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79 results on '"Instituto Geografico Nacional"'

1. Mapa de Marruecos

Author: Rey Pastor, Alfonso, Instituto Geografico Nacional (España), Rey Pastor, Alfonso, and Instituto Geografico Nacional (España)
Abstract: Inserta: 4 mapas en la parte inferior derecha del mapa a escala reducida que representan la pluviometría, hipsometría, población y producciones, Relieve representado por curvas de nivel y sombreado, Claves de signos convencionales representando poblaciones, zocos, hidrografía, divisiones administrativas, vias de comunicación y abreviaturas, Las longitudes están referidas al meridiano de Madrid 3º 41'16"35= 4 g. 097531-0 Greenwich. 6º 1'31"50= 6 g. 694753-0 París, La fecha de realización del mapa es de 1921
Published: 1922

2. Plano de la zona de la Marañosa y Fábrica Nacional de Productos Químicos del Jarama

Author: Instituto Geografico Nacional (España), España. Estado Mayor Central, Brigada Topográfica de Ingenieros, Instituto Geografico Nacional (España), España. Estado Mayor Central, and Brigada Topográfica de Ingenieros
Abstract: Manuscrito en varias tintas, Orientado con flecha, Relieve representado por curvas de nivel equidistantes 10 metros
Published: 1920

3. Fault kinematics in northern Central America and coupling along the subduction interface of the Cocos Plate, from GPS data in Chiapas (Mexico), Guatemala and El Salvador

Author: Laboratoire de géologie de l'ENS (LGE) ; CNRS - INSU - École normale supérieure [ENS] - Paris, Institut des sciences de la Terre (ISTerre) ; INSU - OSUG - Université de Savoie - Université Joseph Fourier - Grenoble I - IFSTTAR - Institut de recherche pour le développement [IRD] : UR219 - CNRS, Instituto de Geofísica ; UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICO, Instituto Nacional de Sismologıa, Vulcanologıa, Meterologıa e Hidrologia ; INSIVUMEH, Centro de Geosciencias ; Universidad Nacional AutÃ³noma de MÃ©xico (UNAM), 6Coordinadora Nacional para la Reduccion de Desastres ; CONRED, Instituto Geografico Nacional ; IGN, Instituto Geografico y Catastro Nacional ; Centro Nacional de Registros, Laboratoire de tectonique (LT) ; CNRS - INSU - Université de Cergy Pontoise - Université Pierre et Marie Curie (UPMC) - Paris VI, Centro Universitario del Norte ; Universidad de San Carlos de Guatemala, Centro de Estudios Superiores de Energia y Minas ; Universidad de San Carlos de Guatemala, Geologia Ambiental e Economia ; Geologia Ambiental e Economia, Instituto de Geofísica (IG) ; UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICO, Franco, Aurore, Lasserre, Cécile, Lyon-Caen, H., Kostoglodov, Vladimir, Molina, E., Guzman-Speziale, M., Monterosso, D., Robles, V., Figueroa, C., Amaya, W., Barrier, E., Chiquin, L., Moran, S., Flores, O., Romero, J., Santiago, J.A., Manea, M., Manea, V.C., Laboratoire de géologie de l'ENS (LGE) ; CNRS - INSU - École normale supérieure [ENS] - Paris, Institut des sciences de la Terre (ISTerre) ; INSU - OSUG - Université de Savoie - Université Joseph Fourier - Grenoble I - IFSTTAR - Institut de recherche pour le développement [IRD] : UR219 - CNRS, Instituto de Geofísica ; UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICO, Instituto Nacional de Sismologıa, Vulcanologıa, Meterologıa e Hidrologia ; INSIVUMEH, Centro de Geosciencias ; Universidad Nacional AutÃ³noma de MÃ©xico (UNAM), 6Coordinadora Nacional para la Reduccion de Desastres ; CONRED, Instituto Geografico Nacional ; IGN, Instituto Geografico y Catastro Nacional ; Centro Nacional de Registros, Laboratoire de tectonique (LT) ; CNRS - INSU - Université de Cergy Pontoise - Université Pierre et Marie Curie (UPMC) - Paris VI, Centro Universitario del Norte ; Universidad de San Carlos de Guatemala, Centro de Estudios Superiores de Energia y Minas ; Universidad de San Carlos de Guatemala, Geologia Ambiental e Economia ; Geologia Ambiental e Economia, Instituto de Geofísica (IG) ; UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICO, Franco, Aurore, Lasserre, Cécile, Lyon-Caen, H., Kostoglodov, Vladimir, Molina, E., Guzman-Speziale, M., Monterosso, D., Robles, V., Figueroa, C., Amaya, W., Barrier, E., Chiquin, L., Moran, S., Flores, O., Romero, J., Santiago, J.A., Manea, M., and Manea, V.C.
Abstract: International audience, New GPS measurements in Chiapas (Mexico), Guatemala and El Salvador are used to constrain the fault kinematics in the North America (NA), Caribbean (CA) and Cocos (CO) plates triple junction area. The regional GPS velocity field is first analysed in terms of strain partitioning across the major volcano-tectonic structures, using elastic half-space modelling, then inverted through a block model. We show the dominant role of the Motagua Fault with respect to the Polochic Fault in the accommodation of the present-day deformation associated with the NA and CA relative motion. The NA/CA motion decreases from 18-22 mm yr−1 in eastern Guatemala to 14-20 mm yr−1 in central Guatemala (assuming a uniform locking depth of 14-28 km), down to a few millimetres per year in western Guatemala. As a consequence, the western tip of the CA Plate deforms internally, with ≃9 mm yr−1 of east-west extension (≃5 mm yr−1 across the Guatemala city graben alone). Up to 15 mm yr−1 of dextral motion can be accommodated across the volcanic arc in El Salvador and southeastern Guatemala. The arc seems to mark the northern boundary of an independent forearc sliver (AR), pinned to the NA plate. The inversion of the velocity field shows that a four-block (NA, CA, CO and AR) model, that combines relative block rotations with elastic deformation at the block boundaries, can account for most of the GPS observations and constrain the overall kinematics of the active structures. This regional modelling also evidences lateral variations of coupling at the CO subduction interface, with a fairly high-coupling (≃0.6) offshore Chiapas and low-coupling (≃0.25) offshore Guatemala and El Salvador.

4. Linking the dust and chemical evolution: Taurus and Perseus: New collisional rates for HCN, HNC, and their C, N, and H isotopologues

Author: Navarro-Almaida, D., Bop, Cheikh T, Lique, François, Esplugues, G., Rodríguez-Baras, M., Kramer, Carsten, Romero, Charles, Fuente, A., Caselli, P., Rivière-Marichalar, P., Kirk, J., Chacón-Tanarro, A., Roueff, E., Mroczkowski, Tony, Bhandarkar, Tanay, Devlin, Mark, Dicker, Simon, Lowe, Ian, Mason, Brian, Sarazin, Craig, Sievers, Jonathan, Observatorio Astronomico Nacional, Madrid, Instituto Geografico Nacional (IGN), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), École Nationale des Travaux Publics de l'État (ENTPE), Max-Planck-Institut für Extraterrestrische Physik (MPE), School of Physics and Astronomy [Cardiff], Cardiff University, LERMA Cergy (LERMA), 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)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), European Southern Observatory (ESO), University of Pennsylvania, University of Virginia, and McGill University = Université McGill [Montréal, Canada]
Subjects: [PHYS]Physics [physics], stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM: kinematic and dynamics, Molecular physics, ISM: abundances, ISM: molecules
Abstract: International audience; Context. HCN, HNC, and their isotopologues are ubiquitous molecules that can serve as chemical thermometers and evolutionary tracers to characterize star-forming regions. Despite their importance in carrying information that is vital to studies of the chemistry and evolution of star-forming regions, the collision rates of some of these molecules have not been available for rigorous studies in the past.Aims. Our goal is to perform an up-to-date gas and dust chemical characterization of two different star-forming regions, TMC 1-C and NGC 1333-C7, using new collisional rates of HCN, HNC, and their isotopologues. We investigated the possible effects of the environment and stellar feedback in their chemistry and their evolution. Methods. We used updated collisional rates of HCN, HNC, and their isotopologues in our analysis of the chemistry of TMC 1-C (Taurus) and NGC 1333-C7 (Perseus). With millimeter observations, we derived their column densities, the C and N isotopic fractions, the isomeric ratios, and the deuterium fractionation. The continuum data at 3 mm and 850 µm allowed us to compute the emissivity spectral index and look for grain growth as an evolutionary tracer.Results. The H 13 CN/HN 13 C ratio is anticorrelated with the deuterium fraction of HCN, thus it can readily serve as a proxy for the temperature. The spectral index ( β ~ 1.34–2.09) shows a tentative anticorrelation with the H 13 CN/HN 13 C ratio, suggesting grain growth in the evolved, hotter, and less deuterated sources. Unlike TMC 1-C, the south-to-north gradient in dust temperature and spectral index observed in NGC 1333-C7 suggests feedback from the main NGC 1333 cloud.Conclusions. With this up-to-date characterization of two star-forming regions, we found that the chemistry and the physical properties are tightly related. The dust temperature, deuterium fraction, and the spectral index are complementary evolutionary tracers. The large-scale environmental factors may dominate the chemistry and evolution in clustered star-forming regions.
Published: 2023
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5. Hydrothermal system of Central Tenerife Volcanic Complex, Canary Islands (Spain), inferred from self-potential measurements

Author: Ilazkiñe Iribarren, Isidoro Martín, Patricia Trigo, Benito Casas, Tullio Ricci, Rafael Abella, Víctor Cabrera, Pedro A. Torres, Guillaume Levieux, Barbara Suski-Ricci, Jorge Tua Pereda, Beatriz Brenes, Itahiza Domínguez, Pablo De Agustín, Juan Guzmán, Víctor Villasante-Marcos, Natividad Luengo-Oroz, Fabio Di Gangi, Carmen López, Olaya García, Enrique Romero, David Moure, Manuel Moreno, Julie Morin, Stéphanie Barde-Cabusson, Claudia Schütze, Almudena Gomis, María José Blanco, Stavros Meletlidis, Anthony Finizola, Observatorio Geofisico Central, Instituto Geografico Nacional, Laboratoire GéoSciences Réunion (LGSR), Université de La Réunion (UR)-Institut de Physique du Globe de Paris, Institute of Earth Sciences Jaume Almera, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro Geofísico de Canarias, Instituto Nazionale di Geofisica e Vulcanologie Sezione di Palermo, Centre d'études et de recherche en informatique et communications (CEDRIC), Ecole Nationale Supérieure d'Informatique pour l'Industrie et l'Entreprise (ENSIIE)-Conservatoire National des Arts et Métiers [CNAM] (CNAM), Instituto Geografico Nacional (IGN), Istituto Nazionale di Geofisica e Vulcanologia – Sezione di Pisa (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Department of Geophysic and Geology, Universitat Leipzig, Department of Geophysic and Geology, and MEMSFIELD
Subjects: 010504 meteorology & atmospheric sciences, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, 01 natural sciences, Hydrothermal circulation, Hydrothermal system, Impact crater, Geochemistry and Petrology, Pico Viejo, [SDU.STU.VO]Sciences of the Universe [physics]/Earth Sciences/Volcanology, Caldera, Geomorphology, 0105 earth and related environmental sciences, geography, Rift, Felsic, geography.geographical_feature_category, Tenerife, Teide, Self-potential, Geophysics, Volcano, 13. Climate action, Meteoric water, Rift zone, Geology
Abstract: An extensive self-potential survey was carried out in the central volcanic complex of Tenerife Island (Canary Islands, Spain). A total amount of ~. 237. km of profiles with 20. m spacing between measurements was completed, including radial profiles extending from the summits of Teide and Pico Viejo, and circular profiles inside and around Las Cañadas caldera and the northern slopes of Teide and Pico Viejo. One of the main results of this mapping is the detection of well-developed hydrothermal systems within the edifices of Teide and Pico Viejo, and also associated with the flank satellite M. Blanca and M. Rajada volcanoes. A strong structural control of the surface manifestation of these hydrothermal systems is deduced from the data, pointing to the subdivision of Teide and Pico Viejo hydrothermal systems in three zones: summit crater, upper and lower hydrothermal systems. Self-potential maxima related to hydrothermal activity are absent from the proximal parts of the NE and NW rift zones as well as from at least two of the mafic historical eruptions (Chinyero and Siete Fuentes), indicating that long-lived hydrothermal systems have developed exclusively over relatively shallow felsic magma reservoirs. Towards Las Cañadas caldera floor and walls, the influence of the central hydrothermal systems disappears and the self-potential signal is controlled by the topography, the distance to the water table of Las Cañadas aquifer and its geometry. Nevertheless, fossil or remanent hydrothermal activity at some points along the Caldera wall, especially around the Roques de García area, is also suggested by the data. Self-potential data indicate the existence of independent groundwater systems in the three calderas of Ucanca, Guajara and Diego Hernández, with a funnel shaped negative anomaly in the Diego Hernández caldera floor related to the subsurface topography of the caldera bottom. Two other important self-potential features are detected: positive values towards the northwestern Santiago rift, possibly due to the relatively high altitude of the water-table in this area; and a linear set of minima to the west of Pico Viejo, aligned with the northwestern rift and related to meteoric water infiltration along its fracture system. © 2014 Elsevier B.V., This work has been funded by the Instituto Geográfico Nacional (Ministerio de Fomento, Gobierno de España). S. Barde-Cabusson was funded by JAE-Doc Program (JAEDoc 09 01319).
Published: 2014
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6. Causes and mechanisms of the 2011-2012 El Hierro (Canary Islands) submarine eruption

Author: Marti, J., Pinel, Virginie, López, Carmen, Geyer, Adelina, Abella, Rafael, Tárraga, Marta, José Blanco, María, Castro, Antonio, Rodríguez, Carmen, Group of Volcanology [Barcelona], Institute of Earth Sciences Jaume Almera, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut des Sciences de la Terre (ISTerre), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Instituto Geografico Nacional (IGN), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro Geofísico de Canarias, Instituto Geografico Nacional, Universidad de Huelva, and Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDE.MCG]Environmental Sciences/Global Changes, [SDU.STU.VO]Sciences of the Universe [physics]/Earth Sciences/Volcanology
Abstract: International audience; El Hierro eruption started on 10 October 2011 after an unrest episode that initiated on 17 July 2011. This is the first eruption in the Canary Islands that has been tracked in real time. Although being submarine and not directly observable, the data recorded allowed its reconstruction and to identify its causes and mechanisms. Seismicity, surface deformation, and petrological data indicate that a batch of basanitic magma coming from a reservoir located at a depth of about 25km below the El Hierro Island was emplaced at shallower depth creating a new reservoir about 10-12km above, where magma evolved until the initiation of the eruption. The characteristics of seismicity and surface deformation suggest that the necessary space to accumulate magma at this shallower position, which coincides with the crust/mantle boundary beneath El Hierro, was created in about 2months by elastic deformation and magma-driven fracturing of the crust. After this first intrusion episode, part of the magma started to migrate laterally toward the SE for nearly 20 km, always keeping the same depth and following a path apparently controlled by stress barriers created by tectonic and rheological contrasts in the upper lithosphere. This lateral migration of magma ended with a submarine eruption at about 5 km offshore from the southern corner of El Hierro Island. The total seismic energy released during the unrest episode was of 8.1 1011 J, and the total uplift previous to the onset of the eruption was of 40 mm. Combining geological, geophysical, and petrological data and numerical modeling, we propose a volcanological model of the causes and mechanisms of El Hierro eruption that shows how the stress distribution in the crust beneath El Hierro, which was influenced by rheological contrasts, tectonic stresses, and gravitational loading, controlled the movement and eruption of magma. We also discuss the implications of this model in terms of eruption forecast in the Canary Islands.
Published: 2013
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7. Análisis de los parámetros de los acelerogramas registrados en los seísmos de Lorca, de interés para la Ingeniería

Author: Myriam Belvaux, Juan Manuel Alcalde Camino, Luis Cabañas Rodríguez, Xavier Goula Suriñach, Teresa Susagna Vidal, Institut geològic de Catalunya (IGC), IGC, Instituto Geografico Nacional (IGN), Institut Geològic de Catalunya-IGC, Instituto Geográfico Nacional, Instituto Geografico Nacional, and Bureau de Recherches Géologiques et Minières (BRGM) (BRGM)
Subjects: 021110 strategic, defence & security studies, Intensity, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SDE.MCG]Environmental Sciences/Global Changes, 0211 other engineering and technologies, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], 02 engineering and technology, 010502 geochemistry & geophysics, 01 natural sciences, Physics - Geophysics, Directivity, EC8 spectral shapes, Strong ground motion, Near field, Engineering parameters, 0105 earth and related environmental sciences
Abstract: La serie sismica ocurrida en Lorca (Murcia) el dia 11 de mayo de 2011 ha permitido registrar numerosos acelerogramas en las distintas estaciones de la red acelerometrica del Instituto Geografico Nacional (IGN). El analisis de parametros calculados de manera uniforme ha dado lugar a resultados de interes para la ingenieria sismica, en particular los correspondientes a los registros de la ciudad de Lorca. La intensidad del movimiento se ha puesto de manifiesto especialmente en la componente horizontal del movimiento, perpendicular a la falla de Alhama de Murcia, que origino el terremoto. Tanto el valor del PGA de de 0.37g, como del CAV de 0.27g•s pueden haberse visto compensados por una duracion corta del movimiento de unos pocos segundos, dando lugar a una intensidad macrosismica no superior a VII en Lorca. La contribucion de una componente de campo proximo al movimiento total, debido a la propagacion de la ruptura hacia la ciudad, queda reflejada tanto en las senales temporales de aceleracion velocidad y desplazamiento como en el espectro de respuesta.
Published: 2012

8. NanoSIMS determination of the water content of staurolite

Author: Azevedo-Vannson, Samantha, Remusat, Laurent, Bureau, Hélène, Béneut, Keevin, Cesare, Bernardo, Khodja, Hicham, Jiménez-Mejías, María, Roskosz, Mathieu, Minéralogie et magnétisme de basses dimensionnalités [IMPMC] (IMPMC_MIMABADI), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Geoscienze [Padova], Università degli Studi di Padova = University of Padua (Unipd), Laboratoire d'Etudes des Eléments Légers (LEEL - UMR 3685), Nanosciences et Innovation pour les Matériaux, la Biomédecine et l'Energie (ex SIS2M) (NIMBE UMR 3685), Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences de la Terre d'Orléans - UMR7327 (ISTO), Bureau de Recherches Géologiques et Minières (BRGM) (BRGM)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), GEO3BCN CSIC, Geosci Barcelona, Grp Dynam Lithosphere GDL, Luis Sole I Sabaris S-N, Barcelona 08028, Instituto Geografico Nacional, Magma - UMR7327, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Bureau de Recherches Géologiques et Minières (BRGM) (BRGM)-Observatoire des Sciences de l'Univers en région Centre (OSUC), European Project: 819587,HYDROMA, IMPMC_Minéralogie et magnétisme de basses dimensionnalités (IMPMC_MIMABADI), Universita degli Studi di Padova, and European Research Council
Subjects: ERDA, FTIR, Staurolite, Water, NanoSIMS, Amphibole, [CHIM.MATE]Chemical Sciences/Material chemistry, Kyanite
Abstract: Staurolite is an important mineral that can reveal much about metamorphic processes. For instance, it dominates the Fe-Mg exchange reactions in amphibolite-facies rocks between about 550 and 700 °C, and can be also found at suprasolidus conditions. Staurolite contains a variable amount of OH in its structure, whose determination is a key petrological parameter. However, staurolite is often compositionally zoned, fine-grained, and may contain abundant inclusions. This makes conventional water analysis (e.g. FTIR or by chemical titration) unsuitable. With its high sensitivity at high spatial resolution, NanoSIMS is potentially a valuable tool for determining water contents in staurolite. However; a calibration with relevant standards covering a large range of water content is required to obtain accurate and reliable analyses, because matrix effects typically prevent direct quantification of water content by SIMS techniques., We are grateful to the mineral collection of the Muséum National d’Histoire Naturelle in Paris for providing us with the kyanite crystal used for the calibration reported in this manuscript, as well as to Etienne Deloule for providing us with the amphibole standards. Thanks to Alessandro Guastoni at the Museum of Mineralogy, University of Padova, for supplying the staurolite sample from Pizzo Forno. We thank Paula Guira for helping to set up FTIR measurements and Roger Hewins for proofreading the manuscript and improving the English. We are grateful to Benoit Baptiste for access to the X-ray diffraction facility at IMPMC to check on the crystal orientations prior to FTIR and NanoSIMS analyses. Monika Koch-Müller, Richard L. Hervig and an anonymous reviewer are thanked for their constructive comments on earlier version of this manuscript. L.R. thanks the European Research Council for funding via the ERC project HYDROMA (grant agreement No. 819587). The NanoSIMS facility in Paris was established by funds from the CNRS, Région Ile de France, Ministère délégué à l’Enseignement Supérieur et à la Recherche, and the Muséum National d'Histoire Naturelle.
Published: 2022
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9. Towards the new Thematic Core Service Tsunami within the EPOS Research Infrastructure

Author: Andrey Babeyko, Stefano Lorito, Francisco Hernandez, Jörn Lauterjung, Finn Løvholt, Alexander Rudloff, Mathilde Sørensen, Alexey Androsov, Inigo Aniel-Quiroga, Alberto Armigliato, Maria Ana Baptista, Enrico Baglione, Roberto Basili, Jörn Behrens, Beatriz Brizuela, Sergio Bruni, Didem Cambaz, Juan Cantavella Nadal, Fernando Carillho, Ian Chandler, Denis Chang-Seng, Marinos Charalampakis, Lorenzo Cugliari, Clea Denamiel, Gözde Güney Doğan, Gaetano Festa, David Fuhrman, Alice-Agnes Gabriel, Pauline Galea, Steven Gibbons, Mauricio González, Laura Graziani, Marc-André Gutscher, Sven Harig, Helene Hebert, Constantin Ionescu, Fatemeh Jalayer, Nikos Kalligeris, Utku Kânoğlu, Piero Lanucara, Jorge Macias Sánchez, Shane Murphy, Öcal Necmioğlu, Rachid Omira, Gerassimos Papadopoulos, Raphaël Paris, Fabrizio Romano, Tiziana Rossetto, Jacopo Selva, Antonio Scala, Roberto Tonini, Konstantinos Trevlopoulos, Ioanna Triantafyllou, Roger Urgeles, Roberto Vallone, Ivica Vilibić, Manuela Volpe, Ahmet Yalciner, Agencia Estatal de Investigación (España), Andrey Babeyko, Stefano Lorito, Francisco Hernandez, Jörn Lauterjung, Finn Løvholt, Alexander Rudloff, Mathilde Sørensen, Alexey Androsov, Inigo Aniel-Quiroga, Alberto Armigliato, Maria Ana Baptista, Enrico Baglione, Roberto Basili, Jörn Behrens, Beatriz Brizuela, Sergio Bruni, M. Didem Cambaz, Juan Cantavella-Nadal, Fernando Carrilho, Ian Chandler, Denis Chang-Seng, Marinos Charalampakis, Lorenzo Cugliari, Clea Denamiel, Gözde Güney Dogan, Gaetano Festa, David Fuhrman, Alice-Agnes Gabriel, Pauline Galea, Steven J. Gibbons, Mauricio Gonzalez, Laura Graziani, Marc-André Gutscher, Sven Harig, Helen Hebert, Constantin Ionescu, Fatemeh Jalayer, Nikos Kalligeris, Utku Kânoğlu, Piero Lanucara, Jorge Macías Sánchez, Shane Murphy, Öcal Necmioğlu, Rachid Omira, Gerassimos A. Papadopoulos, Raphaël Paris, Fabrizio Romano, Tiziana Rossetto, Jacopo Selva, Antonio Scala, Roberto Tonini, Konstantinos Trevlopoulos, Ioanna Triantafyllou, Roger Urgeles, Roberto Vallone, Ivica Vilibić, Manuela Volpe, Ahmet C. Yalciner, GeoForschungsZentrum - Helmholtz-Zentrum Potsdam (GFZ), Istituto Nazionale di Geofisica e Vulcanologia, Flanders Marine Institute (VLIZ), Norwegian Geotechnical Institute (NGI), University of Bergen (UiB), Alfred Wegener Institute [Potsdam], Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), IHCantabria - Instituto de Hidráulica Ambiental de La Universidad de Cantabria, Santander, Alma Mater Studiorum University of Bologna (UNIBO), Instituto Superior de Engenharia de Lisboa (ISEL), Universität Hamburg (UHH), Kandilli Observatory and Earthquake Research Institute (KOERI), Boǧaziçi üniversitesi = Boğaziçi University [Istanbul], Instituto Geografico Nacional (IGN), Instituto Português de Investigação do Mar e da Atmosfera (IPMA), HR Wallingford Limited, Intergovernmental Oceanographic Commission of UNESCO, Institute of Geodynamics [Athens], National Observatory of Athens (NOA), Institut Ruđer Bošković (IRB), Middle East Technical University [Ankara] (METU), University of Naples Federico II = Università degli studi di Napoli Federico II, Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Ludwig-Maximilians-Universität München (LMU), University of Malta [Malta], Geo-Ocean (GEO-OCEAN), Université de Bretagne Sud (UBS)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), 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), National Institute for Earth Physics [Romania] - Institutul Național pentru Fizica Pământului (NIEP), CINECA Consorzio Interuniversitario [Rome, Italy], Universidad de Málaga [Málaga] = University of Málaga [Málaga], International Society for the Prevention and Mitigation of Natural Hazards, Athens, Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), University College of London [London] (UCL), Department of Geology and Geoenvironment, National and Kapodistrian University of Athens (NKUA), Centre d'Investigació i Desenvolupament [Barcelona] (CID-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), European Project: 262229,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2010-1,EPOS(2010), and Universidad de Cantabria
Subjects: [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Geophysics, Tsunami, Natural hazards, Community building, EPOS, Research infrastructure, Tsunami Natural hazards Community building EPOS Research infrastructure
Abstract: Special issue EPOS a Research Infrastructure in solid Earth: open science and innovation .-- 21 pages, 8 figures, Tsunamis constitute a significant hazard for European coastal populations, and the impact of tsunami events worldwide can extend well beyond the coastal regions directly affected. Understanding the complex mechanisms of tsunami generation, propagation, and inundation, as well as managing the tsunami risk, requires multidisciplinary research and infrastructures that cross national boundaries. Recent decades have seen both great advances in tsunami science and consolidation of the European tsunami research community. A recurring theme has been the need for a sustainable platform for coordinated tsunami community activities and a hub for tsunami services. Following about three years of preparation, in July 2021, the European tsunami community attained the status of Candidate Thematic Core Service (cTCS) within the European Plate Observing System (EPOS) Research Infrastructure. Within a transition period of three years, the Tsunami candidate TCS is anticipated to develop into a fully operational EPOS TCS. We here outline the path taken to reach this point, and the envisaged form of the future EPOS TCS Tsunami. Our cTCS is planned to be organised within four thematic pillars: (1) Support to Tsunami Service Providers, (2) Tsunami Data, (3) Numerical Models, and (4) Hazard and Risk Products. We outline how identified needs in tsunami science and tsunami risk mitigation will be addressed within this structure and how participation within EPOS will become an integration point for community development, With the institutional support of the ‘Severo Ochoa Centre of Excellence’ accreditation (CEX2019-000928-S)
Published: 2022
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10. SOLIS XVI. Mass ejection and time variability in protostellar outflows: Cep E

Author: A. de A. Schutzer, P. R. Rivera-Ortiz, B. Lefloch, A. Gusdorf, C. Favre, D. Segura-Cox, A. López-Sepulcre, R. Neri, J. Ospina-Zamudio, M. De Simone, C. Codella, S. Viti, L. Podio, J. Pineda, R. O’Donoghue, C. Ceccarelli, P. Caselli, F. Alves, R. Bachiller, N. Balucani, E. Bianchi, L. Bizzocchi, S. Bottinelli, E. Caux, A. Chacón-Tanarro, F. Dulieu, J. Enrique-Romero, F. Fontani, S. Feng, J. Holdship, I. Jiménez-Serra, A. Jaber Al-Edhari, C. Kahane, V. Lattanzi, Y. Oya, A. Punanova, A. Rimola, N. Sakai, S. Spezzano, I. R. Sims, V. Taquet, L. Testi, P. Theulé, P. Ugliengo, C. Vastel, A. I. Vasyunin, F. Vazart, S. Yamamoto, A. Witzel, A. de A. Schutzer, P. R. Rivera-Ortiz, B. Lefloch, A. Gusdorf, C. Favre, D. Segura-Cox, A. L??pez-Sepulcre, R. Neri, J. Ospina-Zamudio, M. De Simone, C. Codella, S. Viti, L. Podio, J. Pineda, R. O'Donoghue, C. Ceccarelli, P. Caselli, F. Alve, R. Bachiller, N. Balucani, E. Bianchi, L. Bizzocchi, S. Bottinelli, E. Caux, A. Chacón-Tanarro, F. Dulieu, J. Enrique-Romero, F. Fontani, S. Feng, J. Holdship, I. Jiménez-Serra, A. Jaber Al-Edhari, C. Kahane, V. Lattanzi, Y. Oya, A. Punanova, A. Rimola, N. Sakai, S. Spezzano, I. R. Sim, V. Taquet, L. Testi, P. Theulé, P. Ugliengo, C. Vastel, A. I. Vasyunin, F. Vazart, S. Yamamoto, A. Witzel, 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, Observatoire de Paris, Université Paris sciences et lettres (PSL), Astrophysique, 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), Centre de Mathématiques Laurent Schwartz (CMLS), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), University of Texas at Austin [Austin], Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), University College of London [London] (UCL), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Radiopathologie (LRP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de la Santé et de la Recherche Médicale (INSERM), Observatorio Astronomico Nacional, Madrid, Dip. Chimica 'G. Ciamician', Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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), Instituto Geografico Nacional (IGN), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), 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), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), The University of Tokyo (UTokyo), Ural Federal University [Ekaterinburg] (UrFU), Universitat Autònoma de Barcelona (UAB), RIKEN - Institute of Physical and Chemical Research [Japon] (RIKEN), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Torino = University of Turin (UNITO), Based on observations carried out with the IRAM NOEMA interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). AS, BL, PR-RO, acknowledge support from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 811312 for the project 'Astro-Chemical Origins' (ACO) and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program for the Project 'The Dawn of Organic Chemistry' (DOC) grant agreement No 741002. DSC is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2102405. A.V. and A.P. are the members of the Max Planck Partner Group at the Ural Federal University. A.P. and A.V. acknowledge the support of the Russian Ministry of Science and Education via the State Assignment Contract no. FEUZ-2020-0038., European Project: 811312, LERMA Cergy (LERMA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA (UMR_8112)), 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)-CY Cergy Paris Université (CY)-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)-CY Cergy Paris Université (CY), INSU/CNRS (France), MPG (Germany), IGN (Spain), European Union [811312], European Research Council (ERC) under the European Union [741002], NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-2102405], and Russian Ministry of Science and Education [FEUZ-2020-0038]
Subjects: DYNAMICS, MASS EJECTION, JETS AND OUTFLOWS [ISM], KINEMATICS AND DYNAMICS [ISM], ISM JETS AND OUTFLOWS, TIME VARIABILITY, JET FORMATION, HIGH VELOCITY, FORMATION [STARS], ISM: kinematics and dynamic, KINEMATICS, ISM: jets and outflow, ISM: kinematics and dynamics, stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], astrochemistry, STARS FORMATION, ACCRETION PROCESS, PROTOSTARS, Astronomy and Astrophysics, VELOCITY, MASS LOSS RATE, Astrophysics - Astrophysics of Galaxies, ISM: jets and outflows, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], STARS
Abstract: Context. Protostellar jets are an important agent of star formation feedback, tightly connected with the mass-accretion process. The history of jet formation and mass ejection provides constraints on the mass accretion history and on the nature of the driving source. Aims. We characterize the time-variability of the mass-ejection phenomena at work in the class 0 protostellar phase in order to better understand the dynamics of the outflowing gas and bring more constraints on the origin of the jet chemical composition and the mass accretion history. Methods. Using the NOrthern Extended Millimeter Array (NOEMA) interferometer, we have observed the emission of the CO 2–1 and SO NJ = 54–43 rotational transitions at an angular resolution of 1.0 00 (820 au) and 0.400 (330 au), respectively, toward the intermediate mass class 0 protostellar system Cep E. Results. The CO high-velocity jet emission reveals a central component of ≤400 au diameter associated with high-velocity molecular knots that is also detected in SO, surrounded by a collimated layer of entrained gas. The gas layer appears to be accelerated along the main axis over a length scale δ0 ∼ 700 au, while its diameter gradually increases up to several 1000 au at 2000 au from the protostar. The jet is fragmented into 18 knots of mass ∼10−3 M, unevenly distributed between the northern and southern lobes, with velocity variations up to 15 km s−1 close to the protostar. This is well below the jet terminal velocities in the northern (+65 km s−1) and southern (-125 km s-1)lobes. The knot interval distribution is approximately bimodal on a timescale of ∼50–80 yr, which is close to the jet driving protostar Cep E-A and ∼150−20 yr at larger distances >1200. The mass-loss rates derived from knot masses are steady overall, with values of 2.7 x 10−5 M yr−1 and 8.9 x 10−6 M yr−1 in the northern and southern lobe, respectively. Conclusions. The interaction of the ambient protostellar material with high-velocity knots drives the formation of a molecular layer around the jet. This accounts for the higher mass-loss rate in the northern lobe. The jet dynamics are well accounted for by a simple precession model with a period of 2000 yr and a mass-ejection period of 55 yr. © Authors 2022 741002; National Science Foundation, NSF: AST-2102405; Horizon 2020 Framework Programme, H2020; H2020 Marie Skłodowska-Curie Actions, MSCA: 811312; European Research Council, ERC; Ministry of Education and Science of the Russian Federation, Minobrnauka: FEUZ-2020-0038; Centre National de la Recherche Scientifique, CNRS; Ural Federal University, UrFU interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). AS, BL, PR-RO, acknowledge support from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 811312 for the project “Astro-Chemical Origins” (ACO) and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program for the Project “The Dawn of Organic Chemistry” (DOC) grant agreement No 741002. DSC is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2102405. A.V. and A.P. are the members of the Max Planck Partner Group at the Ural Federal University. A.P. and A.V. acknowledge the support of the Russian Ministry of Science and Education via the State Assignment Contract no. FEUZ-2020-0038. Based on observations carried out with the IRAM NOEMA interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). AS, BL, PR-RO, acknowledge support from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 811312 for the project "Astro-Chemical Origins" (ACO) and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program for the Project "The Dawn of Organic Chemistry" (DOC) grant agreement No 741002. DSC is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2102405. A.V. and A.P. are the members of the Max Planck Partner Group at the Ural Federal University. A.P. and A.V. acknowledge the support of the Russian Ministry of Science and Education via the State Assignment Contract no. FEUZ-2020-0038.
Published: 2022
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11. Discovery of CH3CHCO in TMC-1 with the QUIJOTE line survey

Author: R. Fuentetaja, C. Bermúdez, C. Cabezas, M. Agúndez, B. Tercero, N. Marcelino, J. R. Pardo, L. Margulès, R. A. Motiyenko, J.-C. Guillemin, P. de Vicente, J. Cernicharo, Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Universidad de Valladolid [Valladolid] (UVa), Instituto Geografico Nacional (IGN), Laboratoire de Physique des Lasers, Atomes et Molécules - UMR 8523 (PhLAM), Université de Lille-Centre National de la Recherche Scientifique (CNRS), 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), Ministerio de Ciencia e Innovacion of Spain (MICIU) [PID2019-106110GB-I00, ERC-2013-Syg-610256-NANOCOSMOS], ERC [CONVREC-2021-317], Ministerio de Universidades [PID2019-107115GB-C21], and [PID2019-106235GB-I00]
Subjects: individual objects, molecular data, astrochemistry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, TMC-1, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), identification, [CHIM]Chemical Sciences, line, molecules, ISM
Abstract: We report the detection of methyl ketene towards TMC-1 with the QUIJOTE line survey. Nineteen rotational transitions with rotational quantum numbers ranging from J = 3 up to J = 5 and Ka ≤ 2 were identified in the frequency range 32.0–50.4 GHz, 11 of which arise above the 3σ level. We derived a column density for CH3CHCO of N = 1.5 × 1011 cm−2 and a rotational temperature of 9 K. Hence, the abundance ratio between ketene and methyl ketene, CH2CO/CH3CHCO, is 93. This species is the second C3H4O isomer detected. The other, trans-propenal (CH2CHCHO), corresponds to the most stable isomer and has a column density of N = (2.2 ± 0.3)×1011 cm−2, which results in an abundance ratio CH2CHCHO/CH3CHCO of 1.5. The next non-detected isomer with the lowest energy is cis-propenal, which is therefore a good candidate for future discovery. We have carried out an in-depth study of the possible gas-phase chemical reactions involving methyl ketene to explain the abundance detected, achieving good agreement between chemical models and observations.
Published: 2023
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12. Global phylogeography and ancient evolution of the widespread human gut virus crAssphage

Author: Steven R. Head, Emma Billings, Stephen Wandro, Jane M. Carlton, Alexandra Zhernakova, A. Murat Eren, Zhe Xue Quan, Anders S. Nilsson, Gyu Sung Cho, Udi Qimron, Martin M. Kowalewski, John Shimashita, Gillian A.O. Rice, Frank Møller Aarestrup, Elyse Stachler, Vito Adrian Cantu, Linsey C. Marr, Alessandro Rossi, Angela McCann, Colin Hill, Cristina García-Aljaro, Kristen M. Gulino, David A. Lipson, Rene S. Hendriksen, Bryan A. White, Bas E. Dutilh, Bashir Mukhtar Elwasila, Karla Mazankova, Alexander V. Tyakht, Julia M. Maritz, Ronan Strain, Rodrigo De la Iglesia, Ramy K. Aziz, Kyle Levi, Alan Twaddle, Alejandro Reyes Muñoz, Katelyn McNair, Alejandro A. Vega, Nathaniel J. Dominy, Abigail E. Asangba, Robert Edwards, Rasha Odeh, Olivia D. Nigro, Gunduz Ahmadov, Raúl R. Raya, Nam Nguyen, Charles M. A. P. Franz, Nicole Trefault, Adán Ramírez-Rojas, Michael P. Doane, Randall E. Junge, Patrick A. de Jonge, Jingyuan Fu, Taylor O'Connell, Mike Cranfield, German Tapia, Heikki Hyöty, Nicolás A. Villagra, Cisca Wijmenga, Henrike Zschach, Megan M. Morris, Franklin L. Nobrega, Elena N. Ilina, David Thomas McCarthy, Daniel Cazares, Silvia Monteiro, Lawrence Mugisha, Daniel A. Cuevas, Horst Neve, Przemyslaw Decewicz, John M. Haggerty, Ricardo Santos, Deepak Kumaresan, Shahar Molshanski-Mor, Andrew S. Whiteley, Benjamin Moreira-Grez, Rebecca M. Stumpf, Katrine Whiteson, Holly M. Norman, Jeremy J. Barr, Peter C. Fineran, Jeroen Wagemans, Samuel L. Díaz Muñoz, Kim Reasor, Elizabeth A. Dinsdale, Mitchell T. Irwin, Aaron J. Prussin, Mohammadali Khan Mirzaei, Maite Muniesa, Christelle Desnues, Montserrat Llagostera, Rob Lavigne, Abeer Alassaf, Tess Condeff, Petra Rainetova, María Mercedes Zambrano, Adrian Cazares, Elodie Ghedin, Alexander Kurilshikov, Lukasz Dziewit, Thomas C. Jeffries, Mary Ann Ugochi Ibekwe, Eugenia S. Lisitsyna, Juan Jofre, Pedro J. Torres, Maria Ohaeri, Mariana Piuri, Andrew Oliver, Steven R. Leigh, Ondrej Cinek, Stan J. J. Brouns, Josefa Antón, Pilar Cortés, Kyle Bibby, Lars C. Stene, Pablo Vinuesa, Scott T. Kelley, San Diego State University (SDSU), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Microbes évolution phylogénie et infections (MEPHI), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Laboratory of Gene Technology, Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Monash University [Clayton], University Medical Center Groningen [Groningen] (UMCG), Centro de Investigación Oceanográfica en el Pacífico Sur Oriental (COPAS), Universidad de Concepción - University of Concepcion [Chile], Dartmouth College [Hanover], Marine Biological Laboratory (MBL), University of Chicago, Department of Safety and Quality of Fruit and Vegetables, Federal Research Institute for Nutrition and Food, Department of Parasite and Virus Genomics, The Institute for Genomic Research (TIGR), The Scripps Research Institute [La Jolla, San Diego], Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Queen's University [Belfast] (QUB), Hawkesbury Institute for the Environment [Richmond] (HIE), Western Sydney University, CREW - Center for Research on the English-speaking World - EA 4399 (CREW), Université Sorbonne Nouvelle - Paris 3, School of Microbiology, University College Cork (UCC), Université du Cap-Vert, université du Cap-Vert, Department of Microbiology [University of Barcelona], Dept Microbiol & Biotechnol, Max Rubner Inst, Department of Pharmaceutical Biosciences, Uppsala University, University of Manchester [Manchester], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Getulio Vargas Foundation, Centro Geofísico de Canarias, Instituto Geografico Nacional, Laboratorio de Patogénesis Molecular y Antimicrobianos, Facultad de Medicina , Universidad Andres Bello, University of Illinois, University of Illinois System, National Severe Storms Laboratory (NSSL), National Oceanic and Atmospheric Administration (NOAA), Department of Medical Genetics, HMNC Brain Health, Utrecht University [Utrecht], Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU), Universidad de Concepción [Chile], The SCRIPPS Research Institute (SCRIPPS), University of California [Los Angeles] (UCLA), University of California-University of California, Technical University of Denmark [Lyngby] (DTU), Biomolecular Imaging and Proteomics, National Center for Mass Spectrometry Imaging, Uppsala University, Universidad de Alicante. Departamento de Fisiología, Genética y Microbiología, Ecología Microbiana Molecular, Theoretical Biology and Bioinformatics, Sub Bioinformatics, Groningen Institute for Gastro Intestinal Genetics and Immunology (3GI), Translational Immunology Groningen (TRIGR), and Center for Liver, Digestive and Metabolic Diseases (CLDM)
Subjects: DYNAMICS, Male, BACTERIAL, ACCURACY, Lineage (evolution), Filogeografia, Microbiología, Applied Microbiology and Biotechnology, Genome, Biological Coevolution, MULTIPLE SEQUENCE ALIGNMENT, TRACKING, Feces, Tumours of the digestive tract Radboud Institute for Molecular Life Sciences [Radboudumc 14], Bacteriophages, Viral, Clade, Phylogeny, ComputingMilieux_MISCELLANEOUS, 2. Zero hunger, 0303 health sciences, Environmental microbiology, [SDV.BID.EVO]Life Sciences [q-bio]/Biodiversity/Populations and Evolution [q-bio.PE], crAssphage, READ ALIGNMENT, GENOME, Phylogeography, [SDV.MP.VIR]Life Sciences [q-bio]/Microbiology and Parasitology/Virology, Female, Life Sciences & Biomedicine, Primates, Microbiology (medical), Lineage (genetic), Evolution, Immunology, Coronacrisis-Taverne, Microbiota intestinal, BIOLOGY, Biology, Microbiology, Virus, DNA sequencing, Article, 03 medical and health sciences, All institutes and research themes of the Radboud University Medical Center, SDG 3 - Good Health and Well-being, Phylogenetics, Genetics, Animals, Humans, Human virome, ALGORITHM, Microbiome, Genomes, Gastrointestinal microbiome, 030304 developmental biology, [SDV.EE.SANT]Life Sciences [q-bio]/Ecology, environment/Health, Science & Technology, Widespread human gut virus, Bacteroidetes, 030306 microbiology, Genetic Variation, DNA, Cell Biology, biology.organism_classification, Gastrointestinal Microbiome, MICROBIOME, Evolutionary biology, DNA, Viral
Abstract: Microbiomes are vast communities of microorganisms and viruses that populate all natural ecosystems. Viruses have been considered to be the most variable component of microbiomes, as supported by virome surveys and examples of high genomic mosaicism. However, recent evidence suggests that the human gut virome is remarkably stable compared with that of other environments. Here, we investigate the origin, evolution and epidemiology of crAssphage, a widespread human gut virus. Through a global collaboration, we obtained DNA sequences of crAssphage from more than one-third of the world's countries and showed that the phylogeography of crAssphage is locally clustered within countries, cities and individuals. We also found fully colinear crAssphage-like genomes in both Old-World and New-World primates, suggesting that the association of crAssphage with primates may be millions of years old. Finally, by exploiting a large cohort of more than 1,000 individuals, we tested whether crAssphage is associated with bacterial taxonomic groups of the gut microbiome, diverse human health parameters and a wide range of dietary factors. We identified strong correlations with different clades of bacteria that are related to Bacteroidetes and weak associations with several diet categories, but no significant association with health or disease. We conclude that crAssphage is a benign cosmopolitan virus that may have coevolved with the human lineage and is an integral part of the normal human gut virome. ispartof: NATURE MICROBIOLOGY vol:4 issue:10 pages:1727-1736 ispartof: location:England status: published
Published: 2019
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13. Using highly accurate land gravity and 3D geologic modeling to discriminate potential geothermal areas: Application to the Upper Rhine Graben, France

Author: Jacques Hinderer, Yassine Abdelfettah, Vincent Maurer, E. Dalmais, Marta Calvo, Albert Genter, Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto Geografico Nacional (IGN), GEIE Exploitation Minière de la Chaleur, and GEIE
Subjects: Gravity (chemistry), Field (physics), [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], 0211 other engineering and technologies, 02 engineering and technology, Geophysics, 010502 geochemistry & geophysics, 01 natural sciences, Graben, Geochemistry and Petrology, 021108 energy, Geothermal gradient, Bouguer anomaly, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: New land gravity data results acquired in northern Alsace were presented. Compared to the available old Bouguer anomaly, we recovered an accurate Bouguer anomaly field showing data uncertainties [Formula: see text]. A qualitative data analysis using pseudotomographies reveals several negative anomalies suggesting a decrease of the bulk density at the depth of geothermal interest. We have performed a quantitative study on the basis of the existing 3D geologic model derived from a reinterpretation of the vintage seismics. The theoretical gravity response indicates a great mismatch with the observed Bouguer anomaly. The stripping approach was applied, and the stripped Bouguer anomaly indicates that the density values of the Jurassic, but especially for the Triassic, the Buntsandstein, and the upper part of the basement, were overestimated even using the density values measured in the deep geothermal borehole. This suggests that the borehole density values do not reflect the density variations occurring at larger scale. To reduce the Bouguer anomaly during stripping, a negative density contrast should be affected to the Buntsandstein layer overlaying the basement, suggesting that the part located between the Buntsandstein and the upper part of the basement presents a low-density value compared to the reference density, which is not necessarily expected and is not observed in the densities measured in the borehole. Interestingly, a correlation is found between the gravity analyses and the thermal gradient boreholes in the northern part of the study area. For two boreholes, the gravity interpretation suggests a huge density decrease in the Buntsandstein, which may arise from a combination of high-density fracturing and the important quantity of geothermal fluid significantly affecting the bulk density. Analysis of the thermal borehole data suggests that these two boreholes indicate higher geothermal potential compared with the other boreholes.
Published: 2020
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14. Volcanic edifice slip events recorded on the fault plane of the San Andrés Landslide, El Hierro, Canary Islands

Author: Matt Rowberry, Jan Balek, Miloš René, Pierre-Henri Blard, Filip Hartvich, Stavros Meletlidis, Jan Blahůt, Ivo Baroň, Ivanka Mitrovic-Woodell, Institute of Rock Structure and Mechanics of the Czech Academy of Sciences (IRSM / CAS), Czech Academy of Sciences [Prague] (CAS), University of Vienna [Vienna], Centre de Recherches Pétrographiques et Géochimiques (CRPG), Université de Lorraine (UL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centro Geofísico de Canarias, and Instituto Geografico Nacional
Subjects: 010504 meteorology & atmospheric sciences, frictionite, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Slip (materials science), Cataclastic rock, Miloš René, 010502 geochemistry & geophysics, 01 natural sciences, Fault breccia, Matt Rowberry, 14. Life underwater, Clockwise, Filip Hartvich, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth-Surface Processes, cosmogenic radionuclide dating, Pierre-Henri Blard, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, [SDU.STU.TE]Sciences of the Universe [physics]/Earth Sciences/Tectonics, geography, Ivanka Mitrovic-Woodell, geography.geographical_feature_category, Jan Balek, Ivo Baroň, Stavros Meletlidis, Landslide, Debris, volcanic collapse, silica layer, Basanite, Geophysics, Volcano, cataclasis metamorphism, Geology, Seismology, Canary Islands Jan Blahut
Abstract: Volcanic flank collapses often result in giant debris avalanches that are capable of travelling tens of kilometres across the ocean floor and generating tsunamis that devastate distant communities. The San Andres Landslide on El Hierro, Canary Islands, represents one of the few places in the world where it is possible to investigate the landslide mass and fault planes of a volcanic collapse structure. In this study, a new conceptual model for the development of this enormous slump is presented on the basis of structural geological and geomorphological measurements, petrological and microstructural analyses, and cosmogenic radionuclide dating. Structural geological and geomorphological measurements indicate that the fault plane records two distinct events. Petrological and microstructural analyses demonstrate that a thin layer of frictionite covers the surface of the fault in contact with an oxidised tectonic breccia that transitions into the underlying undeformed basanite host rock. This frictionite comprises a heterogeneous cataclastic layer and a translucent silica layer that are interpreted to represent two separate slip events on the basis of their architecture and crosscutting relationships. Cosmogenic 3He dating reveals a maximum exposure age of 183 ± 17 ka to 52 ± 17 ka. Arguments are presented in support of the idea that the first slip event took place between 545 ka and 430 ka, prior to significant clockwise rotation of El Hierro, and the second slip event took place between 183 ka and 52 ka, perhaps in association with one of the giant debris avalanches that occurred around that time. This is the first time that more than one slip event has been recognised from the fault plane of the San Andres Landslide. It is also believed to be the first time a silica layer resulting from frictional melt has been described in a volcanic setting.
Published: 2020
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15. A study of the monsoonal hydrology contribution using a 8-yr record (2010-2018) from superconducting gravimeter OSG-060 at Djougou (Benin, West Africa)

Author: Basile Hector, Séverine Rosat, Jean-Paul Boy, Marta Calvo, Umberto Riccardi, F. Littel, Jean-Daniel Bernard, Jacques Hinderer, Dynamique globale et déformation active (IPGS) (IPGS-DGDA), Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut des Géosciences de l’Environnement (IGE), Institut de Recherche pour le Développement (IRD)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Università degli studi di Napoli Federico II, Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dynamique globale (IPGS) (IPGS-DG), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Scienze della Terra, dell'Ambiente e delle Risorse (DiSTAR), Instituto Geografico Nacional (IGN), Université Grenoble Alpes [2020-....] (UGA [2020-....])-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....])-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Naples Federico II = Università degli studi di Napoli Federico II, Hinderer, J., Hector, B., Riccardi, U., Rosat, S., Boy, J-P., Calvp, M., Littel, F., and Bernard, J-D.
Subjects: 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], hydrology, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], 010502 geochemistry & geophysics, Monsoon, 01 natural sciences, West africa, Hydrology (agriculture), Geochemistry and Petrology, monsoon, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Gravimeter, 15. Life on land, Time variable gravity,Africa,Hydrology,Loading,Monsoon, 6. Clean water, loading, Geophysics, 13. Climate action, Climatology, time variable gravity, Africa, Time variable gravity, Hydrology, Geology
Abstract: SUMMARY We analyse a nearly 8-yr record (2010–2018) of the superconducting gravimeter OSG-060 located at Djougou (Benin, West Africa). After tidal analysis removing all solid Earth and ocean loading tidal contributions and correcting for the long-term instrumental drift and atmospheric loading, we obtain a gravity residual signal which is essentially a hydrological signal due to the monsoon. This signal is first compared to several global hydrology models (ERA, GLDAS and MERRA). Our superconducting gravimeter residual signal is also superimposed onto episodic absolute gravity measurements and to space gravimetry GRACE data. A further comparison is done using local hydrological data like soil moisture in the very superficial layer (0–1.2 m), water table depth and rainfall. The temporal evolution of the correlation coefficient between the gravity observation and both the soil moisture and the water table is well explained by the direct infiltration process of rain water together with the lateral transfer discharging the water table. Finally, we compute the water storage changes (WSC) using a simulation based on the physically based Parflow-CLM numerical model of the catchment, which solves the water and energy budget from the impermeable bedrock to the top of the canopy layer using the 3-D Richards equation for the water transfers in the ground, the kinematic wave equation for the surface runoff and a land surface model (CLM) for the energy budget and evapotranspiration calculation. This model forced by rain is in agreement with evapotranspiration and stream flow data and leads to simulated water storage changes that nicely fit to the observed gravity signal. This study points out the important role played by surface gravity changes in terms of a reliable proxy for water storage changes occurring in small catchments.
Published: 2020
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16. Seeds of Life in Space (SOLIS): VI. Chemical evolution of sulfuretted species along the outflows driven by the low-mass protostellar binary NGC 1333-IRAS4A

Author: V. Taquet, C. Codella, M. De Simone, A. López-Sepulcre, J. E. Pineda, D. Segura-Cox, C. Ceccarelli, P. Caselli, A. Gusdorf, M. V. Persson, F. Alves, E. Caux, C. Favre, F. Fontani, R. Neri, Y. Oya, N. Sakai, C. Vastel, S. Yamamoto, R. Bachiller, N. Balucani, E. Bianchi, L. Bizzocchi, A. Chacón-Tanarro, F. Dulieu, J. Enrique-Romero, S. Feng, J. Holdship, B. Lefloch, A. Jaber Al-Edhari, I. Jiménez-Serra, C. Kahane, V. Lattanzi, J. Ospina-Zamudio, L. Podio, A. Punanova, A. Rimola, I. R. Sims, S. Spezzano, L. Testi, P. Theulé, P. Ugliengo, A. I. Vasyunin, F. Vazart, S. Viti, A. Witzel, Istituto Nazionale di Astrofisica (INAF), 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)-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), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Chalmers University of Technology [Göteborg], Centre National d'Études Spatiales [Toulouse] (CNES), 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 de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), The University of Tokyo (UTokyo), RIKEN - Institute of Physical and Chemical Research [Japon] (RIKEN), Instituto Geografico Nacional (IGN), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), University College of London [London] (UCL), Spanish National Research Council (CSIC), Ural Federal University [Ekaterinburg] (UrFU), Departament de Química [Barcelona] (UAB), Universitat Autònoma de Barcelona (UAB), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Torino (UNITO), IRAM PdBI/NOEMA Interferometer [V05B, V010, U003, L15AA], MPG (Germany)Max Planck Society, IGN (Spain), European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grantEuropean Union (EU) [664931], PRIN-INAF 2016 'The Cradle of Life -GENESIS-SKA (General Conditions in Early Planetary Systems for the rise of life with SKA)', European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programmeEuropean Research Council (ERC) [741002], European MARIE SKLODOWSKA-CURIE ACTIONS under the European Union's Horizon 2020 research and innovation programme [811312], French National Research Agency of the 'Origin of Life' project of the Universite Grenoble-AlpesFrench National Research Agency (ANR) [ANR-15-IDEX-02], INSU/CNRS (France)Centre National de la Recherche Scientifique (CNRS), Ceccarelli, C. [0000-0001-9664-6292], Balucani, N. [0000-0001-5121-5683], Rimola, A. [0000-0002-9637-4554], Al Edhari, A. J. [0000-0003-4089-841X], De Oliveira Alves, F. [0000-0002-7945-064X], Lefloch, B. [0000-0002-9397-3826], Persson, M. V. [0000-0002-1100-5734], Bachiller, R. [0000-0002-5331-5386], Pineda, J. [0000-0002-3972-1978], Segura Cox, D. [0000-0003-3172-6763], IRAM PdBI/NOEMA Interferometer, V05B V010 U003 L15AA, 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, 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), 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), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Torino = University of Turin (UNITO), ANR-15-IDEX-0002,UGA,IDEX UGA(2015), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Agence Nationale de la Recherche (ANR), European Research Council (ERC), 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)-CY Cergy Paris Université (CY), Taquet V., Codella C., De Simone M., Lopez-Sepulcre A., Pineda J.E., Segura-Cox D., Ceccarelli C., Caselli P., Gusdorf A., Persson M.V., Alves F., Caux E., Favre C., Fontani F., Neri R., Oya Y., Sakai N., Vastel C., Yamamoto S., Bachiller R., Balucani N., Bianchi E., Bizzocchi L., Chacon-Tanarro A., Dulieu F., Enrique-Romero J., Feng S., Holdship J., Lefloch B., Jaber Al-Edhari A., Jimenez-Serra I., Kahane C., Lattanzi V., Ospina-Zamudio J., Podio L., Punanova A., Rimola A., Sims I.R., Spezzano S., Testi L., Theule P., Ugliengo P., Vasyunin A.I., Vazart F., Viti S., and Witzel A.
Subjects: MILLIMETER ARRAYS, Binary number, CHEMICAL EVOLUTION, ISM: molecule, Astrophysics, Space (mathematics), 01 natural sciences, ISM: abundances, CHEMICAL CONDITIONS, ISM jets and outflows, ABUNDANCES [ISM], jets and outflows -ISM, CHEMICAL DIFFERENTIATION, 010303 astronomy & astrophysics, ISM abundances, Astrochemistry, Physics, [PHYS]Physics [physics], ASTROCHEMISTRY, Shock (fluid dynamics), INTERSTELLAR ICE, SUBMILLIMETRE TELESCOPES, NGC 1333-IRAS4A, ISM: abundance, ISM: molecules, stars formation, Radial velocity, ISM: jets and outflows, ISM individual objects NGC1333-IRAS4A, ISM: individual objects: NGC 1333-IRAS4A, CHEMICAL HISTORY, Low Mass, molecules -stars, Stars: formation, individual objects, JETS AND OUTFLOWS [ISM], FOS: Physical sciences, Context (language use), INDIVIDUAL OBJECTS: NGC 1333-IRAS4A [ISM], SILICON COMPOUNDS, SULFUR DIOXIDE, ISM molecules, astrochemistry -ISM, FORMATION [STARS], 0103 physical sciences, Protostar, ISM: jets and outflow, formation -ISM, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, abundances -ISM, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MOLECULES [ISM], Outflow, MOLECULAR OUTFLOWS, STARS
Abstract: Context. Low-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows. Aims. The evolution of sulfur chemistry is studied along the outflows driven by the NGC 1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. Methods. We observed various transitions from OCS, CS, SO, and SO2 towards NGC 1333-IRAS4A in the 1.3, 2, and 3 mm bands using the IRAM NOrthern Extended Millimeter Array and we interpreted the observations through the use of the Paris-Durham shock model. Results. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east-south west direction. SO is detected at extremely high radial velocity up to + 25 km s-1 relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 105 cm-3 and relatively warm (T > 100 K) temperatures in most cases. Conclusions. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputtered into the shock gas. In contrast, the longer and likely older outflow triggered by IRAS4A2 is more enriched in species that have a gas phase origin, such as SO2., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
Published: 2020
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17. Controls of magma chamber zonation on eruption dynamics and deposits stratigraphy: The case of El Palomar fallout succession (Tenerife, Canary Islands)

Author: María Jiménez-Mejías, Bruno Scaillet, Stéphane Scaillet, Joan Martí, Dario Pedrazzi, Silvia Zafrilla, Domenico M. Doronzo, Joan Andújar, Institute of Earth Sciences Jaume Almera, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro Geofísico de Canarias, Instituto Geografico Nacional, Magma - UMR7327, Institut des Sciences de la Terre d'Orléans - UMR7327 (ISTO), Bureau de Recherches Géologiques et Minières (BRGM) (BRGM)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Bureau de Recherches Géologiques et Minières (BRGM) (BRGM)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Martí Molist, Joan [0000-0003-3930-8603], Pedrazzi, Dario [0000-0002-6869-1325], Doronzo, Domenico Maria [0000-0002-6866-8870], Martí Molist, Joan, Pedrazzi, Dario, and Doronzo, Domenico Maria
Subjects: 010504 meteorology & atmospheric sciences, Geochemistry, Pyroclastic rock, Magma chamber, Eruption dynamics, Eruption column, 010502 geochemistry & geophysics, 01 natural sciences, Las Cañadas Edifice, Geochemistry and Petrology, El Palomar pumice fall, [SDU.STU.VO]Sciences of the Universe [physics]/Earth Sciences/Volcanology, Caldera, 0105 earth and related environmental sciences, geography, Explosive eruption, geography.geographical_feature_category, Tenerife, Teide, Magma chamber zonation, Geophysics, Volcano, 13. Climate action, Magma, Mafic, Geology
Abstract: Anticipating volcanic eruptions at central volcanoes require knowing how magma chambers prepare for new eruptions. Pre-eruptive processes that occur in such magma chambers are recorded in the products of these eruptions, so their characterisation in terms of magma composition and physics offers the clues to understand past eruptions and predict future ones. Here, we study the very well preserved pyroclastic succession of El Palomar Member (712 ± 41 ka), in Las Cañadas caldera, Teide, Canary Islands. This deposit resulted from a single explosive eruption of a phonolitic magma that started with a sustained eruption column (sub-plinian or plinian) that formed a massive, 40 m thick non-welded fallout deposit, progressively changing into a lower intensity fire fountain that deposited a 25 m thick fallout succession of non-welded to strongly welded pumices. Stratigraphic and petrological data suggest that this eruption was related to a thermally-compositionally zoned and relatively shallow magma chamber in which the arrival of a hotter and more mafic magma rapidly triggered the eruption. The studied deposit shows how this zoned structure was maintained during the whole process, which allows one to reconstruct what happened during the eruption. Comparison of this eruption with the current situation at Teide volcano alerts on the potential rapid preparation for new eruptions in the case that sufficient phonolitic magma was available in the shallow plumbing system of this active volcano if new inputs of deeper magma take place.
Published: 2020
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18. PHIBSS2: survey design and z = 0.5 – 0.8 results

Author: Freundlich, J., Combes, F., Tacconi, L., Genzel, R., García-Burillo, S., Neri, R., Contini, T., Bolatto, A., Lilly, S., Salomé, P., Bicalho, I., Boissier, J., Boone, F., Bouché, N., Bournaud, F., Burkert, A., Carollo, M., Cooper, M., Cox, P., Feruglio, C., Schreiber, N, Juneau, S., Lippa, M., Lutz, D., Naab, T., Renzini, A., Saintonge, A., Sternberg, A., Walter, F., Weiner, B., Weiß, A., Wuyts, S., Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Observatorio Astronómico Nacional (OAN), oan, 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), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, AUTRES, Biologie et écologie tropicale et méditerranéenne [2007-2010] (BETM), Université de Perpignan Via Domitia (UPVD)-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), Laboratoire Nanotechnologies Nanosystèmes (LN2 ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Sherbrooke (UdeS)-École supérieure de Chimie Physique Electronique de Lyon (CPE)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Universitätssternwarte der Ludwig-Maximiliansuniversität, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut of Physics - Riga, Latvian Academy of Sciences, Steward observatory, University of Arizona, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Collège de France - Chaire Galaxies et cosmologie, Observatorio Astronomico Nacional, Madrid, 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), Université de Perpignan Via Domitia (UPVD)-École Pratique des Hautes Études (EPHE), Université de Sherbrooke (UdeS)-École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-École Supérieure de Chimie Physique Électronique de Lyon (CPE)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-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), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Interactions Hôtes-Pathogènes-Environnements (IHPE), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Perpignan Via Domitia (UPVD), Institut Interdisciplinaire d'Innovation Technologique (3IT), Université de Sherbrooke [Sherbrooke], Ludwig-Maximiliansuniversität, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), University of São Paulo, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Versuchsanstalt für Wasserbau, Hydrologie und Glaziologie (VAW), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Biologie et écologie tropicale et méditerranéenne (BETM), Université de Perpignan Via Domitia (UPVD)-École pratique des hautes études (EPHE)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Nanotechnologies Nanosystèmes (LN2), Université de Sherbrooke [Sherbrooke]-École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-École supérieure de Chimie Physique Electronique de Lyon (CPE)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), and Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Following the success of the Plateau de Bure high-z Blue Sequence Survey (PHIBSS), we present the PHIBSS2 legacy program, a survey of the molecular gas properties of star-forming galaxies on and around the star-formation main sequence (MS) at different redshifts using IRAM's NOrthern Extended Millimeter Array (NOEMA). This survey significantly extends the existing sample of star-forming galaxies with CO molecular gas measurements, probing the peak epoch of star formation (z = 1 − 1.6) as well as its building-up (z = 2 − 3) and winding-down (z = 0.5 − 0.8) phases. The targets are drawn from the well-studied GOODS, COSMOS, and AEGIS cosmological deep fields and uniformly sample the MS in the stellar mass (M)-star formation rate (SFR) plane with log(M /M) = 10 − 11.8 and SFR = 3.5 − 500 M yr −1 without morphological selection, thus providing a statistically meaningful census of star-forming galaxies at different epochs. We describe the survey strategy and sample selection before focusing on the results obtained at redshift z = 0.5 − 0.8, where we report 60 CO(2-1) detections out of 61 targets. We determine molecular gas masses between 2 × 10 9 and 5 × 10 10 M and separately obtain disc sizes and bulge-to-total (B/T) luminosity ratios from HST I-band images. The median molecular gas-to-stellar mass ratio µ gas = 0.28 ± 0.04, gas fraction f gas = 0.22 ± 0.02, and depletion time t depl = 0.84 ± 0.07 Gyr as well as their dependence with stellar mass and offset from the MS follow published scaling relations for a much larger sample of galaxies spanning a significantly wider range of redshifts, the cosmic evolution of the SFR being mainly driven by that of the molecular gas fraction. The galaxy-averaged molecular Kennicutt-Schmidt (KS) relation between molecular gas and SFR surface densities is strikingly linear, pointing towards similar star formation timescales within galaxies at any given epoch. In terms of morphology, the molecular gas content, the SFR, the disc stellar mass, and the disc molecular gas fraction do not seem to correlate with B/T and the stellar surface density, which suggests an ongoing supply of fresh molecular gas to compensate for the build-up of the bulge. Our measurements do not yield any significant variation of the depletion time with B/T and hence no strong evidence for morphological quenching within the scatter of the MS.
Published: 2019
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19. Molecular and Ionized Gas Phases of an AGN-driven Outflow in a Typical Massive Galaxy at z ≈ 2

Author: S. J. Lilly, N. M. Foerster Schreiber, Chiara Feruglio, R. D. Davies, Dieter Lutz, Linda J. Tacconi, Luis Colina, Rodrigo Herrera-Camus, M. C. Cooper, Peter Timothy Cox, T. Taro Shimizu, T. Naab, Santiago García-Burillo, Amelie Saintonge, H. Uebler, Eckhard Sturm, A. Burkert, Axel Weiss, Jonathan Freundlich, Stijn Wuyts, Francoise Combes, Alberto Bolatto, S. Belli, Reinhard Genzel, Alvio Renzini, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Max-Planck-Institut für Extraterrestrische Physik (MPE), AUTRES, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Universitätssternwarte der Ludwig-Maximiliansuniversität, Ludwig-Maximiliansuniversität, Department of Physics, Durham University, University of São Paulo, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), and University of Edinburgh
Subjects: active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, high-redshift [Galaxies], Ionization, 0103 physical sciences, ISM [Galaxies], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Velocity gradient, Star formation, Astronomy and Astrophysics, Plasma, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Outflow
Abstract: Nuclear outflows driven by accreting massive black holes are one of the main feedback mechanisms invoked at high-z to reproduce the distinct separation between star-forming, disk galaxies and quiescent spheroidal systems. Yet, our knowledge of feedback at high-z remains limited by the lack of observations of the multiple gas phases in galaxy outflows. In this work we use new deep, high-spatial resolution ALMA CO(3-2) and archival VLT/SINFONI H$\alpha$ observations to study the molecular and ionized components of the AGN-driven outflow in zC400528 ---a massive, main sequence galaxy at z=2.3 in the process of quenching. We detect a powerful molecular outflow that shows a positive velocity gradient and extends for at least ~10 kpc from the nuclear region, about three times the projected size of the ionized wind. The molecular gas in the outflow does not reach velocities high enough to escape the galaxy and is therefore expected to be reaccreted. Keeping in mind the various assumptions involved in the analysis, we find that the mass and energetics of the outflow are dominated by the molecular phase. The AGN-driven outflow in zC400528 is powerful enough to deplete the molecular gas reservoir on a timescale at least twice shorter than that needed to exhaust it by star formation. This suggests that the nuclear outflow is one of the main quenching engines at work in the observed suppression of the central star-formation activity in zC400528., Comment: 20 pages, 14 figures. Submitted to ApJ
Published: 2019
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20. Hybrid gravimetry monitoring of Soultz-sous-Forêts and Rittershoffen geothermal sites (Alsace, France)

Author: Marta Calvo, Yassine Abdelfettah, Jean-Daniel Bernard, Christine Heimlich, Umberto Riccardi, Nolwenn Portier, Jacques Hinderer, G. Ferhat, Institut de physique du globe de Strasbourg (IPGS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Ecole et Observatoire des Sciences de la Terre (EOST), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecole et Observatoire des sciences de la terre (EOST), DG, Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Napoli Federico II, Institut National des Sciences Appliquées - Strasbourg (INSA Strasbourg), Institut National des Sciences Appliquées (INSA), Instituto Geografico Nacional (IGN), Portier, Nolwenn, Hinderer, Jacque, Riccardi, Umberto, Ferhat, Gilbert, Calvo, Marta, Abdelfettah, Yassine, Heimlich, Christine, and Bernard, Jean-Daniel
Subjects: [SPI.OTHER]Engineering Sciences [physics]/Other, 010504 meteorology & atmospheric sciences, Monitoring, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], 010502 geochemistry & geophysics, Enhanced geothermal system, 01 natural sciences, 7. Clean energy, Observatory, Geothermics, Gravimetry, Geothermal gradient, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Hybrid gravimetry, business.industry, Gravimeter, Renewable Energy, Sustainability and the Environment, Geology, Time-lapse gravity, Geodesy, Surface gravity, Geotechnical Engineering and Engineering Geology, Geothermal fluid, 13. Climate action, Geothermic, Global Positioning System, business
Abstract: International audience; We investigate the feasibility of the hybrid gravity technique applied to two geothermal reservoirs in northern Alsace, France, namely the Soultz-sous-Forêts and Rittershoffen sites. Soultz-sous-Forêts site is the first enhanced geothermal system demonstration site producing electricity in France. Here a geothermal fluid at 165 °C allows to produce around 1.5 MW thanks to one injection well and one production well 5 km deep. Rittershoffen site is dedicated to an industrial use and it is designed to produce 24 MWth heat power with 2 wells around 2.5 km deep. The most recent production episodes of Rittershoffen and Soultz-sous-Forêts geothermal plants have started respectively on May and June 2016. To study underground mass redistribution, time-lapse relative microgravity measurements have been done since 2014 on a network designed ad hoc for Soultz-sous-Forêts site and since 2015 for Rittershoffen site. After tide and drift correction, double differences are calculated to retrieve the gravity variation at each measuring point compared to a reference time and station. Absolute gravity measurements have been also collected at one of the reference stations. Before the beginning of the production in 2016, the stability of the Soultz-sous-Forêts reference station was monitored through the repetition of absolute measurements and continuous gravity records. In 2016, regular ties between the reference stations and the Strasbourg gravity observatory STJ9 have been done. Several superconducting gravimeters operate continuously in STJ9. Thus, we approach the concept of hybrid gravity. Vertical deformation is also controlled thanks to six continuous GPS measurements: the height changes are less than 1 cm. So we consider that our gravity variations are only due to subsurface mass changes. For the Soultz-sous-Forêts network, we notice significant changes in agreement with the position of the injection and the production wells. The maximum gravity change is 31 ± 8 μGal. On the contrary, we do not detect any similar signal for the Rittershoffen network. A simplistic model using two spherical sources located at 5 and 2 km for Soultz-sous-Forêts and Rittershoffen sites respectively shows negligeable surface gravity changes when taking into account the known injection and production flow rates.
Published: 2018
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21. Low-level control software for the WEAVE spectrograph

Author: Salasnich, Bernardo, Martín Perez, Carlos, Delgado Hernández, José Miguel, Picó, Sergio, Cano Infantes, Diego, Baruffolo, Andrea, Stuik, Remko, Dalton, Gavin, Trager, Scott, L. Aguerri, J. Alfonso, Bonifacio, Piercarlo, Vallenari, Antonella, Carrasco, Esperanza, Abrams, Carlos, Middleton, Kevin, Guzmán, Juan, Ibsen, Jorge, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Cosmological Impact of the FIrst STars (CIFIST), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centro Geofísico de Canarias, Instituto Geografico Nacional, Joint ALMA Observatory (JAO), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), ITA, GBR, ESP, NLD, Astronomy, and Bonifacio, Piercarlo
Subjects: Software suite, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Computer science, Interface (computing), Process (computing), 02 engineering and technology, First light, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 021001 nanoscience & nanotechnology, 01 natural sciences, 010309 optics, Embedded software, Software, 0103 physical sciences, 0210 nano-technology, business, Software architecture, Spectrograph, Computer hardware, ComputingMilieux_MISCELLANEOUS
Abstract: WEAVE is a wide-field spectroscopy facility for WHT which includes a multi-object dual-beam spectrograph which will operate in the visible wavelength range. The blue beam will cover the range 360-600 nm and the red arm will cover the 580-960 nm range. In these ranges the spectrograph will offer a mid-resolution (~5000), while in three narrower wavelength intervals, two for the blue arm and one for the red one, the instrument will provide a high (~20000) spectrograph resolution. The spectrograph is currently entering the assembly and integration phase and the first light is foreseen in 2019. The entire WEAVE project is managed by an international consortium led by the University of Oxford. The spectrograph is controlled by a coordination process, the so called High-Level Server, which is part of the Observatory Control System (OCS) software suite, and is the single point of access to the embedded control system, the so called Low-Level Control Software, which is based on PAC technology. This paper describes the design of the embedded software for the control of the spectrograph mechanisms. We first describe the interface between high and low level software, then we present the PAC architecture and discuss the low-level state machine. Finally, we provide details on the principal program routines and describe the engineering interface.
Published: 2018

22. Molecular line emission in NGC 4945, imaged with ALMA

Author: Konrad R. W. Tristram, F. Kamali, Felipe O. Alves, Santiago García-Burillo, E. Alkhuja, Ralf S. Klessen, Jenny E. Greene, Francoise Combes, S. Viti, Y. Ao, P. van der Werf, S. Mühle, A. Malawi, C. M. V. Impellizzeri, Sebastien Muller, George J. Bendo, Juergen Ott, Meirong Wang, H. A. Ismail, Jeffrey G. Mangum, Yungui Gong, Gyula I. G. Józsa, Jiangshui Zhang, Francesco Costagliola, Willem A. Baan, Gary A. Fuller, Xindi Tang, R. Mauersberger, Susanne Aalto, Sergio Martín, H. Asiri, L. K. Hunt, Rebeca Aladro, Christian Henkel, Inst Phys, Universität Potsdam, University of Manchester [Manchester], Rhodes University, Grahamstown, Lab of Advanced Manufacturing and Automation, Northeastern University [Boston], Chalmers University of Technology [Göteborg], Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), National Radio Astronomy Observatory [Charlottesville] (NRAO), National Radio Astronomy Observatory (NRAO), Laboratoire de Biophotonique et Pharmacologie - UMR 7213 (LBP), Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Max-Planck-Institut für Radioastronomie (MPIFR), Jodrell Bank Centre for Astrophysics (JBCA), and DEU
Subjects: Nuclear reaction, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Position angle, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Spectral line, law.invention, Space and Planetary Science, law, Nucleosynthesis, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Isotopologue, Maser, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Galaxy rotation curve, ComputingMilieux_MISCELLANEOUS
Abstract: NGC 4945 is one of the nearest (~3.8 Mpc; 1" ~ 19 pc) starburst galaxies. ALMA band 3 (3--4\,mm) observations of HCN, HCO+, CS, C3H2, SiO, HCO, and CH3C2H were carried out with ~2" resolution. The lines reveal a rotating nuclear disk of projected size 10" x 2" with position angle ~45 deg, inclination ~75 deg and an unresolved bright central core of size, 31 pages, 29 figures, 6 tables, accepted for publication in A&A; for the draft showing figures with full resolution, see https://gongyan2444.github.io/pdf/Henkel-NGC4945.pdf
Published: 2018
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23. The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution:The Absence of Large Clumps in the Interstellar Medium at High-redshift

Author: Novak, Mladen, Sargent, Mark, Herrera-Camus, R., Belli, S., Übler, H., Shimizu, T., Davies, R., Sturm, E., Colina, L., Cunha, E. da, Rybak, M., Venemans, B., Brandt, W., Rivera, G. Calistro, Knudsen, K., Werf, P. van der, Freundlich, J., Combes, F., Tacconi, L., Genzel, R., Garcia-Burillo, S., Bolatto, A., Lilly, S., Salomé, P., Bicalho, I., Boissier, J., Boone, F., Bouché, N., Bournaud, F., Burkert, A., Carollo, M., Cooper, M., Feruglio, C., Förster Schreiber, N., Juneau, S., Lippa, M., Lutz, D., Naab, T., Renzini, A., Saintonge, A., Sternberg, A., Weiner, B., Weiß, A., Wuyts, S., Bouwens, Rychard, Brinchmann, Jarle, Maseda, Michael, Matthee, Jorryt, Schaye, Joop, Schouws, Sander, Pavesi, Riccardo, Le Fèvre, Olivier, Yang, C., Gavazzi, R., Beelen, A., Lehnert, M., Gao, Y., Barcos-Muñoz, L., Neri, R., Fu, H., González-Alfonso, E., Michałowski, M., Nightingale, J., Pérez-Fournon, I., Shao, Yali, Wang, Ran, Li, Jianan, Fan, Xiaohui, Jiang, Linhua, Strauss, Michael, Menten, Karl, Ma, Jingzhe, Cooray, Asantha, Nayyeri, Hooshang, Brown, Arianna, Ghotbi, Noah, Oteo, Ivan, Duivenvoorden, Steven, Greenslade, Joshua, Clements, David, Battisti, Andrew, Ashby, Matthew, Perez-Fournon, Ismael, Oliver, Seb, Eales, Stephen, Negrello, Mattia, Dye, Simon, Dunne, Loretta, Omont, Alain, Serjeant, Stephen, Maddox, Steve, Valiante, Elisabetta, Pillepich, Annalisa, Nelson, Dylan, Cunha, Elisabete da, Diemer, Benedikt, González-López, Jorge, Hernquist, Lars, Marinacci, Federico, Rix, Hans-Walter, Swinbank, Mark, Vogelsberger, Mark, Werf, Paul van der, Yung, L., Aravena, Manuel, Decarli, Roberto, Gónzalez-López, Jorge, Boogaard, Leindert, Carilli, Chris, Popping, Gergö, Assef, Roberto, Bacon, Roland, Bauer, Franz Erik, Bouwens, Richard, Contini, Thierry, Cortes, Paulo, Da Cunha, Elisabete, Daddi, Emanuele, Díaz-Santos, Tanio, Elbaz, David, Inami, Hanae, Fevre, Olivier Le, Magnelli, Benjamin, Oesch, Pascal, Riechers, Dominik, Somerville, Rachel, Uzgil, Bade, Wagg, Jeff, Wisotzki, Lutz, Gullberg, B., Swinbank, A. Mark, Smail, Ian, Biggs, A., Bertoldi, Frank, Breuck, C. De, Chapman, S., Chen, Chian-Chou, Cooke, E., Coppin, K., Cox, Pierre, Dannerbauer, H., Dunlop, J., Edge, A., Farrah, D., Geach, J., GREVE, T., Hodge, Jacqueline, Ibar, E., Ivison, Rob, Karim, A., Schinnerer, E., Scott, Douglas, Simpson, J., Stach, S., Thomson, A., Van Der Werf, Paul, Walter, Fabian, Wardlow, Julie, Weiss, Axel, 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), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Department of Physics, Durham University, Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, AUTRES, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Interactions Hôtes-Pathogènes-Environnements (IHPE), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Perpignan Via Domitia (UPVD), Institut Interdisciplinaire d'Innovation Technologique (3IT), Université de Sherbrooke [Sherbrooke], Universitätssternwarte der Ludwig-Maximiliansuniversität, Ludwig-Maximiliansuniversität, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), University of São Paulo, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Steward observatory, University of Arizona, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut of Physics - Riga, Latvian Academy of Sciences, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Guangzhou Marine Geological Survey, Ministry of Land and Resources (MLR), Physics Department [Santa Barbara], University of California [Santa Barbara] (UCSB), University of California-University of California, 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL), Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Universidad de Alcalá - University of Alcalá (UAH), Instituto de Astrofisica de Canarias (IAC), Institute of Plant and Environment Protection, Beijing Academy of Agriculture and Forestry Sciences, Arizona State University [Tempe] (ASU), Max-Planck-Institut für Radioastronomie (MPIFR), California Institute of Technology (CALTECH), Astronomy Centre, University of Sussex, University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires de Marseille (ISM2), Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Max-Planck-Institut für Astronomie (MPIA), Institute for Computational Cosmology (ICC), National Radio Astronomy Observatory [Socorro] (NRAO), National Radio Astronomy Observatory (NRAO), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Yale Center for Astronomy and Astrophysics (YCAA), Yale University [New Haven], Cornell University, Rutgers University, Astrophysikalisches Institut Potsdam (AIP), Institute of Computational Cosmology, Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Université de Lyon, SUPA, Institute for Astronomy, University of Edinburgh, University of Wales, Department of Physics [Blacksburg], Virginia Tech [Blacksburg], Space Plasma Group, Astronomy Unit [London] (AU), Queen Mary University of London (QMUL)-Queen Mary University of London (QMUL), Royal Observatory Edinburgh (ROE), Interactions et dynamique des environnements de surface (IDES), CLRC Daresbury, SFTC, Centre de Recherches sur la Cognition Animale (CRCA), Institut des sciences du cerveau de Toulouse. (ISCT), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Pacific Northwest National Laboratory (PNNL), Department of Astronomy, University of California [Irvine] (UCI), Centre de Biologie Intégrative (CBI), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut des sciences du cerveau de Toulouse. (ISCT), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse - Jean Jaurès (UT2J)-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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 de Perpignan Via Domitia (UPVD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, galaxies [submillimeter], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, evolution [galaxies], Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM [galaxies], 010308 nuclear & particles physics, Resolution (electron density), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Interstellar medium, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Millimeter, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present deep high resolution (0.03", 200pc) ALMA Band 7 observations covering the dust continuum and [CII] $\lambda157.7\mu$m emission in four $z\sim4.4-4.8$ sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160$\mu$m (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS47.0, displays apparent substructure but this is also consistent with a smooth morphology, as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at high angular resolution (0.03") and depth of these observations ($\sigma_{345\text{GHz}} \sim27-47\mu$Jy beam$^{-1}$). The four SMGs are bright [CII] emitters, and we extract [CII] spectra from the high resolution data, and recover $\sim20-100$% of the [CII] flux and $\sim40-80$% of the dust continuum emission, compared to the previous lower resolution observations. When tapered to 0.2" resolution our maps recover $\sim80-100$% of the continuum emission, indicating that $\sim60$% of the emission is resolved out on $\sim200$pc scales. We find that the [CII] emission in high-redshift galaxies is more spatially extended than the rest-frame 160$\mu$m dust continuum by a factor of $1.6\pm0.4$. By considering the $L_{\text{[CII]}}$/$L_{\text{FIR}}$ ratio as a function of the star-formation rate surface density ($\Sigma_{\text{SFR}}$) we revisit the [CII] deficit, and suggest that the decline in the $L_{\text{[CII]}}$/$L_{\text{FIR}}$ ratio as a function of $\Sigma_{\text{SFR}}$ is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs., Comment: 15 pages, 6 figures, 4 tables, accepted for publication in ApJ
Published: 2018
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24. Gas phase Elemental abundances in Molecular cloudS (GEMS) I. The prototypical dark cloud TMC 1

Author: Jean-Christophe Loison, Valerio Lattanzi, Nuria Marcelino, Stéphanie Cazaux, Maryvonne Gerin, Rafael Bachiller, Javier R. Goicoechea, S. P. Treviño-Morales, Paola Caselli, T. Alonso-Albi, C. Kramer, Santiago García-Burillo, Benoît Commerçon, Barbara M. Giuliano, Rafael Martín-Doménech, Belén Tercero, M. Y. Ballester, D. G. Navarro, Alvaro Hacar, Derek Ward-Thompson, Johanna Malinen, Jaime E. Pineda, Asunción Fuente, G. Muñoz-Caro, Izaskun Jiménez-Serra, Pablo Riviere-Marichalar, Jason M. Kirk, Octavio Roncero, Mario Tafalla, E. Roueff, Rachel Friesen, Thomas H. G. Vidal, Pierre Gratier, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AMOR 2019, 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), Observatorio Astronomico Nacional, Madrid, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Radioastronomie, Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Queen Mary University of London (QMUL), 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), INAF - Osservatorio Astronomico di Bologna (OABO), Laboratoire de Radiopathologie (LRP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de la Santé et de la Recherche Médicale (INSERM), foreign laboratories (FL), CERN [Genève], Instituto de Ciencia de Materiales de Madrid (ICMM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Instituto de Radio Astronomía Milimétrica, Departamento de Astrofisica [Madrid], Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Spanish National Research Council (CSIC), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Ministerio de Economía y Competitividad (España), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Laboratoire Univers et Théories (LUTH (UMR_8102)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronómico Nacional (OAN), oan, Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Ctr Astrobiol CSIC INTA, Lab Astofis Mol, Madrid 28850, Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS), Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de la Santé et de la Recherche Médicale (INSERM), Instituto de Ciencia de Materiales de Madrid (ICMM-CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Physics, Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), and Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics, 01 natural sciences, ISM: abundances, Protein filament, Ionization, Phase (matter), Astronomy, Astrophysics and Cosmology, low-mass [stars], TAURUS, 010303 astronomy & astrophysics, Astrochemistry, abundances [ISM], Physics, [PHYS]Physics [physics], astrochemistry, DIFFUSE CLOUDS, ISM: molecules, Meteorology and Atmospheric Sciences, IONIZATION, ROTATIONAL-EXCITATION, Stars: formation, SULFUR, FOS: Physical sciences, Article, IRAM 30m telescope, STAR-FORMATION, CO DEPLETION, 0103 physical sciences, Stars: low-mass, POTENTIAL-ENERGY SURFACE, molecules [ISM], ISM: kinematics and dynamics, formation [stars], 010308 nuclear & particles physics, Star formation, COMPARATIVE CHEMISTRY, Molecular cloud, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, kinematics and dynamics [ISM], Geochemistry, INTERSTELLAR GAS, Cover (topology), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 26 pags., 7 figs., 2 tabs., 2 apps., GEMS is an IRAM 30 m Large Program whose aim is determining the elemental depletions and the ionization fraction in a set of prototypical star-forming regions. This paper presents the first results from the prototypical dark cloud Taurus molecular cloud (TMC) 1. Extensive millimeter observations have been carried out with the IRAM 30 m telescope (3 and 2 mm) and the 40 m Yebes telescope (1.3 cm and 7 mm) to determine the fractional abundances of CO, HCO, HCN, CS, SO, HCS, and N H in three cuts which intersect the dense filament at the well-known positions TMC 1-CP, TMC 1-NH3, and TMC 1-C, covering a visual extinction range from A ~ 3 to ~20 mag. Two phases with differentiated chemistry can be distinguished: (i) the translucent envelope with molecular hydrogen densities of 1-5 × 10 cm; and (ii) the dense phase, located at A > 10 mag, with molecular hydrogen densities >10 cm. Observations and modeling show that the gas phase abundances of C and O progressively decrease along the C/C/CO transition zone (A~ 3 mag) where C/H ~ 8 × 10 and C/O ~ 0.8-1, until the beginning of the dense phase at A ~ 10 mag. This is consistent with the grain temperatures being below the CO evaporation temperature in this region. In the case of sulfur, a strong depletion should occur before the translucent phase where we estimate an S/ H ~ (0.4-2.2) × 10, an abundance ~7-40 times lower than the solar value. A second strong depletion must be present during the formation of the thick icy mantles to achieve the values of S/H measured in the dense cold cores (S H ~ 8 × 10) . Based on our chemical modeling, we constrain the value of ζ to ~(0.5-1.8) × 10 s in the translucent cloud., We thank the Spanish MINECO for funding support from AYA2016-75066-C2-1/2-P, and the ERC under ERC-2013-SyG, G. A. 610256 NANOCOSMOS. JM acknowledges the support of ERC-2015-STG No. 679852 RADFEEDBACK. SPTM acknowledges to the European Union’s Horizon 2020 research and innovation program for funding support given under grant agreement No 639459 (PROMISE). RMD acknowledges support provided by an award from the Simons Foundation (SCOL#321183, KO). GMC acknowedges funding support fromAYA2017-85322-R. MT acknowledges partial support from project AYA2016-79006-P.”
Published: 2018
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25. Laboratory measurements and astronomical search for cyanomethanimine

Author: Rafael Bachiller, Luca Dore, Alessio Melli, Vincenzo Barone, Mattia Melosso, Cecilia Ceccarelli, Lorenzo Spada, Cristina Puzzarini, Claudio Codella, José Cernicharo, Bertrand Lefloch, C. Degli Esposti, Melosso, M., Melli, A., Puzzarini, C., Codella, C., Spada, L., Dore, L., Degli Esposti, C., Lefloch, B., Bachiller, R., Ceccarelli, C., Cernicharo, J., Barone, V., Codella, Claudio, Dipartimento di Chimica 'Giacomo Ciamician', Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), 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 Grenoble Alpes [2016-2019] (UGA [2016-2019])-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)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Edinburgh Napier University, Dipartimento di Chimica 'G. Ciamician', Instituto Geografico Nacional (IGN), Istituto Nazionale di Astrofisica (INAF), Instituto de Ciencia de Materiales de Madrid (ICMM), and Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)
Subjects: 010504 meteorology & atmospheric sciences, Methods: laboratory: molecular, laboratory: molecular [Methods], FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: molecule, 01 natural sciences, Article, 0103 physical sciences, Astronomical interferometer, Sagittarius B2, molecule [ISM], Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Spectrometer, Star formation, Molecular data, Astronomy and Astrophysics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, methods: data analysis, ISM: molecules, 3. Good health, data analysi [Methods], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Antenna (radio), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Radio wave, Methods: data analysi
Abstract: C-cyanomethanimine (HNCHCN), existing in the two $Z$ and $E$ isomeric forms, is a key prebiotic molecule, but, so far, only the $E$ isomer has been detected toward the massive star-forming region. Sagittarius B2(N) using transitions in the radio wavelength domain. With the aim of detecting HNCHCN in Sun-like-star forming regions, the laboratory investigation of its rotational spectrum has been extended to the millimeter-/submillimeter-wave (mm-/submm-) spectral window in which several unbiased spectral surveys have been already carried out. High-resolution laboratory measurements of the rotational spectrum of C-cyanomethanimine were carried out in the 100-420 GHz range using a frequency-modulation absorption spectrometer. We then searched for the C-cyanomethanimine spectral features in the mm-wave range using the high-sensitivity and unbiased spectral surveys obtained with the IRAM 30-m antenna in the ASAI context, the earliest stages of star formation from starless to evolved Class I objects being sampled. For both the $Z$ and $E$ isomers, the spectroscopic work has led to an improved and extended knowledge of the spectroscopic parameters, thus providing accurate predictions of the rotational signatures up to $\sim$700 GHz. So far, no C-cyanomethanimine emission has been detected toward the ASAI targets, and upper limits of the column density of $\sim$ 10$^{11}$--10$^{12}$ cm$^{-2}$ could only be derived. Consequently, the C-cyanomethanimine abundances have to be less than a few 10$^{-10}$ for starless and hot-corinos. A less stringent constraint, $\leq$ 10$^{-9}$, is obtained for shocks sites. The combination of the upper limits of the abundances of C-cyanomethanimine together with accurate laboratory frequencies up to $\sim$ 700 GHz poses the basis for future higher sensitivity searches around Sun-like-star forming regions., 9 pages, 4 figures, 2 tables. A&A accepted
Published: 2018
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26. Spatio-temporal patterns and environmental controls of small pelagic fish body condition from contrasted Mediterranean areas

Author: Isabel Palomera, Pablo Brosset, Ana Giráldez, Gualtiero Basilone, Angelo Bonanno, Pedro Torres, Ali Cemal Gücü, Andrea De Felice, Vanja Čikeš Keč, Magdalena Iglesias, Jean-Marc Fromentin, Frédéric Ménard, Barbara Zorica, Piera Carpi, Iole Leonori, Josep Lloret, Virginie Marques, Claire Saraux, Rosalia Ferreri, Vjekoslav Tičina, Elisabeth Van Beveren, Stylianos Somarakis, Ana Ventero, Denis Gašparević, Fortunata Donato, MARine Biodiversity Exploitation and Conservation (UMR MARBEC), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Department of environmental sciences, Universitat de Girona (UdG), Department of Biology University of Crete, University of Crete [Heraklion] (UOC), Centro Geofísico de Canarias, Instituto Geografico Nacional, Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN), Ministère de l’Enseignement supérieur et de la Recherche (France), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut de Recherche pour le Développement (IRD), and Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 0106 biological sciences, Mediterranean climate, 010504 meteorology & atmospheric sciences, Fishing, Fish health, Marine monitoring, Aquatic Science, Anchovy, Sardine, 01 natural sciences, Pelagic fish, Anchovy, Sardine, Fish health, Marine monitoring, Centro Oceanográfico de Baleares, Mediterranean sea, Regime shift, 14. Life underwater, Pesquerías, 0105 earth and related environmental sciences, [SDV.EE]Life Sciences [q-bio]/Ecology, environment, Biomass (ecology), biology, Ecology, 010604 marine biology & hydrobiology, Geology, Pelagic zone, biology.organism_classification, Fishery, Oceanography, Geography
Abstract: Brosset, Pablo ... et al.-- 14 pages, 7 figures, 2 tables, Small pelagic fish are among the most ecologically and economically important marine fish species and are characterized by large fluctuations all over the world. In the Mediterranean Sea, low catches and biomass of anchovies and sardines have been described in some areas during the last decade, resulting in important fisheries crises. Therefore, we studied anchovy and sardine body condition variability, a key index of population health and its response to environmental and anthropogenic changes. Wide temporal and spatial patterns were investigated by analyzing separately data from scientific surveys and fisheries in eight Mediterranean areas between 1975 and 2015. Results showed that anchovy and sardine body condition as well as maximum size in some areas sharply decreased in most Mediterranean areas along years (except in the Northern Alboran Sea). Despite this general pattern, well-marked environmental differences between sub-regions were highlighted by several analyses and variations in body condition were not found to be homogeneous over all the Mediterranean Sea. Further, other analyses revealed that except for the Adriatic where major changes towards a lower body condition were concomitant with a decrease in river runoffs and chl-a concentration, no concomitant environmental regime shift was detected in other areas. Together, these analyses highlighted the current poor body condition of almost all small pelagic fish populations in the Mediterranean. Yet, global environmental indices could not explain the observed changes and the general decrease in condition might more likely come from regional environmental and/or anthropogenic (fishing) effects. A prolonged state of poor fish body condition, together with an observed reduced size and early age-at-maturity may have strong ecological, economic and social consequences all around the Mediterranean Sea., PB acknowledges doctoral fellowship support from the French Ministère de l’Education Nationale, de la Recherche et de la Technologie
Published: 2017
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27. Optical depth estimates and effective critical densities of dense gas tracers in the inner parts of nearby galaxy discs

Author: A. Usero, Molly J. Gallagher, Alberto D. Bolatto, Andreas Schruba, Mark R. Krumholz, Dario Colombo, David S. Meier, M. J. Jimenez-Donaire, Annie Hughes, Laura K. Zschaechner, J. Pety, Diane Cormier, Neven Tomičić, C. Kramer, Erik Rosolowsky, Frank Bigiel, Eric J. Murphy, Santiago García-Burillo, Eva Schinnerer, Adam K. Leroy, Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Observatorio Astronómico Nacional (OAN), oan, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), 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), University of British Columbia (UBC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Universität Heidelberg [Heidelberg] = Heidelberg University, Observatorio Astronomico Nacional, Madrid, and École normale supérieure - Paris (ENS-PSL)
Subjects: Physics, [PHYS]Physics [physics], Effective density, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, High density, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Optical depth (astrophysics), Isotopologue, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Line (formation)
Abstract: High critical density molecular lines like HCN(1-0) or HCO+(1-0) represent our best tool to study currently star-forming, dense molecular gas at extragalactic distances. The optical depth of these lines is a key ingredient to estimate the effective density required to excite emission. However, constraints on this quantity are even scarcer in the literature than measurements of the high density tracers themselves. Here, we combine new observations of HCN, HCO+ and HNC(1-0) and their optically thin isotopologues H13CN, H13CO+ and HN13C(1-0) to measure isotopologue line ratios. We use IRAM 30-m observations from the large program EMPIRE and new ALMA observations, which together target 6 nearby star-forming galaxies. Using spectral stacking techniques, we calculate or place strong upper limits on the HCN/H13CN, HCO+/H13CO+ and HNC/HN13C line ratios in the inner parts of these galaxies. Under simple assumptions, we use these to estimate the optical depths of HCN(1-0) and HCO+(1-0) to be \tau ~2-11 in the active, inner regions of our targets. The critical densities are consequently lowered to values between 5-20$\times 10^5$, 1-3$\times 10^5$ and 9$\times 10^4$ cm-3 for HCN, HCO+ and HNC, respectively. We study the impact of having different beam-filling factors, $\eta$, on these estimates and find that the effective critical densities decrease by a factor of $\frac{\eta_{12}}{\eta_{13}}\,\tau_{12}$. A comparison to existing work in NGC 5194 and NGC 253 shows HCN/H13CN and HCO+/H13CO+ ratios in agreement with our measurements within the uncertainties. The same is true for studies in other environments such as the Galactic Centre or nuclear regions of AGN-dominated nearby galaxies., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society
Published: 2017
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28. Méthodes de traitement de données lidar

Author: Mallet, Clément, CHEHATA, Nesrine, Bailly, Jean-Stéphane, Méthodes d'Analyses pour le Traitement d'Images et la Stéréorestitution (MATIS), Laboratoire des Sciences et Technologies de l'Information Géographique (LaSTIG), École nationale des sciences géographiques (ENSG), Institut National de l'Information Géographique et Forestière [IGN] (IGN)-Institut National de l'Information Géographique et Forestière [IGN] (IGN)-École nationale des sciences géographiques (ENSG), Institut National de l'Information Géographique et Forestière [IGN] (IGN)-Institut National de l'Information Géographique et Forestière [IGN] (IGN), Instituto Geografico Nacional (IGN), Institut Polytechnique de Bordeaux (Bordeaux INP), AgroParisTech, Laboratoire d'étude des Interactions Sol - Agrosystème - Hydrosystème (UMR LISAH), Institut de Recherche pour le Développement (IRD)-Institut de Recherche pour le Développement (IRD [ Madagascar])-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro)-Institut National de la Recherche Agronomique (INRA)-Centre international d'études supérieures en sciences agronomiques (Montpellier SupAgro), Baghdadi, Nicolas and Zribi, Mehrez, André Mariotti, Institut de Recherche pour le Développement (IRD)-Institut National de la Recherche Agronomique (INRA)-Centre international d'études supérieures en sciences agronomiques (Montpellier SupAgro)-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), 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)
Subjects: trains d'ondes, [STAT.AP]Statistics [stat]/Applications [stat.AP], [STAT.ML]Statistics [stat]/Machine Learning [stat.ML], [SDE.MCG]Environmental Sciences/Global Changes, nuages de points 3D, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, lidar, traitement
Abstract: International audience; Les données lidar brutes sont soit des signaux temporels appelésforme d'onde complète, soit des nuages de points 3D, de forte qualitéaltimétrique. Elles sont acquises par des capteurs géospatiaux et terrestres, avecune seule longueur d'onde, même si les capteurs multi-spectraux fontleur apparition. Les capteurs lidar permettent d'acquérir des données sous couvertforestier en particulier grâce à la séparabilité du faisceau lidarengendrant des rétrodiffusions multiples, nommées échos, pour unemême impulsion laser. Des traitements sont nécessaires sur les formes d'onde lidar pourobtenir les informations de distance entre les cibles atteintes et lecapteur et dériver des nuages de points 3D. Une information d'énergie rétrodiffusée est souvent disponible ensupplément de la position 3D, du numéro et du nombre d'écho. La plupart des techniques d'analyse de données de télédétection(segmentation, reconnaissance de formes, classification) s'appliquentaux données lidar, en 3 dimensions, en intégrant des attributsgéométriques relatifs aux cibles atteintes. La densité de mesures contingente les applications relatives autraitement de données lidar : l'échantillonnage plus ou moins fort dela surface terrestre ne permet pas de détecter ni reconnaître tous lesobjets qui la composent.
Published: 2017

29. Physical conditions of the molecular gas in metal-poor galaxies

Author: Leonardo Testi, Carsten Henkel, Axel Weiß, L. K. Hunt, Andreas Lundgren, Santiago García-Burillo, Karl M. Menten, Viviana Casasola, Roberto Maiolino, Paola Caselli, Francoise Combes, Hunt, LK [0000-0001-9162-2371], Apollo - University of Cambridge Repository, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Institut für Physik (Institut für Physik), Universität Potsdam, 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), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Max-Planck-Institut für Radioastronomie (MPIFR), European Southern Observatory (ESO), ITA, University of Potsdam = Universität Potsdam, École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, and Observatorio Astronomico Nacional, Madrid
Subjects: Mean kinetic temperature, FOS: Physical sciences, galaxies: starburst, Astrophysics, 01 natural sciences, chemistry.chemical_compound, 0103 physical sciences, Isotopologue, 010303 astronomy & astrophysics, [PHYS]Physics [physics], Physics, radio lines: ISM, 010308 nuclear & particles physics, Galactic Center, Astronomy and Astrophysics, galaxies: dwarf, Astrophysics - Astrophysics of Galaxies, Galaxy, ISM: molecules, 3. Good health, Interstellar medium, Stars, chemistry, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Atomic carbon, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Carbon monoxide
Abstract: Studying the molecular component of the interstellar medium in metal-poor galaxies has been challenging because of the faintness of carbon monoxide emission, the most common proxy of H2. Here we present new detections of molecular gas at low metallicities, and assess the physical conditions in the gas through various CO transitions for 8 galaxies. For one, NGC 1140 (Z/Zsun ~ 0.3), two detections of 13CO isotopologues and atomic carbon, [CI](1-0), and an upper limit for HCN(1-0) are also reported. After correcting to a common beam size, we compared 12CO(2-1)/12CO(1-0) (R21) and 12CO(3-2)/12CO(1-0) (R31) line ratios of our sample with galaxies from the literature and find that only NGC 1140 shows extreme values (R21 ~ R31 ~ 2). Fitting physical models to the 12CO and 13CO emission in NGC 1140 suggests that the molecular gas is cool (kinetic temperature Tkin= $10^6$ cm$^{-3}$), with moderate CO column density (NCO ~ $10^{16}$ cm$^{-2}$) and low filling factor. Surprisingly, the [12CO]/[13CO] abundance ratio in NGC 1140 is very low (~ 8-20), lower even than the value of 24 found in the Galactic Center. The young age of the starburst in NGC 1140 precludes 13C enrichment from evolved intermediate-mass stars; instead we attribute the low ratio to charge-exchange reactions and fractionation, because of the enhanced efficiency of these processes in cool gas at moderate column densities. Fitting physical models to 12CO and [CI](1-0) emission in NGC 1140 gives an unusually low [12CO]/[12C] abundance ratio, suggesting that in this galaxy atomic carbon is at least 10 times more abundant than 12CO., 26 pages, 21 figures, 2 appendices, A&A, in press
Published: 2017
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30. Earth's core and inner-core resonances from analysis of VLBI nutation and superconducting gravimeter data

Author: Sébastien Lambert, C. Gattano, Séverine Rosat, Marta Calvo, Dynamique globale et déformation active (IPGS) (IPGS-DGDA), Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Systèmes de Référence Temps Espace (SYRTE), 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 Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatorio Geofisico Central, Instituto Geografico Nacional, Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Gravity (chemistry), 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Monte Carlo method, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], Tidal Waves, 010502 geochemistry & geophysics, 01 natural sciences, Physics::Geophysics, outer core and inner core, Geochemistry and Petrology, Very-long-baseline interferometry, 0105 earth and related environmental sciences, Physics, Gravimeter, Nutation, Inner core, Geophysics, Surface gravity, Geodesy, Probability distributions, 13. Climate action, Physics::Space Physics, Time variable gravity, Astrophysics::Earth and Planetary Astrophysics, Core, Earth rotation variations
Abstract: Geophysical parameters of the deep Earth’s interior can be evaluated through the resonance effects associated with the core and inner-core wobbles on the forced nutations of the Earth’s figure axis, as observed by very long baseline interferometry (VLBI), or on the diurnal tidal waves, retrieved from the time-varying surface gravity recorded by superconducting gravime- ters (SGs). In this paper, we inverse for the rotational mode parameters from both techniques to retrieve geophysical parameters of the deep Earth. We analyse surface gravity data from 15 SG stations and VLBI delays accumulated over the last 35 yr. We show existing correlations between several basic Earth parameters and then decide to inverse for the rotational modes parameters. We employ a Bayesian inversion based on the Metropolis-Hastings algorithm with a Markov-chain Monte Carlo method. We obtain estimates of the free core nutation resonant period and quality factor that are consistent for both techniques. We also attempt an inversion for the free inner-core nutation (FICN) resonant period from gravity data. The most probable solution gives a period close to the annual prograde term (or S1 tide). However the 95 per cent confidence interval extends the possible values between roughly 28 and 725 d for gravity, and from 362 to 414 d from nutation data, depending on the prior bounds. The precisions of the estimated long-period nutation and respective small diurnal tidal constituents are hence not accurate enough for a correct determination of the FICN complex frequency.
Published: 2017
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31. Single-dish and VLBI observations of Cygnus X-3 during the 2016 giant flare episode

Author: M. Buttu, Simona Righini, Paweł Wolak, S. Buttaccio, Andrea Orlati, T. M. Belloni, Victoria Grinberg, Emrah Kalemci, Raimondo Concu, Jörn Wilms, Andrea Melis, Marcin P. Gawronski, C. Stanghellini, Alessandro Navarrini, E. Egron, Jerome Rodriguez, Giuseppe Maccaferri, M. Marongiu, P. de Vicente, Carlo Migoni, Matteo Bachetti, G. P. Vargiu, Marcello Giroletti, M. Cadolle Bel, S. Loru, A. Pellizzoni, Jun Yang, Stephane Corbel, Sera Markoff, Katja Pottschmidt, P. Cassaro, Maura Pilia, Alessio Trois, Matteo Stagni, L. Barbas, Michael Lindqvist, M. N. Iacolina, High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -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), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-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), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), INAF-Cagliari Astronomical Observatory, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Observatorio de Yebes, Instituto Geografico Nacional (IGN), Torun Centre for Astronomy (TCfA), Nicolaus Copernicus University [Toruń], Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], School of Physics and Engineering Physics, Göteberg University and Chalmers University of Technology (CHALMERS), University of Technology-School of Physics and Engineering Physics, Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Center for Research and Exploration in Space Science and Technology [GSFC] (CRESST), NASA Goddard Space Flight Center (GSFC), Faculty of Engineering and Natural Sciences (Sabanci University), Sabanci University [Istanbul], European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), ANR-10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2010), ANR-11-IDEX-0005,USPC,Université Sorbonne Paris Cité(2011), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), ANR-10-LABX-0023,Labex UnivEarthS, and ANR-11-IDEX-0005-02/10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2011)
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, stars: jets, Radio telescope, X-rays: binaries, law, stars: individual: Cyg X-3, 0103 physical sciences, Very-long-baseline interferometry, 010306 general physics, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, Flare star, Astronomy, Astronomy and Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, QB460-466 Astrophysics, stars: individual: Cyg X-3 – radio continuum: stars, stars: flare, Radio frequency, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, radio continuum: stars, Flare
Abstract: In September 2016, the microquasar Cygnus X-3 underwent a giant radio flare, which was monitored for 6 days with the Medicina Radio Astronomical Station and the Sardinia Radio Telescope. Long observations were performed in order to follow the evolution of the flare on a hourly scale, covering six frequency ranges from 1.5 GHz to 25.6 GHz. The radio emission reached a maximum of 13.2 +/- 0.7 Jy at 7.2 GHz and 10 +/- 1 Jy at 18.6 GHz. Rapid flux variations were observed at high radio frequencies at the peak of the flare, together with rapid evolution of the spectral index: alpha steepened from 0.3 to 0.6 within 5 hours. This is the first time that such fast variations are observed, giving support to the evolution from optically thick to optically thin plasmons in expansion moving outward from the core. Based on the Italian network (Noto, Medicina and SRT) and extended to the European antennas (Torun, Yebes, Onsala), VLBI observations were triggered at 22 GHz on five different occasions, four times prior to the giant flare, and once during its decay phase. Flux variations of 2-hour duration were recorded during the first session. They correspond to a mini-flare that occurred close to the core ten days before the onset of the giant flare. From the latest VLBI observation we infer that four days after the flare peak the jet emission was extended over 30 mas., Comment: 13 pages, 9 figures. Accepted for publication in MNRAS
Published: 2017
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32. The first CO + image

Author: Treviño-Morales, S., Fuente, A., Sánchez-Monge, Á., Pilleri, P., Goicoechea, J., Ossenkopf-Okada, V., Roueff, E., Rizzo, J., Gerin, M., Berné, O., Cernicharo, J., González-García, M., Kramer, C., Garcia-Burillo, S., Pety, J., Instituto de Radio Astronomía Milimétrica, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Instituto de Ciencia de Materiales de Madrid (ICMM), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Institut de RadioAstronomie Millimétrique (IRAM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), 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), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Observatorio Astronomico Nacional, Madrid
Subjects: [PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2016
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33. A precessing molecular jet signaling an obscured, growing supermassive black hole in NGC 1377?

Author: Aaron S. Evans, P. van der Werf, Francesco Costagliola, Kalliopi Dasyra, Jari Kotilainen, Santiago García-Burillo, Francoise Combes, Keiichi Wada, Lars E. Kristensen, Kazushi Sakamoto, Sebastien Muller, Jay Gallagher, Susanne Aalto, Sergio Martín, Chalmers University of Technology [Göteborg], Immunologie et chimie thérapeutiques (ICT), Cancéropôle du Grand Est-Centre National de la Recherche Scientifique (CNRS), Institut de biologie et chimie des protéines [Lyon] (IBCP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), 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), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Danish Meat Research Institute (DMRI), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Aberystwyth University, 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), École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, Observatorio Astronomico Nacional, Madrid, Universiteit Leiden, 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Protostar, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Jet (fluid), Supermassive black hole, Accretion (meteorology), Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Galaxy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: With high resolution (0."25 x 0."18) ALMA CO 3-2 observations of the nearby (D=21 Mpc, 1"=102 pc), extremely radio-quiet galaxy NGC1377, we have discovered a high-velocity, very collimated nuclear outflow which we interpret as a molecular jet with a projected length of +-150 pc. Along the jet axis we find strong velocity reversals where the projected velocity swings from -150 km/s to +150 km/s. A simple model of a molecular jet precessing around an axis close to the plane of the sky can reproduce the observations. The velocity of the outflowing gas is difficult to constrain due to the velocity reversals but we estimate it to be between 240 and 850 km/s and the jet to precess with a period P=0.3-1.1 Myr. The CO emission is clumpy along the jet and the total molecular mass in the high-velocity (+-(60 to 150 km/s)) gas lies between 2e6 Msun (light jet) and 2e7 Msun (massive jet). There is also CO emission extending along the minor axis of NGC1377. It holds >40% of the flux in NGC1377 and may be a slower, wide-angle molecular outflow which is partially entrained by the molecular jet. We discuss the driving mechanism of the molecular jet and suggest that it is either powered by a very faint radio jet or by an accretion disk-wind similar to those found towards protostars. The nucleus of NGC1377 harbours intense embedded activity and we detect emission from vibrationally excited HCN J=4-3 v_2=1f which is consistent with hot gas and dust. We find large columns of H2 in the centre of NGC1377 which may be a sign of a high rate of recent gas infall. The dynamical age of the molecular jet is short (, This is a revised and expanded version of a previous submission which now has 13 pages, 6 figures (+ 4 in the Appendix) and is accepted for publication in Astronomy & Astrophysics
Published: 2016
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34. Alma resolves the Torus of NGC 1068: continuum and molecular line emission

Author: Isabel Márquez, Viviana Casasola, Asunción Fuente, Roberto Neri, Linda J. Tacconi, P. van der Werf, Francesco Costagliola, Francoise Combes, Almudena Alonso-Herrero, Melanie Krips, Andreas Eckart, Antonio Usero, Christian Henkel, S. Viti, C. Ramos Almeida, Luis Colina, Susanne Aalto, Santiago García-Burillo, Eva Schinnerer, Sergio Martín, Leslie K. Hunt, Ministerio de Economía y Competitividad (España), 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), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Observatorio Astronómico Nacional (OAN), oan, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Chalmers University of Technology [Göteborg], Istituto Nazionale di Astrofisica (INAF), Laboratoire de Biophotonique et Pharmacologie - UMR 7213 (LBP), Réseau nanophotonique et optique, Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Durham University, Max-Planck-Institut für Radioastronomie (MPIFR), Institut für Physik (Institut für Physik), Universität Potsdam, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Max Planck Institute for Extraterrestrial Physics (MPE), Observatorio Astronomico Nacional, Madrid, École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS), and University of Potsdam = Universität Potsdam
Subjects: Seyfert [Galaxies], Active galactic nucleus, Galaxies: Seyfert, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), Megamaser, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM [Galaxies], 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Galaxies: nuclei, Physics, [PHYS]Physics [physics], kinematics and dynamics [Galaxies], Galaxies: kinematics and dynamics, Astronomy and Astrophysics, Torus, Radius, Atacama Large Millimeter Array, Astrophysics - Astrophysics of Galaxies, Galaxy, Galaxies: ISM, Galaxies: individual (NGC 1068), Space and Planetary Science, nuclei [Galaxies], Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, individual (NGC 1068) [Galaxies], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Garcia-Burillo, S. et. al., We used the Atacama Large Millimeter Array (ALMA) to map the emission of the CO(6-5) molecular line and the 432 μm continuum emission from the 300 pc sized circumnuclear disk (CND) of the nearby Seyfert 2 galaxy NGC 1068 with a spatial resolution of ∼4 pc. These observations spatially resolve the CND and, for the first time, image the dust emission, the molecular gas distribution, and the kinematics from a 7-10 pc diameter disk that represents the submillimeter counterpart of the putative torus of NGC 1068. We fitted the nuclear spectral energy distribution of the torus using ALMA and near- and mid-infrared (NIR/MIR) data with CLUMPY torus models. The mass and radius of the best-fit solution for the torus are both consistent with the values derived from the ALMA data alone: and R torus = 3.5 ± 0.5 pc. The dynamics of the molecular gas in the torus show strong non-circular motions and enhanced turbulence superposed on a surprisingly slow rotation pattern of the disk. By contrast with the nearly edge-on orientation of the H2O megamaser disk, we found evidence suggesting that the molecular torus is less inclined (i = 34°-66°) at larger radii. The lopsided morphology and complex kinematics of the torus could be the signature of the Papaloizou-Pringle instability, long predicted to likely drive the dynamical evolution of active galactic nuclei tori. © 2016. The American Astronomical Society. All rights reserved., S.G.B., A.U., L.C., I.M., and A.F. acknowledge support from Spanish grants AYA2012-32295 and AYA2013-42227-P
Published: 2016
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35. Detailed Analysis of Diurnal Tides and Associated Space Nutation in the Search of the Free Inner Core Nutation Resonance

Author: Rosat, S., Calvo, M., Lambert, S. B., Dynamique globale et déformation active (IPGS) (IPGS-DGDA), Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatorio Geofisico Central, Instituto Geografico Nacional, Systèmes de Référence Temps Espace (SYRTE), 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 Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Rosat, Séverine
Subjects: [PHYS.PHYS.PHYS-GEO-PH] Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], Nutation, Physics::Space Physics, Free inner core nutation, Superconducting gravimeters, Diurnal tides, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], Astrophysics::Earth and Planetary Astrophysics, VLBI, Physics::Geophysics
Abstract: International audience; We propose a comparison of the tidal analysis results obtained from the continuous records of time-varying surface gravity collected by a worldwide network of Superconducting Gravimeters with the analysis results of space nutation observed by the international Very Long Baseline Interferometry (VLBI) network. The length of the surface gravity time series (20 years for the longest) enables now to look for additional diurnal tides that were previously not analyzed. In parallel, we now possess 35 years of VLBI data permitting to look for additional nutation terms. We focus our analysis on the diurnal prograde frequency band in the search for a possible resonance effect linked to the Free Inner Core Nutation. This Earth's normal mode has never been clearly observed. Its direct deformation effect at the Earth’s surface is theoretically predicted to be too small to be detected. However, the tidal forcing at a frequency close to its eigenfrequency could enhance some tidal or nutation amplitude resulting in the characterization of this mode through its resonance effect.
Published: 2016

36. Leveling and hybrid gravimetry monitoring applied to geothermal sites of Soultz-sous- Forêts and Rittershoffen, Rhine Graben, France

Author: Ferhat, G., Lopez-Barraza, M, Clédat, Emmanuel, Hinderer, J., Calvo Garcia-Maroto, Marta, Abdelfettah, Yassine, Hector, B, Riccardi, Umberto, Bernard, J.-D, Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Autonomous University of Sinaloa (UAS), Ecole Polytechnique Fédérale de Lausanne (EPFL), Dynamique globale et déformation active (IPGS) (IPGS-DGDA), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto Geografico Nacional (IGN), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Dipartimento di Scienze della Terra, and Università degli studi di Napoli Federico II
Subjects: hybrid, geothermy, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Leveling, deformation monitoring, gravimetry
Abstract: International audience; Here we report on some case histories of geodetic and gravity surveys for monitoring of geothermal sites. The monitoring of a geothermal reservoir by hybrid gravimetry combining different types of instruments (permanent superconducting gravimeter, absolute ballistic gravimeter and micro-gravimeters) is presented. A relative gravimetric network equipped with levelling benchmarks was designed and surveyed at annual frequencies (2013, 2014 and 2015 for gravity measurements, 2014 and 2015 for the levelling). Repetition of high precision relative gravity measurements on a network developed around a reference station, which is regularly measured with both relative and absolute gravimeters, leads to the knowledge of the time and space changes in surface gravity. The observed gravity changes can be linked to the natural or anthropic activities of the reservoir. A feasibility study using this methodology is applied to two geothermal sites of Soultz-sous-Forêts and Rittershoffen in the Alsace region (France) in the Rhine graben (Hinderer et al. 2015).
Published: 2016

37. Optical Remote Sensing in Urban Environments

Author: Arnaud Le Bris, Christiane Weber, Xavier Briottet, R. Oltra-Carrió, Nesrine Chehata, ONERA / DOTA, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Institut Polytechnique de Bordeaux (Bordeaux INP), University of València C/Catedràtic José Beltrán, Instituto Geografico Nacional (IGN), Territoires, Environnement, Télédétection et Information Spatiale (UMR TETIS), and Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad)-AgroParisTech-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Attractiveness, 010504 meteorology & atmospheric sciences, OPTICAL REMOTE SENSING, 0211 other engineering and technologies, Urban regeneration, 02 engineering and technology, URBANISME, CHARACTERISTICS, 01 natural sciences, REMOTE SENSING, [SPI]Engineering Sciences [physics], VHR, 11. Sustainability, URBAN SYSTEM, OPTICAL PROPERTIES, MAPPING AND PLANNING, Urban heat island, Environmental planning, 021101 geological & geomatics engineering, 0105 earth and related environmental sciences, Remote sensing, [PHYS]Physics [physics], ENVIRONMENT, BIODIVERSITE, 15. Life on land, URBAN HEAT ISLANDS, Variety (cybernetics), Geography, 13. Climate action, Remote sensing (archaeology), Urban system, VEGETATION
Abstract: International audience; Cities today face a variety of issues: attractiveness and economic development, living conditions and urban redevelopment, the quality of life of citizens and the environmental conditions of the urban system as a whole. These challenges reflect the situations in urban territories where the economic development and population growth required for stabilizing the urban system come into conflict with the promotion of esthetic urban improvements appropriate for social cohesion and ensuring the safety of users while guaranteeing a reduction of the environmental impact caused by urban spread [WGI 14, WEB 15, MAC 07, WIL 11]. The process of urbanization, which has significantly transformed our countryside over the last hundred years, was the most important factor of the 20th Century and saw the urban population surpass the rural population in the majority of Western countries. The process of urbanization can be defined as “particular forms and structures of space being occupied by the population [RHE 14]” – in other words the transformation of space (natural, agricultural, forest, etc.) through human activity. A recurrent problem is the objective demarcation of the urban system which is partly artificial and difficult to transpose from one case to another (conurbation, administrative boundaries, etc.). The determinants can vary in time and space (from one country to another1). In fact, identifying the place of study can sometimes get in the way of properly understanding the dynamics of urban growth and expansion, because like any other system, it is not exempt from external factors which in one way or another influence its internal dynamics. For instance, environmentally evaluating the quality of the water supply can be carried out at various locations in the urban system: where the water is extracted from, where it leaves the urban system and in the city center. The quality of the supply can only be determined based on sections that have been artificially developed. What renders the urban space so complex is that it only exists insofar as it is “built, worked and used through social ties” [CAS 72]. It can be thought of as a construction where the organization and the structure impact upon urban society but also as one element of a much wider ecosystem on which it depends and/or which it has an influence over. This system incorporates political, economic, social and, increasingly, environmental dimensions and we therefore regard it as a complex and heterogeneous ecosystem whose social, technical and natural components must be studied in order to understand the way in which it functions [MAT 06]. Taking these dimensions into account is necessary for urban studies, whether this is in terms of evaluating environments, modeling dynamics or outlining evolution scenarios. Over the past few years, the focus has been on gaining a better understanding of how the urban ecosystem works. This has taken place under the guise of different investigations: – a study focusing on the social, economic and spatial aspects of the urban system in order to consider the environmental aspect; – another study which focuses more on the interactions between the urban ecosystem as a whole and the natural systems on which it depends. This study examines both the fluctuations (energy resources, food, raw materials, etc.) and the state of these systems (the state of biodiversity, for example).
Published: 2016
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38. Hybrid Gravimetry as a Tool to Monitor Surface and Underground Mass Changes

Author: Basile Hector, Jacques Hinderer, Anthony Mémin, Marta Calvo, Dynamique globale et déformation active (IPGS) (IPGS-DGDA), Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'étude des transferts en hydrologie et environnement (LTHE), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), 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 Grenoble Alpes [2016-2019] (UGA [2016-2019])-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 Grenoble Alpes [2016-2019] (UGA [2016-2019]), Géoazur (GEOAZUR 7329), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Instituto Geografico Nacional (IGN), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), and Géoazur, Publications
Subjects: Gravity (chemistry), 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Gravimeter, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, 01 natural sciences, Glaciology, 13. Climate action, [SDU.STU] Sciences of the Universe [physics]/Earth Sciences, Environmental science, Gravimetry, Scale (map), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Remote sensing
Abstract: International audience; This paper is devoted to an overview of the use of hybrid gravimetry in Earth and Environmental Sciences. We first recall the concept of hybrid gravimetry which relies on the simultaneous use of different types of gravimeters either superconducting, absolute or relative spring gravimeters. This combination of instruments provides a complete tool for time-lapse gravimetry: while superconducting gravimeters and/or absolute gravimeters are used to obtain temporal gravity changes at one or several base stations, relative gravity surveys provide spatial differences with respect to these base stations, and allow to cover a much wider area than base stations only. Hybrid gravimetry therefore provides time-lapse gravity changes at a survey scale. We present here an overview of different published applications in hydrology, glaciology, volcanology and geothermics in order to point out that hybrid gravimetry is a powerful tool to monitor spatially and temporarily surface and underground mass changes.
Published: 2016
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39. Probing highly obscured, self-absorbed galaxy nuclei with vibrationally excited HCN

Author: Roberto Neri, Carsten Henkel, Francoise Combes, Thomas R. Greve, Gary A. Fuller, P. van der Werf, Francesco Costagliola, Eduardo González-Alfonso, Susanne Aalto, Sergio Martín, Eckhard Sturm, José Cernicharo, Lee Armus, Santiago García-Burillo, S. Muhle, Aaron S. Evans, M. Spaans, K. Sakamoto, Sebastien Muller, S. Viti, Chalmers University of Technology [Göteborg], Centre de Recherches du Service de Santé des Armées (CRSSA), Service de Santé des Armées, Universidad de Alcalá - University of Alcalá (UAH), General Electric Medical Systems [Buc] (GE Healthcare), General Electric Medical Systems, Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], 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), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Institut für Physik (Institut für Physik), Universität Potsdam, Astronomy, Observatorio Astronomico Nacional, Madrid, Universiteit Leiden, École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and University of Potsdam = Universität Potsdam
Subjects: Continuum absorption, Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, High resolution, FOS: Physical sciences, Self-absorbed, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, ISM [Galaxies], molecules [ISM], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, Luminous infrared galaxy, [PHYS]Physics [physics], Supermassive black hole, Astronomy, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, ISM: molecules, Space and Planetary Science, nuclei [Galaxies], Excited state, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: nuclei, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract: We present high resolution (0."4) IRAM PdBI and ALMA mm and submm observations of the (ultra) luminous infrared galaxies ((U)LIRGs) IRAS17208-0014, Arp220, IC860 and Zw049.057 that reveal intense line emission from vibrationally excited ($��_2$=1) J=3-2 and 4-3 HCN. The emission is emerging from buried, compact (r$$5\times 10^{13}$ L$_{\odot}$ kpc$^{-2}$. These nuclei are likely powered by accreting supermassive black holes (SMBHs) and/or hot (>200 K) extreme starbursts. Vibrational, $��_2$=1, lines of HCN are excited by intense 14 micron mid-infrared emission and are excellent probes of the dynamics, masses, and physical conditions of (U)LIRG nuclei when H$_2$ column densities exceed $10^{24}$ cm$^{-2}$. It is clear that these lines open up a new interesting avenue to gain access to the most obscured AGNs and starbursts. Vibrationally excited HCN acts as a proxy for the absorbed mid-infrared emission from the embedded nuclei, which allows for reconstruction of the intrinsic, hotter dust SED. In contrast, we show strong evidence that the ground vibrational state ($��$=0), J=3-2 and 4-3 rotational lines of HCN and HCO$^+$ fail to probe the highly enshrouded, compact nuclear regions owing to strong self- and continuum absorption. The HCN and HCO$^+$ line profiles are double-peaked because of the absorption and show evidence of non-circular motions - possibly in the form of in- or outflows. Detections of vibrationally excited HCN in external galaxies are so far limited to ULIRGs and early-type spiral LIRGs, and we discuss possible causes for this. We tentatively suggest that the peak of vibrationally excited HCN emission is connected to a rapid stage of nuclear growth, before the phase of strong feedback., 13 pages, 7 figures, accepted for publication in Astronomy and Astrophysics
Published: 2015
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40. Gravitational torques imply molecular gas inflow towards the nucleus of M51

Author: C. Kramer, J. Pety, K. F. Schuster, Adam K. Leroy, Annie Hughes, G. Dumas, D. Colombo, Clare Dobbs, Santiago García-Burillo, Eva Schinnerer, Miguel Querejeta, Sharon E. Meidt, Todd A. Thompson, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatorio Astronomico Nacional, Madrid, Service d'ORL et de chirurgie cervicale, CHU Grenoble, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Institut de RadioAstronomie Millimétrique (IRAM), 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] (OAN), Instituto Geografico Nacional (IGN), and École normale supérieure - Paris (ENS Paris)
Subjects: GALACTIC NUCLEI, individual: M 51 [galaxies], Astrophysics::High Energy Astrophysical Phenomena, nuclei [galaxies], FOS: Physical sciences, DWARF SEYFERT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic nuclei, 01 natural sciences, SPIRAL SHOCKS, STAR-FORMATION, Marie curie, SUPERMASSIVE BLACK-HOLES, Seyfert [galaxies], kinematics and dynamics [galaxies], 0103 physical sciences, media_common.cataloged_instance, European union, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, media_common, Physics, [PHYS]Physics [physics], NUCLEI, ISM [galaxies], GALAXIES NUGA, IMAGES. II, 010308 nuclear & particles physics, SPITZER SURVEY, S(4)G IRAC 3.6, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), structure [galaxies], STELLAR MASS DISTRIBUTIONS, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Humanities
Abstract: The transport of gas towards the centre of galaxies is critical for black hole feeding and, indirectly, it can control active galactic nucleus (AGN) feedback. We have quantified the molecular gas inflow in the central R, 19 pages, 12 figures. Accepted by A&A
Published: 2015
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41. HIGH-RESOLUTION IMAGING OF PHIBSS z ∼ 2 MAIN-SEQUENCE GALAXIES IN CO J = 1 → 0

Author: Alberto D. Bolatto, N. M. Förster Schreiber, Linda J. Tacconi, Andreas Burkert, David Fisher, Steven R. Warren, Amélie Saintonge, Stijn Wuyts, Achim Weiss, Reinhard Genzel, F. Bournaud, Francoise Combes, Adam Leroy, Santiago García-Burillo, M. C. Cooper, Nicolas Bouché, Amiel Sternberg, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Extraterrestrische Physik (MPE), Departamento de Ciência do Solo, Universidade de São Paulo (USP), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), 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), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), 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 of Physics - Riga, Latvian Academy of Sciences, 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), Universidade de São Paulo = University of São Paulo (USP), École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, Observatorio Astronomico Nacional, Madrid, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)
Subjects: Physics, [PHYS]Physics [physics], Star formation, Sigma, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Projection (relational algebra), Space and Planetary Science, Brightness temperature, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Excitation, ComputingMilieux_MISCELLANEOUS, Line (formation)
Abstract: We present Karl G. Jansky Very Large Array observations of the CO J=1-0 transition in a sample of four $z\sim2$ main sequence galaxies. These galaxies are in the blue sequence of star-forming galaxies at their redshift, and are part of the IRAM Plateau de Bure HIgh-$z$ Blue Sequence Survey (PHIBSS) which imaged them in CO J=3-2. Two galaxies are imaged here at high signal-to-noise, allowing determinations of their disk sizes, line profiles, molecular surface densities, and excitation. Using these and published measurements, we show that the CO and optical disks have similar sizes in main-sequence galaxies, and in the galaxy where we can compare CO J=1-0 and J=3-2 sizes we find these are also very similar. Assuming a Galactic CO-to-H$_2$ conversion, we measure surface densities of $\Sigma_{mol}\sim1200$ M$_\odot$pc$^{-2}$ in projection and estimate $\Sigma_{mol}\sim500-900$ M$_\odot$pc$^{-2}$ deprojected. Finally, our data yields velocity-integrated Rayleigh-Jeans brightness temperature line ratios $r_{31}$ that are approximately unity. In addition to the similar disk sizes, the very similar line profiles in J=1-0 and J=3-2 indicate that both transitions sample the same kinematics, implying that their emission is coextensive. We conclude that in these two main sequence galaxies there is no evidence for significant excitation gradients or a large molecular reservoir that is diffuse or cold and not involved in active star-formation. We suggest that $r_{31}$ in very actively star-forming galaxies is likely an indicator of how well mixed the star formation activity and the molecular reservoir are., Comment: To appear in ApJ
Published: 2015
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42. Results of the Sixth International Comparison of Absolute Gravimeters, ICAG-2001

Author: Sylvain Bonvalot, M. Amalvict, Zhiheng Jiang, Jacques Hinderer, Simon D. P. Williams, B. Luck, Laurent Longuevergne, Olivier Jamet, James E. Faller, Alessandro Germak, M. F. de Villalta Compagni, I.A. Robinson, T. M. van Dam, E. R. Pujol, J. Liard, François Dupont, J. Mäkinen, Michel Diament, E. N. Maderal, M. Van Ruymbeke, Germinal Gabalda, J. M. Chartier, M. Van Camp, Jan Mrlina, Reinhard Falk, Nicole Debeglia, Bruno Meurers, Matthias Becker, L. Vitushkin, A. Kopaev, S. Desogus, Thierry Gattacceca, G. Jeffries, S. Thies, D. Ruess, A. Reinhold, Shigeki Mizushima, C. G. L. Gagnon, Olivier Francis, P. Richard, Claudio Origlia, A. Lindau, David B. Newell, R. Käker, Bureau International des Poids et Mesures (BIPM), Institut für Geodäsie [Neubiberg] (IfG), Universität der Bundeswehr München [Neubiberg], European Center for Geodynamics and Seismology, Joint Institute for Laboratory Astrophysics (JILA), National Institute of Standards and Technology [Gaithersburg] (NIST)-University of Colorado [Boulder], Dynamique globale et déformation active (IPGS) (IPGS-DGDA), Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Géosciences Environnement Toulouse (GET), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-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), Bureau de Recherches Géologiques et Minières (BRGM) (BRGM), Istituto di Metrologia, IMGC, Institut de Physique du Globe de Paris (IPGP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Bundesamt für Kartographie und Geodäsie, BKG, Natural Resources Canada (NRCan), Institut géographique national [IGN] (IGN), Ecole nationale des sciences géographiques (ENSG), Finnish Geodetic Institute (FGI), Proudman Oceanographic Laboratory, Institut für Erdmessung, Leibniz Universität Hannover [Hannover] (LUH), Sternberg Astronomical Institute [Moscow], Lomonosov Moscow State University (MSU), Structure et fonctionnement des systèmes hydriques continentaux (SISYPHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-MINES ParisTech - École nationale supérieure des mines de Paris, Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Instituto Geográfico Nacional, Instituto Geografico Nacional, Institut für Meteorologie und Geophysik [Wien] (IMGW), Universität Wien, National Metrology Institute of Japan, National Institute of Advanced Industrial Science and Technology (AIST), Institute of Geophysics (ASCR), Czech Academy of Sciences [Prague] (CAS), National Institute of Standards and Technology [Gaithersburg] (NIST), Swiss Federal Office of Metrology and Accreditation, National Physical Laboratory [Teddington] (NPL), Federal Office of Metrology and Surveying [Vienna] (BEV), Observatoire Royal de Belgique, Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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)-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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Leibniz Universität Hannover=Leibniz University Hannover, Université Pierre et Marie Curie - Paris 6 (UPMC)-École Pratique des Hautes Études (EPHE), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Mines Paris - PSL (École nationale supérieure des mines de Paris)
Subjects: Physics, Gravity (chemistry), 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Gravimeter, [SDE.MCG]Environmental Sciences/Global Changes, General Engineering, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], Geodesy, 01 natural sciences, 010309 optics, Acceleration, 0103 physical sciences, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, 0105 earth and related environmental sciences
Abstract: International audience; The Sixth International Comparison of Absolute Gravimeters was held from 5 June to 28 August 2001 at the Bureau International des Poids et Mesures (BIPM), Sèvres. Seventeen absolute gravimeters were used to make measurements at five sites of the BIPM gravity network. The vertical gravity gradients at the sites and the ties between them were also measured using seventeen relative gravimeters. For the first time the ties were also measured using absolute gravimeters. Various methods of processing the absolute and relative data were tested to calculate the results. The final results of ICAG-2001 are presented. The acceleration due to gravity at a height of 0.90 m is given as (980 925 701.2 ± 5.5) µGal and (980 928 018.8 ± 5.5) µGal for sites A and B, respectively, calculated using a combined adjustment of the absolute and relative data.
Published: 2002
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43. AGN feedback in the nucleus of M 51(Corrigendum)

Author: David S. Meier, Dario Colombo, Frank Bigiel, Sharon E. Meidt, Miguel Querejeta, Annie Hughes, Kathryn Kreckel, Adam K. Leroy, Guillermo A. Blanc, Santiago García-Burillo, Eva Schinnerer, J. Pety, K. Sliwa, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], 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), Observatorio Astronomico Nacional, Madrid, Universität Heidelberg [Heidelberg] = Heidelberg University, and École normale supérieure - Paris (ENS-PSL)
Subjects: [PHYS]Physics [physics], Luminous infrared galaxy, Physics, 010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, Quasar, Astrophysics, 01 natural sciences, medicine.anatomical_structure, Space and Planetary Science, 0103 physical sciences, medicine, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Nucleus, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: International audience
Published: 2017
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44. Swarm's Absolute Scalar Magnetometers Burst Mode Results

Author: Coïsson, Pierdavide, Vigneron, Pierre, Hulot, Gauthier, Crespo Grau, R., Brocco, Laura, Lalanne, Xavier, Sirol, Olivier, Leger, J. M., Jager, Thomas, Bertrand, François, Boness, Axel, Fratter, Isabelle, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Observatorio Geofisico Central, Instituto Geografico Nacional, Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, external field, 2499 General or miscellaneous, IONOSPHERE, GEOMAGNETISM AND PALEOMAGNETISM, 2721 Field-aligned currents and current systems
Abstract: International audience; Each of the three Swarm satellites embarks an Absolute Scalar Magnetometer (ASM) to provide absolute scalar measurements of the magnetic field with high accuracy and stability. Nominal data acquisition of these ASMs is 1 Hz. But they can also run in a so-called "burst mode" and provide data at 250 Hz. During the commissioning phase of the mission, seven burst mode acquisition campaigns have been run simultaneously for all satellites, obtaining a total of ten days of burst-mode data. These campaigns allowed the identification of issues related to the operations of the piezo-electric motor and the heaters connected to the ASM, that do not impact the nominal 1 Hz scalar data. We analyze the burst mode data to identify high frequency geomagnetic signals, focusing the analysis in two regions: the low latitudes, where we seek signatures of ionospheric irregularities, and the high latitudes, to identify high frequency signals related to polar region currents. Since these campaigns have been conducted during the initial months of the mission, the three satellites where still close to each other, allowing to analyze the spatial coherency of the signals.
Published: 2014

45. Array analysis of the seismic wavefield of long-period events and volcanic tremor at Arenal volcano, Costa Rica

Author: Javier Almendros, Mauricio M. Mora, Philippe Lesage, Rafael Abella, Instituto Andaluz de Ciencias de la Tierra (IACT), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada (UGR), Observatorio Geofisico Central, Instituto Geografico Nacional, Escuela Centroamericana de Geología, Universidad Nacional de Costa Rica, Géophysique des volcans & géothermie, Institut des Sciences de la Terre (ISTerre), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada = University of Granada (UGR), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-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 Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Lava, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, 01 natural sciences, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), [SDU.STU.VO]Sciences of the Universe [physics]/Earth Sciences/Volcanology, Arenal volcano, Slowness, Volcanic tremor, 0105 earth and related environmental sciences, Array analysis, geography, geography.geographical_feature_category, Fragmentation (computing), Crust, Harmonic tremor, Geophysics, Volcano, 13. Climate action, Space and Planetary Science, Seismic array, Seismology, Geology
Abstract: We use wavefield decomposition methods (time-domain crosscorrelation and frequency-domain MUSIC) to analyze seismic data recorded by a dense, small-aperture array located 2 km West of Arenal volcano, Costa Rica, and operated during 2.5 days. The recorded wavefield is dominated by harmonic tremor and includes also spasmodic tremor and long-period (LP) events. We find that the initial stages of LP events are characterized by three different wave arrivals. These arrivals propagate with similar back-azimuths pointing to the volcano summit (~80◦N) and increasing apparent slownesses of 0.4, 1.1, and 1.7 s/km. Spasmodic tremors can not be regarded as coherent signals. On the contrary, harmonic tremors are highly coherent, characterized by the stability of the apparent slowness vector estimates. Apparent slownesses lay in the range 1-2 s/km. Back-azimuths point in the general direction of the volcano, but with a large variability (40-120◦N). Nevertheless, there are long-term variations and evidences of multiple simultaneous components in the harmonic tremor wavefield. These observations suggest that LP events and tremor are generated in a shallow source area near the volcano summit, although they do not share exactly the same source region or source processes. The tremor source is located in the shallowest part of the plumbing system, beneath the lava crust. This dynamic region is subject to complex fluctuations of the physical conditions. Degassing events at different locations of this region might generate variable seismic radiation patterns. The effects of topography and heterogeneous shallow structure of the volcano may amplify these variations and produce the wide directional span observed for volcanic tremor. On the other hand, the LP source seems to be more repeatable. LP events are likely triggered by fragmentation of the fluid flow in a slightly deeper portion of the volcanic conduits.
Published: 2014
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46. Study of the Time Stability of Tides Using a Long Term (1973-2011) Gravity Record at Strasbourg, France

Author: Jean-Paul Boy, H. Legros, Umberto Riccardi, Marta Calvo, Jacques Hinderer, Séverine Rosat, Instituto Geografico Nacional (IGN), Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Università degli studi di Napoli Federico II, Chris Rizos, Pascal Willis, C. Rizo, P. Willis, M., Calvo, S., Rosat, J., Hinderer, H., Legro, J. P., Boy, and Riccardi, Umberto
Subjects: Gravity (chemistry), 010504 meteorology & atmospheric sciences, Meteorology, Gravimeter, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], 010502 geochemistry & geophysics, Geodesy, calibration, 01 natural sciences, Term (time), Geography, LaCoste-Romberg spring gravimeter, 13. Climate action, Observatory, tide, superconducting gravimeter, Solid earth, 0105 earth and related environmental sciences
Abstract: International audience; The Gravimetric Observatory J9 located near Strasbourg (France), has a long history of recording solid Earth tides. We present here one of the longest available gravity records (1973-2011) from three different instruments operating at the J9 station: a LaCoste-Romberg spring gravimeter (ET005) from 1973 to 1985, a GWR (TT70-T005) superconducting gravimeter from 1987 to 1996 and a GWR compact superconducting gravimeter (C026) since 1996. We give the results of a tidal analysis performed with ETERNA on these data sets. We show the improvement in terms of noise levels from the oldest type to the newest one and check the time stability of the observed tides for every instrument. This stability is also dependent on the stability of the scale factor of the cryogenic gravimeter which is derived from a direct comparison with repeated absolute gravity measurements. The response of the three gravimeters to the atmospheric pressure changes is also checked. With all these results we found that the improvement from a mechanical spring gravimeter to a modern cryogenic instrument is obvious. And also that the improvement from the T005 SG to the C026 SG is less impressive than from L&R to the T005 SG, but still notable.
Published: 2014
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47. Deuteration around the ultracompact HII region Monoceros R2

Author: C. Kramer, José Cernicharo, D. Ginard, M. González-García, O. Berne, Volker Ossenkopf, E. Roueff, J. Pety, Asunción Fuente, P. Pilleri, J. R. Rizzo, Santiago García-Burillo, S. Viti, M. Gerin, S. P. Treviño-Morales, J. R. Goicoechea, Los Alamos National Laboratory (LANL), Observatorio Astronómico Nacional (OAN), oan, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Instituto de Radio Astronomía Milimétrica, Spanish National Research Council [Madrid] (CSIC), 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), Institut de RadioAstronomie Millimétrique (IRAM), Centre d'étude spatiale des rayonnements (CESR), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Atmospheric Physics Laboratory [UCL London], University College of London [London] (UCL), Observatorio Astronomico Nacional, Madrid, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, radio lines: ISM, astrochemistry, Spatially resolved, Hii regions, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Deuterium, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), photon-dominated region (PDR), Protostar, Molecule, Spectral resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: The massive star-forming region Mon R2 hosts the closest ultra-compact HII region that can be spatially resolved with current single-dish telescopes. We used the IRAM-30m telescope to carry out an unbiased spectral survey toward two important positions (namely IF and MP2), in order to studying the chemistry of deuterated molecules toward Mon R2. We found a rich chemistry of deuterated species at both positions, with detections of C2D, DCN, DNC, DCO+, D2CO, HDCO, NH2D, and N2D+ and their corresponding hydrogenated species and isotopologs. Our high spectral resolution observations allowed us to resolve three velocity components: the component at 10 km/s is detected at both positions and seems associated with the layer most exposed to the UV radiation from IRS 1; the component at 12 km/s is found toward the IF position and seems related to the molecular gas; finally, a component at 8.5 km/s is only detected toward the MP2 position, most likely related to a low-UV irradiated PDR. We derived the column density of all the species, and determined the deuterium fractions (Dfrac). The values of Dfrac are around 0.01 for all the observed species, except for HCO+ and N2H+ which have values 10 times lower. The values found in Mon R2 are well explained with pseudo-time-dependent gas-phase model in which deuteration occurs mainly via ion-molecule reactions with H2D+, CH2D+ and C2HD+. Finally, the [H13CN]/[HN13C] ratio is very high (~11) for the 10 km/s component, which also agree with our model predictions for an age of ~0.01-0.1 Myr. The deuterium chemistry is a good tool for studying star-forming regions. The low-mass star-forming regions seem well characterized with Dfrac(N2H+) or Dfrac(HCO+), but it is required a complete chemical modeling to date massive star-forming regions, because the higher gas temperature together with the rapid evolution of massive protostars., Comment: 14 pages of manuscript, 17 pages of apendix, 7 figures in the main text, accepted for publication in A&A
Published: 2014
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48. CO and PAH+/PAH0/VSG maps in external galaxies

Author: E. Bayet, Santiago García-Burillo, Christine Joblin, Maryvonne Gerin, Olivier Berné, Asunción Fuente, Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France, Centre Etud Spatiale Rayonnements Toulouse, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Observatorio Astronómico Nacional (OAN), oan, Kramer, C. and Aalto, S. and Simon, and R.
Subjects: Physics, 010504 meteorology & atmospheric sciences, General Engineering, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Space and Planetary Science, TRACER, 0103 physical sciences, High spatial resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Dust emission
Abstract: We have performed a comparison between the molecular gas emission and the mid IR dust component emission distributions in a sample of nearby galaxies. We have compared CO maps at high spatial resolution, from Wilson et al. (2000), Bayet et al. (2004, 2006) and from Kramer et al. (2005), with the emission distributions of ionised and neutral PAHs (PAH + ; PAH 0 ) and of very small grains (VSGs), obtained using signal processing methods as explained in Berne et al. (2007a) and Rapacioli et al. (2005). In M 82, we have also compared the dust emission maps with dense gas tracer maps (HCO and H 13 CO + data from Garcia-Burillo et al. 2002) as well as with shock tracer maps (SiO data from Garcia-Burillo et al. 2001).
Published: 2008
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49. Preliminary Results from the Superconducting Gravimeter SG-060 Installed in West Africa (Djougou, Benin)

Author: Séverine Rosat, Basile Hector, Umberto Riccardi, Jacques Hinderer, Jean-Paul Boy, Luc Séguis, Marta Calvo, C. Rizo, P. Willis, Hinderer, J., Rosat, S., Calvo, M., Boy, J. P., Hector, B., Riccardi, Umberto, Seguis, L., Dynamique globale et déformation active (IPGS) (IPGS-DGDA), Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecole et Observatoire des Sciences de la Terre (EOST), Instituto Geografico Nacional (IGN), Dipartimento di Scienze della Terra, Università degli studi di Napoli Federico II, Hydrosciences Montpellier (HSM), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD)-Université Montpellier 2 - Sciences et Techniques (UM2)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and Chris Rizos, Pascal Willis
Subjects: Superconductivity, Gravity (chemistry), Admittance, 010504 meteorology & atmospheric sciences, Meteorology, Atmospheric pressure, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Gravimeter, equator site, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], barometric pressure, 010502 geochemistry & geophysics, 01 natural sciences, West africa, Atmosphere, Geography, 13. Climate action, thermal atmospheric tide, Calibration, superconducting gravimeter, initial drift, 0105 earth and related environmental sciences
Abstract: International audience; A GWR superconducting gravimeter of the new generation (OSG-60) has been installed in July 2010 in sub-humid West Africa, at the Djougou station in Benin. This station is located in the AMMA-CATCH long term hydrological observing system. We present the first results in terms of instrumental drift as well as the calibration results using FG5 absolute gravity measurements. We show that geophysical contributions due to hydrological load can bias the initial drift estimate. The noise level is compared to the Strasbourg SG as well as to the reference New Low Noise Model (NLNM) used in seismology. We also investigate the gravity response to atmospheric pressure changes and show that, because of the presence of large thermal tides, the gravity response to mass changes in the atmosphere is more complex than in the simple case of a constant barometric admittance.
Published: 2013
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50. ALMA observations of feeding and feedback in nearby Seyfert galaxies: an AGN-driven outflow in NGC 1433

Author: Francoise Combes, Viviana Casasola, Frédéric Boone, Andrew J. Baker, Santiago García-Burillo, Eva Schinnerer, Leslie K. Hunt, Roberto Neri, Linda J. Tacconi, Melanie Krips, Isabel Márquez, Andreas Eckart, 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), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Arcetri (OAA), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Department of Geography, Newcastle University [Newcastle], 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), Max-Planck-Institut für Radioastronomie (MPIFR), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Max Planck Institute for Extraterrestrial Physics (MPE), École normale supérieure - Paris (ENS-PSL), Observatorio Astronomico Nacional, Madrid, 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), 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Hubble space telescope, 0103 physical sciences, Thermal, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Torus, Redshift, Galaxy, 13. Climate action, Space and Planetary Science, Outflow, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report ALMA observations of CO(3-2) emission in the Seyfert 2 double-barred galaxy NGC1433, at the unprecedented spatial resolution of 0.5"=24 pc. Our aim is to probe AGN feeding and feedback phenomena through the morphology and dynamics of the gas inside the central kpc. The CO map, which covers the whole nuclear region (nuclear bar and ring), reveals a nuclear gaseous spiral structure, inside the nuclear ring encircling the nuclear stellar bar. This gaseous spiral is well correlated with the dusty spiral seen in Hubble Space Telescope images. The nuclear spiral winds up in a pseudo-ring at 200 pc radius, which might correspond to the inner ILR. Continuum emission is detected at 0.87 mm only at the very centre, and its origin is more likely thermal dust emission than non-thermal emission from the AGN. It might correspond to the molecular torus expected to exist in this Seyfert 2 galaxy. The HCN(4-3) and HCO+(4-3) lines were observed simultaneously, but only upper limits are derived, with a ratio to the CO(3-2) line lower than 1/60 at 3sigma, indicating a relatively low abundance of very dense gas. The kinematics of the gas over the nuclear disk reveal rather regular rotation only slightly perturbed by streaming motions due to the spiral; the primary and secondary bars are too closely aligned with the galaxy major or minor axis to leave a signature in the projected velocities. Near the nucleus, there is an intense high-velocity CO emission feature redshifted to 200 km/s (if located in the plane), with a blue-shifted counterpart, at 2" (100 pc) from the centre. While the CO spectra are quite narrow in the centre, this wide component is interpreted as an outflow involving a molecular mass of 3.6 10^6 Mo and a flow rate 7 Mo/yr. The flow could be in part driven by the central star formation, but is mainly boosted by the AGN through its wind or radio jets., 11 pages, 9 figures, Accepted in Astronomy and Astrophysics
Published: 2013
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