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Making sense of the implications of climate engineering approaches (solar radiation management, SRM; and carbon dioxide removal, CDR) at planetary scales occurs via a host of methods that calculate, project, and imagine the future in distinct ways. We take a systemic and synthesizing view of some of the (inter)disciplinary methods by which these futures are derived: climate and integrated assessment modeling, 'deductive' modes of social science inquiry, deliberative stakeholder engagement, and foresight-based scenarios. We speak to the epistemologies, objectives, and user communities surrounding these research practices, highlighting that different modes of constructing and interpreting evidence about an unformed future yield different kinds of results and signals for actions to be taken. We show how different methods for exploring 'futures' form an evolving history of how the risks of CE have been assessed (or constructed), and conclude by echoing calls for a stronger shared understanding of the practices and politics that underpin future-oriented research. © 2019, The Author(s).

Climate models aiming to explore how global warming can be limited to the Paris Agreement targets of 1.5 or 2 degrees Celsius usually invoke sweeping technical and societal transformations, including the extensive use of carbon dioxide removal technologies. In our Perspective, we argue that this reliance on technologies that may be difficult or impossible to implement at the required scale makes the Paris temperature goals increasingly less plausible, drawing into question a key basis and shared anchor of current climate science, politics, and activism. A way forward is the innovative concept of nationally determined contributions to climate risk reduction, introduced in the Paris Agreement, which fosters greater democratic engagement, accountability, and meaningful change toward mitigating and adapting to climate change.

Making sense of the implications of climate engineering approaches (solar radiation management, SRM; and carbon dioxide removal, CDR) at planetary scales occurs via a host of methods that calculate, project, and imagine the future in distinct ways. We take a systemic and synthesizing view of some of the (inter)disciplinary methods by which these futures are derived: climate and integrated assessment modeling, 'deductive' modes of social science inquiry, deliberative stakeholder engagement, and foresight-based scenarios. We speak to the epistemologies, objectives, and user communities surrounding these research practices, highlighting that different modes of constructing and interpreting evidence about an unformed future yield different kinds of results and signals for actions to be taken. We show how different methods for exploring 'futures' form an evolving history of how the risks of CE have been assessed (or constructed), and conclude by echoing calls for a stronger shared understanding of the practices and politics that underpin future-oriented research.

Zukünftige Antriebstechnologien sowie neue Fabrik- und Logistikkonzepte verändern die Rahmenbedingungen der Automobilproduktion grundlegend. Schon heute muss die Strukturlayoutplanung Innovationen und Unsicherheiten in Form von mehr Varianten, abgestimmt in sehr kurzer Zeit, durch die Einbeziehung von weiteren Know-how-Trägern berücksichtigen. Neue Herausforderungen, wie die Planung der Batteriefertigungen, müssen schnell und intuitiv gelöst werden. Einen Beitrag dafür liefert dieser Artikel.
 
Future technologies in automotive mobility as well as new factory and logistic concepts are changing the framework in car production. Innovations and uncertainties (e. g. the impact of new technologies) have to be taken in consideration for the factory of the future. New tasks, such as planning the assembly of batteries, need to be solved fast and intuitively. This paper presents an approach to this topic.

Despite extensive efforts, greenhouse gases continue to be emitted in vastamounts, with potentially devastating consequences around the world. This iswhy targeted interventions in the climate system, known collectively as 'climateengineering', are receiving increased attention. Proposed approaches are oftendivided into two groups: those intended to remove carbon dioxide from theatmosphere and those intended to reduce the amount of solar energy that reachesthe Earth's surface or is trapped in the atmosphere. There are some similaritiesbetween the two classes of activities, but they often raise different physical,political, and governance concerns. This series provides an introduction to eachset of approaches.

Despite extensive efforts, greenhouse gases continue to be emitted in vastamounts, with potentially devastating consequences around the world. This iswhy targeted interventions in the climate system, known collectively as 'climateengineering', are receiving increased attention. Proposed approaches are oftendivided into two groups: those intended to remove carbon dioxide from theatmosphere and those intended to reduce the amount of solar energy that reachesthe Earth's surface or is trapped in the atmosphere. There are some similaritiesbetween the two classes of activities, but they often raise different physical,political, and governance concerns. This series provides an introduction to eachset of approaches.

Das Forschungsprojekt THG-Holzbau hat das Ziel darzustellen, welchen Einfluss Bauen mit Holz im Rahmen des Klimaschutzes auf nationaler Ebene haben kann. Hierzu verknüpft das Projekt die Erfassung der ökologischen Qualität von Holzhäusern gegenüber mineralischen Gebäuden mit Hilfe von Gebäudeökobilanzen mit den politischen Zielen des Klimaschutzes. Der mögliche Einfluss von Bauen mit Holz - durch die Substitution von mineralischen Gebäuden mit Holzgebäuden - kann so auf großer Maßstabsebene dargestellt werden.

The high-resolution, dual channel, visible and near-infrared spectrograph CARMENES offers exciting opportunities for stellar and exoplanetary research on M dwarfs. In this work we address the challenge of reaching the highest radial velocity precision possible with a complex, actively cooled, cryogenic instrument, such as the near-infrared channel. We describe the performance of the instrument and the work flow used to derive precise Doppler measurements from the spectra. The capability of both CARMENES channels to detect small exoplanets is demonstrated with the example of the nearby M5.0 V star CD Cet (GJ 1057), around which we announce a super-Earth (4.0 ± 0.4 M· ) companion on a 2.29 d orbit. ; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

The high-resolution, dual channel, visible and near-infrared spectrograph CARMENES offers exciting opportunities for stellar and exoplanetary research on M dwarfs. In this work we address the challenge of reaching the highest radial velocity precision possible with a complex, actively cooled, cryogenic instrument, such as the near-infrared channel. We describe the performance of the instrument and the work flow used to derive precise Doppler measurements from the spectra. The capability of both CARMENES channels to detect small exoplanets is demonstrated with the example of the nearby M5.0 V star CD Cet (GJ 1057), around which we announce a super-Earth (4.0 ± 0.4 M· ) companion on a 2.29 d orbit. © 2020 ESO. ; CARMENES is an instrument for the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto (Almeria, Spain), operated jointly by the Junta de Andalucia and the Instituto de Astrofisicade Andalucia (CSIC). CARMENES was funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Program and DFG Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. Based on data from the CARMENES data archive at CAB (INTA-CSIC). We acknowledge financial support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 83 24 28, the Deutsche Forschungsgemeinschaft through project RE 1664/14-1, the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the European FEDER/ERF funds through projects AYA2018-84089, ESP2016-80435-C2-1-R, AYA2016-79425-C3-1/2/3-P, AYA2015-69350-C3-2-P, the Centre of Excellence "Severo Ochoa" and "Maria de Maeztu" awards to the Instituto de Astrofisica de Canarias (SEV-2015-0548), Instituto de Astrofisica de Andalucia (SEV-2017-0709), and Centro de Astrobiologia (MDM-2017-0737), and the Generalitat de Catalunya/CERCA program. ; Peer reviewed

Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science ; This research was supported by the following programs, grants, and fellowships: Spanish Ministry for Science, Innovation and Universities (MCIU) ESP2014-54062-R, ESP2014-54362P, AYA2015-69350-C3-2-P, BES-2015-074542, AYA2016-79425-C3-1/2/3-P, ESP2016-76076-R, ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87143-R, ESP2017-87676-C05-02-R, ESP-2017-87676-2-2, RYC-2012-09913 (>Ramon y Cajal> program), and FPU15/01476; Israel Science Foundation grant 848/16, CONICYT-FONDECYT/Chile Postdoctorado 3180405; Deutsches Zentrum fur Luft-un Raumfahrt (DLR) 50OW0204 and 50OO1501; Italian Minister of Instruction, University and Research (MIUR), FFABR 2017; University of Rome Tor Vergata, >Mission: Sustainability 2016> fund; European Research Council under the European Union Horizon 2020 research and innovation program 694513; Mexican national council for science and technology CONACYT, CVU 448248; the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709); Generalitat de Catalunya/CERCA program; Fondo Europeo de Desarollo Regional (FEDER); German Science Foundation (DFG) Research Unit FOR2544 >Blue Planets around Red Stars> and Priority Programs SPP 1833, >Building a Habitable Earth> and SPP 1992, >Exploring the Diversity of Extrasolar Planets> NSF grants PHY17-48958 and PHY-1607761; Swiss National Science Foundation under grant BSGIO_155816 >PlaneltsInTime' and within the framework of the NCCR PlanetS; Queen Mary University of London Scholarship and STFC Consolidated Grant ST/P000592/1; Spanish MCIU FPI-SO predoctoral contract BES-2017-082610 and the Knut and Alice Wallenberg Foundation.

The CARMENES radial velocity (RV) survey is observing 324 M dwarfs to search for any orbiting planets. In this paper, we present the survey sample by publishing one CARMENES spectrum for each M dwarf. These spectra cover the wavelength range 520¿1710 nm at a resolution of at least R >80 000, and we measure its RV, H¿ emission, and projected rotation velocity. We present an atlas of high-resolution M-dwarf spectra and compare the spectra to atmospheric models. To quantify the RV precision that can be achieved in low-mass stars over the CARMENES wavelength range, we analyze our empirical information on the RV precision from more than 6500 observations. We compare our high-resolution M-dwarf spectra to atmospheric models where we determine the spectroscopic RV information content, Q, and signal-to-noise ratio. We find that for all M-type dwarfs, the highest RV precision can be reached in the wavelength range 700¿900 nm. Observations at longer wavelengths are equally precise only at the very latest spectral types (M8 and M9). We demonstrate that in this spectroscopic range, the large amount of absorption features compensates for the intrinsic faintness of an M7 star. To reach an RV precision of 1 m s¿1 in very low mass M dwarfs at longer wavelengths likely requires the use of a 10 m class telescope. For spectral types M6 and earlier, the combination of a red visual and a near-infrared spectrograph is ideal to search for low-mass planets and to distinguish between planets and stellar variability. At a 4 m class telescope, an instrument like CARMENES has the potential to push the RV precision well below the typical jitter level of 3-4 m s-1. © ESO 2018. ; We thank an anonymous referee for prompt attention and helpful comments that helped to improve the quality of this paper. CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 >Blue Planets around Red Stars>, the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. This work has made use of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. We acknowledge the following funding programs: European Research Council (ERC-279347), Deutsche Forschungsgemeinschaft (RE 1664/12-1, RE 2694/4-1), Bundesministerium fur Bildung und Forschung (BMBF-05A14MG3, BMBF-05A17MG3), Spanish Ministry of Economy and Competitiveness (MINECO, grants AYA2015-68012-C2-2-P, AYA2016-79425-C3-1,2,3-P, AYA2015-69350-C3-2-P, AYA2014-54348-C03-01, AYA2014-56359-P, AYA2014-54348-C3-2R, AYA2016-79425-C3-3-P and 2013 Ramon y Cajal program RYC-2013-14875), Fondo Europeo de Desarrollo Regional (FEDER, grant ESP2016-80435-C2-1-R, ESP2015-65712-C5-5-R), Generalitat de Catalunya/CERCA programme, Spanish Ministerio de Educacion, Cultura y Deporte, programa de Formacion de Profesorado Universitario (grant FPU15/01476), Deutsches Zentrum fur Luft- und Raumfahrt (grants 50OW0204 and 50OO1501), Office of Naval Research Global (award no. N62909-15-1-2011), Mexican CONACyT grant CB-2012-183007.