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Oil-producing yeast cells are a valuable alternative source for palm oil production and, hence, may be one important piece of the puzzle for a more sustainable future. To achieve a high-quality product, the lipid composition inside oil-producing yeast cells is a crucial parameter for effective process control. Typically, the lipid composition is determined by off-line gas chromatography. A faster, less cumbersome approach is proposed here, by using non-invasive in-line Raman spectroscopy. A fed-batch fermentation of C. oleaginosus – a well-known oleaginous yeast – is used as model experiment to highlight the potential of Raman spectroscopy for in-line lipidomics. The temporal progression of biomass formation, lipid production and glucose consumption are determined based on PLS-regression models allowing process-relevant information on time to be accessed. Additionally, Gaussian curve fitting was applied to extract increasing and decreasing trends of saturated and unsaturated fatty acids produced by C. oleaginosus throughout the fermentation process.

J.M.O. acknowledges financial support from the Portuguese Foundation for Science and Technology (FCT) and the European Social Fund (ESF) through the PhD grant SFRH/BD/131700/2017. The work leading to these results has received funding from the European Research Council under the European Community's H2020 2014-2021 ERC grant Agreement nffi 669416 "Lucky Star". We thank S. Para who supported some travels to observe the 5 October 2017 occultation. T.B. was supported for this research by an appointment to the National Aeronautics and Space Administration (NASA) Post-Doctoral Program at the Ames Research Center administered by Universities Space Research Association (USRA) through a contract with NASA. We acknowledge useful exchanges with Mark Gurwell on the ALMA CO observations. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. J.L.O., P.S.-S., N.M. and R.D. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709), they also acknowledge the financial support by the Spanish grant AYA-2017-84637-R and the Proyecto de Excelencia de la Junta de Andalucia J.A. 2012-FQM1776. The research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no. 687378, as part of the project "Small Bodies Near and Far" (SBNAF). P.S.-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 "LEO-SBNAF". The work was partially based on observations made at the Laboratorio Nacional de Astrofisica (LNA), Itajuba-MG, Brazil. The following authors acknowledge the respective CNPq grants: F.B.-R. 309578/2017-5; R.V.-M. 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3 and 305917/2019-6; M.A. 427700/20183, 310683/2017-3, 473002/2013-2. This study was financed in part by the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior -Brasil (CAPES) -Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). G.B.R. acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 and CAPES-PRINT/UNESP grant 88887.571156/2020-00, M.A. FAPERJ grant E26/111.488/2013 and A.R.G.Jr. FAPESP grant 2018/11239-8. B.E.M. thanks CNPq 150612/2020-6 and CAPES/Cofecub-394/2016-05 grants. Part of the photometric data used in this study were collected in the frame of the photometric observations with the robotic and remotely controlled telescope at the University of Athens Observatory (UOAO; Gazeas 2016). The 2.3 m Aristarchos telescope is operated on Helmos Observatory by the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing of the National Observatory of Athens. Observations with the 2.3 m Aristarchos telescope were carried out under OPTICON programme. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. The 1. 2m Kryoneri telescope is operated by the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing of the National Observatory of Athens. The Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA) is managed by the Fondazione Clement Fillietroz-ONLUS, which is supported by the Regional Government of the Aosta Valley, the Town Municipality of Nus and the "Unite des Communes valdotaines Mont-Emilius". The 0.81 m Main Telescope at the OAVdA was upgraded thanks to a Shoemaker NEO Grant 2013 from The Planetary Society. D.C. and J.M.C. acknowledge funds from a 2017 'Research and Education' grant from Fondazione CRT-Cassa di Risparmio di Torino. P.M. acknowledges support from the Portuguese Fundacao para a Ciencia e a Tecnologia ref. PTDC/FISAST/29942/2017 through national funds and by FEDER through COMPETE 2020 (ref. POCI010145 FEDER007672). F.J. acknowledges Jean Luc Plouvier for his help. S.J.F. and C.A. would like to thank the UCL student support observers: Helen Dai, Elise Darragh-Ford, Ross Dobson, Max Hipperson, Edward Kerr-Dineen, Isaac Langley, Emese Meder, Roman Gerasimov, Javier Sanjuan, and Manasvee Saraf. We are grateful to the CAHA, OSN and La Hita Observatory staffs. This research is partially based on observations collected at Centro Astronomico HispanoAleman (CAHA) at Calar Alto, operated jointly by Junta de Andalucia and Consejo Superior de Investigaciones Cientificas (IAA-CSIC). This research was also partially based on observation carried out at the Observatorio de Sierra Nevada (OSN) operated by Instituto de Astrofisica de Andalucia (CSIC). This article is also based on observations made with the Liverpool Telescope operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Partially based on observations made with the Tx40 and Excalibur telescopes at the Observatorio Astrofisico de Javalambre in Teruel, a Spanish Infraestructura Cientifico-Tecnica Singular (ICTS) owned, managed and operated by the Centro de Estudios de Fisica del Cosmos de Aragon (CEFCA). Tx40 and Excalibur are funded with the Fondos de Inversiones de Teruel (FITE). A.R.R. would like to thank Gustavo Roman for the mechanical adaptation of the camera to the telescope to allow for the observation to be recorded. R.H., J.F.R., S.P.H. and A.S.L. have been supported by the Spanish projects AYA2015-65041P and PID2019-109467GB-100 (MINECO/FEDER, UE) and Grupos Gobierno Vasco IT1366-19. Our great thanks to Omar Hila and their collaborators in Atlas Golf Marrakech Observatory for providing access to the T60cm telescope. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege, and performed in collaboration with Cadi Ayyad University of Marrakesh. E.J. is a FNRS Senior Research Associate., Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range similar to 8 km to similar to 190 km, corresponding to pressure levels from 9 mu bar down to a few nanobars. Results. (i) A pressure of 1.18 +/- 0.03 mu bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 mu bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude., Portuguese Foundation for Science and Technology SFRH/BD/131700/2017, European Social Fund (ESF) SFRH/BD/131700/2017, European Research Council under the European Community's H2020 2014-2021 ERC grant 669416, Spanish Government SEV-2017-0709 AYA-2017-84637-R AYA-RTI2018-098657-J-I00, Junta de Andalucia 2012-FQM1776, European Union's Horizon 2020 Research and Innovation Programme, as part of the project "Small Bodies Near and Far" (SBNAF) 687378, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Fundacao de Apoio a Pesquisa do Distrito Federal (FAPDF) 309578/2017-5 304544/2017-5 401903/2016-8 308150/2016-3 305917/2019-6 427700/2018-3 310683/2017-3 473002/2013-2, Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) 001, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) 465376/2014-2 CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 CAPES-PRINT/UNESP grant 88887.571156/2020-00, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ) E26/111.488/2013, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2018/11239-8, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) 150612/2020-6, European Union's Horizon 2020 research and innovation programme 730890, Regional Government of the Aosta Valley, Town Municipality of Nus, Unite des Communes valdotaines Mont-Emilius, Planetary Society, Fondazione CRT-Cassa di Risparmio di Torino, Portuguese Foundation for Science and Technology PTDC/FISAST/29942/2017, FEDER through COMPETE 2020 POCI010145 FEDER007672, UK Research & Innovation (UKRI), Science & Technology Facilities Council (STFC), Fondos de Inversiones de Teruel (FITE), Spanish Government AYA2015-65041P PID2019-109467GB-100, Grupos Gobierno Vasco IT1366-19, Fonds de la Recherche Scientifique - FNRS PDR T.0120.21, University of Liege, CAPES/Cofecub-394/2016-05

The landscape of the Rhine River valley between Chur and Ilanz bears the signature of two remarkable events that happened shortly after the end of the Last Glacial Period. Two huge rockslides blocked the river and formed upstream lakes. The Flims rockslide (10 km3) liquefied about 1 km3 of alluvial and lacustrine sediments, and the liquefied slurry flowed down the Vorderrhein Valley, over the older Tamins rockslide barrier, and far up the Hinterrhein Valley. The deposit of this slurry, termed Bonaduz gravel, rafted huge masses of rockslide material (‘tumas’). Soon after these momentous events, the Vorderrhein and Hinterrhein rivers cut down through the rockslide deposits and the Bonaduz gravel, while Lake Ilanz, impounded behind the Flims rockslide barrier, drained in a series of huge downstream floods. A legacy of these events is the Rhine gorge, which was cut by the Vorderrhein River where it flowed across the Flims rockslide barrier.

The origin of the Bonaduz gravel (Switzerland) in the vicinity of the large Holocene Flims rock slide deposits has been discussed for a century. The internal structure shows many features that imply transport as an over-sized mud/debris stream. This flow of gravel, sand and fines must have been triggered by the mobilisation of the valley alluvium by the impact of the rock slide. The mobilised mud with a volume of several 100 million m 3 must have had enormous transport capacities as large units of loose material were transported over kilometres without breaking apart. Accordingly, the shear forces in the flow must have been negligible. Similar features have been found at several other sites in the Alps, all in the vicinity of large rock slides. Our interpretation of these sediments as catastrophic mass movement deposits suggests that such events could happen again, also in other parts of the world.

The huge Flims rockslide in the Swiss Alps has been the focus of scientific study for over 100 years, whereas a nearby rockslide at Tamins that occurred only slightly earlier, is understudied. Field investigations of the Tamins rockslide has provided new insights in its history, as well as that of the Flims rockslide. These investigations, complemented by interpretation of LiDAR imagery, has allowed us to document the sequence of postglacial events in the Vorderrhein river valley. We confirm the hypothesis that the Flims rockslide induced a large debris stream that transported huge volumes of liquefied alluvium, as well as large rafts of rock slide debris (Toma hills), many kilometers both down the Vordderrhein and up the Hinterrhein, its major tributary. The older Tamins rockslide partially impeded and was overrun by the debris stream, dividing it into two lobes.

A concept to electrically control the scattering of light is introduced. The idea is to embed noble metal nanoparticles in an electro-optical material such as a liquid crystal in order to induce a spectral shift of the particle plasmon resonance by applying an electric field. Light scattering experiments on single gold nanoparticles show that spherically shaped nanoparticles become optically spheroidal when covered by an anisotropic liquid crystal. The two particle plasmon resonances of the optically spheroidal gold nanoparticles can be spectrally shifted by up to 50 meV when electric fields of more than 10 kV/cm are applied.

The Flims rockslide blocked at about 8,200 year BP the Vorderrhein river and so gave rise to the Paleo-Lake Ilanz. Shortly after the filling of the lake a severe flood event happened. The lake emptied not totally, but remained at a lower level for a long time. After important and perhaps even complete filling of the remaining basin with sediments the incision in the dam restarted and progressed in several smaller steps. Based on the detailed field works, the following sequence of the events can be envisioned: The Tamins rockslide occurred first, damming Lake Bonaduz; the Flims slide come down soon after and probably entered in this lake; at the same time the alluvium was mobilized and resedimented as Bonaduz gravel; Lake Ilanz was dammed to a level between 820 and 936 m for very short time; the dam broke partly and a flood happened; the remaining lake survived for a long time and was filled up; the Rhein river eroded the floodplain down to the actual level.

Im Gebiet der Zugspitze, dem mit 2962 m ü.M. höchsten Berg Deutschlands, sind auch die bedeutendsten Permafrostvorkommen des Landes zu finden. Der Felsgrat der Zugspitze ist steil und stark bebaut. Schon während der Bauarbeiten in den 1960er Jahren wurden massives Eis in Klüften und gefrorene Lockersedimente entdeckt. Allfällige Stabilitätsprobleme durch Permafrostdegradation können entscheidende Konsequenzen auf Bauwerke haben. Deshalb wurde im August 2007 für langfristige Permafrostbeobachtung eine Bohrung quer durch den Gipfelgrat gemacht und mit einer Thermistorenkette ausgestattet. In einer Vorstudie wurden die Temperaturverhältnisse mit Computermodellen simuliert. Resultate zeigen Permafrost mit Temperaturen bis etwa -3 °C in der Nordseite und in Teilen der Südseite. Die Permafrostgrenze verläuft im Inneren des Grates und ist im oberen Bereich fast senkrecht. Die nach der Realisierung der Bohrung gemessenen Temperaturen sind etwas niedriger als im Modell, stimmen aber im Allgemeinen gut mit den Ergebnissen der Simulation überein, insbesondere wenn auch transiente Effekte und der Einfluss latenter Wärme berücksichtigt werden. Monitoring und Modellstudien des Permafrosts in der Zugspitze werden im Rahmen von internationalen Projekten weitergeführt und ausgebaut.

We report on electrically controlled light scattering where electric fields are used to spectrally shift the plasmon resonance of spherical noble metal nanoparticles. Applying external electric fields to the liquid crystal induces a reorientation of the molecules and therefore a reorientation of the anisotropy. This results in a field-induced shift of the plasmon peak , which may be useful for the realization of novel optoelectronic switching devices.

Summary form only given. Electrically controlled switching of light is a key ingredient in modern optical communication and display systems. Up to now such optoelectronic scattering devices do not take advantage of noble metal nanoparticles, which are known to act as strong light scatterers when the frequency of the light is in the spectral range of the particle plasmon resonance. This resonance frequency not only depends on particle properties but also on the refractive index of the surrounding medium. We report on electrically controllable light scattering where electric fields are used to spectrally shift the particle plasmon resonance of spherical noble metal nanoparticles. The basic idea is that the electric field alters the refractive index of the embedding dielectric matrix. For this purpose, spherical noble metal nanoparticles are incorporated in a liquid crystal. An applied electric field aligns the liquid crystal molecules leading to an anisotropic refractive index and thus to a polarization dependent spectral shift of the particle plasmon. Light scattering spectra of an individual gold nanoparticle taken with a dark-field microscope setup are shown.