. ; NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA. ; Space Physics Research Laboratory, The University of Michigan, Ann Arbor, MI 48109, USA. ; Universita di Perugia, Perugia, Italy. ; Lunar Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. ; National Central University, Taipei, Taiwan. ; Departement of Physics, Oxford University, Oxford, UK. ; Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Berlin, Germany. Free University of Berlin, Institute of Geosciences, Malteserstrasse 74-100, Building Haus A, 12249 Berlin, Germany. ; Universita "Parthenope," Napoli, Italy. ; Helmholtz-Zentrum Berlin fur Materialien und Energie, Berlin, Germany. ; Osservatorio Astrofisico di Arcetri, INAF, Firenze, Italy. ; Agenzia Spaziale Italiana, Rome, Italy. ; NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA. Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742, USA. ; Istituto di Radioastronomia, INAF, Bologna, Italy. ; Institut fur Optische Sensorsysteme, DLR, Berlin, Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25613895" target="_blank"〉PubMed〈/a〉

Description: The New Horizons mission has provided resolved measurements of Pluto's moons Styx, Nix, Kerberos, and Hydra. All four are small, with equivalent spherical diameters of ~40 kilometers for Nix and Hydra and ~10 kilometers for Styx and Kerberos. They are also highly elongated, with maximum to minimum axis ratios of ~2. All four moons have high albedos (~50 to 90%) suggestive of a water-ice surface composition. Crater densities on Nix and Hydra imply surface ages of at least 4 billion years. The small moons rotate much faster than synchronous, with rotational poles clustered nearly orthogonal to the common pole directions of Pluto and Charon. These results reinforce the hypothesis that the small moons formed in the aftermath of a collision that produced the Pluto-Charon binary.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Weaver, H A -- Buie, M W -- Buratti, B J -- Grundy, W M -- Lauer, T R -- Olkin, C B -- Parker, A H -- Porter, S B -- Showalter, M R -- Spencer, J R -- Stern, S A -- Verbiscer, A J -- McKinnon, W B -- Moore, J M -- Robbins, S J -- Schenk, P -- Singer, K N -- Barnouin, O S -- Cheng, A F -- Ernst, C M -- Lisse, C M -- Jennings, D E -- Lunsford, A W -- Reuter, D C -- Hamilton, D P -- Kaufmann, D E -- Ennico, K -- Young, L A -- Beyer, R A -- Binzel, R P -- Bray, V J -- Chaikin, A L -- Cook, J C -- Cruikshank, D P -- Dalle Ore, C M -- Earle, A M -- Gladstone, G R -- Howett, C J A -- Linscott, I R -- Nimmo, F -- Parker, J Wm -- Philippe, S -- Protopapa, S -- Reitsema, H J -- Schmitt, B -- Stryk, T -- Summers, M E -- Tsang, C C C -- Throop, H H B -- White, O L -- Zangari, A M -- New York, N.Y. -- Science. 2016 Mar 18;351(6279):aae0030. doi: 10.1126/science.aae0030.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. hal.weaver@jhuapl.edu. ; Southwest Research Institute, Boulder, CO 80302, USA. ; NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. ; Lowell Observatory, Flagstaff, AZ 86001, USA. ; National Optical Astronomy Observatory, Tucson, AZ 26732, USA. ; SETI Institute, Mountain View, CA 94043, USA. ; Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA. ; Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA. ; Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA. ; Lunar and Planetary Institute, Houston, TX 77058, USA. ; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. ; Department of Astronomy, University of Maryland, College Park, MD 20742, USA. ; SETI Institute, Mountain View, CA 94043, USA. Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA. ; Massachusetts Institute of Technology, Cambridge, MA 02139, USA. ; University of Arizona, Tucson, AZ 85721, USA. ; Independent science writer, Arlington, VT, USA. ; Southwest Research Institute, San Antonio, TX 78238, USA. ; Stanford University, Stanford, CA 94305, USA. ; University of California, Santa Cruz, CA 95064, USA. ; Universite Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. ; Roane State Community College, Oak Ridge, TN 37830, USA. ; George Mason University, Fairfax, VA 22030, USA. ; Planetary Science Institute, Tucson, AZ 85719, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26989256" target="_blank"〉PubMed〈/a〉

Description: The New Horizons spacecraft mapped colors and infrared spectra across the encounter hemispheres of Pluto and Charon. The volatile methane, carbon monoxide, and nitrogen ices that dominate Pluto's surface have complicated spatial distributions resulting from sublimation, condensation, and glacial flow acting over seasonal and geological time scales. Pluto's water ice "bedrock" was also mapped, with isolated outcrops occurring in a variety of settings. Pluto's surface exhibits complex regional color diversity associated with its distinct provinces. Charon's color pattern is simpler, dominated by neutral low latitudes and a reddish northern polar region. Charon's near-infrared spectra reveal highly localized areas with strong ammonia absorption tied to small craters with relatively fresh-appearing impact ejecta.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Grundy, W M -- Binzel, R P -- Buratti, B J -- Cook, J C -- Cruikshank, D P -- Dalle Ore, C M -- Earle, A M -- Ennico, K -- Howett, C J A -- Lunsford, A W -- Olkin, C B -- Parker, A H -- Philippe, S -- Protopapa, S -- Quirico, E -- Reuter, D C -- Schmitt, B -- Singer, K N -- Verbiscer, A J -- Beyer, R A -- Buie, M W -- Cheng, A F -- Jennings, D E -- Linscott, I R -- Parker, J Wm -- Schenk, P M -- Spencer, J R -- Stansberry, J A -- Stern, S A -- Throop, H B -- Tsang, C C C -- Weaver, H A -- Weigle, G E 2nd -- Young, L A -- New Horizons Science Team -- New York, N.Y. -- Science. 2016 Mar 18;351(6279):aad9189. doi: 10.1126/science.aad9189.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lowell Observatory, Flagstaff, AZ 86001, USA. w.grundy@lowell.edu. ; Massachusetts Institute of Technology, Cambridge, MA 02139, USA. ; NASA Jet Propulsion Laboratory, La Canada Flintridge, CA 91011, USA. ; Southwest Research Institute, Boulder, CO 80302, USA. ; NASA Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. ; NASA Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. Carl Sagan Center, SETI Institute, Mountain View, CA 94043, USA. ; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. ; Universite Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. ; Department of Astronomy, University of Maryland, College Park, MD 20742, USA. ; Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA. ; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; Stanford University, Stanford, CA 94305, USA. ; Lunar and Planetary Institute, Houston, TX 77058, USA. ; Space Telescope Science Institute, Baltimore, MD, USA. ; Planetary Science Institute, Mumbai, India. ; Southwest Research Institute, San Antonio, TX 28510, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26989260" target="_blank"〉PubMed〈/a〉

Description: The appeasement effect of a United Nations climate summit on the German public Nature Climate Change, Published online: 9 October 2017; doi:10.1038/nclimate3409 As a global media event, COP 21 had the potential to enhance understanding and motivate political action. This study shows that although media coverage reached the German public and promoted conference-specific knowledge, this did not translate into active engagement.

Description: 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.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Filacchione, G -- De Sanctis, M C -- Capaccioni, F -- Raponi, A -- Tosi, F -- Ciarniello, M -- Cerroni, P -- Piccioni, G -- Capria, M T -- Palomba, E -- Bellucci, G -- Erard, S -- Bockelee-Morvan, D -- Leyrat, C -- Arnold, G -- Barucci, M A -- Fulchignoni, M -- Schmitt, B -- Quirico, E -- Jaumann, R -- Stephan, K -- Longobardo, A -- Mennella, V -- Migliorini, A -- Ammannito, E -- Benkhoff, J -- Bibring, J P -- Blanco, A -- Blecka, M I -- Carlson, R -- Carsenty, U -- Colangeli, L -- Combes, M -- Combi, M -- Crovisier, J -- Drossart, P -- Encrenaz, T -- Federico, C -- Fink, U -- Fonti, S -- Ip, W H -- Irwin, P -- Kuehrt, E -- Langevin, Y -- Magni, G -- McCord, T -- Moroz, L -- Mottola, S -- Orofino, V -- Schade, U -- Taylor, F -- Tiphene, D -- Tozzi, G P -- Beck, P -- Biver, N -- Bonal, L -- Combe, J-Ph -- Despan, D -- Flamini, E -- Formisano, M -- Fornasier, S -- Frigeri, A -- Grassi, D -- Gudipati, M S -- Kappel, D -- Mancarella, F -- Markus, K -- Merlin, F -- Orosei, R -- Rinaldi, G -- Cartacci, M -- Cicchetti, A -- Giuppi, S -- Hello, Y -- Henry, F -- Jacquinod, S -- Reess, J M -- Noschese, R -- Politi, R -- Peter, G -- England -- Nature. 2016 Jan 21;529(7586):368-72. doi: 10.1038/nature16190. Epub 2016 Jan 13.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉INAF-IAPS, Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy. ; LESIA, Observatoire de Paris/CNRS/UPMC/Universite Paris-Diderot, Meudon, France. ; Institute for Planetary Research, DLR, Berlin, Germany. ; Universite Grenoble Alpes, CNRS, IPAG, Grenoble, France. ; INAF-Osservatorio di Capodimonte, Napoli, Italy. ; UCLA, Los Angeles, California, USA. ; European Space Agency-ESTEC, Noordwijk, The Netherlands. ; Institut d'Astrophysique Spatial CNRS, Orsay, France. ; Dipartimento di Matematica e Fisica "Ennio De Giorgi", Universita del Salento, Lecce, Italy. ; Space Research Centre, Polish Academy of Sciences, Warsaw, Poland. ; NASA JPL, Pasadena, California, USA. ; Space Physics Research Laboratory, The University of Michigan, Michigan, Ann Arbor, USA. ; Universita di Perugia, Perugia, Italy. ; Lunar Planetary Laboratory, University of Arizona, Tucson, Arizona, USA. ; National Central University, Taipei, Taiwan. ; Department of Physics, Oxford University, Oxford, UK. ; Bear Fight Institute, Winthrop, Washington, USA. ; Helmholtz-Zentrum Berlin fur Materialien und Energie, Berlin, Germany. ; INAF-Osservatorio Astrofisico di Arcetri, Firenze, Italy. ; Agenzia Spaziale Italiana, Rome, Italy. ; Istituto di Radioastronomia-INAF, Bologna, Italy. ; Institute of Optical Sensor Systems, DLR, Berlin, Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26760209" target="_blank"〉PubMed〈/a〉

Description: Observations of cometary nuclei have revealed a very limited amount of surface water ice, which is insufficient to explain the observed water outgassing. This was clearly demonstrated on comet 9P/Tempel 1, where the dust jets (driven by volatiles) were only partially correlated with the exposed ice regions. The observations of 67P/Churyumov-Gerasimenko have revealed that activity has a diurnal variation in intensity arising from changing insolation conditions. It was previously concluded that water vapour was generated in ice-rich subsurface layers with a transport mechanism linked to solar illumination, but that has not hitherto been observed. Periodic condensations of water vapour very close to, or on, the surface were suggested to explain short-lived outbursts seen near sunrise on comet 9P/Tempel 1. Here we report observations of water ice on the surface of comet 67P/Churyumov-Gerasimenko, appearing and disappearing in a cyclic pattern that follows local illumination conditions, providing a source of localized activity. This water cycle appears to be an important process in the evolution of the comet, leading to cyclical modification of the relative abundance of water ice on its surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉De Sanctis, M C -- Capaccioni, F -- Ciarniello, M -- Filacchione, G -- Formisano, M -- Mottola, S -- Raponi, A -- Tosi, F -- Bockelee-Morvan, D -- Erard, S -- Leyrat, C -- Schmitt, B -- Ammannito, E -- Arnold, G -- Barucci, M A -- Combi, M -- Capria, M T -- Cerroni, P -- Ip, W-H -- Kuehrt, E -- McCord, T B -- Palomba, E -- Beck, P -- Quirico, E -- VIRTIS Team -- England -- Nature. 2015 Sep 24;525(7570):500-3. doi: 10.1038/nature14869.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Istituto di Astrofisica e Planetologia Spaziali - INAF, via del fosso del cavaliere 100, 00133 Rome, Italy. ; Institute for Planetary Research, DLR, Rutherfordstrasse 2, 12489 Berlin, Germany. ; LESIA-Observatoire de Paris, CNRS, Universite Pierre et Marie Curie, Universite Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France. ; Universite Grenoble Alpes - CNRS Institut de Planetologie et Astrophysique de Grenoble, Batiment D de Physique, BP 53, 38041 Grenoble Cedex 9, France. ; University of California, Los Angeles, California 90095, USA. ; Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward Street, Ann Arbor, Michigan 48109, USA. ; National Central University, No. 300, Jhongda Road, Jhongli District, Taoyuan City, 32001 Taipei, Taiwan. ; Bear Fight Institute, 22 Fiddler's Road, Box 667, Winthrop, Washington 98862, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26399830" target="_blank"〉PubMed〈/a〉