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347 results on '"Universität zu Köln = University of Cologne"'

1. Widespread amyloidogenicity potential of multiple myeloma patient-derived immunoglobulin light chains

Author: Rebecca Sternke-Hoffmann, Thomas Pauly, Rasmus K. Norrild, Jan Hansen, Florian Tucholski, Magnus Haraldson Høie, Paolo Marcatili, Mathieu Dupré, Magalie Duchateau, Martial Rey, Christian Malosse, Sabine Metzger, Amelie Boquoi, Florian Platten, Stefan U. Egelhaaf, Julia Chamot-Rooke, Roland Fenk, Luitgard Nagel-Steger, Rainer Haas, Alexander K. Buell, Heinrich Heine Universität Düsseldorf = Heinrich Heine University [Düsseldorf], Paul Scherrer Institute (PSI), Forschungszentrum Jülich GmbH, Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Spectrométrie de Masse pour la Biologie – Mass Spectrometry for Biology (UTechS MSBio), Institut Pasteur [Paris] (IP)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, RSH thanks the Manchot foundation for support. AKB and RKN thank the Novo Nordisk Foundation for support (NNFSA170028392). This work has been supported by EPIC-XS, project number 823839, funded by the Horizon 2020 programme of the European Union, the Institut Pasteur and CNRS., and European Project: 823839,H2020-INFRAIA-2018-1,EPIC-XS(2019)
Subjects: Amyloid, Light chain, Multiparametric approach, Physiology, Cell Biology, Plant Science, General Biochemistry, Genetics and Molecular Biology, Structural Biology, Multiple myeloma, Immunoglobulin, AL amyloidosis, General Agricultural and Biological Sciences, Ecology, Evolution, Behavior and Systematics, [SDV.MHEP]Life Sciences [q-bio]/Human health and pathology, Developmental Biology, Biotechnology
Abstract: Background In a range of human disorders such as multiple myeloma (MM), immunoglobulin light chains (IgLCs) can be produced at very high concentrations. This can lead to pathological aggregation and deposition of IgLCs in different tissues, which in turn leads to severe and potentially fatal organ damage. However, IgLCs can also be highly soluble and non-toxic. It is generally thought that the cause for this differential solubility behaviour is solely found within the IgLC amino acid sequences, and a variety of individual sequence-related biophysical properties (e.g. thermal stability, dimerisation) have been proposed in different studies as major determinants of the aggregation in vivo. Here, we investigate biophysical properties underlying IgLC amyloidogenicity. Results We introduce a novel and systematic workflow, Thermodynamic and Aggregation Fingerprinting (ThAgg-Fip), for detailed biophysical characterisation, and apply it to nine different MM patient-derived IgLCs. Our set of pathogenic IgLCs spans the entire range of values in those parameters previously proposed to define in vivo amyloidogenicity; however, none actually forms amyloid in patients. Even more surprisingly, we were able to show that all our IgLCs are able to form amyloid fibrils readily in vitro under the influence of proteolytic cleavage by co-purified cathepsins. Conclusions We show that (I) in vivo aggregation behaviour is unlikely to be mechanistically linked to any single biophysical or biochemical parameter and (II) amyloidogenic potential is widespread in IgLC sequences and is not confined to those sequences that form amyloid fibrils in patients. Our findings suggest that protein sequence, environmental conditions and presence and action of proteases all determine the ability of light chains to form amyloid fibrils in patients.
Published: 2023

2. Rotational spectroscopy of mono-deuterated oxirane (c-C2H3DO) and its detection towards IRAS 16293−2422 B

Author: Holger S P Müller, Jes K Jørgensen, Jean-Claude Guillemin, Frank Lewen, Stephan Schlemmer, Universität zu Köln = University of Cologne, University of Copenhagen = Københavns Universitet (UCPH), Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Deutsche Forschungsgemeinschaft [SFB 956, 184018867, SCHL 341/15-1], European Research Council through the ERC Consolidator Grant 'S4F' [646908], Centre for Star and Planet Formation - Danish National Research Foundation, Centre National d'Etudes Spatiales (CNES) [4500065585], Programme National Physique et Chimie du Milieu Interstellaire (PCMI) of CNRS/INSU, INC/INP - CEA, INC/INP - CNES, and European Project: 646908,H2020,ERC-2014-CoG,S4F(2015)
Subjects: laboratory [methods], INTERSTELLAR, ALMA-PILS SURVEY, FOS: Physical sciences, ISM: abundances, methods: laboratory, H2CS, Physics - Chemical Physics, [CHIM]Chemical Sciences, SPECTRA, Physics - Atomic and Molecular Clusters, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), molecules [ISM], Chemical Physics (physics.chem-ph), abundances [ISM], astrochemistry, ETHYLENE-OXIDE, PROTOSTELLAR, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ISM: individual objects: IRAS 16293-2422, ISM: molecules, Astrophysics - Solar and Stellar Astrophysics, individual objects: IRAS 16293-2422 [ISM], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), identification [line], Astrophysics - Instrumentation and Methods for Astrophysics, Atomic and Molecular Clusters (physics.atm-clus), line: identification
Abstract: We prepared a sample of mono-deuterated oxirane and studied its rotational spectrum in the laboratory between 490 GHz and 1060 GHz in order to improve its spectroscopic parameters and consequently the calculated rest frequencies of its rotational transitions. The updated rest frequencies were employed to detect $c$-C$_2$H$_3$DO for the first time in the interstellar medium in the Atacama Large Millimetre/submillimetre Array (ALMA) Protostellar Interferometric Line Survey (PILS) of the Class 0 protostellar system IRAS 16293$-$2422. Fits of the detected lines using the rotation diagrams yield a temperature of $T_{\rm rot} = 103 \pm 19$ K, which in turn agrees well with 125 K derived for the $c$-C$_2$H$_4$O main isotopologue previously. The $c$-C$_2$H$_3$DO to $c$-C$_2$H$_4$O ratio is found to be $\sim$0.15 corresponding to a D-to-H ratio of $\sim$0.036 per H atom which is slightly higher than the D-to-H ratio of species such as methanol, formaldehyde, ketene and but lower than those of the larger complex organic species such as ethanol, methylformate and glycolaldehyde. This may reflect that oxirane is formed fairly early in the evolution of the prestellar cores. The identification of doubly deuterated oxirane isotopomers in the PILS data may be possible judged by the amount of mono-deuterated oxirane and the observed trend that multiply deuterated isotopologues have higher deuteration rates than their mono-deuterated variants., Comment: 10 pages total; Mon. Not. R. Astron. Soc., accepted
Published: 2022

3. Globules and Pillars in Cygnus X I. Herschel Far-infrared imaging of the Cyg OB2 environment

Author: Nicola Schneider, L. D. Anderson, A. Blazere, Glenn J. White, Ph. André, Doris Arzoumanian, M. G. Guarcello, Sylvain Bontemps, A. Roy, Ana Duarte-Cabral, Luigi Spinoglio, Tracey Hill, M. Hennemann, A. Marston, Kazi L.J. Rygl, F. Comerón, Vincent Minier, Markus Röllig, J. Di Francesco, Vera Könyves, Frédérique Motte, Nicholas J. Wright, Pascal Tremblin, Pierre Didelon, DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), FORMATION STELLAIRE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Procédés, Matériaux et Energie Solaire (PROMES), Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, Faculty of Arts and Science, Concordia University [Montreal], University of Exeter, Maison de la Simulation (MDLS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de Recherche en Informatique et en Automatique (Inria)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln-Universität zu Köln, ITA, USA, GBR, FRA, DEU, ESP, CAN, and CHL
Subjects: Physics, interstellar medium, H II region, 010308 nuclear & particles physics, Molecular cloud, Young stellar object, Cygnus X, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, clouds – individual objects, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Photoevaporation, Interstellar medium, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Spectral energy distribution, Cygnus OB2, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 010303 astronomy & astrophysics
Abstract: The radiative feedback of massive stars on molecular clouds creates pillars, globules and other features at the interface between the HII region and molecular cloud. We present here Herschel observations between 70 and 500 micron of the immediate environment of the Cygnus OB2 association, performed within the HOBYS program. All structures were detected based on their appearance at 70 micron, and have been classified as pillars, globules, evaporating gasous globules (EGGs), proplyd-like objects, and condensations. From the 70 and 160 micron flux maps, we derive the local FUV field on the PDR surfaces. In parallel, we use a census of the O-stars to estimate the overall FUV-field, that is 10^3-10^4 G_0 close to the central OB cluster (within 10 pc) and decreases down to a few tens G_0, in a distance of 50 pc. From a SED fit to the four longest Herschel wavelengths, we determine column density and temperature maps and derive masses, volume densities and surface densities for these structures. We find that the morphological classification corresponds to distinct physical properties. Pillars and globules have the longest estimated photoevaporation lifetimes, a few 10^6 yr, while all other features should survive less than that. These lifetimes are consistent with that found in simulations of turbulent, UV-illuminated clouds. We propose a tentative evolutionary scheme in which pillars can evolve into globules, which in turn then evolve into EGGs, condensations and proplyd-like objects., Received February 18, 2016; accepted April 5, 2016, by A&A
Published: 2016

4. Velocity resolved [C ii] spectroscopy of the center and the BCLMP 302 region of M 33 (HerM 33es)

Author: Bhaswati Mookerjea, Frank P. Israel, C. Kramer, P. van der Werf, F. F. S. van der Tak, Martina C. Wiedner, J. Braine, Carsten Henkel, Volker Ossenkopf, Markus Röllig, T. Nikola, foreign laboratories (FL), CERN [Genève], FORMATION STELLAIRE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, SRON Netherlands Institute for Space Research (SRON), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln-Universität zu Köln, École normale supérieure - Paris (ENS Paris), and Astronomy
Subjects: H II region, Analytical chemistry, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, ISM: clouds, Spectral line, photon-dominated region (PDR), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral resolution, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Hiiregions, Galaxy, galaxies: individual: M 33, Interstellar medium, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies: ISM
Abstract: We aim to understand the contribution of the ionized, atomic and molecular phases of the ISM to the [CII] emission from clouds near the dynamical center and the BCLMP302 HII region in the north of the nearby galaxy M33 at a spatial resolution of 50pc. We combine high resolution [CII] spectra taken with the HIFI spectrometer onboard the Herschel satellite with [CII] Herschel-PACS maps and ground-based observations of CO(2-1) and HI. All data are at a common spatial resolution of 50pc. Typically, the [CII] lines have widths intermediate between the narrower CO(2-1) and broader HI line profiles. We decomposed the [CII] spectra in terms of contribution from molecular and atomic gas detected in CO(2-1) and HI, respectively. We find that the relative contribution of molecular and atomic gas traced by CO(2-1) and HI varies depends mostly on the local physical conditions and geometry. We estimate that 11-60% and 5-34% of the [CII] intensities in the center and in BCLMP302, respectively, arise at velocities showing no CO(2-1) or HI emission and could arise in CO-dark molecular gas. The deduced strong variation in the [CII] emission not associated with CO and HI cannot be explained in terms of differences in A_v, far-ultraviolet radiation field, and metallicity between the two studied regions. Hence the relative amounts of diffuse (CO-dark) and dense molecular gas possibly vary on spatial scales smaller than 50pc. Based on the emission measure observed at radio wavelengths we estimate the contribution of ionized gas at a few positions to lie between 10-25%. The correlations between the intensities of tracers corresponding to the same velocity range as [CII], differ from the correlation derived from PACS data. The results in this paper emphasize the need for velocity-resolved observations to discern the contribution of different components of the ISM to [CII] emission. (abridged), Comment: Accepted for publication in A&A
Published: 2016

5. Loss of Agricultural Soils to Urban & Suburban Development in France (2000-2018)

Author: Fox, Dennis, Caglioni, M., Benitez, B., Hillen, S., Vogt, A., Lulovicova, A., Études des Structures, des Processus d’Adaptation et des Changements de l’Espace (ESPACE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Avignon Université (AU)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Université Côte d'Azur (UCA), Institut für Kernphysik der Universität zu Köln, Universität zu Köln = University of Cologne, Académie 5 - Homme, Idées et Milieux, and ANR-15-IDEX-0001,UCA JEDI,Idex UCA JEDI(2015)
Subjects: [SHS]Humanities and Social Sciences
Abstract: International audience
Published: 2023

6. Cross-linguistic patterns in the lexicalisation of bring and take

Author: Anna Margetts, Katharina Haude, Nikolaus P. Himmelmann, Dagmar Jung, Sonja Riesberg, Stefan Schnell, Frank Seifart, Harriet Sheppard, Claudia Wegener, University of Zurich, Margetts, Anna, Monash university, Structure et Dynamique des Langues (SeDyL), Institut National des Langues et Civilisations Orientales (Inalco)-Institut de recherche pour le développement [IRD] : UR135-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, Universität Zürich [Zürich] = University of Zurich (UZH), Langues et civilisations à tradition orale (LACITO), Université Sorbonne Nouvelle - Paris 3-Institut National des Langues et Civilisations Orientales (Inalco)-Centre National de la Recherche Scientifique (CNRS), Dynamique Du Langage (DDL), Université Lumière - Lyon 2 (UL2)-Centre National de la Recherche Scientifique (CNRS), Leibniz-Zentrum Allgemeine Sprachwissenschaft [Berlin] (ZAS), Volkswagenstiftung, and Cross-linguistic patterns in the encoding of three-participant events
Subjects: Linguistics and Language, Communication, 410 Linguistics, liri Linguistic Research Infrastructure (LiRI), event representation, EVOL NCCR Evolving Language, Language and Linguistics, [SHS]Humanities and Social Sciences, 3310 Linguistics and Language, 10104 Department of Comparative Language Science, 490 Other languages, accompanied motion, Caused motion, ISLE Center for the Interdisciplinary Study of Language Evolution, text-based typology, 890 Other literatures, 1203 Language and Linguistics, 3315 Communication, semantic typology
Abstract: This study investigates the linguistic expression of bring and take events and more generally of the semantic domain of directed caused accompanied motion (‘directed CAM’) across a sample of eight languages of the Pacific and the Americas. Unlike English, the majority of languages in our sample do not lexicalise directed CAM events by simple verbs, but rather encode the defining meaning components – caused motion, accompaniment, and directedness – in morphosyntactically complex constructions. The study shows a high degree of crosslinguistic diversity, even among closely related languages. Meaning components are contributed to directed CAM expressions by a mix of lexical semantics, morphosyntax, and pragmatic means. The study proposes a text-based, semantic typology of directed CAM events by drawing on corpus data from endangered languages.
Published: 2022

7. PDRs4All: A JWST Early Release Science Program on Radiative Feedback from Massive Stars

Author: Olivier Berné, Émilie Habart, Els Peeters, Alain Abergel, Edwin A. Bergin, Jeronimo Bernard-Salas, Emeric Bron, Jan Cami, Emmanuel Dartois, Asunción Fuente, Javier R. Goicoechea, Karl D. Gordon, Yoko Okada, Takashi Onaka, Massimo Robberto, Markus Röllig, Alexander G. G. M. Tielens, Sílvia Vicente, Mark G. Wolfire, Felipe Alarcón, C. Boersma, Amélie Canin, Ryan Chown, Daniel Dicken, David Languignon, Romane Le Gal, Marc W. Pound, Boris Trahin, Thomas Simmer, Ameek Sidhu, Dries Van De Putte, Sara Cuadrado, Claire Guilloteau, Alexandros Maragkoudakis, Bethany R. Schefter, Thiébaut Schirmer, Stéphanie Cazaux, Isabel Aleman, Louis Allamandola, Rebecca Auchettl, Giuseppe Antonio Baratta, Salma Bejaoui, Partha P. Bera, Goranka Bilalbegović, John H. Black, Francois Boulanger, Jordy Bouwman, Bernhard Brandl, Philippe Brechignac, Sandra Brünken, Andrew Burkhardt, Alessandra Candian, Jose Cernicharo, Marin Chabot, Shubhadip Chakraborty, Jason Champion, Sean W. J. Colgan, Ilsa R. Cooke, Audrey Coutens, Nick L. J. Cox, Karine Demyk, Jennifer Donovan Meyer, Cécile Engrand, Sacha Foschino, Pedro García-Lario, Lisseth Gavilan, Maryvonne Gerin, Marie Godard, Carl A. Gottlieb, Pierre Guillard, Antoine Gusdorf, Patrick Hartigan, Jinhua He, Eric Herbst, Liv Hornekaer, Cornelia Jäger, Eduardo Janot-Pacheco, Christine Joblin, Michael Kaufman, Francisca Kemper, Sarah Kendrew, Maria S. Kirsanova, Pamela Klaassen, Collin Knight, Sun Kwok, Álvaro Labiano, Thomas S.-Y. Lai, Timothy J. Lee, Bertrand Lefloch, Franck Le Petit, Aigen Li, Hendrik Linz, Cameron J. Mackie, Suzanne C. Madden, Joëlle Mascetti, Brett A. McGuire, Pablo Merino, Elisabetta R. Micelotta, Karl Misselt, Jon A. Morse, Giacomo Mulas, Naslim Neelamkodan, Ryou Ohsawa, Alain Omont, Roberta Paladini, Maria Elisabetta Palumbo, Amit Pathak, Yvonne J. Pendleton, Annemieke Petrignani, Thomas Pino, Elena Puga, Naseem Rangwala, Mathias Rapacioli, Alessandra Ricca, Julia Roman-Duval, Joseph Roser, Evelyne Roueff, Gaël Rouillé, Farid Salama, Dinalva A. Sales, Karin Sandstrom, Peter Sarre, Ella Sciamma-O’Brien, Kris Sellgren, Matthew J. Shannon, Sachindev S. Shenoy, David Teyssier, Richard D. Thomas, Aditya Togi, Laurent Verstraete, Adolf N. Witt, Alwyn Wootten, Nathalie Ysard, Henning Zettergren, Yong Zhang, Ziwei E. Zhang, Junfeng Zhen, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Western Ontario (UWO), Carl Sagan Center, SETI Institute, University of Michigan [Ann Arbor], University of Michigan System, Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional, Madrid, Instituto de Física Fundamental [Madrid] (IFF), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universiteit Gent = Ghent University (UGENT), Space Telescope Science Institute (STSci), Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Meisei University, The University of Tokyo (UTokyo), Leiden Observatory [Leiden], Universiteit Leiden, Johns Hopkins University (JHU), Instituto de Astrofísica e Ciências do Espaço (IASTRO), University of Maryland [College Park], University of Maryland System, NASA Ames Research Center (ARC), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Signal et Communications (IRIT-SC), Institut de recherche en informatique de Toulouse (IRIT), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Toulouse Mind & Brain Institut (TMBI), Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Institut National Polytechnique (Toulouse) (Toulouse INP), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Delft University of Technology (TU Delft), Universidade Federal de Itajubá, Bay Area Environmental Research Institute (BAER), Australian Synchrotron [Clayton], INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), University of Zagreb, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Colorado [Boulder], Institute for Molecules and Materials [Nijmegen], Radboud University [Nijmegen], Wellesley College, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), University of British Columbia (UBC), National Radio Astronomy Observatory [Charlottesville] (NRAO), National Radio Astronomy Observatory (NRAO), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Rice University [Houston], Yunnan Observatories, Chinese Academy of Sciences [Changchun Branch] (CAS), Universidad de Chile = University of Chile [Santiago] (UCHILE), University of Virginia, Aarhus University [Aarhus], Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo = University of São Paulo (USP), San Jose State University [San Jose] (SJSU), European Southern Observatory (ESO), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Telespazio, Services par satellites, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), University of Missouri [Columbia] (Mizzou), University of Missouri System, Max Planck Institute for Astronomy (MPIA), CAS Key Laboratory of Crust–Mantle Materials and Environments [Hefei], School of Earth and Space Sciences [Hefei], University of Science and Technology of China [Hefei] (USTC)-University of Science and Technology of China [Hefei] (USTC)-Chinese Academy of Sciences [Beijing] (CAS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), University of California [Berkeley] (UC Berkeley), University of California (UC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut des Sciences Moléculaires (ISM), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1 (UB)-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Massachusetts Institute of Technology (MIT), Instituto de Ciencia de Materiales de Madrid (ICMM), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Steward Observatory, University of Arizona, INAF - Osservatorio Astronomico di Cagliari (OAC), United Arab Emirates University (UAEU), National Astronomical Observatory of Japan (NAOJ), Banaras Hindu University [Varanasi] (BHU), University of Amsterdam [Amsterdam] (UvA), Laboratoire de Chimie et Physique Quantiques Laboratoire (LCPQ), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche « Matière et interactions » (FeRMI), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Universidade Federal do Rio Grande do Sul [Porto Alegre] (UFRGS), University of California [San Diego] (UC San Diego), University of Nottingham, UK (UON), Ohio State University [Columbus] (OSU), Space Science Institute [Boulder] (SSI), Stockholm University, Texas State University, Ritter Astrophysical Research Center, University of Toledo, National Sun Yat-Sen University (NSYSU), Star and Planet Formation Laboratory, ITA, USA, GBR, FRA, DEU, ESP, AUS, BEL, BRA, CHL, TWN, HRV, DNK, JPN, IND, NLD, PRT, CHN, RUS, SWE, National Aeronautics and Space Administration (US), University of Maryland, University of Michigan, Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Natural Sciences and Engineering Research Council of Canada, Ministerio de Ciencia e Innovación (España), German Research Foundation, Japan Society for the Promotion of Science, San José State University Research Foundation, Berné, Olivier, Habart, Émilie, Peeters, Els, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Bron, Emeric, Cami, Jan, Dartois, Emmanuel, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Okada, Yoko, Onaka, Takashi, Robberto, Massimo, Röllig, Markus, Tielens, Alexander G.G.M., Vicente, Sílvia, Wolfire, Mark G., Alarcón, Felipe, Boersma, C., Canin, Amélie, Chown, Ryan, Dicken, Daniel, Le Gal, Romane, Pound, Marc W., Trahin, Boris, Sidhu, Ameek, Van De Putte, Dries, Cuadrado, Sara, Guilloteau, Claire, Maragkoudakis, Alexandros, Schefter, Bethany R., Schirmer, Thiébaut, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Antonio Baratta, Giuseppe, Bejaoui, Salma, Bera, Partha P., Bilalbegović, Goranka, Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brünken, Sandra, Burkhardt, Andrew, Candian, Alessandra, Cernicharo, José, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W.J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L.J., Demyk, Karine, Donovan Meyer, Jennifer, Engrand, Cécile, Foschino, Sacha, Gavilan, Lisseth, Gerin, Maryvonne, Godard, Marie, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Janot-Pacheco, Eduardo, Joblin, Christine, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Knight, Collin, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S.Y., Lee, Timothy J., Lefloch, Bertrand, Le Petit, Franck, Li, Aigen, Linz, Hendrik, MacKie, Cameron J., Madden, Suzanne C., Mascetti, Joëlle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Morse, Jon A., Molecular Spectroscopy (HIMS, FNWI), and HIMS (FNWI)
Subjects: Gaseous Nebulae, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, FELIX Infrared and Terahertz Spectroscopy, Star Forming Regions, Astrophysics - Astrophysics of Galaxies, Infrared Telescopes, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], Photodissociation Regions, Astrophysics::Earth and Planetary Astrophysics, Polycyclic Aromatic Hydrocarbons, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], James Webb Space Telescope (JWST), Photo-Dissociation Regions (PDRs), Massive stars, Orion Bar, MIRI, NIRSpec, NIRCam, Astrophysics::Galaxy Astrophysics
Abstract: 22 pags., 8 figs., 1 tab., Massive stars disrupt their natal molecular cloud material through radiative and mechanical feedback processes. These processes have profound effects on the evolution of interstellar matter in our Galaxy and throughout the universe, from the era of vigorous star formation at redshifts of 1-3 to the present day. The dominant feedback processes can be probed by observations of the Photo-Dissociation Regions (PDRs) where the far-ultraviolet photons of massive stars create warm regions of gas and dust in the neutral atomic and molecular gas. PDR emission provides a unique tool to study in detail the physical and chemical processes that are relevant for most of the mass in inter-and circumstellar media including diffuse clouds, proto-planetary disks, and molecular cloud surfaces, globules, planetary nebulae, and star-forming regions. PDR emission dominates the infrared (IR) spectra of star-forming galaxies. Most of the Galactic and extragalactic observations obtained with the James Webb Space Telescope (JWST) will therefore arise in PDR emission. In this paper we present an Early Release Science program using the MIRI, NIRSpec, and NIRCam instruments dedicated to the observations of an emblematic and nearby PDR: the Orion Bar. These early JWST observations will provide template data sets designed to identify key PDR characteristics in JWST observations. These data will serve to benchmark PDR models and extend them into the JWST era. We also present the Science-Enabling products that we will provide to the community. These template data sets and Science-Enabling products will guide the preparation of future proposals on star-forming regions in our Galaxy and beyond and will facilitate data analysis and interpretation of forthcoming JWST observations., Support for JWST-ERS program ID 1288 was provided through grants from the STScI under NASA contract NAS5-03127 to STScI (K.G., D.V.D.P., M.R.), Univ. of Maryland (M.W., M.P.), Univ. of Michigan (E.B., F.A.), and Univ. of Toledo (T.S.-Y.L.). O.B. and E.H. are supported by the Programme National “Physique et Chimie du Milieu Interstellaire” (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES, and through APR grants 6315 and 6410 provided by CNES. E. P. and J.C. acknowledge support from the National Science and Engineering Council of Canada (NSERC) Discovery Grant program (RGPIN-2020-06434 and RGPIN-2021-04197 respectively). E.P. acknowledges support from a Western Strategic Support Accelerator Grant (ROLA ID 0000050636). J.R.G. and S.C. thank the Spanish MCINN for funding support under grant PID2019-106110GB-I00. Work by M.R. and Y.O. is carried out within the Collaborative Research Centre 956, subproject C1, funded by the Deutsche Forschungsgemeinschaft (DFG)—project ID 184018867. T.O. acknowledges support from JSPS Bilateral Program, grant No. 120219939. M.P. and M.W. acknowledge support from NASA Astrophysics Data Analysis Program award #80NSSC19K0573. C.B. is grateful for an appointment at NASA Ames Research Center through the San José State University Research Foundation (NNX17AJ88A) and acknowledges support from the Internal Scientist Funding Model (ISFM) Directed Work Package at NASA Ames titled: “Laboratory Astrophysics—The NASA Ames PAH IR Spectroscopic Database.”
Published: 2022

8. Improving crop Yield potential: Underlying biological processes and future prospects

Author: Burgess, Alexandra, Masclaux-Daubresse, Céline, Strittmatter, Günter, Weber, Andreas, Taylor, Samuel Harry, Harbinson, Jeremy, Yin, Xinyou, Long, Stephen, Paul, Matthew, Westhoff, Peter, Loreto, Francesco, Ceriotti, Aldo, Saltenis, Vandasue, Pribil, Mathias, Nacry, Philippe, Scharff, Lars, Jensen, Poul Erik, Muller, Bertrand, Cohan, Jean‐pierre, Foulkes, John, Rogowsky, Peter, Debaeke, Philippe, Meyer, Christian, Nelissen, Hilde, Inzé, Dirk, Klein Lankhorst, René, Parry, Martin, Murchie, Erik, Baekelandt, Alexandra, University of Nottingham, UK (UON), Institut Jean-Pierre Bourgin (IJPB), AgroParisTech-Université Paris-Saclay-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Cluster of Excellence on Plant Sciences (CEPLAS), Heinrich Heine Universität Düsseldorf = Heinrich Heine University [Düsseldorf]-Max Planck Institute for Plant Breeding Research (MPIPZ)-Universität zu Köln = University of Cologne, Lancaster Environment Centre, Lancaster University, Wageningen University and Research [Wageningen] (WUR), University College of London [London] (UCL), University of Illinois at Urbana-Champaign [Urbana], University of Illinois System, Rothamsted Research, Biotechnology and Biological Sciences Research Council (BBSRC), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), University of Copenhagen = Københavns Universitet (UCPH), Biochimie et Physiologie Moléculaire des Plantes (BPMP), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Department of Food Science [Copenhagen] (UCPH FOOD), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Écophysiologie des Plantes sous Stress environnementaux (LEPSE), Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut Agro Montpellier, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), ARVALIS - Institut du végétal [Paris], Reproduction et développement des plantes (RDP), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), AGroécologie, Innovations, teRritoires (AGIR), Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Department of Plant Systems Biology, VIB, and Department of Plant Biotechnology and Bioinformatics, Universiteit Gent = Ghent University (UGENT), European Commission 817690, and European Project: 817690,ERC
Subjects: food supply, photosynthesis, [SDV]Life Sciences [q-bio], [SDV.BV]Life Sciences [q-bio]/Vegetal Biology, crop yield, nutrient remobilisation, crop improvement, organ growth
Abstract: International audience; The growing world population and global increases in the standard of living both result in an increasing demand for food, feed and other plant- derived products. In the coming years, plant- based research will be among the major drivers ensuring food security and the expansion of the bio- based economy. Crop productivity is determined by several factors, including the available physical and agricultural resources, crop management, and the resource use efficiency, quality and intrinsic yield potential of the chosen crop. This review focuses on intrinsic yield potential, since understanding its determinants and their biological basis will allow to maximize the plant's potential in food and energy production. Yield potential is determined by a variety of complex traits that integrate strictly regulated processes and their underlying gene regulatory networks. Due to this inherent complexity, numerous potential targets have been identified that could be exploited to increase crop yield. These encompass diverse metabolic and physical processes at the cellular, organ and canopy level. We present an overview of some of the distinct biological processes considered to be crucial for yield determination that could further be exploited to improve future crop productivity.
Published: 2023

9. N-graphene synthesized in astrochemical ices

Author: B. Sivaraman, K. K. Rahul, M. Ambresh, D. Sahu, J. K. Meka, S.-L. Chou, Y.-J. Wu, D. Gupta, A. Das, J.-I. Lo, B.-M. Cheng, B. N. Rajasekhar, Anil Bhardwaj, H. Hill, P. Janardhan, N. J. Mason, Physical Research Laboratory [Ahmedabad] (PRL), Indian Space Research Organisation (ISRO), Indian Institute of Science [Bangalore] (IISc Bangalore), Academia Sinica, National Synchrotron Radiation Research Center (NSRRC), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, Bhabha Atomic Research Centre (BARC), Government of India, Department of Atomic Energy, International Space University (ISU), University of Kent [Canterbury], Horizon 2020 Framework Programme, H2020: 654208, 871149, Indian Space Research Organisation, इसरो, National Synchrotron Radiation Research Center, NSRRC: IFA-11CH-11, Physical Research Laboratory, PRL, European Project: 654208,H2020,H2020-INFRAIA-2014-2015,EPN2020-RI(2015), and European Project: 8711495(1988)
Subjects: Synthesised, Aromatic compounds, Nitrogen, Vacuum ultraviolets, Graphene sheets, Laboratory experiments, Physics::Optics, FOS: Physical sciences, High resolution transmission electron microscopy, Energy dispersive spectroscopy, Physics::Atomic and Molecular Clusters, Semiconductor quantum dots, Physics::Chemical Physics, Condition, Instrumentation and Methods for Astrophysics (astro-ph.IM), [PHYS]Physics [physics], Side-chains, Carbon structures, Ice, Benzonitriles, Interstellar medias, Atomic and Molecular Physics, and Optics, Complex molecules, Irradiation, Graphene, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Icy mantles of benzonitrile, an aromatic with a cyanide side chain that has recently been detected in the interstellar medium, were subjected to vacuum ultraviolet photon irradiation and found to form a residue. The residue was removed from the substrate and placed on a Quantifoil grid for electron microscopy analysis. Transmission electron microscopy showed Quantum Dot (QD) and Nitrogen-doped Graphene (N-Graphene) sheets. Diffraction and Energy Dispersive X-ray Spectroscopy revealed the crystalline nature and carbon-nitrogen composition, of the observed graphene sheet. This is the first result showing QD and N-Graphene synthesis in ice irradiation at interstellar temperatures., Comment: 10 pages, 3 figures
Published: 2023

10. Democratizing knowledge representation with BioCypher

Author: Lobentanzer, Sebastian, Aloy, Patrick, Baumbach, Jan, Bohar, Balazs, Charoentong, Pornpimol, Danhauser, Katharina, Doğan, Tunca, Dreo, Johann, Dunham, Ian, Fernandez-Torras, Adrià, Gyori, Benjamin, Hartung, Michael, Hoyt, Charles Tapley, Klein, Christoph, Korcsmaros, Tamas, Maier, Andreas, Mann, Matthias, Ochoa, David, Pareja-Lorente, Elena, Preusse, Martin, Probul, Niklas, Schwikowski, Benno, Sen, Bünyamin, Strauss, Maximilian, Turei, Denes, Ulusoy, Erva, Wodke, Judith, Waltemath, Dagmar, Saez-Rodriguez, Julio, Carey, Vincent, Farr, Elias, Popp, Ferdinand, Universität Heidelberg [Heidelberg] = Heidelberg University, Institute for Research in Biomedicine [Barcelona, Spain] (IRB), University of Barcelona-Barcelona Institute of Science and Technology (BIST), University of Hamburg, Earlham Institute [Norwich], Biological Research Centre [Szeged] (BRC), Dr von Hauner Children's Hospital [Munich, Germany], Ludwig-Maximilians-Universität München (LMU), Hacettepe University = Hacettepe Üniversitesi, Biomédecine computationelle des systèmes / Computational systems biomedicine, Institut Pasteur [Paris] (IP)-Université Paris Cité (UPCité), Hub Bioinformatique et Biostatistique - Bioinformatics and Biostatistics HUB, European Bioinformatics Institute [Hinxton] (EMBL-EBI), EMBL Heidelberg, Harvard Medical School [Boston] (HMS), Dr Von Hauner Children's Hospital, Partenaires INRAE, Quadram Institute Bioscience [Norwich, U.K.] (QIB), Biotechnology and Biological Sciences Research Council (BBSRC), Imperial College London, Universität zu Köln = University of Cologne, Max-Planck-Institut für Biochemie = Max Planck Institute of Biochemistry (MPIB), Max-Planck-Gesellschaft, German Center for Diabetes Research - Deutsches Zentrum für Diabetesforschung [Neuherberg] (DZD), University of Medicine Greifswald, Brigham & Women’s Hospital [Boston] (BWH), German Cancer Research Center - Deutsches Krebsforschungszentrum [Heidelberg] (DKFZ), European Project: 965193, H2020-EU.3.1. - SOCIETAL CHALLENGES - Health, demographic change and well-being H2020-EU.3.1.5. - Methods and data ,DECIDER(2021), European Project: 066490,WT::(2003), European Project: 031L0181B,LaMarck, European Project: 031L0212A,SMART-CARE, European Project: W911NF-20-1-0255, and European Project: 01ZZ2019,MIRACUM
Subjects: prior knowledge, knowledge graph, federated learning, harmonisation, FAIRness, ontology, [INFO.INFO-BI]Computer Science [cs]/Bioinformatics [q-bio.QM], database
Abstract: International audience; Standardising the representation of biomedical knowledge among allresearchers is an insurmountable task, hindering the effectiveness of manycomputational methods. To facilitate harmonisation and interoperability despitethis fundamental challenge, we propose to standardise the framework ofknowledge graph creation instead. We implement this standardisation inBioCypher, a FAIR (findable, accessible, interoperable, reusable) framework totransparently build biomedical knowledge graphs while preserving provenances ofthe source data. Mapping the knowledge onto biomedical ontologies helps tobalance the needs for harmonisation, human and machine readability, and ease ofuse and accessibility to non-specialist researchers. We demonstrate the usefulnessof the framework on a variety of use cases, from maintenance of task-specificknowledge stores, to interoperability between biomedical domains, to on-demandbuilding of task-specific knowledge graphs for federated learning. BioCypher(https://biocypher.org) thus facilitates automating knowledge-based biomedicalresearch, and we encourage the community to further develop and use it.
Published: 2023

11. Mesoscopic Klein-Schwinger effect in graphene

Author: A. Schmitt, P. Vallet, D. Mele, M. Rosticher, T. Taniguchi, K. Watanabe, E. Bocquillon, G. Fève, J. M. Berroir, C. Voisin, J. Cayssol, M. O. Goerbig, J. Troost, E. Baudin, B. Plaçais, Physique Mésoscopique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire Ondes et Matière d'Aquitaine (LOMA), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Carbon - IEMN (CARBON - IEMN), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA), Université catholique de Lille (UCL)-Université catholique de Lille (UCL)-Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA), Université catholique de Lille (UCL)-Université catholique de Lille (UCL), National Institute for Materials Science (NIMS), Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Nano-Optique, Laboratoire de Physique des Solides (LPS), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Champs, Gravitation et Cordes, AcknowledgementsThe research leading to these results has received partial funding from the European Union Horizon 2020 research and innovation programme under Grant Agreement No. 881603 Graphene Core 3 (D.M., M.R., E. Baudin, B.P.). P.V. and J.C. were supported by the 'LIGHT S&T Graduate Program' (PIA3 Investment for the Future Program, ANR17-EURE-0027) and GPR LIGHT., ANR-17-EURE-0027,LIGHTS&T,University of Bordeaux Graduate Scholl in Light Sciences & Technologies(2017), European Project: 881603,H2020,H2020-SGA-FET-GRAPHENE-2019, GrapheneCore3(2020), Laboratoire Ondes et Matière d'Aquitaine [LOMA], Carbon - IEMN [CARBON - IEMN], Laboratoire de physique de l'ENS - ENS Paris [LPENS], National Institute for Materials Science [NIMS], and Laboratoire de Physique des Solides [LPS]
Subjects: High Energy Physics - Theory, Condensed Matter - Mesoscale and Nanoscale Physics, High Energy Physics - Theory (hep-th), Mesoscale and Nanoscale Physics (cond-mat.mes-hall), General Physics and Astronomy, FOS: Physical sciences, [PHYS.COND.CM-MSQHE]Physics [physics]/Condensed Matter [cond-mat]/Mesoscopic Systems and Quantum Hall Effect [cond-mat.mes-hall]
Abstract: Strong electric field annihilation by particle-antiparticle pair creation, also known as the Schwinger effect, is a non-perturbative prediction of quantum electrodynamics. Its experimental demonstration remains elusive, as threshold electric fields are extremely strong and beyond current reach. Here, we propose a mesoscopic variant of the Schwinger effect in graphene, which hosts Dirac fermions with an approximate electron-hole symmetry. Using transport measurements, we report on universal 1d-Schwinger conductance at the pinchoff of ballistic graphene transistors. Strong pinchoff electric fields are concentrated within approximately 1 $\mu$m of the transistor's drain, and induce Schwinger electron-hole pair creation at saturation. This effect precedes a collective instability toward an ohmic Zener regime, which is rejected at twice the pinchoff voltage in long devices. These observations advance our understanding of current saturation limits in ballistic graphene and provide a direction for further quantum electrodynamic experiments in the laboratory., Comment: 39 pages, 13 figures, final version with extended discussion of the pinchoff effect in supplementary informations, abstract updated
Published: 2023

12. Rotational spectroscopy of oxirane-2,2-d2, c-CD2CH2O, and its tentative detection toward IRAS 16293-2422 B

Author: Müller, Holger S. P., Jørgensen, Jes K., Guillemin, Jean-Claude, Lewen, Frank, Schlemmer, Stephan, Universität zu Köln = University of Cologne, University of Copenhagen = Københavns Universitet (UCPH), Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), National Science Foundation, NSF, National Aeronautics and Space Administration, NASA, National Radio Astronomy Observatory, NRAO, Associated Universities, AUI, Centre national d'études spatiales, CNES, National Research Council Canada, NRC, Deutsche Forschungsgemeinschaft, DFG: 184018867, SCHL 341/15-1, National Science Council, NSC, Centre National d’Etudes Spatiales, CNES: 4500065585, Korea Astronomy and Space Science Institute, KASI, National Institutes of Natural Sciences, NINS, National Astronomical Observatory of Japan, NAOJ, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, CEA, and Danmarks Frie Forskningsfond, DFF: 0135-00123B
Subjects: Rotational spectroscopy, Reduced Hamiltonian, FOS: Physical sciences, Interstellar molecule, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), [CHIM]Chemical Sciences, Physics - Atomic and Molecular Clusters, Submillimeter spectroscopy, Astrophysics - Instrumentation and Methods for Astrophysics, Atomic and Molecular Clusters (physics.atm-clus), Molecular symmetry, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We prepared a sample of oxirane doubly deuterated at one C atom and studied its rotational spectrum in the laboratory for the first time between 120~GHz and 1094~GHz. Accurate spectroscopic parameters up to eighth order were determined, and the calculated rest frequencies were used to identify $c$-CD$_2$CH$_2$O tentatively in the interstellar medium in the Atacama Large Millimeter/submillimeter Array Protostellar Interferometric Line Survey (PILS) of the Class 0 protostellar system IRAS 16293$-$2422. The $c$-CD$_2$CH$_2$O to $c$-C$_2$H$_4$O ratio was estimated to be $\sim$0.054 with $T_{\rm rot} = 125$ K. This value translates to a D-to-H ratio of $\sim$0.16 per H atom which is higher by a factor of 4.5 than the $\sim$0.036 per H atom obtained for $c$-C$_2$H$_3$DO. Such increase in the degree of deuteration referenced to one H atom in multiply deuterated isotopologs compared to their singly deuterated variants have been observed commonly in recent years., Comment: Journal of Molecular Spectroscopy, in press; Per Jensen special issue. 12 pages here
Published: 2023

13. Search for $^{22}$Na in novae supported by a novel method for measuring femtosecond nuclear lifetimes

Author: Chloé Fougères, Francois de Oliveira Santos, Jordi Jose, Caterina Michelagnoli, Emmanuel Clément, Yung Hee Kim, Antoine Lemasson, Valdir Guimaraes, Diego Barrientos, Daniel Bemmerer, Giovanna Benzoni, Andrew Boston, Roman Bottger, Florent Boulay, Angela Bracco, Igor Celikovic, Bo Cederwall, Michal Ciemala, Clement Delafosse, Cesar Domingo-Pardo, Jeremie Dudouet, Jurgen Eberth, Zsolt Fulop, Vicente Gonzalez, Johan Goupil, Herbert Hess, Andrea Jungclaus, Ayse Kaşkaş, Amel Korichi, Silvia Lenzi, Silvia Leoni, Hongjie Li, Joa Ljungvall, Araceli Lopez-Martens, Roberto Menegazzo, Daniele Mengoni, Benedicte Million, Jaromir Mrazek, Daniel Napoli, Alahari Navin, Johan Nyberg, Zsolt Podolyak, Alberto Pullia, Begona Quintana, Damien Ralet, Nadine Redon, Peter Reiter, Kseniia Rezynkina, Frédéric Saillant, Marie-Delphine Salsac, Angel Sánchez-Benítez, Enrique Sanchis, Menekse Senyigit, Marco Siciliano, Nadezda Smirnova, Dorottya Sohler, mihai stanoiu, Christophe Theisen, Jose Javier Valiente-Dobon, Predrag Ujic, Madalena Zielinska, Argonne National Laboratory [Lemont] (ANL), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya [Barcelona] (UPC), Institut Laue-Langevin (ILL), Institute for Basic Science [Daejeon] (IBS), Instituto de Fisica da Universidade de São Paulo (IFUSP), Universidade de São Paulo = University of São Paulo (USP), CERN [Genève], Helmholtz-Zentrum Dresden-Rossendorf (HZDR), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), University of Liverpool, Vinca Institute of Nuclear Sciences, University of Belgrade (VINCA), Department of Physics, Royal Institute of Technology (KTH), Institute of Nuclear Physics PAN, Krakow, Poland, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Universidad de Valencia, Universitat de València (UV), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut für Kernphysik der Universität zu Köln, Universität zu Köln = University of Cologne, Institute for Nuclear Research [Budapest] (ATOMKI), Hungarian Academy of Sciences (MTA), Instituto de Estructura de la Materia, CSIC, E-28006 Madrid, Physics Department, Ankara University, Ankara University, Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Università degli Studi di Padova = University of Padua (Unipd), Dipartimento di Fisica, Università degli studi di Milano, Istituto Nazionale di Fisica Nucleare (INFN)-Università degli Studi di Milano = University of Milan (UNIMI), Nuclear Physics Institute of the Czech Academy of Sciences, INFN, Laboratori Nazionali di Legnaro, Department of Physics and Astronomy, Uppsala University, Uppsala University, Department of Physics, University of Surrey, University of Surrey (UNIS), Universidad de Salamanca, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CEAFMC, University of Huelva, Laboratoire de Physique des Deux Infinis Bordeaux (LP2I - Bordeaux), Université de Bordeaux (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Horia Hulubei National Institute for R&D in Physics and Nuclear Engineering, IFIN-HH Bucharest, ANR-17-CE31-0026,OASIS,Optimisation d'Agata pour la physique(2017), and European Project: 212692,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2007-1,SPIRAL2PP(2007)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, [PHYS]Physics [physics], Astrophysics and Astronomy, astro-ph.SR, Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Nuclear Physics - Experiment, Nuclear Experiment (nucl-ex), nucl-ex, Astrophysics - High Energy Astrophysical Phenomena, Nuclear Experiment, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Classical novae are thermonuclear explosions in stellar binary systems, and important sources of $^{26}$Al and $^{22}$Na. While gamma rays from the decay of the former radioisotope have been observed throughout the Galaxy, $^{22}$Na remains untraceable. The half-life of $^{22}$Na (2.6 yr) would allow the observation of its 1.275 MeV gamma-ray line from a cosmic source. However, the prediction of such an observation requires good knowledge of the nuclear reactions involved in the production and destruction of this nucleus. The $^{22}$Na($p,\gamma$)$^{23}$Mg reaction remains the only source of large uncertainty about the amount of $^{22}$Na ejected. Its rate is dominated by a single resonance on the short-lived state at 7785.0(7) keV in $^{23}$Mg. In the present work, a combined analysis of particle-particle correlations and velocity-difference profiles is proposed to measure femtosecond nuclear lifetimes. The application of this novel method to the study of the $^{23}$Mg states, combining magnetic and highly-segmented tracking gamma-ray spectrometers, places strong limits on the amount of $^{22}$Na produced in novae, explains its non-observation to date in gamma rays (flux < 2.5x$10^{-4}$ ph/(cm$^2$s)), and constrains its detectability with future space-borne observatories., Comment: 18 pages, 3 figures, 1 table
Published: 2022

14. Variation in the dust emissivity index across M 33 with Herschel and Spitzer (HerM 33es)

Author: Francoise Combes, Carsten Henkel, Monica Relaño, Pierre Gratier, Martina C. Wiedner, Markus Röllig, Simon Verley, Fatemeh Tabatabaei, J. Braine, Frank P. Israel, P. van der Werf, C. Kramer, E. M. Xilouris, Médéric Boquien, K. F. Schuster, FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut für Physik (Institut für Physik), Universität Potsdam, Dpto. Fisica Teorica y del Cosmos, Universidad de Granada (UGR), Dept. fısica Teorica y del Cosmos, Institut de RadioAstronomie Millimétrique (IRAM), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln-Universität zu Köln, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Potsdam = Universität Potsdam, Universidad de Granada = University of Granada (UGR), Universiteit Leiden, Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Metallicity, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, 0103 physical sciences, Emissivity, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Local Group, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Galaxy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the wavelength dependence of the dust emission as a function of position and environment across the disk of M33 at a linear resolution of 160 pc using Spitzer and Herschel photometric data. Expressing the emissivity of the dust as a power law, the power-law exponent (beta) is estimated from two independent approaches designed to properly treat the degeneracy between beta and the dust temperature. Both beta and the dust temperature are higher in the inner disk than in the outer disk, contrary to reported beta-T anti-correlations found in other sources. In the cold + warm dust model, the warm component and the ionized gas (Halpha) have a very similar distribution across the galaxy, demonstrating that the model separates the components in an appropriate fashion. The flocculent spiral arms and the dust lanes are evident in the map of the cold component. Both cold and warm dust column densities are high in star forming regions and reach their maxima toward the giant star forming complexes NGC604 and NGC595. beta declines from close to 2 in the center to about 1.3 in the outer disk. beta is positively correlated with star formation and with molecular gas column, as traced by Halpha and CO emission. The lower dust emissivity index in the outer parts of M33 is likely related to the reduced metallicity (different grain composition) and possibly different size distribution. It is not due to the decrease in stellar radiation field or temperature in a simple way because the FIR-bright regions in the outer disk also have a low beta. Like most spirals, M33 has a (decreasing) radial gradient in star formation and molecular-to-atomic gas ratio such that the regions bright in Halpha or CO tend to trace the inner disk, making it difficult to distinguish between their effects on the dust., 18 pages, 16 figures, Accepted for Publication in Astronomy & Astrophysics Journal
Published: 2014

15. Energy Envelope and Attenuation Characteristics of High-Frequency (HF) and Very-High-Frequency (VF) Martian Events

Author: Simon Stähler, Raphaël F. Garcia, Jules Marti, Sabrina Menina, Nicholas Schmerr, William B. Banerdt, Nicolas Compaire, Grégory Sainton, Mélanie Drilleau, Martin van Driel, Sebastián Carrasco, Domenico Giardini, Ludovic Margerin, Marie Calvet, Philippe Lognonné, Matthieu Plasman, Taichi Kawamura, Brigitte Knapmeyer-Endrun, Foivos Karakostas, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), University of Maryland [College Park], University of Maryland System, Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Bologna (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universität zu Köln, Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, NASA-California Institute of Technology (CALTECH), and ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019)
Subjects: Martian, Physics, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Attenuation, Very high frequency, 010502 geochemistry & geophysics, 01 natural sciences, Computational physics, Geophysics, 13. Climate action, Geochemistry and Petrology, Mars seismology, Energy (signal processing), 0105 earth and related environmental sciences, Envelope (waves)
Abstract: Since its deployment at the surface of Mars, the Seismic Experiment for Interior Structure (SEIS) instrument of the InSight mission has detected hundreds of small-magnitude seismic events. In this work, we highlight some features of two specific families: high-frequency (HF) and very-high-frequency (VF) events. We characterize the shape of the energy envelopes of HF and VF events with two parameters: (1) the delay time td between the onset and the peak of the dominant arrival; and (2) the quality factor Qc, which quantifies the energy decay rate in the coda. We observe that the envelope of HF and VF events is frequency independent. As a consequence, a single delay time suffices to characterize envelope broadening in the 2.5–7.5 Hz band. The typical coda decay time is also frequency independent, as attested by the close to linear increase of Qc with frequency. Finally, we use elastic radiative transfer theory to perform a series of inversion of seismogram envelopes for the attenuation properties of the Martian lithosphere. The good fit between synthetic and observed envelopes confirms that multiple scattering of elastic waves released by internal sources is a plausible explanation of the events characteristics. We quantify scattering and attenuation properties of Mars and highlight the differences and similarities with the Earth and the Moon. The albedo, that is, the contribution of scattering to the total attenuation, derived from VF events is very high, which we interpret as a signature of a mostly dry medium. Our results also suggest a stratification of the scattering and attenuation properties.
Published: 2021

16. Ainos (moderne Enez), ville et territoire : résultats de la mission du Ministère des Affaires Étrangères et du projet CNRS Legecartas (2017-2022)

Author: Dan, Anca, Başaran, Sait, Brückner, Helmut, Erkul, Ercan, Houal, Jean-Baptiste, Marchand-Beaulieu, Frédérique, Pint, Anna, Rabbel, Wolfgang, Reize, Felix, Kircin, Sahan, Mitchell, Piers, Schmidts, Thomas, Seeliger, Martin, Shumilovskikh, Lyudmila, Wilken, Dennis, Wunderlich, Tina, Wang, Tianyi, Archéologie et Philologie d'Orient et d'Occident (AOROC), École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Département des Sciences de l'Antiquité - ENS Paris (DSA ENS-PSL), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL), Université d'Istanbul, Mathematisch-Naturwissenschaftliche Fakultät [Köln], Universität zu Köln = University of Cologne, Université de Kiel, Centre National de la Recherche Scientifique (CNRS), Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Institut für Geowissenschaften [Kiel], Christian-Albrechts-Universität zu Kiel (CAU), Römisch-Germanisches Zentralmuseum, Leibniz-Forschungsinstitut für Archäologie, Institut méditerranéen de biodiversité et d'écologie marine et continentale (IMBE), Avignon Université (AU)-Aix Marseille Université (AMU)-Institut de recherche pour le développement [IRD] : UMR237-Centre National de la Recherche Scientifique (CNRS), Christian-Albrechts University of Kiel, Department of Geography [Mainz], Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), and Dan, Anca
Subjects: [SHS.ARCHEO] Humanities and Social Sciences/Archaeology and Prehistory, [SHS.ARCHEO]Humanities and Social Sciences/Archaeology and Prehistory, Lagunes, ports, [SDE.MCG]Environmental Sciences/Global Changes, Deltas, [SHS.ART]Humanities and Social Sciences/Art and art history, [SDE.ES]Environmental Sciences/Environmental and Society, [SDE.MCG] Environmental Sciences/Global Changes, Ainos, [SHS.CLASS] Humanities and Social Sciences/Classical studies, [SHS.ART] Humanities and Social Sciences/Art and art history, [SDE.ES] Environmental Sciences/Environmental and Society, [SHS.CLASS]Humanities and Social Sciences/Classical studies, Hebros River
Abstract: International audience; Pendant les trois derniers millénaires, Ainos (moderne Enez, dans la province turqued’Edirne, en Europe) a été un des carrefours commerciaux de la Méditerranée orientale, entrel’Asie Mineure, l’Europe du Sud et les Balkans. Située sur une île qui est définitivementdevenue, au Néolithique, une presqu’île, entre les embouchures du fleuve Hèbre (en turcMeriç) et la mer Égée, Ainos/Enez a contrôlé tout le trafic Ouest-Est le long de la côteégéenne, mais aussi Nord-Sud, le long de la vallée du fleuve et de ses affluents. À l’époqueantique et médiévale, le delta de l’Hèbre n’avait pas encore atteint la ville elle-même, qui étaitentourée par la mer. Des bancs de sable ont progressivement fermé les golfes autour de lapresqu’île, donnant naissance à des lagunes propices à l’installation des ports, des salines etdes pêcheries. Cette importance stratégique d’Ainos est confirmée par les auteurs anciens etmodernes, mais aussi par les découvertes archéologiques extrêmement riches, surtout dans lesnécropoles fouillées par Sait Başaran autour de la ville.Dans cet exposé, nous évoquerons l’histoire d’Ainos, reconstituée à partir de sourceslittéraires confrontées à la documentation archéologique et géoarchéologique. Dans lapremière partie, nous nous concentrons sur l’espace urbain (l’« Acropole » et l’espace habitéautour), depuis le VI e siècle av. J.-C. à l’époque ottomane. Dans la seconde partie, nousprésentons les espaces frontaliers : les fortifications et quelques découvertes des nécropoles,actuellement à l’étude au Musée d’Edirne. Dans la dernière partie, nous synthétisons nosrésultats sur les ports urbains et extra-urbains, et sur les routes reliant Ainos (et Gala Gölü) aureste du monde.
Published: 2022

17. Formation of the acenaphthylene cation as a common C2H2-loss fragment in dissociative ionization of the PAH isomers anthracene and phenanthrene

Author: Shreyak Banhatti, Daniël B. Rap, Aude Simon, Heloïse Leboucher, Gabi Wenzel, Christine Joblin, Britta Redlich, Stephan Schlemmer, Sandra Brünken, Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Radboud University, Institute for Molecules and Materials, FELIX Laboratory, Modélisation, Agrégats, Dynamique (LCPQ) (MAD), Laboratoire de Chimie et Physique Quantiques Laboratoire (LCPQ), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche « Matière et interactions » (FeRMI), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, University of Aarhus, Institut de recherche en astrophysique et planétologie (IRAP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: [CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry, General Physics and Astronomy, Physical and Theoretical Chemistry, FELIX Infrared and Terahertz Spectroscopy
Abstract: International audience; Polycyclic aromatic hydrocarbons (PAHs) are thought to be a major constituent of astrophysical environments, being the carriers of the ubiquitous aromatic infrared bands (AIBs) observed in the spectra of galactic and extra-galactic sources that are irradiated by ultraviolet (UV) photons. Small (2-cycles) PAHs were unambiguously detected in the TMC-1 dark cloud, showing that PAH growth pathways exist even at low temperatures. The processing of PAHs by UV photons also leads to their fragmentation, which has been recognized in recent years as an alternative route to the generally accepted bottom-up chemical pathways for the formation of complex hydrocarbons in UV-rich interstellar regions. Here we consider the C12H8+ ion that is formed in our experiments from the dissociative ionization of the anthracene and phenanthrene (C14H10) molecules. By employing the sensitive action spectroscopic scheme of infrared pre-dissociation (IRPD) in a cryogenic ion trap instrument coupled to the free-electron lasers at the FELIX Laboratory, we have recorded the broadband and narrow line-width gas-phase IR spectra of the fragment ions (C12H8+) and also the reference spectra of three low energy isomers of C12H8+. By comparing the experimental spectra to those obtained from quantum chemical calculations we have identified the dominant structure of the fragment ion formed in the dissociation process to be the acenaphthylene cation for both isomeric precursors. Ab initio molecular dynamics simulations are presented to elucidate the fragmentation process. This result reinforces the dominant role of species containing a pentagonal ring in the photochemistry of small PAHs
Published: 2022

18. A dataset of temperature, humidity, and liquid water path retrievals from a network of ground-based microwave radiometers dedicated to fog investigation

Author: Pauline Martinet, Vinciane Unger, Frédéric Burnet, Jean-François Georgis, Maxime Hervo, Thierry Huet, Ulrich Löhnert, Eugene Miller, Emiliano Orlandi, Jeremy Price, Mathias Schröder, Guillaume Thomas, Centre national de recherches météorologiques (CNRM), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'aérologie (LAERO), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Federal Office of Meteorology and Climatology MeteoSwiss, ONERA / DOTA, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Universität zu Köln = University of Cologne, United Kingdom Met Office [Exeter], Università degli Studi dell'Aquila = University of L'Aquila (UNIVAQ), Istituto di Metodologie per l'Analisi Ambientale (IMAA), and Consiglio Nazionale delle Ricerche [Potenza] (CNR)
Subjects: Fog, [INFO.INFO-DB]Computer Science [cs]/Databases [cs.DB], Brightness temperatures, Temperature, General Earth and Planetary Sciences, Microwave radiometer, Humidity, Liquid water path, [SDU.STU.ME]Sciences of the Universe [physics]/Earth Sciences/Meteorology, Integrated water vapor, General Environmental Science
Abstract: International audience; The database presented in this study has been acquired during the SOuth west FOGs 3D (SOFOG3D) experiment for processes study. This international campaign led by Météo-France during the winter 2019-2020 aimed at deploying a unique network of both in situ and remote sensing measurements in order to document spatial and temporal variabilities of fog events. To support this scientific objective but also to conduct first data assimilation experiments within the French convective scale model AROME, an unprecedented network of 8 ground-based microwave radiometers (MWR) has been deployed in 7 different locations known to be prone to fog occurrences. The database gives access to vertical profiles of temperature and humidity (both absolute and relative) from the surface up to 10 km altitude as well as integrated water vapor and liquid water path estimates. The retrieved profiles offer a very large database that can be exploited for several scientific purposes: fog process studies at specific location, documentation on the variability of fog properties at the regional scale, better understanding of the atmospheric boundary layer (ABL) height and dynamics during wintertime conditions, development of nowcasting products dedicated to fog alerts, data assimilation experiments to improve fog forecasts, development of synergetical advanced products, and evaluation of new model configurations with advanced parameterization or resolutions. Keywords Microwave radiometer • Brightness temperatures • Fog • Temperature • Humidity • Liquid water path • Integrated water vapor All the authors contributed to the instrumental deployment of microwave radiometers. Pauline Martinet and Vinciane Unger conducted the scientific evaluation, data preparation, and the data delivery on the AERIS portal.
Published: 2022

19. Ainos, Its Territory and the Hebros Delta: Geoarchaeological Results

Author: Dan, Anca, Başaran, Sait, Brückner, Helmut, Erkul, Ercan, Pint, Anna, Rabbel, Wolfgang, Reize, Felix, Seeliger, Martin, Shumilovskikh, Lyudmila, Wunderlich, Tina, École française d'Athènes (EfA), Istanbul University, Universität zu Köln = University of Cologne, Université de Kiel, Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Institut méditerranéen de biodiversité et d'écologie marine et continentale (IMBE), Avignon Université (AU)-Aix Marseille Université (AMU)-Institut de recherche pour le développement [IRD] : UMR237-Centre National de la Recherche Scientifique (CNRS), Department of Geography [Mainz], Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), and Dan, Anca
Subjects: [SHS.ARCHEO] Humanities and Social Sciences/Archaeology and Prehistory, [SHS.ARCHEO]Humanities and Social Sciences/Archaeology and Prehistory, [SHS.ENVIR] Humanities and Social Sciences/Environmental studies, [SHS.GEO] Humanities and Social Sciences/Geography, [SHS.ENVIR]Humanities and Social Sciences/Environmental studies, [SHS.CLASS] Humanities and Social Sciences/Classical studies, [SDE.ES] Environmental Sciences/Environmental and Society, [SHS.GEO]Humanities and Social Sciences/Geography, [SHS.CLASS]Humanities and Social Sciences/Classical studies, [SDE.ES]Environmental Sciences/Environmental and Society
Abstract: Νησί των Νεολιθικών χρόνων, χερσόνησος από την Εποχή του Χαλκού, η πόλη του Αίνουυπήρξε ένα από τα κύρια εμπορικά σταυροδρόμια του Βορείου Αιγαίου, στις εκβολές τουΈβρου, μεταξύ της ελληνικής θάλασσας και της θρακικής ενδοχώρας. Οι ετήσιες τουρκικέςαρχαιολογικές ανασκαφές (ξεκίνησαν το 1973, υπό τη διεύθυνση του Sait Başaran για σχεδόν40 χρόνια, έως το 2019) έχουν αποκαλύψει αρκετά στοιχεία της χώρας (νεκροπόλεις, δρόμοι,οχυρώσεις). Η γεωαρχαιολογική έρευνα, που ξεκίνησε από τους Helmut Brückner, WolfgangRabbel και Thomas Schmidts στο 2011-2012, συνεχίστηκε τώρα στο πλαίσιο μιας γαλλικήςδιεθνούς αποστολής που συντονίστηκε από την Anca Dan, παρήγαγε δεδομένα για τη θέσηκαι την χρονολογίαν των λιμανιών της πόλης και για τις περιβαλλοντικές αλλαγές στηνεπικράτεια. Σε αυτή την εργασία, θα παρουσιάσουμε τα κύρια αποτελέσματα των κοινών μαςέργων σχετικά με τη φυσική εξέλιξη του ακρωτηρίου του Αίνου και του δέλτα του Έβρου,καθώς και για τις ανθρώπινες επιπτώσεις στην περιοχή., Island in Neolithic times, peninsula from the Bronze Age onwards, Ainos has been one of themain hubs of the Northern Aegean, at the mouth of the Hebros, between the Greek sea and theThracian hinterland. Annual Turkish archaeological excavations and surveys (started in 1973,directed by Sait Bașaran for nearly 40 years, until 2019) have revealed several components ofthe chora (necropoleis, roads, fortifications). The geoarchaeological research, initiated byHelmut Brückner, Wolfgang Rabbel and Thomas Schmidts in 2011-2012, now continued inthe frame of a French international mission coordinated by Anca Dan, produced data for thelocation and evolution of the city’s lagoonal harbours as well as for the environmentalchanges in the territory. In this paper, we will present the main results of our joint projectsabout the natural evolution of the Ainos promontory and Hebros delta, as well as about thehuman impact in the region.
Published: 2022

20. Gas and dust cooling along the major axis of M 33 (HerM33es). ISO/LWS [C ii] observations

Author: M. Boquien, Pierre Gratier, P. van der Werf, Christof Buchbender, S. Verley, C. Kramer, J. Abreu-Vicente, M. Roellig, E. M. Xilouris, Susanne Aalto, J. Braine, T. Nikola, Monica Relaño, Santiago García-Burillo, Frank P. Israel, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Dpto. Fisica Teorica y del Cosmos, Universidad de Granada (UGR), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institut de RadioAstronomie Millimétrique (IRAM), KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln-Universität zu Köln, Dept. fısica Teorica y del Cosmos, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Observatorio Astronomico Nacional, Madrid, Universidad de Granada = University of Granada (UGR), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, and Universiteit Leiden
Subjects: Physics, Spiral galaxy, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Metallicity, Molecular cloud, Semi-major axis, Local Group, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, Photoelectric effect, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 7. Clean energy, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We aim to better understand the heating of the gas by observing the prominent gas cooling line [CII] at 158um in the low-metallicity environment of the Local Group spiral galaxy M33 at scales of 280pc. In particular, we aim at describing the variation of the photoelectric heating efficiency with galactic environment. In this unbiased study, we used ISO/LWS [CII] observations along the major axis of M33, in combination with Herschel PACS and SPIRE continuum maps, IRAM 30m CO 2-1 and VLA HI data to study the variation of velocity integrated intensities. The ratio of [CII] emission over the far-infrared continuum is used as a proxy for the heating efficiency, and models of photon-dominated regions are used to study the local physical densities, FUV radiation fields, and average column densities of the molecular clouds. The heating efficiency stays constant at 0.8% in the inner 4.5kpc radius of the galaxy where it starts to increase to reach values of ~3% in the outskirts at about 6kpc radial distance. The rise of efficiency is explained in the framework of PDR models by lowered volume densities and FUV fields, for optical extinctions of only a few magnitudes at constant metallicity. In view of the significant fraction of HI emission stemming from PDRs, and for typical pressures found in the Galactic cold neutral medium (CNM) traced by HI emission, the CNM contributes ~15% to the observed [CII] emission in the inner 2kpc radius of M33. The CNM contribution remains largely undetermined in the south, while positions between 2 and 7.3kpc radial distance in the north of M33 show a contribution of ~40%+-20%., (16 pages, a version with higher resolution figures may be downloaded from http://www.iram.es/IRAMES/hermesWiki/HermesPublications)
Published: 2013

21. Dust and gas power-spectrum in M33 (HERM33ES)

Author: S. D. Lord, Fatemeh Tabatabaei, S. Verley, Frank P. Israel, Remo P. J. Tilanus, Baerbel Koribalski, P. van der Werf, C. Kramer, E. M. Xilouris, G. Quintana-Lacaci, J. Braine, M. Boquien, Francoise Combes, Frank Bertoldi, Christof Buchbender, D. Calzetti, M. Roellig, G. Stacey, F. F. S. van der Tak, Monica Relaño, Pierre Gratier, Kapteyn Astronomical Institute, Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Department of Astronomy, University of Massachusetts System (UMASS), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dpto. Fisica Teorica y del Cosmos, Universidad de Granada (UGR), KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln-Universität zu Köln, Dept. fısica Teorica y del Cosmos, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Universiteit Leiden, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad de Granada = University of Granada (UGR), Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, FLOCCULANT SPIRAL STRUCTURE, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, EXTENDED SURVEY HERM33ES, 01 natural sciences, Spectral line, STAR-FORMATION, DIFFUSE IONIZED-GAS, Bulge, 0103 physical sciences, DARK-MATTER, SMALL-MAGELLANIC-CLOUD, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Spectral density, Astronomy and Astrophysics, Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], galaxies: general, Galaxy, galaxies: individual: M 33, NGC 891, GALACTIC NEUTRAL HYDROGEN, Interstellar medium, Wavelength, Supernova, Space and Planetary Science, Local Group, MOLECULAR CLOUDS, galaxies: structure, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics, H-I
Abstract: Power spectra of de-projected images of late-type galaxies in gas and/or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power-laws, a shallow one at large scales (larger than 500 pc) and a steeper one at small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The large dynamical range (2-3 dex in scale) of most images allow us to determine clearly the change in slopes from -1.5 to -4, with some variations with wavelength. The break scale is increasing with wavelength, from 100 pc at 24 and 100micron to 350 pc at 500micron, suggesting that the cool dust lies in a thicker disk than the warm dust, may be due to star formation more confined to the plane. The slope at small scale tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, like M33, are carried out, in order to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power-spectra, with two power-law slopes and breaks, which nicely bracket the data. The small-scale power-law is indeed reflecting the 3D behaviour of the gas layer, steepening strongly while the feedback smoothes the structures, by increasing the gas turbulence. M33 appears to correspond to a fiducial model with an SFR of $\sim$ 0.7 Mo/yr, with 10% supernovae energy coupled to the gas kinematics., Comment: 11 pages, 24 figures, accepted in Astronomy & Astrophysics
Published: 2012

22. The SEDIGISM survey: Molecular cloud morphology

Author: Neralwar, K., Colombo, D., Duarte-Cabral, A., Urquhart, J., Mattern, M., Wyrowski, F., Menten, K., Barnes, P., Sánchez-Monge, Á., Rigby, A., Mazumdar, P., Eden, D., Csengeri, T., Dobbs, C., Veena, V., Neupane, S., Henning, T., Schuller, F., Leurini, S., Wienen, M., Yang, A., Ragan, S., Medina, S., Nguyen-Luong, Q., School of Physics and Astronomy [Cardiff], Cardiff University, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Max-Planck-Institut für Radioastronomie (MPIFR), Max Planck Institute for Radio Astronomy, Universität zu Köln = University of Cologne, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), FORMATION STELLAIRE 2020, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Tampere [Finland], INAF - Osservatorio Astronomico di Cagliari (OAC), and Istituto Nazionale di Astrofisica (INAF)
Subjects: [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU]Sciences of the Universe [physics]
Abstract: International audience; The Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium (SEDIGISM) survey has produced high (spatial and spectral) resolution 13 CO (2−1) maps of the Milky Way. It has allowed us to investigate the molecular interstellar medium in the inner Galaxy at an unprecedented level of detail and characterise it into molecular clouds (MCs). In a previous paper, we classified the SEDIGISM clouds into four morphologies. However, how the properties of the clouds vary for these four morphologies is not well understood. Here, we use the morphological classification of SEDIGISM clouds to find connections between the cloud morphologies, their integrated properties, and their location on scaling relation diagrams. We observe that ring-like clouds show the most peculiar properties, having, on average, higher masses, sizes, aspect ratios, and velocity dispersions, compared to other morphologies. We speculate that this is related to the physical mechanisms that regulate their formation and evolution; for example, turbulence from stellar feedback can often result in the creation of bubble-like structures. We also see a trend of morphology with the virial parameter, whereby ring-like, elongated, clumpy, and concentrated clouds have virial parameters in decreasing order. Our findings provide a foundation for a better understanding of MC behaviour, based on their measurable properties.
Published: 2022

23. Kôm Ombo (2021). Temple ptolémaïque d’Haroéris et de Sobek au nord d’Assouan

Author: Françoise Labrique, Ali Abdelhalim Ali, Marion Claude, Emmanuel Laroze, Aurélie Terrier, Universität zu Köln = University of Cologne, Université Ain Shams, Archéologie des Sociétés Méditerranéennes (ASM), Université Paul-Valéry - Montpellier 3 (UPVM)-Centre National de la Recherche Scientifique (CNRS)-Ministère de la Culture (MC), Institut français d'archéologie orientale du Caire (IFAO), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), ORIENT ET MÉDITERRANÉE : Textes, Archéologie, Histoire (OM), Université Paris 1 Panthéon-Sorbonne (UP1)-École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche sur l'architecture antique (IRAA), and Université Lumière - Lyon 2 (UL2)-Aix Marseille Université (AMU)-Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SHS.ARCHEO]Humanities and Social Sciences/Archaeology and Prehistory, General Earth and Planetary Sciences, General Environmental Science
Abstract: International audience
Published: 2022

24. Molecular and Atomic Gas in the Local Group Galaxy M33

Author: Wiedner, M., Bontemps, S., Henkel, C., Van Der Werf, P., Herpin, F., Van Der Tak, F., Rodriguez-Fernandez, N., Calzetti, D., Mookerjea, B., Gratier, P., Sievers, A., Brouillet, N., Israel, F., Henkel, Carsten, Schuster, K., Braine, J., Tabatabaei, F., Xilouris, E., Combes, F., Herpin, Fabrice, Garcia-Burillo, S., Corbelli, E., Wiklind, T., Koribalski, B., Roellig, M., Kramer, C., Aalto, S., Bontemps, Sylvain, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Institut für Physik (Institut für Physik), Universität Potsdam, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Department of Astronomy, University of Massachusetts System (UMASS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Onsala Space Observatory, Chalmers University of Technology [Göteborg], Australia Telescope National Facility, Australian National University (ANU), KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln-Universität zu Köln, KOSMA, I. Physikalisches Institut, Universität zu Köln, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), University of Potsdam = Universität Potsdam, Universiteit Leiden, Observatorio Astronomico Nacional, Madrid, École normale supérieure - Paris (ENS-PSL), Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, Universität zu Köln = University of Cologne, and Astronomy
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Metallicity, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: clouds, STAR-FORMATION EFFICIENCY, 01 natural sciences, Luminosity, CO EMISSION, 0103 physical sciences, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, M33, Physics, FORMATION HISTORY, stars: formation, Spiral galaxy, FORMING GALAXIES, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Astronomy and Astrophysics, Radius, Cosmology and Extragalactic Astrophysics, RADIO-CONTINUUM SURVEY, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], galaxies: individual: M 33, FAR-ULTRAVIOLET, Galaxy, SCHMIDT LAW, Space and Planetary Science, Local Group, galaxies: evolution, SPIRAL GALAXIES, galaxies: ISM, STELLAR POPULATION, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present high resolution large scale observations of the molecular and atomic gas in the Local Group Galaxy M33. The observations were carried out using the HERA at the 30m IRAM telescope in the CO(2-1) line achieving a resolution of 12"x2.6 km/s, enabling individual GMCs to be resolved. The observed region mainly along the major axis out to a radius of 8.5 kpc, and covers the strip observed with HIFI/PACS Spectrometers as part of the HERM33ES Herschel key program. The achieved sensitivity in main beam temperature is 20-50 mK at 2.6 km/s velocity resolution. The CO(2-1) luminosity of the observed region is 1.7\pm0.1x10^7 Kkm/s pc^2, corresponding to H2 masses of 1.9x10^8 Msun (including He), calculated with a NH2/ICO twice the Galactic value due to the half-solar metallicity of M33. HI 21 cm VLA archive observations were reduced and the mosaic was imaged and cleaned using the multi-scale task in CASA, yielding a series of datacubes with resolutions ranging from 5" to 25". The HI mass within a radius of 8.5 kpc is estimated to be 1.4x10^9 Msun. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9\pm0.1 kpc whereas the atomic gas surface density is constant at Sigma_HI=6\pm2 Msun/pc^2 deprojected to face-on. The central kiloparsec H_2 surface density is Sigma_H2=8.5\pm0.2 Msun/pc^2. The star formation rate per unit molecular gas (SF Efficiency, the rate of transformation of molecular gas into stars), as traced by the ratio of CO to Halpha and FIR brightness, is constant with radius. The SFE appears 2-4 times greater than of large spiral galaxies. A morphological comparison of molecular and atomic gas with tracers of star formation shows good agreement between these maps both in terms of peaks and holes. A few exceptions are noted. Several spectra, including those of a molecular cloud situated more than 8 kpc from the galaxy center, are presented., Accepted for publication in A&A. Higher resolution version available at : http://www.obs.u-bordeaux1.fr/radio/gratier/M33_CO_HI_accepted.pdf
Published: 2010

25. PACS and SPIRE photometer maps of M33: First results of the Herschel M33 extended survey (HERM33ES)

Author: C. Kramer, C. Buchbender, E. M. Xilouris, M. Boquien, J. Braine, D. Calzetti, S. Lord, B. Mookerjea, G. Quintana-Lacaci, M. Relaño, G. Stacey, F. S. Tabatabaei, S. Verley, S. Aalto, S. Akras, M. Albrecht, S. Anderl, R. Beck, F. Bertoldi, F. Combes, M. Dumke, S. Garcia-Burillo, M. Gonzalez, P. Gratier, R. Güsten, C. Henkel, F. P. Israel, B. Koribalski, A. Lundgren, J. Martin-Pintado, M. Röllig, E. Rosolowsky, K. F. Schuster, K. Sheth, A. Sievers, J. Stutzki, R. P. J. Tilanus, F. van der Tak, P. van der Werf, M. C. Wiedner, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, University of Massachusetts System (UMASS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), KOSMA, I. Physikalisches Institut, Universität zu Köln = University of Cologne, Dpto. Fisica Teorica y del Cosmos, Universidad de Granada = University of Granada (UGR), Dept. fısica Teorica y del Cosmos, Institute of Physics, Berlin, HUMBOLT UNIV., Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional, Madrid, Fundación Venezolana de Investigaciones Sismológicas (FUNVISIS), FUNVISIS, Instituto de Ciencias de la Tierra, Universidad Central de Venezuela (UCV), Institut für Physik (Institut für Physik), University of Potsdam = Universität Potsdam, Australia Telescope National Facility, Australian National University (ANU), KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, University of British Columbia (UBC), Institut de RadioAstronomie Millimétrique (IRAM), Spitzer Science Center, California Institute of Technology, Pasadena, California Institute of Technology (CALTECH), Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Universität zu Köln, Universidad de Granada (UGR), École normale supérieure - Paris (ENS Paris), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Universität Potsdam, Universität zu Köln-Universität zu Köln, École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), and UNIVERSIDAD CENTRAL DE VENEZUELA
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Metallicity, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GALAXY M33, STAR-FORMATION, NEARBY, 0103 physical sciences, Emissivity, Astrophysics::Solar and Stellar Astrophysics, COLD DUST, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Spiral galaxy, extinction, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Radius, galaxies: individual: M33, Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Galaxy, CLOUD, Interstellar medium, INFRARED STRUCTURE, Wavelength, Spire, Space and Planetary Science, Local Group, MILKY-WAY, dust, dust, extinction, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, EMISSION, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Within the framework of the HERM33ES key project, we are studying the star forming interstellar medium in the nearby, metal-poor spiral galaxy M33, exploiting the high resolution and sensitivity of Herschel. We use PACS and SPIRE maps at 100, 160, 250, 350, and 500 micron wavelength, to study the variation of the spectral energy distributions (SEDs) with galacto-centric distance. Detailed SED modeling is performed using azimuthally averaged fluxes in elliptical rings of 2 kpc width, out to 8 kpc galacto-centric distance. Simple isothermal and two-component grey body models, with fixed dust emissivity index, are fitted to the SEDs between 24 and 500 micron using also MIPS/Spitzer data, to derive first estimates of the dust physical conditions. The far-infrared and submillimeter maps reveal the branched, knotted spiral structure of M33. An underlying diffuse disk is seen in all SPIRE maps (250-500 micron). Two component fits to the SEDs agree better than isothermal models with the observed, total and radially averaged flux densities. The two component model, with beta fixed at 1.5, best fits the global and the radial SEDs. The cold dust component clearly dominates; the relative mass of the warm component is less than 0.3% for all the fits. The temperature of the warm component is not well constrained and is found to be about 60K plus/minus 10K. The temperature of the cold component drops significantly from about 24K in the inner 2 kpc radius to 13K beyond 6 kpc radial distance, for the best fitting model. The gas-to-dust ratio for beta=1.5, averaged over the galaxy, is higher than the solar value by a factor of 1.5 and is roughly in agreement with the subsolar metallicity of M33., Comment: 5 pages, 3 figures, accepted for publication in the A&A Herschel Special Issue
Published: 2010
Full Text: View/download PDF

26. Cool gas and dust in M33: Results from the Herschel M33 extended survey (HERM33ES)

Author: K. F. Schuster, Martina C. Wiedner, Bhaswati Mookerjea, G. Quintana-Lacaci, Susanne Aalto, Erik Rosolowsky, J. Braine, Fatemeh Tabatabaei, M. Gonzalez, B. S. Koribalski, P. van der Werf, C. Kramer, S. Verley, Carsten Henkel, F. F. S. van der Tak, Emmanuel M. Xilouris, Pierre Gratier, Frank P. Israel, Médéric Boquien, Monica Relaño, Christof Buchbender, Frank Bertoldi, Santiago García-Burillo, M. Roellig, Francoise Combes, D. Calzetti, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy and Astrophysics, National Observatory of Athens (NOA), University of British Columbia (UBC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, University of Massachusetts System (UMASS), Institut für Physik (Institut für Physik), University of Potsdam = Universität Potsdam, Dept. fısica Teorica y del Cosmos, Universidad de Granada = University of Granada (UGR), Leiden Observatory [Leiden], Universiteit Leiden, SRON Netherlands Institute for Space Research (SRON), Max-Planck-Institut für Radioastronomie (MPIFR), TKK Helsinki University of Technology (TKK), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional, Madrid, Fundación Venezolana de Investigaciones Sismológicas (FUNVISIS), FUNVISIS, Instituto de Ciencias de la Tierra, Universidad Central de Venezuela (UCV), Australia Telescope National Facility, Australian National University (ANU), KOSMA, I. Physikalisches Institut, Universität zu Köln = University of Cologne, KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne, Institut de RadioAstronomie Millimétrique (IRAM), Dpto. Fisica Teorica y del Cosmos, Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Instituto de RadioAstronomía Milimétrica ( IRAM ), Centre National de la Recherche Scientifique ( CNRS ), National Observatory of Athens ( NOA ), University of British Columbia ( UBC ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), University of Massachusetts, Institut für Physik ( Institut für Physik ), Universität Potsdam, Universidad de Granada ( UGR ), Universiteit Leiden [Leiden], SRON Netherlands Institute for Space Research ( SRON ), Max-Planck-Institut für Radioastronomie ( MPIFR ), TKK Helsinki University of Technology, Helsinki University of Technology ( TKK ) -TKK, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), Observatorio Astron ́omico Nacional (OAN), Observatorio de Madrid, Fundación Venezolana de Investigaciones Sismológicas ( FUNVISIS ), UNIVERSIDAD CENTRAL DE VENEZUELA, Australian National University ( ANU ), Universität zu Köln, Universität zu Köln-Universität zu Köln, Institut de RadioAstronomie Millimétrique ( IRAM ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universidad de Granada (UGR), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Astronomy, and École normale supérieure - Paris (ENS Paris)
Subjects: Systematic error, GRAPHITE, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, ISM: Clouds, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Galaxies: Local Group, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, [ PHYS.ASTR.SR ] Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Galaxies: evolution, Astronomy and Astrophysics, galaxies: individual: M33, Mass ratio, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Galaxy, Spire, Galaxies: ISM, 13. Climate action, Space and Planetary Science, Galaxies: Individual: M 33, Content (measure theory), Local Group, Astrophysics::Earth and Planetary Astrophysics, Stars: Formation, [ SDU.ASTR.SR ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Cosmology and Nongalactic Astrophysics, Dust emission
Abstract: We present an analysis of the first space-based far-IR-submm observations of M 33, which measure the emission from the cool dust and resolve the giant molecular cloud complexes. With roughly half-solar abundances, M33 is a first step towards young low-metallicity galaxies where the submm may be able to provide an alternative to CO mapping to measure their H$_2$ content. In this Letter, we measure the dust emission cross-section $\sigma$ using SPIRE and recent CO and \HI\ observations; a variation in $\sigma$ is present from a near-solar neighborhood cross-section to about half-solar with the maximum being south of the nucleus. Calculating the total H column density from the measured dust temperature and cross-section, and then subtracting the \HI\ column, yields a morphology similar to that observed in CO. The H$_2$/\HI\ mass ratio decreases from about unity to well below 10% and is about 15% averaged over the optical disk. The single most important observation to reduce the potentially large systematic errors is to complete the CO mapping of M 33., Comment: 5 pages, 5 figures Accepted for publication in Astronomy and Astrophysics
Published: 2010

27. Mixotrophic growth of the extremophile Galdieria sulphuraria reveals the flexibility of its carbon assimilation metabolism

Author: Andreas P.M. Weber, Phillip Westhoff, Marianne Tardif, Denis Falconet, Erika Guglielmino, Dagmar Lyska, Benoit Gallet, Giovanni Finazzi, Gilles Curien, Clément Hallopeau, Michele Carone, Davide Dal Bo, Claire Remacle, Johan Decelle, Sabine Brugière, Myriam Ferro, Janina Janetzko, Light Photosynthesis & Metabolism (Photosynthesis), Physiologie cellulaire et végétale (LPCV), Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Cluster of Excellence on Plant Sciences (CEPLAS), Heinrich Heine Universität Düsseldorf = Heinrich Heine University [Düsseldorf]-Max Planck Institute for Plant Breeding Research (MPIPZ)-Universität zu Köln = University of Cologne, Etude de la dynamique des protéomes (EDyP), BioSanté (UMR BioSanté), Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Photosymbiose, Institut de biologie structurale (IBS - UMR 5075), LIPID, Université de Liège, ARC grant (DARKMET proposal) for Concerted Research Actions (17/21-08), financed by the French Community of Belgium (Wallonia-Brussels Federation)., Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany´s Excellence Strategy – EXC-2048/1 – project ID 390686111, ANR-17-CE05-0029,MoMix,Modélisation de la Mixotrophie chez l'algue extrêmophile Galdieria sulphuraria(2017), ANR-10-LABX-0049,GRAL,Grenoble Alliance for Integrated Structural Cell Biology(2010), ANR-17-EURE-0003,CBH-EUR-GS,CBH-EUR-GS(2017), ANR-10-INBS-0008,ProFI,Infrastructure Française de Protéomique(2010), European Project: 833184, ChloroMito, Martin-Laffon, Jacqueline, Modélisation de la Mixotrophie chez l'algue extrêmophile Galdieria sulphuraria - - MoMix2017 - ANR-17-CE05-0029 - AAPG2017 - VALID, Grenoble Alliance for Integrated Structural Cell Biology - - GRAL2010 - ANR-10-LABX-0049 - LABX - VALID, CBH-EUR-GS - - CBH-EUR-GS2017 - ANR-17-EURE-0003 - EURE - VALID, Infrastructure Française de Protéomique - - ProFI2010 - ANR-10-INBS-0008 - INBS - VALID, Chloroplast and Mitochondria interactions for microalgal acclimation - ChloroMito - 833184 - INCOMING, Universität zu Köln-Heinrich Heine Universität Düsseldorf = Heinrich Heine University [Düsseldorf]-Max Planck Institute for Plant Breeding Research (MPIPZ), and InBios/Phytosystems Research Unit, University of Liege
Subjects: Proteomics, 0106 biological sciences, 0301 basic medicine, photorespiration, Physiology, Heterotroph, Plant Science, Photosynthesis, 7. Clean energy, 01 natural sciences, Galdieria sulphuraria, Extremophiles, 03 medical and health sciences, mixotrophy, Total inorganic carbon, Botany, [SDV.BBM] Life Sciences [q-bio]/Biochemistry, Molecular Biology, [SDV.BBM]Life Sciences [q-bio]/Biochemistry, Molecular Biology, red algae, photosynthesis, biology, Chemistry, Research, RuBisCO, Heterotrophic Processes, Carbon Dioxide, Full Papers, 15. Life on land, Carbon, 030104 developmental biology, Rhodophyta, biology.protein, Photorespiration, Energy source, Mixotroph, 010606 plant biology & botany
Abstract: Summary Galdieria sulphuraria is a cosmopolitan microalga found in volcanic hot springs and calderas. It grows at low pH in photoautotrophic (use of light as a source of energy) or heterotrophic (respiration as a source of energy) conditions, using an unusually broad range of organic carbon sources. Previous data suggested that G. sulphuraria cannot grow mixotrophically (simultaneously exploiting light and organic carbon as energy sources), its photosynthetic machinery being repressed by organic carbon.Here, we show that G. sulphuraria SAG21.92 thrives in photoautotrophy, heterotrophy and mixotrophy. By comparing growth, biomass production, photosynthetic and respiratory performances in these three trophic modes, we show that addition of organic carbon to cultures (mixotrophy) relieves inorganic carbon limitation of photosynthesis thanks to increased CO2 supply through respiration. This synergistic effect is lost when inorganic carbon limitation is artificially overcome by saturating photosynthesis with added external CO2.Proteomic and metabolic profiling corroborates this conclusion suggesting that mixotrophy is an opportunistic mechanism to increase intracellular CO2 concentration under physiological conditions, boosting photosynthesis by enhancing the carboxylation activity of Ribulose‐1,5‐bisphosphate carboxylase‐oxygenase (Rubisco) and decreasing photorespiration.We discuss possible implications of these findings for the ecological success of Galdieria in extreme environments and for biotechnological applications.
Published: 2021

28. The current state of laboratory mycology and access to antifungal treatment in Europe: a European Confederation of Medical Mycology survey

Author: Jon Salmanton-García, Martin Hoenigl, Jean-Pierre Gangneux, Esther Segal, Ana Alastruey-Izquierdo, Sevtap Arikan Akdagli, Katrien Lagrou, Volkan Özenci, Antonio Vena, Oliver A Cornely, Universität zu Köln = University of Cologne, Medical University of Graz, Institut de recherche en santé, environnement et travail (Irset), Université d'Angers (UA)-Université de Rennes (UR)-École des Hautes Études en Santé Publique [EHESP] (EHESP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Structure Fédérative de Recherche en Biologie et Santé de Rennes ( Biosit : Biologie - Santé - Innovation Technologique ), École des Hautes Études en Santé Publique [EHESP] (EHESP), Kfar Saba and Sackler School of Medicine, Instituto de Salud Carlos III [Madrid] (ISC), Faculty of Medicine [Hacettepe University], Hacettepe University = Hacettepe Üniversitesi, Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Karolinska Institute, and Università degli studi di Genova = University of Genoa (UniGe)
Subjects: Microbiology (medical), Europe, Echinocandins, Infectious Diseases, Antifungal Agents, Virology, [SDV]Life Sciences [q-bio], Humans, Mycology, Microbiology, Invasive Fungal Infections
Abstract: Access to the appropriate tools is crucial for early diagnosis and clinical management of invasive fungal infections. This Review aims to describe the invasive fungal infection diagnostic capacity of Europe to better understand the status and the most pressing aspects that need improvement. To our knowledge, this is the first time that the mycological diagnostic capability and access to antifungal treatments of institutions has been evaluated at a pan-European level. Between Nov 1, 2021, and Jan 31, 2022, 388 institutions in Europe self-assessed their invasive fungal infection management capability. Of the 388 participating institutions from 45 countries, 383 (99%) had access to cultures, 375 (97%) to microscopy, 363 (94%) to antigen-detection assays, 329 (85%) to molecular tests (mostly PCR), and 324 (84%) to antibody tests for diagnosis and management. With the exception of microscopy, there were considerable differences in access to techniques among countries according to their gross domestic product. At least one triazole was available in 363 (94%) of the institutions, one echinocandin in 346 (89%), and liposomal amphotericin B in 301 (78%), with country gross domestic product-based differences. Differences were also observed in the access to therapeutic drug monitoring. Although Europe is well prepared to manage invasive fungal infections, some institutions do not have access to certain diagnostic tools and antifungal drugs, despite most being considered essential by WHO. These limitations need to be overcome to ensure that all patients receive the best diagnostic and therapeutic management. ispartof: Lancet Microbe vol:4 issue:1 pages:e47-e56 ispartof: location:England status: published
Published: 2022

29. FGF21 modulates mitochondrial stress response in cardiomyocytes only under mild mitochondrial dysfunction

Author: Marijana Croon, Karolina Szczepanowska, Milica Popovic, Christina Lienkamp, Katharina Senft, Christoph Paul Brandscheid, Theresa Bock, Leoni Gnatzy-Feik, Artem Ashurov, Richard James Acton, Harshita Kaul, Claire Pujol, Stephan Rosenkranz, Marcus Krüger, Aleksandra Trifunovic, Universität zu Köln = University of Cologne, Polish Academy of Sciences (PAN), Max planck Institute for Biology of Ageing [Cologne], Biologie mitochondriale – Mitochondrial biology, Institut Pasteur [Paris] (IP)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), This work was supported by German Research Foundation [Deutsche Forschungsgemeinschaft (DFG)] SFB 1218 Projektnummer 269925409, German Research Foundation (DFG) TR 1018/8-1, and Centre for Molecular Medicine Cologne, University of Cologne C15 (to A.T.). M.C. received a scholarship from Marie Curie ITN—Marriage (Grant Agreement ID:316964). M.P and L.G.-F. were supported by the German Research Foundation (DFG, GRK-2407). S.R. is supported by the German Research Foundation (DFG, GRK-2407 and SFB-TRR259)., and European Project: 316964,EC:FP7:PEOPLE,FP7-PEOPLE-2012-ITN,MARRIAGE(2012)
Subjects: Multidisciplinary, [SDV.SPEE]Life Sciences [q-bio]/Santé publique et épidémiologie
Abstract: International audience; The mitochondrial integrated stress response (mitoISR) has emerged as a major adaptive pathway to respiratory chain deficiency, but both the tissue specificity of its regulation, and how mitoISR adapts to different levels of mitochondrial dysfunction are largely unknown. Here, we report that diverse levels of mitochondrial cardiomyopathy activate mitoISR, including high production of FGF21, a cytokine with both paracrine and endocrine function, shown to be induced by respiratory chain dysfunction. Although being fully dispensable for the cell-autonomous and systemic responses to severe mitochondrial cardiomyopathy, in the conditions of mild-to-moderate cardiac OXPHOS dysfunction, FGF21 regulates a portion of mitoISR. In the absence of FGF21, a large part of the metabolic adaptation to mitochondrial dysfunction (one-carbon metabolism, transsulfuration, and serine and proline biosynthesis) is strongly blunted, independent of the primary mitoISR activator ATF4. Collectively, our work highlights the complexity of mitochondrial stress responses by revealing the importance of the tissue specificity and dose dependency of mitoISR.
Published: 2022

30. Bloodstream Infections Caused by Magnusiomyces capitatus and Magnusiomyces clavatus : Epidemiological, Clinical, and Microbiological Features of Two Emerging Yeast Species

Author: Janina Noster, Martin B. Koeppel, Marie Desnos-Olivier, Maria Aigner, Oliver Bader, Karl Dichtl, Stephan Göttig, Andrea Haas, Oliver Kurzai, Arthur B. Pranada, Yvonne Stelzer, Grit Walther, Axel Hamprecht, Carl Von Ossietzky Universität Oldenburg = Carl von Ossietzky University of Oldenburg (OFFIS), Ludwig-Maximilians-Universität München (LMU), Mycologie moléculaire - Molecular Mycology, Institut Pasteur [Paris] (IP)-Centre National de la Recherche Scientifique (CNRS), Centre National de Référence Mycoses Invasives et Antifongiques - National Reference Center Invasive Mycoses & Antifungals (CNRMA), Institut Pasteur [Paris] (IP), Innsbruck Medical University = Medizinische Universität Innsbruck (IMU), University Medical Center Göttingen (UMG), Goethe-Universität Frankfurt am Main, Julius-Maximilians-Universität Würzburg (JMU), Leibniz Institute for Natural Product Research and Infection Biology (Hans Knoell Institute), MVZ Dr. Eberhard & Partner Dortmund, German Centre for Infection Research (DZIF), Universität zu Köln = University of Cologne, and Work in the NRZMyk is supported by the Robert-Koch-Institute from funds provided by the German Ministry of Health (grant no. 1369-240). This study was supported by internal funding.
Subjects: Pharmacology, Saprochaete capitata, Infectious Diseases, Magnusiomyces clavatus, [SDV]Life Sciences [q-bio], Saprochaete clavata, Pharmacology (medical), bloodstream infection, MIC, Magnusiomyces capitatus, Geotrichum
Abstract: International audience; Magnusiomyces clavatus and Magnusiomyces capitatus are emerging yeasts with intrinsic resistance to many commonly used antifungal agents. Identification is difficult, and determination of susceptibility patterns with commercial and reference methods is equally challenging. For this reason, few data on invasive infections by Magnusiomyces spp. are available. Our objectives were to determine the epidemiology and susceptibility of Magnusiomyces isolates from bloodstream infections (BSI) isolated in Germany and Austria from 2001 to 2020. In seven institutions, a total of 34 Magnusiomyces BSI were identified. Identification was done by internal transcribed spacer (ITS) sequencing and matrix-assisted laser desorption ionization–time of flight mass spectrometry (MALDI-TOF MS). Antifungal susceptibility was determined by EUCAST broth microdilution and gradient tests. Of the 34 isolates, M. clavatus was more common (n = 24) than M. capitatus (n = 10). BSI by Magnusiomyces spp. were more common in men (62%) and mostly occurred in patients with hemato-oncological malignancies (79%). The highest in vitro antifungal activity against M. clavatus/M. capitatus was observed for voriconazole (MIC50, 0.03/0.125 mg/L), followed by posaconazole (MIC50, 0.125/0.25 mg/L). M. clavatus isolates showed overall lower MICs than M. capitatus. With the exception of amphotericin B, low essential agreement between gradient test and microdilution was recorded for all antifungals (0 to 70%). Both species showed distinct morphologic traits on ChromAgar Orientation medium and Columbia blood agar, which can be used for differentiation if no MALDI-TOF MS or molecular identification is available. In conclusion, most BSI were caused by M. clavatus. The lowest MICs were recorded for voriconazole. Gradient tests demonstrated unacceptably low agreement and should preferably not be used for susceptibility testing of Magnusiomyces spp.
Published: 2022

31. Rotational spectroscopy of isotopic oxirane, c-C2H4O

Author: M��ller, Holger S. P., Guillemin, Jean-Claude, Lewen, Frank, Schlemmer, Stephan, Universität zu Köln = University of Cologne, Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), The work in Köln was supported by the Deutsche Forschungsgemeinschaft through the collaborative research center SFB 956 (project ID 184018867) project B3 and through the Gerätezentrum SCHL 341/15-1 ('Cologne Center for Terahertz Spectroscopy'). J.-C. G. acknowledges support by the Centre National d’Etudes Spatiales (CNES, France, and grant number 4500065585) and by the Programme National Physique et Chimie du Milieu Interstellaire (PCMI) of CNRS/INSU with INC/INP, France co-funded by CEA, France and CNES . Our research benefited from NASA’s Astrophysics Data System (ADS).
Subjects: Chemical Physics (physics.chem-ph), Rotational spectroscopy, Centrifugal distortion, Reduced Hamiltonian, FOS: Physical sciences, Cyclic molecule, Interstellar molecule, Astrophysics - Astrophysics of Galaxies, Astrophysics of Galaxies (astro-ph.GA), Physics - Chemical Physics, [CHIM]Chemical Sciences, Submillimeter spectroscopy, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: We studied the rotational spectrum of oxirane in a sample of natural isotopic composition in selected regions between 158 GHz and 1093 GHz. Investigations of the isotopologs with one $^{13}$C or one $^{18}$O were the primary focus in order to facilitate searches for them in space. We also examined the main isotopic species mainly to look into the performance of Watson's A and S reductions both in an oblate and in a prolate representation. Even though oxirane is a rather asymmetric oblate rotor, the A reduction in the III$^l$ representation did not yield a satisfactory fit, as was observed frequently earlier for other molecules. The other three combinations yielded satisfactory fits of similar quality among each other; the A reduction in the I$^r$ representation required two parameters less than both S reduction fits., 11 pages, including tables and figure; minor update; J. Mol. Spectrosc., published
Published: 2022

32. Detecting selection using extended haplotype homozygosity (EHH)-based statistics in unphased or unpolarized data

Author: Mathieu Gautier, Alexander Klassmann, Universität zu Köln = University of Cologne, Centre de Biologie pour la Gestion des Populations (UMR CBGP), Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad)-Institut de Recherche pour le Développement (IRD [France-Sud])-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut Agro Montpellier, and Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Université de Montpellier (UM)
Subjects: Heredity, Genomics Statistics, Mammalian Genomics, Multidisciplinary, Single Nucleotide Polymorphisms, Simulation and Modeling, Science, [SDV]Life Sciences [q-bio], Homozygote, Biology and Life Sciences, Computational Biology, Genomics, Research and Analysis Methods, Homozygosity, Genetic Mapping, Haplotypes, Genetic Loci, Animal Genomics, Genetics, Medicine, Alleles, Research Article
Abstract: Analysis of population genetic data often includes a search for genomic regions with signs of recent positive selection. One of such approaches involves the concept of extended haplotype homozygosity (EHH) and its associated statistics. These statistics typically require phased haplotypes, and some of them necessitate polarized variants. Here, we unify and extend previously proposed modifications to loosen these requirements. We compare the modified versions with the original ones by measuring the false discovery rate in simulated whole-genome scans and by quantifying the overlap of inferred candidate regions in empirical data. We find that phasing information is indispensable for accurate estimation of within-population statistics (for all but very large samples) and of cross-population statistics for small samples. Ancestry information, in contrast, is of lesser importance for both types of statistic. Our publicly available R package rehh incorporates the modified statistics presented here.
Published: 2022

33. MATISSE, the VLTI mid-infrared imaging spectro-interferometer

Author: Lopez, B., Lagarde, S., Petrov, R.G., Jaffe, W., Antonelli, P., Allouche, F., Berio, P., Matter, A., Meilland, A., Millour, F., Robbe-Dubois, S., Henning, T., Weigelt, G., Glindemann, A., Agocs, T., Bailet, C., Beckmann, U., Bettonvil, F., Boekel, R. van, Bourget, P., Bresson, Y., Bristow, P., Cruzalèbes, P., Eldswijk, E., Fanteï Caujolle, Y., González Herrera, J.C., Graser, U., Guajardo, P., Heininger, M., Hofmann, K.H., Kroes, G., Laun, W., Lehmitz, M., Leinert, C., Meisenheimer, K., Morel, S., Neumann, U., Paladini, C., Percheron, I., Riquelme, M., Schoeller, M., Stee, P., Venema, L., Woillez, J., Zins, G., Ábrahám, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Alonso, J., Augereau, J.-C., Böhm, A., Bazin, G., Beltran, J., Bensberg, A., Boland, W., Brast, R., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J.-M., Connot, C., Conzelmann, R.D., Danchi, W.C., Delbo, M., Drevon, J., Dominik, C., Duin, A. van, Ebert, M., Eisenhauer, F., Flament, S., Frahm, R., Gámez Rosas, V., Gabasch, A., Gallenne, A., Garces, E., Girard, P., Glazenborg, A., Gonté, F.Y.J., Guitton, F., Haan, M. de, Hanenburg, H., Haubois, X., Hocdé, V., Hogerheijde, M., Horst, R. ter, Hron, J., Hummel, C.A., Hubin, N., Huerta, R., Idserda, J., Isbell, J.W., Ives, D., Jakob, G., Jaskó, A., Jochum, L., Klarmann, L., Klein, R., Kragt, J., Kuindersma, S., Kokoulina, E., Labadie, L., Lacour, S., Leftley, J., Le Poole, R., Lizon, J.L., Lopez, M., Lykou, F., Mérand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L.H., Meisner, J., Meixner, K., Mellein, M., Menut, J.L., Mohr, L., Mosoni, L., Navarro, R., Nußbaum, E., Pallanca, L., Pantin, E., Pasquini, L., Phan Duc, T., Pott, J.U., Pozna, E., Richichi, A., Ridinger, A., Rigal, F., Rivinius, T., Roelfsema, R., Rohloff, R.-R., Rousseau, S., Salabert, D., Schertl, D., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., Toledo, P., Tristram, K., Tromp, N., Vakili, F., Varga, J., Vinther, J., Waters, L.B.F.M., Wittkowski, M., Wolf, S., Wrhel, F., Yoffe, G., Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Max-Planck-Institut für Radioastronomie (MPIFR), European Southern Observatory (ESO), Low Energy Astrophysics (API, FNWI), Université Côte d'Azur (UCA), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Centre de Développement des Energies Renouvelables (CDER), Ministère de l'Enseignement Supérieur et de la Recherche Scientifique [Algérie] (MESRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Astronomy (MPIA), European Southern Observatory Headquarters, NOVA Optical IR Instrumentation Group, Centre Hospitalier Universitaire d'Angers (CHU Angers), PRES Université Nantes Angers Le Mans (UNAM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Kiel University, NASA Goddard Space Flight Center (GSFC), Universiteit van Amsterdam (UvA), Max Planck Institute for Extraterrestrial Physics (MPE), Miniaturisation pour la Synthèse, l’Analyse et la Protéomique - UAR 3290 (MSAP), Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universidad de Concepción - University of Concepcion [Chile], médialab (Sciences Po) (médialab), Sciences Po (Sciences Po), Polish Academy of Sciences (PAN), Universität zu Köln = University of Cologne, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), École, mutations, apprentissages (EMA), CY Cergy Paris Université (CY), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Zselic Park of Stars, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Department of Hematology, Instituto Superiore di Sanita Roma, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institut National du Cancer [Boulogne Billancourt] (INC), and Radboud University [Nijmegen]
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, instrumentation: high angular resolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, methods: observational, instrumentation: interferometers, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Context:Optical interferometry is at a key development stage. ESO's VLTI has established a stable, robust infrastructure for long-baseline interferometry for general astronomical observers. The present second-generation instruments offer a wide wavelength coverage and improved performance. Their sensitivity and measurement accuracy lead to data and images of high reliability. Aims:We have developed MATISSE, the Multi AperTure mid-Infrared SpectroScopic Experiment, to access high resolution imaging in a wide spectral domain and explore topics such: stellar activity and mass loss; planet formation and evolution in the gas and dust disks around young stars; accretion processes around super massive black holes in AGN. Methods:The instrument is a spectro-interferometric imager covering three atmospheric bands (L,M,N) from 2.8 to 13.0 mu, combining four optical beams from the VLTI's telscopes. Its concept, related observing procedure, data reduction and calibration approach are the product of 30 years of instrumental research. The instrument utilizes a multi-axial beam combination that delivers spectrally dispersed fringes. The signal provides the following quantities at several spectral resolutions: photometric flux, coherent fluxes, visibilities, closure phases, wavelength differential visibilities and phases, and aperture-synthesis imaging. Results:We provide an overview of the physical principle of the instrument and its functionalities, the characteristics of the delivered signal, a description of the observing modes and of their performance limits. An ensemble of data and reconstructed images are illustrating the first acquired key observations. Conclusion:The instrument has been in operation at Cerro Paranal, ESO, Chile since 2018, and has been open for science use by the international community since April 2019. The first scientific results are being published now., 24 pages, 26 figures, submitted to Astronomy & Astrophysics
Published: 2022

34. The Formation of Physician Altruism

Author: Arthur E. Attema, Matteo M. Galizzi, Mona Groß, Heike Hennig-Schmidt, Yassin Karay, Olivier L’Haridon, Daniel Wiesen, Health Economics (HE), Applied Economics, Erasmus School of Health Policy and Management |Rotterdam], London School of Economics and Political Science (LSE), Universität zu Köln = University of Cologne, Universität Bonn = University of Bonn, Centre de recherche en économie et management (CREM), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), and Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.)
Subjects: Medical education, Online experiment, H Social Sciences, SDG 3 - Good Health and Well-being, Health Policy, Public Health, Environmental and Occupational Health, Structural estimation, [SHS.ECO]Humanities and Social Sciences/Economics and Finance, Laboratory experiment, Specialty choice, Patient-regarding altruism
Abstract: International audience; We study how patient-regarding altruism is formed by medical education. We elicit and structurally estimate altruistic preferences using experimental data from a large sample of medical students (N = 733) in Germany at different progress stages in their studies. The estimates reveal substantial heterogeneity in altruistic preferences of medical students. Patient-regarding altruism is highest for freshmen, significantly declines for students in the course of medical studies, and tends to increase again for last year students, who assist in clinical practice. Also, patient-regarding altruism is higher for females and positively associated to general altruism. Altruistic medical students have gained prior practical experience in healthcare, have lower income expectations, and are more likely to choose surgery and pediatrics as their preferred specialty.
Published: 2022

35. The stem rust effector protein AvrSr50 escapes Sr50 recognition by a substitution in a single surface-exposed residue

Author: Diana Ortiz, Jian Chen, Megan A. Outram, Isabel M.L. Saur, Narayana M. Upadhyaya, Rohit Mago, Daniel J. Ericsson, Stella Cesari, Chunhong Chen, Simon J. Williams, Peter N. Dodds, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Génétique et Amélioration des Fruits et Légumes (GAFL), Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Australian National University (ANU), Max Planck Institute for Plant Breeding Research (MPIPZ), University of Cologne, Cluster of Excellence on Plant Sciences (CEPLAS), Heinrich Heine Universität Düsseldorf = Heinrich Heine University [Düsseldorf]-Max Planck Institute for Plant Breeding Research (MPIPZ)-Universität zu Köln = University of Cologne, Australian Synchrotron [Clayton], Plant Health Institute of Montpellier (UMR PHIM), Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad)-Institut de Recherche pour le Développement (IRD)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut Agro Montpellier, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Université de Montpellier (UM), Australian Research Council Future fellowship (FT200100135), Chinese Scholarship Council (CSC) postgraduate fellowship, Daimler and Benz Foundation, and European Project: 0742263(2008)
Subjects: wheat resistance, Physiology, effector structure, Basidiomycota, resistance breakdown, food and beverages, Plant Science, [SDV.BV.PEP]Life Sciences [q-bio]/Vegetal Biology/Phytopathology and phytopharmacy, Plant Breeding, stem rust, Sr50, Triticum, AvrSr50, Disease Resistance, Plant Diseases, effector evolution
Abstract: International audience; Pathogen effectors are crucial players during plant colonisation and infection. Plant resistance mostly relies on effector recognition to activate defence responses. Understanding how effector proteins escape from plant surveillance is important for plant breeding and resistance deployment. Here we examined the role of genetic diversity of the stem rust (Puccinia graminis f. sp. tritici (Pgt)) AvrSr50 gene in determining recognition by the corresponding wheat Sr50 resistance gene. We solved the crystal structure of a natural variant of AvrSr50 and used site-directed mutagenesis and transient expression assays to dissect the molecular mechanisms explaining gain of virulence. We report that AvrSr50 can escape recognition by Sr50 through different mechanisms including DNA insertion, stop codon loss or by amino-acid variation involving a single substitution of the AvrSr50 surface-exposed residue Q121. We also report structural homology of AvrSr50 to cupin superfamily members and carbohydrate-binding modules indicating a potential role in binding sugar moieties. This study identifies key polymorphic sites present in AvrSr50 alleles from natural stem rust populations that play important roles to escape from Sr50 recognition. This constitutes an important step to better understand Pgt effector evolution and to monitor AvrSr50 variants in natural rust populations.
Published: 2022

36. Millimetre-wave laboratory study of glycinamide and a search for it with ALMA towards Sagittarius B2(N)

Author: Arnaud Belloche, Lech Pszczółkowski, E. Białkowska-Jaworska, Robin T. Garrod, José L. Alonso, Holger S. P. Müller, Jean-Claude Guillemin, Karl M. Menten, Zbigniew Kisiel, Iker León, Elena R. Alonso, L. Kolesniková, Institute of Physics, Polish Academy of Sciences, Polska Akademia Nauk = Polish Academy of Sciences (PAN), Spanish National Research Council (CSIC), Universidad de Valladolid [Valladolid] (UVa), Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Virginia, Universität zu Köln = University of Cologne, Max-Planck-Institut für Radioastronomie (MPIFR), National Science Foundation, NSF: AST 19-06489, G61-6, Providence Health Care, PHC, European Research Council, ERC, Deutsche Forschungsgemeinschaft, DFG: 184018867, Centre National d’Etudes Spatiales, CNES, Centre National de la Recherche Scientifique, CNRS, Ministerio de Ciencia e Innovación, MICINN: CTQ2016-76393-P, PID2019-111396GB-I00, Institut de Cardiologie de Montréal, MHI, and Junta de Castilla y León, JCYL: VA077U16, VA244P20
Subjects: Physics, Line: identification, Galactic Center, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Molecular physics, Spectral line, ISM: molecules, Rotational energy, Astronomical databases: miscellaneous, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Excited state, [CHIM]Chemical Sciences, Sagittarius B2, Rotational spectroscopy, Ground state, Astrophysics::Galaxy Astrophysics, Quantum tunnelling, Astrochemistry, ISM: individual objects: Sagittarius B2
Abstract: Glycinamide is considered to be one of the possible precursors of the simplest amino acid glycine. Its only rotational spectrum reported so far has been in the cm-wave region. The aim of this work is to extend its laboratory spectrum into the mm wave region to support its searches in the ISM. Glycinamide was synthesised chemically and was studied with broadband rotational spectroscopy in the 90-329 GHz region. Tunneling across a low energy barrier between two symmetry equivalent configurations of the molecule resulted in splitting of each vibrational state and many perturbations in associated rotational energy levels, requiring careful coupled state fits for each vibrational doublet. We searched for emission of glycinamide in the imaging spectral line survey ReMoCA performed with ALMA toward Sgr B2(N). We report the first analysis of the mm-wave rotational spectrum of glycinamide, resulting in fitting to experimental measurement accuracy of over 1200 transition frequencies for the ground state tunneling doublet, of many lines for tunneling doublets for two singly excited vibrational states, and determination of precise vibrational separation in each doublet. We did not detect emission from glycinamide in the hot core Sgr B2(N1S). We found that glycinamide is at least seven times less abundant than aminoacetonitrile and 1.8 times less abundant than urea in this source. A comparison with results of astrochemical kinetics models for species related to glycinamide suggests that its abundance may be at least one order of magnitude below the upper limit obtained toward Sgr B2(N1S). This means that glycinamide emission in this source likely lies well below the spectral confusion limit in the frequency range covered by the ReMoCA survey. Targetting sources with a lower level of spectral confusion, such as the Galactic Center shocked region G+0.693-0.027, may be a promising avenue. [abridged], Accepted for publication in A&A
Published: 2022

37. Millimeter wave spectrum and search for vinyl isocyanate toward Sgr B2(N) with ALMA

Author: K. Vávra, L. Kolesniková, A. Belloche, R. T. Garrod, J. Koucký, T. Uhlíková, K. Luková, J.-C. Guillemin, P. Kania, H. S. P. Müller, K. M. Menten, Š. Urban, University of Chemistry and Technology Prague (UCT Prague), Max-Planck-Institut für Radioastronomie (MPIFR), University of Virginia, Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, Czech Science Foundation (GACR) [19-25116Y], Ministry of Education, Youth and Sports of the Czech Republic (MSMT) within the Mobility grant [8J21FR006], Ministry of Education, Youth and Sports of the Czech Republic [LM2018140], ELIXIRCZ project [LM2018131], Astronomy and Astrophysics program of the National Science Foundation [AST 19-06489], Barrande project [46662VH], Centre National d'Etudes Spatiales (CNES), 'Programme National Physique et Chimie du Milieu Interstellaire' (PCMI) of CNRS/INSU, and INC/INP - CEA
Subjects: astrochemistry, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ISM: individual objects: Sgr B2, methods: laboratory: molecular, [CHIM]Chemical Sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ISM: molecules, line: identification
Abstract: The interstellar detections of isocyanic acid, methyl isocyanate, and very recently also ethyl isocyanate, open the question of the possible detection of vinyl isocyanate in the interstellar medium. The aim of this study is to extend the laboratory rotational spectrum of vinyl isocyanate into the millimeter wave region and to undertake a check for its presence in the high-mass star forming region Sgr B2. The rotational spectrum of vinyl isocyanate was recorded in the frequency regions 127.5-218 and 285-330 GHz using the Prague millimeter wave spectrometer. The spectral analysis was supported by high-level quantum-chemical calculations. We assumed local thermodynamic equilibrium to compute synthetic spectra of vinyl isocyanate and to search for it in the ReMoCA survey performed with ALMA toward Sgr B2(N). We also searched for ethyl isocyanate in the same source. Accurate values for the rotational and centrifugal distortion constants are reported for the ground vibrational states of trans and cis vinyl isocyanate. We report nondetections of vinyl and ethyl isocyanate toward the main hot core of Sgr B2(N). We find that vinyl and ethyl isocyanate are at least 11 and 3 times less abundant than methyl isocyanate in this source, respectively. Although the precise formation mechanism of interstellar methyl isocyanate itself remains uncertain, we infer from existing astrochemical models that our observational upper limit for the CH3NCO:C2H5NCO ratio in Sgr B2(N) is consistent with ethyl isocyanate being formed on dust grains via the abstraction or photodissociation of an H atom from methyl isocyanate, followed by the addition of a methyl radical. The dominance of such a process for ethyl isocyanate production, combined with the absence of an analogous mechanism for vinyl isocyanate, would indicate that the ratio C2H3NCO:C2H5NCO should be rather less than unity., Comment: Accepted for publication in A&A
Published: 2022
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38. Morpho-Functional Traits Reveal Differences in Size Fractionated Phytoplankton Communities but Do Not Significantly Affect Zooplankton Grazing

Author: Patrick Fink, Jessica Titocci, Melanie Bon, Helmholtz Zentrum für Umweltforschung = Helmholtz Centre for Environmental Research (UFZ), Universität zu Köln = University of Cologne, Facultad de Ciencias del Mar y Recursos Biológicos, Laboratoire des Sciences de l'Environnement Marin (LEMAR) (LEMAR), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Institut Universitaire Européen de la Mer (IUEM), and Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 0106 biological sciences, Microbiology (medical), QH301-705.5, 010604 marine biology & hydrobiology, [SDV]Life Sciences [q-bio], selectivity, geometrical shapes, 15. Life on land, 010603 evolutionary biology, 01 natural sciences, Microbiology, Article, size fractionation, traits, food web interactions, Virology, phytoplankton, freshwater zooplankton, 14. Life underwater, community structure, Biology (General)
Abstract: The recent emergence of approaches based on functional traits allows a more comprehensive evaluation of the role of functions and interactions within communities. As phytoplankton size and shape are the major determinants of its edibility to herbivores, alteration or loss of some morpho-functional phytoplankton traits should affect zooplankton grazing, fitness and population dynamics. Here, we investigated the response of altered phytoplankton morpho-functional trait distribution to grazing by zooplankton with contrasting food size preferences and feeding behaviors. To test this, we performed feeding trials in laboratory microcosms with size-fractionated freshwater phytoplankton (3 size classes, >30 µm; 5–30 µm and
Published: 2022

39. A Kiloparsec-scale Molecular Wave in the Inner Galaxy: Feather of the Milky Way?

Author: Ralf S. Klessen, Dario Colombo, M. Mattern, Peter Schilke, V. S. Veena, Álvaro Sánchez-Monge, James Urquhart, Mattia C. Sormani, F. Schuller, Timea Csengeri, Universität zu Köln, Centre de résonance magnétique biologique et médicale (CRMBM), Aix Marseille Université (AMU)-Assistance Publique - Hôpitaux de Marseille (APHM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), IFP Energies nouvelles (IFPEN), FEMIS 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), University of Kent [Canterbury], Universität zu Köln = University of Cologne, and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Galaxy structure, Aspect ratio, Milky Way, FOS: Physical sciences, Norma Arm, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, Milky Way Galaxy, 01 natural sciences, Protein filament, Interstellar medium, 0103 physical sciences, QB460, 010303 astronomy & astrophysics, Galaxy kinematics, Astrophysics::Galaxy Astrophysics, Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Galactic Center, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Giant molecular clouds, Submillimeter astronomy
Abstract: We report the discovery of a velocity coherent, kpc-scale molecular structure towards the Galactic center region with an angular extent of 30deg and an aspect ratio of 60:1. The kinematic distance of the CO structure ranges between 4.4 to 6.5 kpc. Analysis of the velocity data and comparison with the existing spiral arm models support that a major portion of this structure is either a sub-branch of the Norma arm or an inter-arm giant molecular filament, likely to be a kpc-scale feather (or spur) of the Milky Way, similar to those observed in nearby spiral galaxies. The filamentary cloud is at least 2.0 kpc in extent, considering the uncertainties in the kinematic distances, and it could be as long as 4 kpc. The vertical distribution of this highly elongated structure reveals a pattern similar to that of a sinusoidal wave. The exact mechanisms responsible for the origin of such a kpc-scale filament and its wavy morphology remains unclear. The distinct wave-like shape and its peculiar orientation makes this cloud, named as the Gangotri wave, one of the largest and most intriguing structures identified in the Milky Way., 10 pages, 7 figures, accepted for publication in ApJ Letters
Published: 2021

40. Chiral order and multiferroic domain relaxation in NaFeGe$_2$O$_6$

Author: Biesenkamp, S., Gorkov, D., Schmidt, W., Schmalzl, K., Sidis, Y., Becker, P., Bohat��, L., Braden, M., Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Heinz Maier-Leibnitz Zentrum (MLZ), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Forschungszentrum Jülich GmbH, Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), LLB - Nouvelles frontières dans les matériaux quantiques (NFMQ), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Institut für Geologie und Mineralogie [Köln]
Subjects: [PHYS]Physics [physics], Condensed Matter - Strongly Correlated Electrons, Strongly Correlated Electrons (cond-mat.str-el), FOS: Physical sciences, [PHYS.COND.CM-SCE]Physics [physics]/Condensed Matter [cond-mat]/Strongly Correlated Electrons [cond-mat.str-el]
Abstract: International audience; The magnetic structure and the multiferroic relaxation dynamics of NaFeGe$_2$O$_6$ were studied by neutron scattering on single crystals partially utilizing polarization analysis. In addition to the previously reported transitions, the incommensurate spiral ordering of Fe$^{3+}$ moments in the $ac$ plane develops an additional component along the crystallographic b direction below T ≈ 5 K, which coincides with a lock-in of the incommensurate modulation. The quasistatic control of the spin-spiral handedness, respectively of the vector chirality, by external electric fields proves the invertibility of multiferroic domains down to the lowest temperature. Time-resolved measurements of the multiferroic domain inversion in NaFeGe$_2$O$_6$ reveal a simple temperature and electric-field dependence of the multiferroic relaxation that is well described by a combined Arrhenius-Merz relation, as it has been observed for TbMnO$_3$. The maximum speed of domain wall motion is comparable to the spin-wave velocity deduced from an analysis of the magnon dispersion.
Published: 2021

41. Mediterranean tephrostratigraphy and peri-Tyrrhenian explosive activity revaluated in light of the 430-365 ka record from Fucino Basin (central Italy)

Author: Monaco L.[1], Palladino D.M.[1], Gaeta M.[1], Marra F.[2], Sottili G.[1], Leicher N.[3], Mannella G.[4], Nomade S.[5], Pereira A.[6], Regattieri E.[7], Wagner B.[3], Zanchetta G.[2, 4, 12], Albert P.G.[8], Arienzo I.[9], D'Antonio M.[10], Petrosino P.[10], Manning C.J.[11], Giaccio B.[2, Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Paléocéanographie (PALEOCEAN), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Roma (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Universität zu Köln = University of Cologne, University of Pisa - Università di Pisa, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Saclay (GEOPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CNR Istituto di Geoscienze e Georisorse [Pisa] (IGG-CNR), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Swansea University, Monaco, L., Palladino, D. M., Gaeta, M., Marra, F., Sottili, G., Leicher, N., Mannella, G., Nomade, S., Pereira, A., Regattieri, E., Wagner, B., Zanchetta, G., Albert, P. G., Arienzo, I., D'Antonio, M., Petrosino, P., Manning, C. J., and Giaccio, B.
Subjects: 010504 meteorology & atmospheric sciences, Geochemistry, Pyroclastic rock, Peri-Tyrrhenian explosive volcanism, Volcanism, 010502 geochemistry & geophysics, 01 natural sciences, Marine Isotope Stage 11, [SDU.STU.VO]Sciences of the Universe [physics]/Earth Sciences/Volcanology, Mediterranean tephrochronology, Tephra, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, geography, Vulcanian eruption, geography.geographical_feature_category, Volcano, 13. Climate action, [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, General Earth and Planetary Sciences, Sedimentary rock, Geology, Volcanic ash
Abstract: International audience; Accurately reconstructing the scale and timing of dynamic processes, such as Middle-Late Pleistocene explosive volcanism and rapid climatic changes, requires rigorous and independent chronological constraints. In this framework, the study of distal volcanic ash layers, or tephra, transported and deposited over wide regions during explosive volcanic eruptions, is increasingly being recognised as a fundamental chronostratigraphic tool for addressing these challenging issues. Here we present a high-resolution distal tephra record preserved in the lacustrine sedimentary succession of the Fucino Basin, central Italy. The investigated record spans the 430-365 ka time interval, covering the entirety of Marine Isotope Stage 11 (MIS 11), and provides important insights into peri-Tyrrhenian potassic explosive volcanism from sources located in central Italy against a backdrop of Mediterranean palaeooclimate records. The succession of ash fall events of this time interval is reconstructed through a detailed lithostratigraphic, geochemical and 40Ar/39Ar geochronological characterization of the deposits preserved as discrete layers in the Fucino F4-F5 sediment core. This work is complemented by similarly detailed characterization of selected proximal pyroclastic units from the peri-Tyrrhenian potassic volcanoes. Geochemical fingerprinting of the tephra deposits by means of their major, minor and trace elements and Sr isotope composition indicates that all the thirty-two investigated ash layers derived from the peri-Tyrrhenian potassic volcanoes. The stratigraphically continuous succession of the Fucino tephra layers allowed the development of a fully independent, 40Ar/39Ar age-constrained, Bayesian age-depth model for the investigated time interval. The age-model allows us to establish modelled ages for the tephra layers within the succession that are not directly dated. The resulting dated tephra record clearly reveals a highly time resolved and previously unparalelled chronicle of explosive activity from the Vulsini, Vico, Sabatini, Colli Albani and Roccamonfina volcanic complexes. Our study provides a benchmark and valuable geochemical and geochronological dataset to be used as a reference for any future development and application of the tephrostratigraphic methods across the central Mediterranean area both during the investigated 430-365 ka time interval, and deeper in time. This contribution underlines the importance of integrating proximal and distal sedimentary records to more accurately establish long-term and comprehensive volcanic eruption records.
Published: 2021

42. TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

Author: S. D. Lord, T. Nikola, Monica Relaño, P. van der Werf, Pierre Gratier, C. Kramer, Frank P. Israel, S. Verley, Bhaswati Mookerjea, Susanne Aalto, M. Boquien, J. Braine, F. F. S. van der Tak, M. Roellig, Santiago García-Burillo, Francoise Combes, Gordon J. Stacey, D. Calzetti, Carsten Henkel, Christof Buchbender, G. Quintana-Lacaci, Fatemeh Tabatabaei, KOSMA, I. Physikalisches Institut, Universität zu Köln, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Department of Astronomy, University of Massachusetts System (UMASS), Dept. fısica Teorica y del Cosmos, Universidad de Granada (UGR), Dpto. Fisica Teorica y del Cosmos, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Institut für Physik (Institut für Physik), Universität Potsdam, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), KOSMA, I. Physikalisches Institut [Köln], Universität zu Köln-Universität zu Köln, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Universität zu Köln = University of Cologne, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidad de Granada = University of Granada (UGR), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Observatorio Astronomico Nacional, Madrid, University of Potsdam = Universität Potsdam, Universiteit Leiden, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Universität zu Köln = University of Cologne-Universität zu Köln = University of Cologne
Subjects: HII regions, Spatial correlation, Photon, 010504 meteorology & atmospheric sciences, M33 HERM33ES, FOS: Physical sciences, Astrophysics, PHOTODISSOCIATION REGIONS, 01 natural sciences, PHOTON-DOMINATED REGIONS, H-II REGIONS, photon-dominated region (PDR), 0103 physical sciences, M EMISSION, NEARBY GALAXIES, PHYSICAL CONDITIONS, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spiral galaxy, INTERSTELLAR-MEDIUM, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, LONG-WAVELENGTH SPECTROMETER, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, galaxies: individual: M 33, Galaxy, Interstellar medium, 13. Climate action, Space and Planetary Science, galaxies: star formation, Astrophysics of Galaxies (astro-ph.GA), Local Group, FAR-INFRARED SPECTROSCOPY, galaxies: ISM, Galaxy Astrophysics
Abstract: Context: The emission line of [CII] at 158 micron is one of the strongest cooling lines of the interstellar medium (ISM) in galaxies. Aims: Disentangling the relative contributions of the different ISM phases to [CII] emission, is a major topic of the HerM33es program, a Herschel key project to study the ISM in the nearby spiral galaxy M33. Methods: Using PACS, we have mapped the emission of [CII] 158 micron, [OI] 63 micron, and other FIR lines in a 2'x2' region of the northern spiral arm of M33, centered on the HII region BCLMP302. At the peak of H-alpha emission, we have observed in addition a velocity resolved [CII] spectrum using HIFI. We use scatterplots to compare these data with PACS 160 micron continuum maps, and with maps of CO and HI data, at a common resolution of 12 arcsec or 50 pc. Maps of H-alpha and 24 micron emission observed with Spitzer are used to estimate the SFR. We have created maps of the [CII] and [OI] 63 micron emission and detected [NII] 122 micron and NIII 57 micron at individual positions. Results: The [CII] line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between [CII] observed with PACS and CO over the mapped region. There is even less spatial correlation between [CII] and the atomic gas traced by HI. Detailed comparison of the observed intensities towards the HII region with models of photo ionization and photon dominated regions, confirms that a significant fraction, 20--30%, of the observed [CII] emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio between [CII] and the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the HII region., Comment: Accepted for publication in A&A. 12 pages, 12 figures
Published: 2011

43. On the Realism of the Rain Microphysics Representation of a Squall Line in the WRF Model. Part I: Evaluation with Multifrequency Cloud Radar Doppler Spectra Observations

Author: Kamil Mroz, Frédéric Tridon, Wolfram Wobrock, Alessandro Battaglia, Sandra Banson, Joël Van Baelen, Céline Planche, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Laboratoire de météorologie physique (LaMP), Centre National de la Recherche Scientifique (CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS), Earth Observation Science, Department of Physics and Astronomy, National Center for Earth Observation, University of Leicester, Leicester, UK, Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire de Météorologie Physique (LaMP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and University of Leicester
Subjects: [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Atmospheric Science, Cloud radar, 010504 meteorology & atmospheric sciences, Microphysics, Meteorology, 0208 environmental biotechnology, Representation (systemics), 02 engineering and technology, 01 natural sciences, Spectral line, 020801 environmental engineering, symbols.namesake, 13. Climate action, Weather Research and Forecasting Model, symbols, Doppler effect, Squall line, ComputingMilieux_MISCELLANEOUS, Geology, 0105 earth and related environmental sciences
Abstract: This study investigates how multifrequency cloud radar observations can be used to evaluate the representation of rain microphysics in the WRF Model using two bulk microphysics schemes. A squall line observed over Oklahoma on 12 June 2011 is used as a case study. A recently developed retrieval technique combining observations of two vertically pointing cloud radars provides quantitative description of the drop size distribution (DSD) properties of the transition and stratiform regions of the squall-line system. For the first time, the results of this multifrequency cloud radar retrieval are compared to more conventional retrievals from a nearby polarimetric radar, and a supplementary result of this work is that this new methodology provides a much more detailed description of the DSD vertical and temporal variations. While the extent and evolution of the squall line is well reproduced by the model, the 1-h low-reflectivity transition region is not. In the stratiform region, simulations with both schemes are able to reproduce the observed downdraft and the associated significative subsaturation below the melting level, but with a slight overestimation of the relative humidity. Under this subsaturated air, the simulated rain mixing ratio continuously decreases toward the ground, in agreement with the observations. Conversely, the profiles of the mean volume diameter and the concentration parameter of the DSDs are not well reproduced. These discrepancies pinpoint at an issue in the representation of rain microphysics. The companion paper, investigates the sources of the biases in the microphysics processes in the rain layer by performing numerical sensitivity studies.
Published: 2019

44. On the Realism of the Rain Microphysics Representation of a Squall Line in the WRF Model. Part II: Sensitivity Studies on the Rain Drop Size Distributions

Author: Sandra Banson, Marie Monier, Alessandro Battaglia, Frédéric Tridon, Wolfram Wobrock, Céline Planche, Gregory Thompson, Laboratoire de météorologie physique (LaMP), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut für Geophysik und Meteorologie [Köln], Universität zu Köln = University of Cologne, Laboratoire de Météorologie Physique (LaMP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), National Center for Atmospheric Research [Boulder] (NCAR), University of Leicester, Centre National de la Recherche Scientifique (CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS), Universität zu Köln, and Earth Observation Science, Department of Physics and Astronomy, National Center for Earth Observation, University of Leicester, Leicester, UK
Subjects: Atmospheric Science, Cloud radar, 010504 meteorology & atmospheric sciences, Meteorology, 0207 environmental engineering, Squall lines, Precipitation, 02 engineering and technology, 01 natural sciences, Cloud resolving models, Cloud microphysics, Sensitivity (control systems), Radars, 020701 environmental engineering, Representation (mathematics), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Drop size distribution, Radar observations, Microphysics, 13. Climate action, Weather Research and Forecasting Model, Environmental science, Rain drop, Squall line
Abstract: A comparison between retrieved properties of the rain drop size distributions (DSDs) from multifrequency cloud radar observations and WRF Model results using either the Morrison or the Thompson bulk microphysics scheme is performed in order to evaluate the model’s ability to predict the rain microphysics. This comparison reveals discrepancies in the vertical profile of the rain DSDs for the stratiform region of the squall-line system observed on 12 June 2011 over Oklahoma. Based on numerical sensitivity analyses, this study addresses the bias at the top of the rain layer and the vertical evolution of the DSD properties (i.e., of Dm and N0*). In this way, the Thompson scheme is used to explore the sensitivity to the melting process. Moreover, using the Thompson and Morrison schemes, the sensitivity of the DSD vertical evolution to different breakup and self-collection parameterizations is studied. Results show that the DSDs are strongly dependent on the representation of the melting process in the Thompson scheme. In the Morrison scheme, the simulations with more efficient breakup reproduce the DSD properties with better fidelity. This study highlights how the inaccuracies in simulated Dm and N0* for both microphysics schemes can impact the evaporation rate, which is systematically underestimated in the model.
Published: 2019

45. Accessing tens-to-hundreds femtoseconds nuclear state lifetimes with low-energy binary heavy-ion reactions

Author: M. Zieblinski, J. Grebosz, K. Mazurek, Simone Coelli, S. Brambilla, H. J. Li, B. Million, M. Rejmund, Bertrand Jacquot, P. Bednarczyk, N. Cieplicka-Oryńczak, M. Ciemala, M. Bast, S. Ziliani, O. Dorvaux, S. Erturk, Eric Clément, Ł. W. Iskra, C. Fransen, S. M. Lenzi, B. Fornal, P. J. Napiorkowski, C. Müller-Gatermann, M. Zielińska, B. Wasilewska, I. Matea, A. Maj, M. Kmiecik, Y. H. Kim, M. Kicińska-Habior, C. Michelagnoli, I. Stefan, M. Beckers, F. C. L. Crespi, O. Wieland, M. Lewitowicz, R. Palit, D. R. Napoli, Ch. Schmitt, A. V. Karpov, M. Stanoiu, F. Camera, Emanuele Vardaci, M. Matejska-Minda, A. Bracco, G. Benzoni, S. Bottoni, S. Leoni, V. Nanal, C. Boiano, A. Lemasson, Mohsen Harakeh, Thomas Braunroth, A. Goldkuhle, Grand Accélérateur National d'Ions Lourds (GANIL), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Laue-Langevin (ILL), ILL, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Ciemala, M., Ziliani, S., Crespi, F. C. L., Leoni, S., Fornal, B., Maj, A., Bednarczyk, P., Benzoni, G., Bracco, A., Boiano, C., Bottoni, S., Brambilla, S., Bast, M., Beckers, M., Braunroth, T., Camera, F., Cieplicka-Orynczak, N., Clement, E., Coelli, S., Dorvaux, O., Erturk, S., De France, G., Fransen, C., Goldkuhle, A., Grebosz, J., Harakeh, M. N., Iskra, L. W., Jacquot, B., Karpov, A., Kicinska-Habior, M., Kim, Y. -H., Kmiecik, M., Lemasson, A., Lenzi, S. M., Lewitowicz, M., Li, H., Matea, I., Mazurek, K., Michelagnoli, C., Matejska-Minda, M., Million, B., Muller-Gatermann, C., Nanal, V., Napiorkowski, P., Napoli, D. R., Palit, R., Rejmund, M., Schmitt, C., Stanoiu, M., Stefan, I., Vardaci, E., Wasilewska, B., Wieland, O., Zieblinski, M., Zielinska, M., H. Niewodniczanski Institute of Nuclear Physics, Polska Akademia Nauk = Polish Academy of Sciences (PAN), Dipartimento di Fisica (Milano), Università degli Studi di Milano [Milano] (UNIMI), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Institut für Kernphysik der Universität zu Köln, Universität zu Köln, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano = University of Milan (UNIMI), Universität zu Köln = University of Cologne, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Nuclear Energy
Subjects: Nuclear reaction, Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Monte Carlo method, Hadron, FOS: Physical sciences, Binary number, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Excited state, 0103 physical sciences, Nuclear fusion, AGATA, Nuclear Experiment (nucl-ex), Connection (algebraic framework), Atomic physics, Nuclear Experiment, 010306 general physics
Abstract: A novel Monte Carlo technique has been developed to determine lifetimes of excited states in the tens-to-hundreds femtoseconds range in products of low-energy heavy-ion binary reactions, with complex velocity distributions. The method is based on a detailed study of Doppler-broadened $$\gamma $$ γ -ray lineshapes. Its relevance is demonstrated in connection with the $$^{18}\text {O}(7.0\, \text {MeV/u})+\,^{181}\text {Ta}$$ 18 O ( 7.0 MeV/u ) + 181 Ta experiment, performed at GANIL with the AGATA+VAMOS+PARIS setup, to study neutron-rich O, C, N, ... nuclei. Excited states in $$^{17}\text {O}$$ 17 O and $$^{19}\text {O}$$ 19 O , with known lifetimes, are used to validate the method over the $$\sim 20{-}400\,\text {fs}$$ ∼ 20 - 400 fs lifetime-sensitivity range. Emphasis is given to the unprecedented position resolution provided by $$\gamma $$ γ -tracking arrays, which turns out to be essential for reaching the required accuracy in Doppler-shift correction. The technique is anticipated to be an important tool for lifetime investigations in exotic neutron-rich nuclei, produced with intense ISOL-type beams.
Published: 2021

46. Description of turbulent dynamics in the interstellar medium: Multifractal-microcanonical analysis: I. Application to Herschel observations of the Musca filament

Author: Yahia, Hussein, Schneider, Nicola, Bontemps, Sylvain, Bonne, Lars, Attuel, Guillaume, Dib, Sami, Ossenkopf, Volker, Turiel, Antonio, Zebadua, Augusto, Elia, Davide, Maji, Suman Kumar, Schmitt, François G, Robitaille, Jean-François, Geometry and Statistics in acquisition data (GeoStat), Inria Bordeaux - Sud-Ouest, Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria), I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, FEMIS 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Physikalisches Institut [Köln], Institute of Marine Sciences / Institut de Ciències del Mar [Barcelona] (ICM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto Nazionale di Astrofisica (INAF), Indian Institute of Technology Patna (IITP), Laboratoire d’Océanologie et de Géosciences (LOG) - UMR 8187 (LOG), Institut national des sciences de l'Univers (INSU - CNRS)-Université du Littoral Côte d'Opale (ULCO)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Nord]), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, This work is supported by the GENESIS project (GENeration and Evolution of Structure in the ISm), via the french ANR and the german DFG through grant numbers ANR-16-CE92-0035-01 and DFG1591/2-1. N. Schneider acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG project number SFB 956. L. Bonne acknowledges support by the Région Nouvelle-Aquitaine, France., ANR-16-CE92-0035,GENESIS,GENeration et Evolution des Structures du milieu InterStellaire(2016), Universität zu Köln, Centre National de la Recherche Scientifique (CNRS)-Université du Littoral Côte d'Opale (ULCO)-Université de Lille-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Université du Littoral Côte d'Opale (ULCO), Université de Lille, Université Grenoble-Alpes, IPAG, PCMI, and PNPS
Subjects: Turbulence, ISM: individual objects: Musca, Magnetohydrodynamics, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [INFO.INFO-TS]Computer Science [cs]/Signal and Image Processing, ISM: structure, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, ISM: clouds
Abstract: International audience; Observations of the interstellar medium (ISM) show a complex density and velocity structure, which is in part attributed to turbulence. Consequently, the multifractal formalism should be applied to observation maps of the ISM in order to characterize its turbulent and multiplicative cascade properties. However, the multifractal formalism, even in its more advanced and recent canonical versions, requires a large number of realizations of the system, which usually cannot be obtained in astronomy. We present a self-contained introduction to the multifractal formalism in a "microcanonical" version, which allows us, for the first time, to compute precise turbulence characteristic parameters from a single observational map without the need for averages in a grand ensemble of statistical observables (e.g., a temporal sequence of images). We compute the singularity exponents and the singularity spectrum for both observations and magnetohydrodynamic simulations, which include key parameters to describe turbulence in the ISM. For the observations we focus on the 250 µm Herschel map of the Musca filament. Scaling properties are investigated using spatial 2D structure functions, and we apply a two-point log-correlation magnitude analysis over various lines of the spatial observation, which is known to be directly related to the existence of a multiplicative cascade under precise conditions. It reveals a clear signature of a multiplicative cascade in Musca with an inertial range from 0.05 to 0.65 pc. We show that the proposed microcanonical approach provides singularity spectra that are truly scale invariant, as required to validate any method used to analyze multifractality. The obtained singularity spectrum of Musca, which is sufficiently precise for the first time, is clearly not as symmetric as usually observed in log-normal behavior. We claim that the singularity spectrum of the ISM toward Musca features a more log-Poisson shape. Since log-Poisson behavior is claimed to exist when dissipation is stronger for rare events in turbulent flows, in contrast to more homogeneous (in volume and time) dissipation events, we suggest that this deviation from log-normality could trace enhanced dissipation in rare events at small scales, which may explain, or is at least consistent with, the dominant filamentary structure in Musca. Moreover, we find that subregions in Musca tend to show different multifractal properties: While a few regions can be described by a log-normal model, other regions have singularity spectra better fitted by a log-Poisson model. This strongly suggests that different types of dynamics exist inside the Musca cloud. We note that this deviation from log-normality and these differences between subregions appear only after reducing noise features, using a sparse edge-aware algorithm, which have the tendency to "log-normalize" an observational map. Implications for the star formation process are discussed. Our study establishes fundamental tools that will be applied to other galactic clouds and simulations in forthcoming studies.
Published: 2021

47. Triple oxygen isotope systematics of evaporation and mixing processes in a dynamic desert lake system

Author: C. Voigt, D. Herwartz, C. Dorador, M. Staubwasser, Universität zu Köln, Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Universidad de Antofagasta, and Universität zu Köln = University of Cologne
Subjects: 010504 meteorology & atmospheric sciences, δ18O, Evaporation, 010502 geochemistry & geophysics, Atmospheric sciences, lcsh:Technology, 01 natural sciences, lcsh:TD1-1066, Isotopes of oxygen, Hydrology (agriculture), [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, lcsh:Environmental technology. Sanitary engineering, [SDU.STU.HY]Sciences of the Universe [physics]/Earth Sciences/Hydrology, lcsh:Environmental sciences, Pan evaporation, 0105 earth and related environmental sciences, General Environmental Science, lcsh:GE1-350, lcsh:T, lcsh:Geography. Anthropology. Recreation, Groundwater recharge, 6. Clean water, lcsh:G, 13. Climate action, Isotope hydrology, General Earth and Planetary Sciences, Environmental science, Groundwater
Abstract: This study investigates the combined hydrogen deuterium and triple oxygen isotope hydrology of the Salar del Huasco, an endorheic salt flat with shallow lakes at its centre that is located on the Altiplano Plateau, N Chile. This lacustrine system is hydrologically dynamic and complex because it receives inflow from multiple surface and groundwater sources. It undergoes seasonal flooding, followed by rapid shrinking of the water body at the prevailing arid climate with very high evaporation rates. At any given point in time, ponds, lakes, and recharge sources capture a large range of evaporation degrees. Samples taken between 2017 and 2019 show a range of δ18O between −13.3 ‰ and 14.5 ‰, d-excess between 7 ‰ and −100 ‰, and 17O-excess between 19 and −108 per meg. A pan evaporation experiment conducted on-site was used to derive the turbulence coefficient of the Craig–Gordon isotope evaporation model for the local wind regime. This, along with sampling of atmospheric vapour at the salar (-21.0±3.3 ‰ for δ18O, 34±6 ‰ for d-excess and 23±9 per meg for 17O-excess), enabled the accurate reproduction of measured ponds and lake isotope data by the Craig–Gordon model. In contrast to classic δ2H–δ18O studies, the 17O-excess data not only allow one to distinguish two different types of evaporation – evaporation with and without recharge – but also to identify mixing processes between evaporated lake water and fresh flood water. Multiple generations of infiltration events can also be inferred from the triple oxygen isotope composition of inflow water, indicating mixing of sources with different evaporation histories. These processes cannot be resolved using classic δ2H–δ18O data alone. Adding triple oxygen isotope measurements to isotope hydrology studies may therefore significantly improve the accuracy of a lake's hydrological balance – i.e. the evaporation-to-inflow ratio (E / I) – estimated by water isotope data and application of the Craig–Gordon isotope evaporation model.
Published: 2021

48. Angular momentum generation in nuclear fission

Author: B. Fornal, M. S. Yavahchova, C. Delafosse, A. Boso, V. Sánchez-Tembleque, K. Rezynkina, M. Lebois, K. Hauschild, T. Kröll, Muriel Fallot, P. Adsley, J. Ljungvall, Ł. W. Iskra, F. Ibrahim, E. Adamska, C. Henrich, A. Gottardo, Stephan Oberstedt, R. Chakma, C. Sürder, V. Guadilla, C. Porzio, P. H. Regan, J. Benito, A. Korgul, R. Lozeva, L. Le Meur, M. Piersa, P. Ivanov, V. Vedia, J. Nemer, B. Wasilewska, N. Jovančević, Y. Popovitch, W. Paulsen, C. Schmitt, N. Cieplicka-Oryńczak, R. B. Gerst, Sunniva Siem, G. Tocabens, P. A. Söderström, K. Belvedere, S. Courtin, S. Ziliani, R. Canavan, D. Gjestvang, L. Qi, D. Etasse, P. Koseoglou, G. Häfner, I. Matea, I. Homm, M. Heine, L. M. Fraile, T. Kurtukian-Nieto, Fabio Zeiser, P. Davies, D. Thisse, M. L. Cortés, A. Blazhev, S. Jazrawi, M. Bunce, A. Lopez-Martens, K. Miernik, Alejandro Algora, M. Rudigier, J. N. Wilson, N. Warr, J. Wiederhold, D. Verney, D. Ralet, M. Babo, L. Gaudefroy, G. Benzoni, S. Bottoni, S. Leoni, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), University of Oslo (UiO), Department of Physics, University of Surrey, University of Surrey (UNIS), Technische Universität Darmstadt - Technical University of Darmstadt (TU Darmstadt), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CEA, Bruyeres le Chatel, France, affiliation inconnue, University of Warsaw (UW), Facultat de Fisica [València] (UV), Universitat de València (UV), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Università degli Studi di Milano = University of Milan (UNIMI), Institut für Kernphysik der Universität zu Köln, Universität zu Köln = University of Cologne, National Physical Laboratory [Teddington] (NPL), Instytut Fizyki Jądrowej PAN (IFJ), Polskiej Akademii Nauk, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), RIKEN - Institute of Physical and Chemical Research [Japon] (RIKEN), University of Manchester [Manchester], Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), European Commission - Joint Research Centre [Geel] (JRC), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Horia Hulubei Natl Inst Phys & Nucl Engn IFIN HH, ELI NP Dept, Reactorului Str 30, Magurele 077125, Romania, Софийски университет = Sofia University, Technische Universität Darmstadt (TU Darmstadt), Universidad Complutense de Madrid [Madrid] (UCM), Università degli studi di Milano [Milano], Universität zu Köln, Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Technical University Darmstadt (TU), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), University of Sofia, Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Università degli Studi di Milano [Milano] (UNIMI), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Direction des Applications Militaires (DAM), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)
Subjects: Physics, [PHYS]Physics [physics], Angular momentum, Multidisciplinary, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Spins, 010308 nuclear & particles physics, Fission, Nuclear Theory, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 7. Clean energy, 01 natural sciences, Nuclear physics, Nuclear fission, 0103 physical sciences, Atomic nucleus, Nuclear Experiment, 010306 general physics, Nucleon, Excitation, ComputingMilieux_MISCELLANEOUS, Spin-½
Abstract: When a heavy atomic nucleus splits (fission), the resulting fragments are observed to emerge spinning1; this phenomenon has been a mystery in nuclear physics for over 40 years2,3. The internal generation of typically six or seven units of angular momentum in each fragment is particularly puzzling for systems that start with zero, or almost zero, spin. There are currently no experimental observations that enable decisive discrimination between the many competing theories for the mechanism that generates the angular momentum4–12. Nevertheless, the consensus is that excitation of collective vibrational modes generates the intrinsic spin before the nucleus splits (pre-scission). Here we show that there is no significant correlation between the spins of the fragment partners, which leads us to conclude that angular momentum in fission is actually generated after the nucleus splits (post-scission). We present comprehensive data showing that the average spin is strongly mass-dependent, varying in saw-tooth distributions. We observe no notable dependence of fragment spin on the mass or charge of the partner nucleus, confirming the uncorrelated post-scission nature of the spin mechanism. To explain these observations, we propose that the collective motion of nucleons in the ruptured neck of the fissioning system generates two independent torques, analogous to the snapping of an elastic band. A parameterization based on occupation of angular momentum states according to statistical theory describes the full range of experimental data well. This insight into the role of spin in nuclear fission is not only important for the fundamental understanding and theoretical description of fission, but also has consequences for the γ-ray heating problem in nuclear reactors13,14, for the study of the structure of neutron-rich isotopes15,16, and for the synthesis and stability of super-heavy elements17,18. γ-ray spectroscopy experiments on the origin of spin in the products of nuclear fission of spin-zero nuclei suggest that the fission fragments acquire their spin after scission, rather than before.
Published: 2021

49. An Approximation Algorithm for Fully Planar Edge-Disjoint Paths

Author: Claire Mathieu, Chien-Chung Huang, Mathieu Mari, Jens Vygen, Kevin Schewior, Département d'informatique - ENS Paris (DI-ENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut National de Recherche en Informatique et en Automatique (Inria)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche en Informatique Fondamentale (IRIF (UMR_8243)), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universität zu Köln, University of Bonn, Département d'informatique de l'École normale supérieure (DI-ENS), École normale supérieure - Paris (ENS-PSL), Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universität zu Köln = University of Cologne, Universität Bonn = University of Bonn, ANR-18-CE40-0025,ASSK,Algorithmes avec décomposition moins connu: graphes et matroids(2018), and ANR-19-CE48-0016,AlgoriDAM,Théorie algorithmique de nouveaux modèles de données(2019)
Subjects: FOS: Computer and information sciences, Discrete Mathematics (cs.DM), General Mathematics, [INFO.INFO-DS]Computer Science [cs]/Data Structures and Algorithms [cs.DS], 0102 computer and information sciences, Disjoint sets, Edge (geometry), [INFO.INFO-CG]Computer Science [cs]/Computational Geometry [cs.CG], 01 natural sciences, Combinatorics, symbols.namesake, Planar, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, Computer Science - Data Structures and Algorithms, FOS: Mathematics, Mathematics - Combinatorics, [INFO]Computer Science [cs], Data Structures and Algorithms (cs.DS), ComputingMilieux_MISCELLANEOUS, Mathematics, Discrete mathematics, Approximation algorithm, Maximization, Planar graph, 010201 computation theory & mathematics, symbols, Graph (abstract data type), Combinatorics (math.CO), Computer Science - Discrete Mathematics, MathematicsofComputing_DISCRETEMATHEMATICS
Abstract: International audience; We devise a constant-factor approximation algorithm for the maximization version of the edge-disjoint paths problem if the supply graph together with the demand edges form a planar graph. By planar duality this is equivalent to packing cuts in a planar graph such that each cut contains exactly one demand edge. We also show that the natural linear programming relaxations have constant integrality gap, yielding an approximate max-multiflow min-multicut theorem.
Published: 2021

50. Self-absorption in [CII], $^{12}$CO, and HI in RCW120. Building up a geometrical and physical model of the region

Author: S. Kabanovic, N. Schneider, V. Ossenkopf-Okada, F. Falasca, R. Güsten, J. Stutzki, R. Simon, C. Buchbender, L. Anderson, L. Bonne, C. Guevara, R. Higgins, B. Koribalski, M. Luisi, M. Mertens, Y. Okada, M. Röllig, D. Seifried, M. Tiwari, F. Wyrowski, A. Zavagno, A. G. G. M. Tielens, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), ANR-16-CE92-0035,GENESIS,GENeration et Evolution des Structures du milieu InterStellaire(2016), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Universität zu Köln = University of Cologne, Division for Submm Technologies, Max-Planck-Institut für Radioastronomie (MPIFR), Physikalisches Institut [Köln], Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Michigan [Ann Arbor], University of Michigan System, Australia Telescope National Facility, Australian National University (ANU), West Virginia University [Morgantown], and Max Planck Institute for Radio Astronomy
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: clouds, methods: data analysis, Astrophysics - Astrophysics of Galaxies, methods data analysis, ISM: molecules, ISM clouds, ISM molecules, Space and Planetary Science, [SDU]Sciences of the Universe [physics], ISM bubbles, photon-dominated region (PDR), Astrophysics of Galaxies (astro-ph.GA), H II regions, ISM: bubbles, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Aims: Revealing the 3D dynamics of H II region bubbles and their associated molecular clouds and H I envelopes is important for developing an understanding of the longstanding problem as to how stellar feedback affects the density structure and kinematics of the different phases of the interstellar medium. Methods: We employed observations of the H II region RCW 120 in the [C II] 158 μm line, observed within the Stratospheric Observatory for Infrared Astronomy (SOFIA) legacy program FEEDBACK, and in the 12CO and 13CO (3 →2) lines, obtained with the Atacama Pathfinder Experiment (APEX) to derive the physical properties of the gas in the photodissociation region (PDR) and in the molecular cloud. We used high angular resolution H I data from the Southern Galactic Plane Survey to quantify the physical properties of the cold atomic gas through H I self-absorption. The high spectral resolution of the heterodyne observations turns out to be essential in order to analyze the physical conditions, geometry, and overall structure of the sources. Two types of radiative transfer models were used to fit the observed [C II] and CO spectra. A line profile analysis with the 1D non-LTE radiative transfer code SimLine proves that the CO emission cannot stem from a spherically symmetric molecular cloud configuration. With a two-layer multicomponent model, we then quantified the amount of warm background and cold foreground gas. To fully exploit the spectral-spatial information in the CO spectra, a Gaussian mixture model was introduced that allows for grouping spectra into clusters with similar properties. Results: The CO emission arises mostly from a limb-brightened, warm molecular ring, or more specifically a torus when extrapolated in 3D. There is a deficit of CO emission along the line-of-sight toward the center of the H II region which indicates that the H II region is associated with a flattened molecular cloud. Self-absorption in the CO line may hide signatures of infalling and expanding molecular gas. The [C II] emission arises from an expanding [C II] bubble and from the PDRs in the ring/torus. A significant part of [C II] emission is absorbed in a cool (~60-100 K), low-density (−3) atomic foreground layer with a thickness of a few parsec. Conclusions: We propose that the RCW 120 H II region formed in a flattened, filamentary, or sheet-like, molecular cloud and is now bursting out of its parental cloud. The compressed surrounding molecular layer formed a torus around the spherically expanding H II bubble. This scenario can possibly be generalized for other H II bubbles and would explain the observed "flat" structure of molecular clouds associated with H II bubbles. We suggest that the [C II] absorption observed in many star-forming regions is at least partly caused by low-density, cool, H I -envelopes surrounding the molecular clouds. The 12CO and 13CO (3 →2) data shown in Fig. 4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/659/A36 The [C II] data are provided at the NASA/IPAC Infrared science archive at https://irsa.ipac.caltech.edu/Missions/sofia.html
Published: 2021
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