The Moon is an integral part of the Earth-Moon system, it is a witness to more than 4.5 b. y. of solar system history, and it is the only planetary body except Earth for which we have samples from known locations. The Moon is thus a key object to understand our Solar System. The Moon is our closest companion and can easily be reached from Earth at any time, even with a relatively modest financial budget. Consequently, the Moon was the first logical step in the exploration of our solar system before we pursued more distant targets such as Mars and beyond. The vast amount of knowledge gained from the Apollo and other lunar missions of the late 1960's and early 1970's demonstrates how valuable the Moon is for the understanding of our planetary system (e.g. [1], [2]). Even today, the Moon remains an extremely interesting target scientifically and technologically. New data have helped to address some of our questions about the Earth-Moon system, but many remain and new questions arose. In particular, the discovery of water at the lunar poles, and water and hydroxyl bearing surface materials and volatiles, as well as the discovery of young volcanism have changed our view of the Moon. Therefore, returning to the Moon is the critical stepping-stone to further exploring our immediate planetary neighborhood. Here, we present scientific and technological arguments for a Small Lunar Explorations Orbiter (S-LEO) dedicated to investigate so far unsolved questions and processes. Numerous space-faring nations have realized and identified the unique opportunities related to lunar exploration and have planned missions to the Moon within the next few years. Among these missions, S-LEO will be unique, because of its unprecedented spatial and spectral resolutions. S-LEO will significantly improve our understanding of the lunar environment in terms of composition, surface ages, mineralogy, physical properties, and volatile and regolith processes. S-LEO will carry an entire suite of innovative, complementary technologies, including high-resolution camera systems, several spectrometers that cover previously unexplored parts of the electromagnetic spectrum over a broad range of wavelengths, and a communication system to interact with landed equipment on the farside. The Small Lunar Explorations Orbiter concept is technologically challenging but feasible, and will gather unique, integrated, interdisciplinary data sets that are of high scientific interest and will provide an unprecedented new context for all other international lunar missions. The most visible mission goal of S-LEO will be the identification and mapping of lunar volatiles and investigating their origin and evolution with high spatial as well as spectral resolution. Therefore, in addition to mapping the geological context in the sub-meter range, a screening of the electromagnetic spectrum within a very broad range will be performed. In particular, spectral mapping in the ultraviolet and mid-infrared will provide insight into mineralogical and thermal properties so far unexplored in these wavelength ranges. The determination of the dust distribution in the lunar orbit will provide information about processes between the lunar surface and exosphere supported by direct observations of lunar flashes. Measuring of the radiation environment will finally complete the exosphere investigations. Combined observations based on simultaneous instrument adjustment and correlated data processing will provide an integrated geological, geochemical and geophysical database that enables: • the exploration and utilization of the Moon in the 21st century; • the solution of fundamental problems of planetology concerning the origin and evolution of terrestrial bodies; • understanding the uniqueness of the Earth-Moon System and its formation and evolution; • the absolute calibration of the impact chronology for the dating of solar system processes; • deciphering the lunar regolith as record for space environmental conditions; • mapping lunar resources. S-LEO is featuring a set of unique scientific capabilities w.r.t. other planned missions including: (1) dedicated observation of volatiles (mainly H2O and OH), their formation and evolution in direct context with the geological and mineralogical surface with high spectral and spatial resolution (< 1m/px); (2) besides the VIS-NIR spectral range so far uncovered wavelengths in the ultraviolet (0.2 – 0.4 µm) and mid-infrared (7 - 14 µm) will be mapped to provide mineralogical context for volatile processes (e.g. sources of oxygen); (3) detection of rock-forming elements by means of x-ray fluorescence in the spectral range of .5-10 keV in order to constrain the composition of key elements of lunar surface materials; (4) monitoring of dust and radiation in the lunar environment and its interaction with the surface; and (5) monitoring of present-day meteoroitic impacts. In 2009 ESA commissioned a Mobile Payload Element (MPE) to assist the ESA Lunar Lander mission. The MPE, currently under study in Germany, is designed to be a small, autonomous, innovative vehicle of roughly 10 12 kg for scouting the environment in the vicinity of the lunar landing site. The novel capability of the MPE will be to acquire samples of lunar soil in an area of >100m around the lander and to bring them back to the spacecraft for analysis by on-board instruments. This will enable access to soils that are less contaminated by the descent propulsion system plumes to increase the chances of detection of any indigenous lunar volatiles. The MPE shall acquire samples of regolith with landing-induced contamination being below the detection limit of the associated volatile-seeking instruments. Subsurface regolith sampling is preferable to understand the concentration of volatiles as a function of depth. Additional benefits for the overall science accomplished by a Lunar Lander mission could be obtained if the MPE were to conduct ‘field geology’ type observations and measurements along its traverses, such as geochemical and mineralogical in situ investigations with dedicated instruments on rocks, boulders and regolith. This would dramatically expand the effective area studied by the ESA Lunar Lander mission. Based on technology trades the baseline concept for the MPE system is composed by a 4-wheel active chassis with wheels, a power supply with fixed solar generators plus a secondary battery, a thermal system with active heating and passive insulation, a sensor package for autonomous operations and a VHF/UHF communication system between MPE and the Lander. One unique scientific aspect of the MPE could be the in situ study of rocks, boulders and lithic (rock) fragments which otherwise would only be amenable to measurements using any instrument heads mounted on the lander robotic arm (provided any rocks were within reach of the arm). To fulfill the science objectives, the MPE will be equipped with a stereo camera, the PLUTO mole subsurface regolith sampling system (as flown on Beagle 2) as well as a close-up imager. This instrument package allows acquisition of regolith samples from both illuminated and locally shaded terrain, sampling from the subsurface and from underneath large boulders and documentation of the samples acquired by close-up imaging of the sample site, ideally before and after sample acquisition. A suite of terrain temperature sensors is implicitly included to provide context for the samples acquired from permanently shadowed locations or below the surface, but also to contribute to landing site general science. As an option for the in-situ characterization of the sample material with respect to mineralogy and possibly volatile content, spectrometer experiments or a color capability of the camera could be added. Further, a laboratory environment is currently being established at Freie Universitat Berlin in order to allow sample-based geochemical measurements of key rock-forming elements in the soft X-Ray domain (.5-10 keV). The laboratory is used for the hardware development of X-Ray spectrometer experiments to be employed on lunar orbiter and on lunar lander missions. References: [1] H. Hiesinger, J.W. Head, New Views of Lunar Geoscience: An Introduction and Overview, In: Ne Views of the Moon (B.L. Jolliff et al. eds.) Rev. Min. Geochem., 60, 1-81 (2006). [2] R. Jaumann, The Moon, In: Encyclopedia of Astrobiology, M. Gargaud et al. (eds.), Vol. 2, Springer, 280-282 (2011).

Scientific objectives R. Jaumann1, 2, A. Coates3, E. Hauber1, H. Hoffmann1, N. Schmitz1, L. Le Deit1, D. Tirsch1, G. Paar3, A. Griffiths3, and the PanCam Team 1Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, Berlin, Germany. 2Institute for Geological Sciences, Free University Berlin, Germany. 3Mullard Space Science Laboratory, Univ. College London, UK. mail to: ralf.jaumann@dlr.de

The aim was to evaluate a method for visualizing fs laser pulse induced microincisions inside crystalline lens tissue. Porcine lenses were modified ex vivo by fs laser pulses to create defined planes at which lens fibers separate. Lens fiber orientation and fs laser-induced micro-incisions were examined using a confocal laser scanning microscope. Microincision visualization revealed different cutting effects depending on fs laser pulse energy, ranging from altered tissue scattering properties with all fibers intact to definite fiber separation with a wide gap. CLSM permits visualization and analysis and thereby control of fs laser pulse induced microincisions inside crystalline lens tissue.

One of the unique features of the Martian climate is the existence of CO2 ice clouds formed from the main atmospheric constituent. These clouds were thought to form only in the polar night, where the CO2 condenses on the winter pole. Recently, Mars Express has observed several occurrences of high-altitude CO2 clouds mainly in the equatorial areas. We use observations by OMEGA (Bibring et al., 2004) and HRSC (Jaumann et al., 2007) to analyse these high-altitude CO2 cloud occurrences. As shown by Montmessin et al. (2007), the spectral signature of CO2 clouds seen in OMEGA spectra exhibits one or two distinct peaks that appear inside a strong CO2 gas absorption band centered at 4.3 microns. We have mapped this spectral signature with a 3-sigma detection method. The mapping of the clouds in three Martian years of OMEGA data have provided a cloud dataset of about 60 occurrences. These observations provide information on the spatial and seasonal distribution of CO2 cloud formation at the equatorial region and information on variations of cloud particle size, related to the variations in the spectral signature of the clouds. The clouds exhibit variable morphology from clearly convective type, round structures (about 15% of all cases), to more filamented, cirrus type clouds. We have also analysed some properties of the clouds (altitude, particle size, opacity) using two shadow observations by OMEGA. We will present the results acquired so far using the datasets of the two instruments. OMEGA shows that the clouds exhibit interannual variations, but in general the clouds are concentrated on specific spatial and seasonal bins, mainly around the equator and around Ls=45 and Ls=135, before and after the northern summer solstice. Most high-altitude clouds are observed in a longitudinally limited area, between 150 W and 30 E. During the first year of observations the cloud shadow was also observed on two orbits. The analysis of the cloud observations have revealed that the clouds are thick with near-infrared opacities (at 1 micron) between 0.2–0.7, they are at around 80 km altitude in the atmosphere and the mean particle effective radius is mainly 1-2microns, although submicronic particles are also observed. HRSC images have also been analysed and the presence of these high-altitude clouds in them has been confirmed. The HRSC observes through a set of colour filters, which allows for the determination of the cloud altitude through photogrammetry analysis and westward wind speeds at cloud altitude through relative cloud movement between images taken through two filters at different times. HRSC observations provide also a higher spatial resolution, as well as a wider image, providing more context for mapping the cloud morphology. Preliminary analysis of the HRSC orbits have revealed CO2 cloud altitudes ranging from 59 km to 83 km, each with an altitude accuracy of +/- 1-2 km and cloud (wind) speeds of 15-107 m/s (+/-15m/s). One cloud, observed far from the equator, shows a varying altitude of 53-67 km in a latitude bin of 46-53 S. We will present the datasets and cloud characteristics acquired so far in the analysis.

Angewandte ChemieVolume 94, Issue 6 p. 464-465 Zuschriften Einfacher Syntheseweg zu 7,7-Dimethyl-6-methylentricyclo[6.2.1.01,5]undec-9-en und Sesquiterpenen vom Zizaen-Typ† Prof. H. M. R. Hoffmann, Prof. H. M. R. Hoffmann Institut für Organische Chemie der Universität Schneiderberg 1 B, D-3000 HannoverSearch for more papers by this authorRolf Henning, Rolf Henning Institut für Organische Chemie der Universität Schneiderberg 1 B, D-3000 HannoverSearch for more papers by this authorDr. Olgierd R. Lalko, Dr. Olgierd R. Lalko Institut für Organische Chemie der Universität Schneiderberg 1 B, D-3000 HannoverSearch for more papers by this author Prof. H. M. R. Hoffmann, Prof. H. M. R. Hoffmann Institut für Organische Chemie der Universität Schneiderberg 1 B, D-3000 HannoverSearch for more papers by this authorRolf Henning, Rolf Henning Institut für Organische Chemie der Universität Schneiderberg 1 B, D-3000 HannoverSearch for more papers by this authorDr. Olgierd R. Lalko, Dr. Olgierd R. Lalko Institut für Organische Chemie der Universität Schneiderberg 1 B, D-3000 HannoverSearch for more papers by this author First published: Juni 1982 https://doi.org/10.1002/ange.19820940630Citations: 11 † Diese Arbeit wurde von der Deutschen Forschungsgemeinschaft und dem Fonds der Chemischen Industrie unterstützt. Wir danken Prof. G. Ohloff für eine Probe Zizansäure 5d. AboutPDF ToolsRequest permissionAdd to favorites ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinked InRedditWechat No abstract is available for this article.Citing Literature Volume94, Issue6Juni 1982Pages 464-465 This is the German version of Angewandte Chemie. Note for articles published since 1962: Do not cite this version alone. Take me to the International Edition version with citable page numbers, DOI, and citation export. We apologize for the inconvenience. RelatedInformation

The synthesis of a protected 9,9',10,10'-tetradehydro-disorazole C-1 is described. A C1-C8 oxazole fragment with an E-vinylic iodide terminus is coupled to a suitable C9-C19 enyne. The resulting omega-hydroxycarboxylic acid is cyclodimerized stepwise via intermolecular esterification, followed by lactonization. In addition, simplified masked analogues of disorazole C, with truncated side chains are prepared. ((c) Wiley-VCH Verlag GmbH & Co. KGaA, 69451 Weinheim, Germany, 2006).

1,1-Dimethoxy-2-propanone Chlorotriethylsilane Trimethylsilyl trifluromethanesulfonate Chlorotrimethlysilane 2,5-Dimethylfuran Keywords: cycloaddition; 2-alpha-benzyloxy-8-oxabicyclo[3.2.1]oct-6-en-3-one; oxyallyl cations; oxyally dienes; cycloadducts; halogenated precursors; intramolecular cycloadditions; bicyclic scaffold; tetrahydropyrans; waste disposal

AbstractFor Abstract see ChemInform Abstract in Full Text.

Scopolines 4 and the noradamantane scaffold are accessible from 8-oxabicyclo[3.2.1]oct-6-en-3-ones such as 6 by a concise route involving introduction of an axial amino nitrogen at C3, epoxidation, and cyclization. The resulting cage molecules are versatile drug leads.