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22 results on '"Johana Panduro"'

1. Infrared Wavefront Sensing for Adaptive Optics Assisted Galactic Center Observations with the VLT Interferometer and GRAVITY: Operation and Results

Author

Stefan Hippler, Wolfgang Brandner, Silvia Scheithauer, Martin Kulas, Johana Panduro, Peter Bizenberger, Henry Bonnet, Casey Deen, Françoise Delplancke-Ströbele, Frank Eisenhauer, Gert Finger, Zoltan Hubert, Johann Kolb, Eric Müller, Laurent Pallanca, Julien Woillez, Gérard Zins, and GRAVITY Collaboration

Subjects
near-infrared wavefront sensing, VLT interferometer, Galactic Center, CIAO, adaptive optics, SAPHIRA detector, Physics, QC1-999, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract

This article describes the operation of the near-infrared wavefront sensing based Adaptive Optics (AO) system CIAO. The Coudé Infrared Adaptive Optics (CIAO) system is a central auxiliary component of the Very Large Telescope (VLT) interferometer (VLTI). It enables in particular the observations of the Galactic Center (GC) using the GRAVITY instrument. GRAVITY is a highly specialized beam combiner, a device that coherently combines the light of the four 8-m telescopes and finally records interferometric measurements in the K-band on 6 baselines simultaneously. CIAO compensates for phase disturbances caused by atmospheric turbulence, which all four 8 m Unit Telescopes (UT) experience during observation. Each of the four CIAO units generates an almost diffraction-limited image quality at its UT, which ensures that maximum flux of the observed stellar object enters the fibers of the GRAVITY beam combiner. We present CIAO performance data obtained in the first 3 years of operation as a function of weather conditions. We describe how CIAO is configured and used for observations with GRAVITY. In addition, we focus on the outstanding features of the near-infrared sensitive Saphira detector, which is used for the first time on Paranal, and show how it works as a wavefront sensor detector.

Published
2020
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2. Infrared wavefront sensing for adaptive optics assisted galactic center observations with GRAVITY

Author

Julien Woillez, Gérard Zins, Johann Kolb, F. Delplancke-Ströbele, Wolfgang Brandner, Frank Eisenhauer, Casey Deen, Henri Bonnet, Silvia Scheithauer, Peter Bizenberger, Gert Finger, Eric Müller, Johana Panduro, Stefan Hippler, Laurent Pallanca, Z. Hubert, and Martin Kulas

Subjects
Wavefront, Physics, Very Large Telescope, business.industry, Galactic Center, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Wavefront sensor, Interferometry, Optics, Computer Science::Programming Languages, Astrophysics::Earth and Planetary Astrophysics, business, Focus (optics), Adaptive optics
Abstract

We describe the operation of the infrared wavefront sensing based Adaptive Optics system CIAO. The Coude Infrared Adaptive Optics (CIAO) system is a central auxiliary component of the Very Large Telescope interferometer (VLTI). It enables in particular Galactic Center observations using the GRAVITY interferometric instrument. CIAO compensates for phase disturbances caused by atmospheric turbulence, which all four 8 m Unit Telescopes (UT) experience during observation. Each of the four CIAO units generates an almost diffraction-limited image quality at its UT, which ensures that maximum flux of the observed stellar object enters the input fibers of GRAVITY. We present CIAO performance data obtained in the first 3 years of operation. We describe how CIAO is configured and used for observations with GRAVITY. We focus on the outstanding features of the infrared sensitive Saphira detector, which is used for the first time on Paranal, and show how it works as a wavefront sensor detector.

Published
2020

3. The CARMENES search for exoplanets around M dwarfs Two temperate Earth-mass planet candidates around Teegarden's Star

Author

A. Claret, E. Casal, Jorge Sanz-Forcada, D. Montes, Juan Luis Cano, N. Casasayas-Barris, M. Lampón, C. Rodríguez López, E. de Guindos, Michael Perryman, N. Lodieu, S. Pedraz, Johana Panduro, Otmar Stahl, Guillem Anglada-Escudé, Peter H. Hauschildt, E. Solano, A. López-Comazzi, Ralf Launhardt, J. I. Vico Linares, E. Herrero, M. J. López-González, J. Kemmer, P. Schöfer, T. Stuber, A. Klutsch, J. H. M. M. Schmitt, S. Reinhardt, Manuel López-Puertas, M. Ammler-von Eiff, M. Lafarga, Manuel Perger, R. Hernández Arabí, M. R. Zapatero Osorio, J. Garcia de la Fuente, Hugo M. Tabernero, Priyanka Chaturvedi, Ulrich Grözinger, M. López del Fresno, Grzegorz Nowak, F. J. Alonso-Floriano, M. Brinkmöller, F. Labarga, Lluis Gesa, R. Calvo Ortega, L. M. Lara, Juan Pablo Pascual, Francesc Vilardell, M. C. Cárdenas Vázquez, Andreas Schweitzer, Denis Shulyak, Aviv Ofir, A. Rosich, J. Klüter, Alfredo Sota, Ernesto Sánchez-Blanco, Ignasi Ribas, M. Tala Pinto, A. Fernández-Martín, V. Casanova, Sebastian Schafer, Vianak Naranjo, P. Martín-Fernández, S. Czesla, I. Hermelo, P. Rhode, Hannu Parviainen, Karl Wagner, M. Kürster, Hubert Klahr, Juan Carlos Suárez, Florian Rodler, V. Wolthoff, P. Bluhm, Birgit Fuhrmeister, M. Llamas, Emilio Marfil, S. V. Jeffers, Philipp Huke, H. Magán Madinabeitia, Jose A. Caballero, R. Antona Jiménez, Fei Yan, S. Lalitha, C. del Burgo, E. Díez-Alonso, A. Rodríguez Trinidad, A. Pavlov, F. F. Bauer, J. Góngora Rueda, M. Azzaro, Jesus M. Carro, I. Gallardo Cava, L. F. Sarmiento, M. Kim, A. Guijarro, Susana Martín-Ruiz, M. L. García Vargas, M. A. Sánchez Carrasco, Sabine Reffert, Lisa Nortmann, Andreas Quirrenbach, A. Fukui, M. Cortés-Contreras, Pedro J. Amado, H. Anwand-Heerwart, Ricardo Dorda, F. J. Lázaro, A. P. Hatzes, F. Hernández Otero, Javier López-Santiago, Jesús Aceituno, E. Mirabet, D. Baroch, Mahmoudreza Oshagh, Ana Pérez-Calpena, J. B. P. Strachan, Juan Carlos Morales, Evangelos Nagel, Th. Henning, R. González-Peinado, J. Helmling, David Barrado, E. N. Johnson, S. Dreizler, Lev Tal-Or, Enric Palle, Víctor J. S. Béjar, M. Fernandez, J. Guàrdia, S. Stock, E. L. Martin, S. Becerril, D. Pérez Medialdea, Armin Huber, D. Hintz, L. Hernández Castaño, I. M. Ferro, M. Zechmeister, H. W. Rix, C. Cardona Guillén, Gilles Bergond, S. Sadegi, W. Xu, G. Veredas, A. Ramón Ballesta, B. Arroyo-Torres, R. P. Hedrosa, Rafael Rebolo, J. A. Marín Molina, A. Sánchez-López, Norio Narita, F. J. Aceituno, Ovidio Rabaza, J. I. González Hernández, A. Garcia-Piquer, M. E. Moreno-Raya, Rafael Luque, Paula Sarkis, J. Stürmer, Trifon Trifonov, P. Redondo, E. Gonzalez-Alvarez, E. Rodriguez, Ralf Klein, L. Mancini, Diana Kossakowski, D. Benítez, J. F. López Salas, D. Galadí-Enríquez, Josep Colomé, C. J. Marvin, E. de Juan, Z. M. Berdinas, D. Maroto Fernández, Ansgar Reiners, Carlos Cifuentes, Walter Seifert, Pilar Montañés-Rodríguez, Ulrich Mall, V. M. Passegger, A. Kaminski, L. Gonzalez-Cuesta, Holger Mandel, Miguel Abril, Max Planck Institute for Astronomy, CSIC - Instituto de Astrofísica de Andalucía (IAA), Landessternwarte Königstuhl, CSIC - Instituto de Ciencias del Espacio (ICE), Institute for Astrophysics in Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg Karl Schwarzschild-Observatorium, Instituto de Astrofísica de Canarias, Hamburg Observatory, Max Planck Society, Observatorio de Calar Alto, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Junta de Andalucía, German Research Foundation, German Centre for Air and Space Travel, European Research Council, CSIC-INTA - Centro de Astrobiología (CAB), Consejo Superior de Investigaciones Científicas (España), European Commission, Ministero dell'Istruzione, dell'Università e della Ricerca, Science and Technology Facilities Council (UK), Israel Science Foundation, Consejo Nacional de Ciencia y Tecnología (México), and Japan Society for the Promotion of Science

Subjects
Astrofísica, Brightness, 010504 meteorology & atmospheric sciences, individual: Teegarden’s Star [Stars], methods: data analysis, planetary systems, stars: late-type, stars: individual: Teegarden's Star, FOS: Physical sciences, Minimum mass, Stars: late-type, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), Settore FIS/05 - Astronomia e Astrofisica, Methods: data analysis, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, data analysis [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, individual: Teegarden's Star [Stars], 0105 earth and related environmental sciences, Stars: individual: Teegarden's Star, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy, Astronomy and Astrophysics, Earth mass, Exoplanet, Radial velocity, Planetary systems, Slow rotation, 13. Climate action, Space and Planetary Science, late-type [Stars], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Teegarden's Star is the brightest and one of the nearest ultra-cool dwarfs in the solar neighbourhood. For its late spectral type (M7.0 V), the star shows relatively little activity and is a prime target for near-infrared radial velocity surveys such as CARMENES. Aims. As part of the CARMENES search for exoplanets around M dwarfs, we obtained more than 200 radial-velocity measurements of Teegarden's Star and analysed them for planetary signals. Methods. We find periodic variability in the radial velocities of Teegarden's Star. We also studied photometric measurements to rule out stellar brightness variations mimicking planetary signals. Results. We find evidence for two planet candidates, each with 1.1 M minimum mass, orbiting at periods of 4.91 and 11.4 d, respectively. No evidence for planetary transits could be found in archival and follow-up photometry. Small photometric variability is suggestive of slow rotation and old age. Conclusions. The two planets are among the lowest-mass planets discovered so far, and they are the first Earth-mass planets around an ultra-cool dwarf for which the masses have been determined using radial velocities.© ESO 2019., M.Z. acknowledges support from the Deutsche Forschungsgemeinschaft under DFG RE 1664/12-1 and Research Unit FOR2544 >Blue Planets around Red Stars>, project no. RE 1664/14-1. CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 >Blue Planets around Red Stars>, the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. Based on data from the CARMENES data archive at CAB (INTA-CSIC). This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sanchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. Data were partly collected with the 150-cm and 90-cm telescopes at the Sierra Nevada Observatory (SNO) operated by the Instituto de Astrofisica de Andalucia (IAA-CSIC). Data were partly obtained with the MONET/South telescope of the MOnitoring NEtwork of Telescopes, funded by the Alfried Krupp von Bohlen und Halbach Foundation, Essen, and operated by the Georg-August-Universitat Gottingen, the McDonald Observatory of the University of Texas at Austin, and the South African Astronomical Observatory. We acknowledge financial support from the Spanish Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the European FEDER/ERF funds through projects AYA2015-69350-C3-2-P, AYA2016-79425-C3-1/2/3-P, AYA2018-84089, BES-2017-080769, BES-2017-082610, ESP2015-65712-C5-5-R, ESP2016-80435-C2-1/2-R, ESP2017-87143-R, ESP2017-87676-2-2, ESP2017-87676-C5-1/2/5-R, FPU15/01476, RYC-2012-09913, the Centre of Excellence >Severo Ochoa> and >Maria de Maeztu> awards to the Instituto de Astrofisica de Canarias (SEV-2015-0548), Instituto de Astrofisica de Andalucia (SEV-2017-0709), and Centro de Astrobiologia (MDM-2017-0737), the Generalitat de Catalunya through CERCA programme>, the Deutsches Zentrum fur Luft-und Raumfahrt through grants 50OW0204 and 50OO1501, the European Research Council through grant 6 94 513, the Italian Ministero dell'instruzione, dell'universita de della ricerca and Universita degli Studi di Roma Tor Vergata through FFABR 2017 and >Mission: Sustainability 2016>, the UK Science and Technology Facilities Council through grant ST/P000592/1, the Israel Science Foundation through grant 848/16, the Chilean CONICYT-FONDECYT through grant 31 80 405, the Mexican CONACYT through grant CVU 4 48 248, the JSPS KAKENHI through grants JP18H01265 and 18H05439, and the JST PRESTO through grant JPMJPR1775.

Published
2019

4. Detection of orbital motions near the last stable circular orbit of the massive black hole SgrA*

Author

Linda J. Tacconi, Eckhard Sturm, Laurent Jocou, Julien Woillez, Guy Perrin, Bernard Lazareff, Christian Straubmeier, P. M. Plewa, Stefan Hippler, H. Bonnet, Feng Gao, Eric Gendron, Th. Henning, Gérard Rousset, N. M. Förster Schreiber, Thomas Ott, Johana Panduro, Jean-Philippe Berger, P. Guajardo, Frank Eisenhauer, Karine Perraut, S. von Fellenberg, Yann Clénet, P. T. de Zeeuw, Felix Widmann, Pierre Léna, Thibaut Paumard, Oliver Pfuhl, Xavier Haubois, Erich Wiezorrek, V. Coudé du Foresto, Casey Deen, Sylvestre Lacour, Stefan Gillessen, Jason Dexter, Amiel Sternberg, Gilles Duvert, Matthew Horrobin, Odele Straub, J.-B. Le Bouquin, Armin Huber, Reinhard Genzel, Paulo J. V. Garcia, Sebastian Rabien, António Amorim, G. Rodríguez-Coira, Wolfgang Brandner, Frederic H. Vincent, Roberto Abuter, V. Lapeyrère, Idel Waisberg, Andreas Eckart, S. Yazici, Maryam Habibi, M. Bauböck, Pierre Kervella, Magdalena Lippa, A. Jiménez-Rosales, Ekkehard Wieprecht, European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Max Planck Institute for Extraterrestrial Physics (MPE), Laboratoire de Physique Statistique de l'ENS (LPS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Transport et Environnement (INRETS/LTE), Institut National de Recherche sur les Transports et leur Sécurité (INRETS), 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), Swedish Space Corporation (SSC), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Laboratoire Univers et Théories (LUTH (UMR_8102)), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Universität zu Köln, AUTRES, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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]), Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-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), 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 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)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, Gravitation, Telescope, General Relativity and Quantum Cosmology, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Circular orbit, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Solar mass, 010308 nuclear & particles physics, Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Interferometry, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Orbital motion, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Schwarzschild radius
Abstract

We report the detection of continuous positional and polarization changes of the compact source SgrA* in high states ('flares') of its variable near- infrared emission with the near-infrared GRAVITY-Very Large Telescope Interferometer (VLTI) beam-combining instrument. In three prominent bright flares, the position centroids exhibit clockwise looped motion on the sky, on scales of typically 150 micro-arcseconds over a few tens of minutes, corresponding to about 30% the speed of light. At the same time, the flares exhibit continuous rotation of the polarization angle, with about the same 45(+/-15)-minute period as that of the centroid motions. Modelling with relativistic ray tracing shows that these findings are all consistent with a near face-on, circular orbit of a compact polarized 'hot spot' of infrared synchrotron emission at approximately six to ten times the gravitational radius of a black hole of 4 million solar masses. This corresponds to the region just outside the innermost, stable, prograde circular orbit (ISCO) of a Schwarzschild-Kerr black hole, or near the retrograde ISCO of a highly spun-up Kerr hole. The polarization signature is consistent with orbital motion in a strong poloidal magnetic field., Comment: accepted by A&A; 16 pages

Published
2018

5. PANIC: A general-purpose panoramic near-infrared camera for the calar alto observatory

Author

Werner Laun, Peter Bizenberger, Bernd Funke, Clemens Storz, Marcos Ubierna, M. Fernandez, Lourdes Verdes-Montenegro, V. Terron, A. Garcia Segura, J. Fried, I. M. Ferro Rodríguez, Armin Huber, Matthias Alter, J. Rodríguez Gómez, B. Dorner, J. Helmling, Harald Baumeister, Johana Panduro, M. C. Cárdenas Vázquez, Ulrich Mall, Ernesto Sánchez-Blanco, Vianak Naranjo, Klaus Meisenheimer, R.-R. Rohloff, P. Fopp, J. M. Ibáñez Mengual, Richard J. Mathar, H. Bouy, Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, Institut Universitari de Ciencia dels Materials (ICMUV), Universitat de València (UV), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Max-Planck-Institut für Astronomie (MPIA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), M2A 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and 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)

Subjects
Techniques: image processing, Astronomy, Astronomy and Astrophysics, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010309 optics, General purpose, Space and Planetary Science, Observatory, Political science, 0103 physical sciences, image processing [Techniques], Instrumentation: detectors, miscellaneous [Instrumentation], 0210 nano-technology, Instrumentation: miscellaneous, ComputingMilieux_MISCELLANEOUS, detectors [Instrumentation]
Abstract

PANIC is the new PAnoramic Near-Infrared Camera for Calar Alto and is a project jointly developed by the MPIA in Heidelberg, Germany, and the IAA in Granada, Spain, for the German-Spanish Astronomical Center at Calar Alto Observatory (CAHA; Almería, Spain). This new instrument works with the 2.2 m and 3.5 m CAHA telescopes covering a field of view of 30×30 arcmin and 15×15 arcmin, respectively, with a sampling of 4096×4096 pixels. It is designed for the spectral bands from Z to K, and can also be equipped with narrowband filters. The instrument was delivered to the observatory in 2014 October and was commissioned at both telescopes between 2014 November and 2015 June. Science verification at the 2.2 m telescope was carried out during the second semester of 2015 and the instrument is now at full operation. We describe the design, assembly, integration, and verification process, the final laboratory tests and the PANIC instrument performance. We also present first-light data obtained during the commissioning and preliminary results of the scientific verification. The final optical model and the theoretical performance of the camera were updated according to the as-built data. The laboratory tests were made with a star simulator. Finally, the commissioning phase was done at both telescopes to validate the camera real performance on sky. The final laboratory test confirmed the expected camera performances, complying with the scientific requirements. The commissioning phase on sky has been accomplished.© 2017. The Astronomical Society of the Pacific. All rights reserved., Part of this work was supported by the Spanish CSIC grants PIE-200450E175, 200450E458, 201250E108, 201250E012, and 201450E093, and MINECO grants AYA2010-10728 and ICTS-2009-32. L.V.M. acknowledges support from the grant AYA2015-65973-C3-1-R (MINECO/FEDER, UE).

Published
2018

6. The CARMENES search for exoplanets around M dwarfs: High-resolution optical and near-infrared spectroscopy of 324 survey stars

Author

S. Becerril, S. Reinhart, I. M. Ferro, Philipp Huke, E. Díez-Alonso, R. González-Peinado, M. Azzaro, Richard J. Mathar, Jose Antonio Pascual, A. Lamert, Javier López-Santiago, E. Mirabet, M. A. Sánchez Carrasco, Gilles Bergond, Ulrich Mall, D. Pérez Medialdea, Armin Huber, E. Herrero, E. Casal, S. V. Jeffers, Grzegorz Nowak, Sebastian Schafer, J. Helmling, S. Sadegi, H. Magán Madinabeitia, G. Veredas, M. Lampón, E. N. Johnson, W. Xu, Karl Wagner, M. L. García Vargas, David Barrado, J. H. M. M. Schmitt, Enric Palle, R. Oreiro, D. Baroch, B. Arroyo-Torres, Pedro J. Amado, C. Cifuentes, J. A. Marín Molina, D. Galadí-Enríquez, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, A. Rodríguez Trinidad, M. Lafarga, I. Hermelo, V. M. Passegger, H. W. Rix, H. Anwand-Heerwart, Juan Carlos Suárez, Florian Rodler, Martin Kürster, M. Kim, P. Schöfer, J. Klüter, M. Tala, R.-R. Rohloff, D. Benítez, Johana Panduro, Lisa Nortmann, Andreas Quirrenbach, Z. M. Berdiñas, J. Schiller, J. López-González, S. Czesla, P. Rhode, Adrian Kaminski, A. Pavlov, Holger Mandel, L. Hernández Castaño, J. I. Vico Linares, C. Feiz, Guillem Anglada-Escudé, L. F. Sarmiento, Susana Martín-Ruiz, Simon Tulloch, A. P. Hatzes, Jesús Aceituno, Eike W. Guenther, M. Pluto, Juan Carlos Morales, Manuel López-Puertas, M. Ammler-von Eiff, M. R. Zapatero Osorio, R. G. Ulbrich, Otmar Stahl, M. López del Fresno, Emilio Marfil, Reinhard Mundt, Lluis Gesa, Evangelos Nagel, Werner Laun, Josep Colomé, Francesc Vilardell, M. C. Cárdenas Vázquez, J. F. López Salas, Jose A. Caballero, M. Blümcke, A. Ramón, Aviv Ofir, E. de Guindos, Ana Pérez-Calpena, S. Pedraz, Ralf Launhardt, Rainer Lenzen, A. Claret, Sabine Reffert, U. Lemke, Luigi Mancini, J. B. P. Strachan, F. J. Alonso-Floriano, M. A. C. Perryman, Fei Yan, Mathias Zechmeister, Ernesto Sánchez-Blanco, Vianak Naranjo, A. Klutsch, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, Ulrich Grözinger, Walter Seifert, V. Gómez Galera, Luisa Lara, R. P. Hedrosa, Rafael Rebolo, A. Guijarro, E. de Juan, A. Sánchez-López, Rafael Luque, M. Brinkmöller, Paula Sarkis, J. Stürmer, Ovidio Rabaza, J. I. González Hernández, C. del Burgo, A. Rosich, Andreas Schweitzer, D. Montes, Miguel Abril, M. E. Moreno-Raya, H. J. Hagen, S. Grohnert, Birgit Fuhrmeister, P. Redondo, F. F. Bauer, E. Rodriguez, Ralf Klein, R. Antona, A. Garcia-Piquer, J. Cano, Trifon Trifonov, A. Moya, Ansgar Reiners, Jorge Sanz-Forcada, Peter H. Hauschildt, E. Solano, J. Winkler, Manuel Perger, R. Hernández Arabí, Ignasi Ribas, C. J. Marvin, Th. Henning, V. Wolthoff, D. Maroto Fernández, Juan Gutiérrez-Soto, M. Cortés-Contreras, Eduardo L. Martín, Hugo M. Tabernero, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, German Research Foundation, Junta de Andalucía, Universidad Complutense de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), Comisión Nacional de Investigación Científica y Tecnológica (Chile), German Centre for Air and Space Travel, European Research Council, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, and Astrofísica Estelar (AE)

Subjects
Astrofísica, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Stars: late-type, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 7. Clean energy, 01 natural sciences, law.invention, Telescope, Settore FIS/05 - Astronomia e Astrofisica, Planet, law, low-mass [Stars], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Stars: low-mass, 010303 astronomy & astrophysics, Spectrograph, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astronomía y Astrofísica, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Near-infrared spectroscopy, Stars: rotation, Astronomy and Astrophysics, Atlases, Catalogues, Exoplanet, Infrared: stars, Radial velocity, Astronomía, rotation [Stars], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, late-type [Stars], stars [Infrared], Astrophysics::Earth and Planetary Astrophysics, Catalogs, Astrophysics - Earth and Planetary Astrophysics
Abstract

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

Published
2018

7. GRAVITY chromatic imaging of η Car's core. Milliarcsecond resolution imaging of the wind-wind collision zone (Brγ, He I)

Author

S. Kellner, Pierre Kervella, Faustine Cantalloube, Johana Panduro, Magdalena Lippa, V. Coudé du Foresto, Y. Clénet, R. Abuter, G. Avila, Matteo Accardo, Konrad R. W. Tristram, Dan Popovic, Alejandra Rosales, A. Buron, R. Genzel, C. Deen, Laurent Jocou, Markus Schöller, T. Ott, H. Bonnet, P. Fédou, Frank Eisenhauer, R. van Boekel, Stefan Hippler, André Müller, Pierre Léna, Thibaut Moulin, Julien Woillez, L. Pallanca, Ekkehard Wieprecht, P.-O. Petrucci, N. Hubin, Leander Mehrgan, Sylvestre Lacour, Markus Wittkowski, Vincent Lapeyrere, Christian A. Hummel, M. Haug, Eckhard Sturm, Frederic Derie, Thanh Phan Duc, Sarah Kendrew, Burkhard Wolff, Mario Kiekebusch, Nicolas Blind, Andreas Kaufer, W. J. de Wit, Feng Gao, C. Collin, Silvia Scheithauer, L. Kern, Roderick Dembet, Matthew Horrobin, J.-U. Pott, Stefan Gillessen, Johann Kolb, Narsireddy Anugu, R.-R. Rohloff, M. Riquelme, J. Sanchez-Bermudez, Andreas Eckart, J. Moreno-Ventas, R. Brast, Z. Hubert, Isabelle Percheron, M. Mellein, F. Delplancke-Ströbele, M. Karl, Udo Neumann, Imke Wank, Rainer Lenzen, Odele Straub, Michael Esselborn, Armin Huber, J.-B. Le Bouquin, Ralf Klein, Juan-Luis Ramos, Erich Wiezorrek, Samuel Lévêque, K. Perraut, Frédéric Cassaing, C. E. Garcia Dabo, F. Müller, P. M. Plewa, Ewald Müller, N. Ventura, F. Chapron, Gerd Weigelt, M. Ebert, Martin Kulas, M. Wiest, Elodie Choquet, Luca Pasquini, A. Caratti o Garatti, A. Pflüger, T. de Zeeuw, Guy Perrin, Myriam Benisty, Yves Magnard, Joachim M. Bestenlehner, S. Oberti, António Amorim, Nicolas Schuhler, B. Lazareff, Paulo J. V. Garcia, Jason Dexter, Christian Straubmeier, Th. Henning, Jason Spyromilio, F. H. Vincent, A. Mérand, Senol Yazici, Felix Widmann, C. Rau, Pierre Bourget, R. J. García López, Xavier Haubois, Eric Gendron, Gérard Zins, G. Rousset, Andres J. Ramirez, Gilles Duvert, T. Paumard, Lieselotte Jochum, Idel Waisberg, F. Haussmann, O. Pfuhl, Sebastian Rabien, G. Rodríguez-Coira, Gerd Jakob, J. P. Berger, Wolfgang Brandner, D. Ziegler, and Marcos Suarez

Subjects
Physics, 010308 nuclear & particles physics, Binary number, Astronomy and Astrophysics, Astrophysics, Collision, 01 natural sciences, Galaxy, Wavelength, 13. Climate action, Space and Planetary Science, Angular diameter, 0103 physical sciences, Radiative transfer, Chromatic scale, 010303 astronomy & astrophysics, Cavity wall
Abstract

Context. η Car is one of the most intriguing luminous blue variables in the Galaxy. Observations and models of the X-ray, ultraviolet, optical, and infrared emission suggest a central binary in a highly eccentric orbit with a 5.54 yr period residing in its core. 2D and 3D radiative transfer and hydrodynamic simulations predict a primary with a dense and slow stellar wind that interacts with the faster and lower density wind of the secondary. The wind-wind collision scenario suggests that the secondary’s wind penetrates the primary’s wind creating a low-density cavity in it, with dense walls where the two winds interact. However, the morphology of the cavity and its physical properties are not yet fully constrained. Aims. We aim to trace the inner ∼5–50 au structure of η Car’s wind-wind interaction, as seen through Brγ and, for the first time, through the He I 2s-2p line. Methods. We have used spectro-interferometric observations with the K-band beam-combiner GRAVITY at the VLTI. The analyses of the data include (i) parametrical model-fitting to the interferometric observables, (ii) a CMFGEN model of the source’s spectrum, and (iii) interferometric image reconstruction. Results. Our geometrical modeling of the continuum data allows us to estimate its FWHM angular size close to 2 mas and an elongation ratio ϵ = 1.06 ± 0.05 over a PA = 130° ± 20°. Our CMFGEN modeling of the spectrum helped us to confirm that the role of the secondary should be taken into account to properly reproduce the observed Brγ and He I lines. Chromatic images across the Brγ line reveal a southeast arc-like feature, possibly associated to the hot post-shocked winds flowing along the cavity wall. The images of the He I 2s-2p line served to constrain the 20 mas (∼50 au) structure of the line-emitting region. The observed morphology of He I suggests that the secondary is responsible for the ionized material that produces the line profile. Both the Brγ and the He I 2s-2p maps are consistent with previous hydrodynamical models of the colliding wind scenario. Future dedicated simulations together with an extensive interferometric campaign are necessary to refine our constraints on the wind and stellar parameters of the binary, which finally will help us predict the evolutionary path of η Car.

Published
2018

8. CARMENES: high-resolution spectra and precise radial velocities in the red and infrared

Author

R. Gonzalez Peinado, Ralf Launhardt, Lluis Gesa, C. del Burgo, F. F. Bauer, M. Doellinger, R. P. Hedrosa, J. Carro, Jose A. Caballero, Z. M. Berdiñas, D. Montes, Ulrich Mall, M. Blümcke, M. Kehr, S. Schäfer, D. Pérez-Medialdea, M. Salz, Mercedes López-Morales, E. N. Johnson, V. Wolthoff, A. Rosich, Mathias Zechmeister, P. Redondo, E. Mirabet, E. Díez-Alonso, Johana Panduro, L. Hernández Castaño, P. Rhode, I. Hermelo, David Barrado, Enric Palle, Walter Seifert, Manuel Perger, Javier López-Santiago, D. Benítez, E. Herrero, S. Sabotta, Víctor J. S. Béjar, M. L. García-Vargas, S. Becerril, M. J. López González, Rainer Lenzen, Luigi Mancini, M. Lafarga, A. Kaminski, P. Schöfer, M. E. Moreno-Raya, R.-R. Rohloff, H. W. Rix, C. J. Marvin, Ignasi Ribas, R. Garrido, J. A. Marín Molina, D. Hermann, Emilio Marfil, J. H. M. M. Schmitt, M. Pluto, M. Cortés-Contreras, Reinhard Mundt, M. A. Sánchez Carrasco, L. González-Cuesta, Th. Henning, J. Klüter, M. Tala Pinto, D. Galadí-Enríquez, P. Huke, J. Pascual, M. López del Fresno, Grzegorz Nowak, Trifon Trifonov, M. Llamas, P. H. Hauschildt, G. Veredas, N. Lodieu, E. de Juan, J. B. P. Strachan, S. Sadegi, W. Xu, O. Herbort, E. de Guindos, J. Sanz-Forcada, M. Lampón, Michael Perryman, K. F. Huber, Josep Colomé, Denis Shulyak, M. Kim, J. Aceituno, Lisa Nortmann, Andreas Quirrenbach, Juan Carlos Suárez, C. Cardona Guillén, Ana Pérez-Calpena, A. Claret, Martin Kürster, Werner Laun, J. Cano, Lev Tal-Or, A. Garcia-Piquer, F. J. Alonso-Floriano, B. Arroyo-Torres, A. Klutsch, Hubert Klahr, H. Martínez-Rodríguez, Ulrich Grözinger, O. Stahl, S. Pedraz, S. Martin-Ruiz, M. Azzaro, J. L. Lizon, C. Feiz, Manuel López-Puertas, M. Ammler-von Eiff, M. R. Zapatero Osorio, Rafael Luque, I. Gallardo, Guillem Anglada-Escudé, L. Sairam, J. F. López Salas, H. Mandel, A. Ramón, D. Hidalgo, N. Labiche, J. Guàrdia, F. Hernández Hernando, U. Lemke, Francesc Vilardell, E. González-Álvarez, J. Stürmer, Hugo M. Tabernero, G. Bergondy, R. Hernández Arabí, Vianak Naranjo, J. Winkler, Armin Huber, Fei Yan, B. Fuhrmeister, Rafael Rebolo, Simon Tulloch, Ansgar Reiners, F. J. Lázaro, A. P. Hatzes, H. Magán Madinabeitia, Paula Sarkis, J. Helmling, Z. Zhao, Sabine Reffert, E. Casal, A. Sánchez-López, M. C. Gálvez-Ortiz, J. I. González Hernández, D. Hintz, D. Baroch, A. Lamert, E. L. Martín, A. Schweitzer, Evangelos Nagel, V. Gómez Galera, M. Fernández, A. Guijarro, C. Cifuentes, E. Sánchez-Blanco, R. G. Ulbrich, Carlo Schmidt, F. Labarga, Pedro J. Amado, V. M. Passegger, F. J. Abellán, S. Grohnert, F. Rodler, Ricardo Dorda, Clemens Storz, G. Gaisné, K. Frölich, A. Moya, Juan Carlos Morales, E. W. Guenther, E. Rodriguez, H. J. Hagen, Ralf Klein, D. Maroto Fernández, I. M. Ferro, Karl Wagner, L. M. Lara, S. Dreizler, S. Czesla, M. Brinkmöller, M. C. Cardenas, Enrique Solano, M. Vidal-Dasilva, C. Rodríguez López, M. Abril, G. Holgado, J. Schiller, L. F. Sarmiento, A. Pavlov, H. Anwand-Heerwart, S. V. Jeffers, S. Reinhart, J. L. Vico Linares, and Richard J. Mathar

Subjects
Astrofísica, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, 010309 optics, Planet, Spectrographs, Cool Stars, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), M Dwarfs, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Optical Instrumentation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Extrasolar Planets, Exoplanet, Radial velocity, Stars, 13. Climate action, Terrestrial planet, Spectral atlas, Astrophysics::Earth and Planetary Astrophysics, Circumstellar habitable zone, Near-Infrared Instrumentation
Abstract

The design and construction of CARMENES has been presented at previous SPIE conferences. It is a next-generation radial-velocity instrument at the 3.5m telescope of the Calar Alto Observatory, which was built by a consortium of eleven Spanish and German institutions. CARMENES consists of two separate échelle spectrographs covering the wavelength range from 0.52 to 1.71¿m at a spec-tral resolution of R < 80,000, fed by fibers from the Cassegrain focus of the telescope. CARMENES saw ¿First Light¿ on Nov 9, 2015. During the commissioning and initial operation phases, we established basic performance data such as throughput and spectral resolution. We found that our hollow-cathode lamps are suitable for precise wavelength calibration, but their spectra contain a number of lines of neon or argon that are so bright that the lamps cannot be used in simultaneous exposures with stars. We have therefore adopted a calibration procedure that uses simultaneous star / Fabry Pérot etalon exposures in combination with a cross-calibration between the etalons and hollow-cathode lamps during daytime. With this strategy it has been possible to achieve 1-2 m/s precision in the visible and 5-10 m/s precision in the near-IR; further improvements are expected from ongoing work on temperature control, calibration procedures and data reduction. Comparing the RV precision achieved in different wavelength bands, we find a ¿sweet spot¿ between 0.7 and 0.8¿m, where deep TiO bands provide rich RV information in mid-M dwarfs. This is in contrast to our pre-survey models, which predicted comparatively better performance in the near-IR around 1¿m, and explains in part why our near-IR RVs do not reach the same precision level as those taken with the visible spectrograph. We are now conducting a large survey of 340 nearby M dwarfs (with an average distance of only 12pc), with the goal of finding terrestrial planets in their habitable zones. We have detected the signatures of several previously known or suspected planets and also discovered several new planets. We find that the radial velocity periodograms of many M dwarfs show several significant peaks. The development of robust methods to distinguish planet signatures from activity-induced radial velocity jitter is therefore among our priorities. Due to its large wavelength coverage, the CARMENES survey is generating a unique data set for studies of M star atmospheres, rotation, and activity. The spectra cover important diagnostic lines for activity (H alpha, Na I D1 and D2, and the Ca II infrared triplet), as well as FeH lines, from which the magnetic field can be inferred. Correlating the time series of these features with each other, and with wavelength-dependent radial velocities, provides excellent handles for the discrimination between planetary companions and stellar radial velocity jitter. These data are also generating new insight into the physical properties of M dwarf atmospheres, and the impact of activity and flares on the habitability of M star planets. © 2018 SPIE., CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Science, the German Science Foundation through the Major Research Instrumentation Program and DFG Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia.

Published
2018

9. Submilliarcsecond Optical Interferometry of the High-mass X-Ray Binary BP Cru with VLTI/GRAVITY

Author

Christian Straubmeier, Th. Henning, Stefan Hippler, Gert Finger, Antoine Mérand, W. J. de Wit, H. Bonnet, Stefan Gillessen, R.-R. Rohloff, T. Ott, F. Haussmann, Eckhard Sturm, Laurent Jocou, Andreas Eckart, Yann Clénet, Martin Kulas, Oliver Pfuhl, Nicolas Blind, Jean-Philippe Berger, Pierre Léna, Jason Dexter, Senol Yazici, Markus Schöller, Julien Woillez, R. Genzel, Lieselotte Jochum, Sebastian Rabien, Gérard Rousset, Silvia Scheithauer, C. Rau, Z. Hubert, Frederic H. Vincent, Joany Andreina Manjarres Ramos, P. Fédou, V. Lapeyrère, Marcus Haug, Guy Perrin, Laurent Pallanca, Wolfgang Brandner, Ewald Müller, R. Garcia Lopez, Imke Wank, Roberto Abuter, F. Delplancke-Ströbele, Sylvestre Lacour, Karine Perraut, J.-B. Le Bouquin, Frank Eisenhauer, A. Buron, Idel Waisberg, Yitping Kok, Matthew Horrobin, Paulo J. V. Garcia, J. Sanchez-Bermudez, Erich Wiezorrek, Casey Deen, R. Dembet, Pierre Kervella, Magdalena Lippa, A. Ramirez, Ekkehard Wieprecht, Markus Wittkowski, Johana Panduro, Thibaut Paumard, Narsireddy Anugu, António Amorim, Eric Gendron, Xavier Haubois, M. Wiest, Gilles Duvert, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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 Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), GRAVITY, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), 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]), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), and 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 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 ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
Physics, Final version, Gravity (chemistry), 010308 nuclear & particles physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], X-ray binary, techniques: high angular resolution, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, circumstellar matter, Interferometry, X-rays: binaries, 13. Climate action, Space and Planetary Science, techniques: interferometric, 0103 physical sciences, High mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, X-rays: individual
Abstract

International audience; We observe the high-mass X-ray binary (HMXB) BP Cru using interferometry in the near-infrared K band with VLTI/GRAVITY. Continuum visibilities are at most partially resolved, consistent with the predicted size of the hypergiant. Differential visibility amplitude (${\rm{\Delta }}| V| \sim 5 \% $) and phase (${\rm{\Delta }}\phi \sim 2^\circ $) signatures are observed across the He i $2.059\,\mu {\rm{m}}$ and Brγ lines, the latter seen strongly in emission, unusual for the donor star’s spectral type. For a baseline $B\sim 100$ m, the differential phase rms $\sim 0\buildrel{\circ}\over{.} 2$ corresponds to an astrometric precision of $\sim 2\,\mu \mathrm{as}$. We generalize expressions for image centroid displacements and variances in the marginally resolved limit of interferometry to spectrally resolved data, and use them to derive model-independent properties of the emission such as its asymmetry, extension, and strong wavelength dependence. We propose geometric models based on an extended and distorted wind and/or a high-density gas stream, which has long been predicted to be present in this system. The observations show that optical interferometry is now able to resolve HMXBs at the spatial scale where accretion takes place, and therefore to probe the effects of the gravitational and radiation fields of the compact object on its environment.

Published
2017

10. CARMENES: an overview six months after first light

Author

E. de Juan, Ignasi Ribas, R.-R. Rohloff, D. Benítez, A. Lamert, Th. Henning, P. Rhode, Karl Wagner, Josep Colomé, Sebastian Schafer, M. Cortés-Contreras, R. G. Ulbrich, F. J. Alonso-Floriano, R. Gonzalez Peinado, Simon Tulloch, H. Anwand-Heerwart, Juan Carlos Suárez, Florian Rodler, M. C. Gálvez-Ortiz, Hugo M. Tabernero, A. P. Hatzes, Jesús Aceituno, Birgit Fuhrmeister, Clemens Storz, R. Morales Muñoz, Ana Pérez-Calpena, J. Schiller, M. Llamas, Evangelos Nagel, Mercedes Lopez-Morales, Sabine Reffert, A. Garcia-Piquer, F. F. Bauer, E. Rodriguez, Ulrich Mall, Eike W. Guenther, Holger Mandel, A. Claret, Ralf Klein, Ralf Launhardt, A. Quirrenbach, P. Schöfer, David Barrado, Javier López-Santiago, E. Mirabet, Jorge Sanz-Forcada, Enric Palle, U. Lemke, V. M. Passegger, Stefan Dreizler, Víctor J. S. Béjar, J. Stürmer, C. Rodríguez López, Werner Laun, Grzegorz Nowak, M. Lafarga, Peter H. Hauschildt, E. Solano, J. Winkler, K. F. Huber, Rafael Rebolo, M. Kehr, M. C. Cardenas, D. Galadí, J. F. López Salas, A. Ramón, Manuel Perger, R. Hernández Arabí, E. de Guindos, J. Klüter, M. Tala, A. Rosich, Armin Huber, Paula Sarkis, Miguel Abril, S. Pedraz, V. Gómez Galera, Susana Martín-Ruiz, C. Feiz, C. del Burgo, M. Doellinger, Adrian Kaminski, M. L. García-Vargas, P. Redondo, M. Pluto, D. Montes, Ansgar Reiners, S. Becerril, C. J. Marvin, C. Schmidt, Mathias Zechmeister, Philipp Huke, J. I. González Hernández, I. M. Ferro, D. Maroto Fernández, Walter Seifert, H. W. Rix, Martin Kürster, M. Azzaro, Trifon Trifonov, I. Gallardo, Guillem Anglada-Escudé, Z. M. Berdiñas, M. A. Sánchez Carrasco, A. Pavlov, Sandra V. Jeffers, M. Brinkmöller, J. Helmling, L. F. Sarmiento, W. Xu, Andreas Schweitzer, A. Klutsch, Ulrich Grözinger, J. H. M. M. Schmitt, R. Garrido, H. J. Hagen, H. Magán Madinabeitia, S. Reinhart, L. M. Lara, Richard J. Mathar, Pedro J. Amado, Juan Carlos Morales, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, Johana Panduro, D. Hermann, Otmar Stahl, Luigi Mancini, E. L. Martin, L. Hernández Castaño, Denis Shulyak, M. A. C. Perryman, J. B. P. Strachan, J. L. Lizon, Manuel López-Puertas, M. Ammler-von Eiff, S. Czesla, M. R. Zapatero Osorio, Ernesto Sánchez-Blanco, J. I. Vico Linares, Lluis Gesa, Vianak Naranjo, Jose A. Caballero, M. López del Fresno, Reinhard Mundt, Francesc Vilardell, Aviv Ofir, D. Pérez-Medialdea, E. Herrero, E. Casal, G. Veredas, J. A. Marín Molina, M. Kim, Rainer Lenzen, and Enrique Pérez

Subjects
Astrofísica, Physics, Instrument control, Astronomy, First light, 01 natural sciences, Exoplanet, law.invention, Astronomía, 010309 optics, Telescope, Observatory, law, 0103 physical sciences, Interlock, 010303 astronomy & astrophysics, Spectrograph, Data reduction, Remote sensing
Abstract

The CARMENES instrument is a pair of high-resolution (R greater than or similar to 80, 000) spectrographs covering the wavelength range from 0.52 to 1.71 mu m, optimized for precise radial velocity measurements. It was installed and commissioned at the 3.5 m telescope of the Calar Alto observatory in Southern Spain in 2015. The first large science program of CARMENES is a survey of similar to 300 M dwarfs, which started on Jan 1, 2016. We present an overview of all subsystems of CARMENES (front end, fiber system, visible-light spectrograph, near-infrared spectrograph, calibration units, etalons, facility control, interlock system, instrument control system, data reduction pipeline, data flow, and archive), and give an overview of the assembly, integration, verification, and commissioning phases of the project. We show initial results and discuss further plans for the scientific use of CARMENES.

Published
2016

11. GRAVITY detector systems

Author

Leander H. Mehrgan, Gert Finger, Frank Eisenhauer, and Johana Panduro

Subjects
010309 optics, 0103 physical sciences, 010303 astronomy & astrophysics, 01 natural sciences
Published
2016

12. CIAO: wavefront sensors for GRAVITY

Author

Frank Eisenhauer, M. Ebert, Ralf-Rainer Rohloff, Frédéric Gonté, Lieselotte Jochum, Gert Finger, J. Moreno-Ventas, Johann Kolb, Stefan Hippler, Sarah Kendrew, Michael Esselborn, Armin Huber, Marcos Suarez, Jose Ramos, Tobias Adler, Martin Kulas, M. Riquelme, Johana Panduro, Sylvain Oberti, Adrian M. Glauser, Jürgen Ott, Laurent Jocou, Gérard Zins, Yann Clénet, Fanny Chemla, E. Müller, Zoltan Hubert, Rainer Lenzen, G. Rousset, M. Mellein, Gerd Jakob, Nicolas Schuhler, Henri Bonnet, Wolfgang Brandner, Pierre Bourget, Werner Laun, Francoise Delplancke, Casey Deen, Udo Neumann, Eric Gendron, Thomas Henning, Silvia Scheithauer, Ralf Klein, Laurent Pallanca, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and 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)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Orbital mechanics, 01 natural sciences, law.invention, Telescope, Optics, Observatory, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Adaptive optics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Wavefront, Physics, business.industry, Galactic Center, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Wavefront sensor, Astrophysics::Earth and Planetary Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

GRAVITY is a second generation near-infrared VLTI instrument that will combine the light of the four unit or four auxiliary telescopes of the ESO Paranal observatory in Chile. The major science goals are the observation of objects in close orbit around, or spiraling into the black hole in the Galactic center with unrivaled sensitivity and angular resolution as well as studies of young stellar objects and evolved stars. In order to cancel out the effect of atmospheric turbulence and to be able to see beyond dusty layers, it needs infrared wave-front sensors when operating with the unit telescopes. Therefore GRAVITY consists of the Beam Combiner Instrument (BCI) located in the VLTI laboratory and a wave-front sensor in each unit telescope Coude room, thus aptly named Coude Infrared Adaptive Optics (CIAO). This paper describes the CIAO design, assembly, integration and verification at the Paranal observatory.

Published
2016

13. System tests and on-sky commissioning of the GRAVITY-CIAO wavefront sensors

Author

Christian Straubmeier, Gérard Zins, Frank Eisenhauer, Sylvain Oberti, Michael Esselborn, R.-R. Rohloff, Martin Kulas, Rainer Lenzen, Z. Hubert, Francoise Delplancke, Thomas Henning, Pierre Bourget, Armin Huber, Silvia Scheithauer, E. Müller, Eric Gendron, Karine Perraut, Ralf Klein, Guy Perrin, Johana Panduro, Pierre Haguenauer, M. Suarez-Valles, Johann Kolb, Udo Neumann, António Amorim, Lorenzo Pettazzi, Joany Andreina Manjarres Ramos, Casey Deen, Wolfgang Brandner, H. Bonnet, Yann Clénet, Max Planck Institut fur Astronomie (Germany), European Southern Observatory (Germany), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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]), Univ. of Cologne (Germany), Laboratório de Sistemas, Faculdade de Engenharia, Universidade do Porto, and Max-Planck-Institut für Extraterrestriche Physik (MPE)

Subjects
Physics, Wavefront, Very Large Telescope, media_common.quotation_subject, Galactic Center, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrometry, 01 natural sciences, law.invention, 010309 optics, Telescope, Interferometry, law, Sky, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Remote sensing, media_common
Abstract

International audience; GRAVITY is a near-infrared interferometric instrument that allows astronomers to combine the light of the four unit or four auxiliary telescopes of the ESO Very Large Telescope in Paranal, Chile. GRAVITY will deliver extremely precise relative astrometry and spatially resolved spectra. In order to study objects in regions of high extinction (e.g. the Galactic Center, or star forming regions), GRAVITY will use infrared wavefront sensors. The suite of four wavefront sensors located in the Coudé room of each of the unit telescopes are known as the Coudé Integrated Adaptive Optics (CIAO). The CIAO wavefront sensors are being constructed by the Max Planck Institute for Astronomy (MPIA) and are being installed and commissioned at Paranal between February and September of 2016. This presentation will focus on system tests performed in the MPIA adaptive optics laboratory in Heidelberg, Germany in preparation for shipment to Paranal, as well as on-sky data from the commissioning of the first instrument. We will discuss the CIAO instruments, control strategy, optimizations, and performance at the telescope.

Published
2016

14. An overview of the mid-infrared spectro-interferometer MATISSE: science, concept, and current status

Author

Paul Jolley, M. Heininger, Martin Vannier, Marco Delbo, Y. Fantei, Udo Beckmann, Thomas Henning, Tibor Agócs, Farrokh Vakili, Stephane Lagarde, Eric Pantin, G. Martinot-Lagarde, C. Connot, Walter Jaffe, P. Antonelli, Pierre Cruzalèbes, R. Brast, Pierre Haguenauer, E. Nussbaum, Klaus Meisenheimer, L. Labadie, S. Morel, Karl-Heinz Hofmann, Bruno Lopez, Andreas Glindemann, G. Kroes, Werner Laun, M. Schuil, William C. Danchi, Sebastian Wolf, Paul Bristow, C. Bailet, Ch. Lucuix, F. Allouche, Dieter Schertl, A. van Duin, Eszter Pozna, Ralf Conzelmann, M. Lehmitz, Gert Finger, M. Mellein, Florentin Millour, Jean-Charles Augereau, Romain Petrov, Isabelle Percheron, Ralf Palsa, F. Martinache, Derek Ives, Eddy Elswijk, Gero Rupprecht, Ralph Hofferbert, N. Mauclert, S. Kiraly, Markus Schoeller, G. Csepany, A. Marcotto, Yves Bresson, C. Schmidt, Leander Mehrgan, Udo Neumann, T. Lanz, Pierre Bourget, Alain Spang, Michiel R. Hogerheijde, Ronald Roelfsema, S. Ottogalli, Carsten Dominik, Jean-Michel Clausse, M. de Haan, A. Gabasch, Felix Bettonvil, Josef Hron, Johana Panduro, Uwe Graser, J. Isderda, H. Hanenburg, Alexis Matter, Lars Venema, Christian A. Hummel, Sylvie Robbe-Dubois, A. Jasko, Anthony Meilland, Frédéric Gonté, R. van Boekel, Serge Menardi, Ph. Berio, Karl Wagner, J.-L. Lizon, Julien Woillez, Jean-Phillipe Berger, J. Kragt, Jörg-Uwe Pott, Serge Guniat, J. Behrend, R. ter Horst, G. Avila, Antoine Mérand, G. van Belle, F. Guitton, T. Phan Duc, N. Tromp, S. Kuindersma, J. Stegmeier, Gerd Jakob, Gerd Weigelt, T. Kroener, and Christoph Leinert

Subjects
Physics, Very Large Telescope, Active galactic nucleus, Young stellar object, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, First light, 01 natural sciences, 010309 optics, Interferometry, 0103 physical sciences, Astronomical interferometer, Astrophysics::Earth and Planetary Astrophysics, Spectral resolution, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

MATISSE is the second-generation mid-infrared spectrograph and imager for the Very Large Telescope Interferometer (VLTI) at Paranal. This new interferometric instrument will allow significant advances by opening new avenues in various fundamental research fields: studying the planet-forming region of disks around young stellar objects, understanding the surface structures and mass loss phenomena affecting evolved stars, and probing the environments of black holes in active galactic nuclei. As a first breakthrough, MATISSE will enlarge the spectral domain of current optical interferometers by offering the L and M bands in addition to the N band. This will open a wide wavelength domain, ranging from 2.8 to 13 um, exploring angular scales as small as 3 mas (L band) / 10 mas (N band). As a second breakthrough, MATISSE will allow mid-infrared imaging - closure-phase aperture-synthesis imaging - with up to four Unit Telescopes (UT) or Auxiliary Telescopes (AT) of the VLTI. Moreover, MATISSE will offer a spectral resolution range from R ~ 30 to R ~ 5000. Here, we present one of the main science objectives, the study of protoplanetary disks, that has driven the instrument design and motivated several VLTI upgrades (GRA4MAT and NAOMI). We introduce the physical concept of MATISSE including a description of the signal on the detectors and an evaluation of the expected performances. We also discuss the current status of the MATISSE instrument, which is entering its testing phase, and the foreseen schedule for the next two years that will lead to the first light at Paranal., Comment: SPIE Astronomical Telescopes and Instrumentation conference, June 2016, 11 pages, 6 Figures

Published
2016
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15. Integration and bench testing for the GRAVITY Coudé IR adaptive optics (CIAO) wavefront sensor

Author

Rainer Lenzen, Karine Perraut, Stefan Hippler, A. Salzinger, Sarah Kendrew, Joany Andreina Manjarres Ramos, Christian Straubmeier, Neil T. Zimmerman, Casey Deen, Th. Henning, Eric Gendron, Yann Clénet, Wolfgang Brandner, Pengqian Yang, Armin Huber, M. Suarez-Valles, Udo Neumann, Guy Perrin, António Amorim, Johana Panduro, Werner Laun, Frank Eisenhauer, R.-R. Rohloff, Ralf Klein, and Adrian M. Glauser

Subjects
Physics, Wavefront, Very Large Telescope, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Wavefront sensor, Interferometry, Optics, Upgrade, Software, Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Adaptive optics, Astrophysics::Galaxy Astrophysics, Remote sensing
Abstract

GRAVITY, a second generation instrument for the Very Large Telescope Interferometer (VLTI), will provide an astrometric precision of order 10 micro-arcseconds, an imaging resolution of 4 milli-arcseconds, and low/medium resolution spectro-interferometry. These improvements to the VLTI represent a major upgrade to its current infrared interferometric capabilities, allowing detailed study of obscured environments (e.g. the Galactic Center, young dusty planet-forming disks, dense stellar cores, AGN, etc...). Crucial to the final performance of GRAVITY, the Coude IR Adaptive Optics (CIAO) system will correct for the effects of the atmosphere at each of the VLT Unit Telescopes. CIAO consists of four new infrared Shack-Hartmann wavefront sensors (WFS) and associated real-time computers/software which will provide infrared wavefront sensing from 1.45-2.45 microns, allowing AO corrections even in regions where optically bright reference sources are scarce. We present here the latest progress on the GRAVITY wavefront sensors. We describe the adaptation and testing of a light-weight version of the ESO Standard Platform for Adaptive optics Real Time Applications (SPARTA-Light) software architecture to the needs of GRAVITY. We also describe the latest integration and test milestones for construction of the initial wave front sensor.

Published
2014

16. MATISSE status report and science forecast

Author

S. Bonhomme, Marco Delbo, Andrea Richichi, J.-U. Pott, Martin Vannier, Paul Jolley, M. Heininger, Farrokh Vakili, Johana Panduro, Gero Rupprecht, S. Ottogalli, Jean-Philippe Berger, P. Antonelli, J. L. Lizon, A. Jaskó, William C. Danchi, Francoise Delplancke, Jan Kragt, G. Martinot-Lagarde, Eric Pantin, Lucas Labadie, Isabelle Percheron, Dieter Schertl, Felix Bettonvil, Udo Neumann, Frank Przygodda, M. Lehmitz, Th. Henning, Jean-Charles Augereau, Michiel R. Hogerheijde, Yves Bresson, E. Nussbaum, Uwe Graser, Gert Finger, Werner Laun, Gerd Weigelt, T. Lanz, Y. Fantei, F. Martinache, L. Thiam, A. Crida, Tibor Agócs, C. Connot, Niels Tromp, Florentin Millour, Leander Mehrgan, Karl-Heinz Hofmann, R. Brast, Eszter Pozna, Sebastien Morel, J. Hron, F. Rigal, Stephane Lagarde, Sebastian Wolf, Walter Jaffe, Philippe B. Gitton, Ramón Navarro, Ch. Leinert, A. Glazenborg, Carsten Dominik, M. Mellein, L. Mosoni, Gabby Kroes, Pierre Haguenauer, A. Gabasch, C. Bailet, Pierre Bourget, J. C. Gonzalez, Jean-Michel Clausse, M. de Haan, Andreas Glindemann, G. Csepany, Paul Bristow, Eddy Elswijk, G. T. van Belle, Y. Hughes, Ch. Lucuix, Romain Petrov, N. Mauclert, Ralf Palsa, V. Girault, Roy von Boekel, A. Marcotto, Markus Schöller, D. Ives, H. Hanenburg, Alexis Matter, Olivier Chesneau, J. L. Menut, M. Dugué, F. Guitton, Anthony Meilland, Lars Venema, Sylvie Robbe-Dubois, G. Avila, Frédéric Gonté, U. Beckman, Serge Menardi, Klaus Meisenheimer, Ph. Berio, Karl Wagner, Julien Woillez, Rainer Köhler, Serge Guniat, J. Behrend, R. ter Horst, T. Kroener, Gerd Jakob, P. Girard, T. Phan Duc, J. Stegmeier, and Bruno Lopez

Subjects
Physics, Very Large Telescope, Young stellar object, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics, Interferometry, Planet, Astronomical interferometer, Astrophysics::Earth and Planetary Astrophysics, Spectral resolution, Spectrograph, Astrophysics::Galaxy Astrophysics, Data reduction
Abstract

MATISSE is the mid-infrared spectrograph and imager for the Very Large Telescope Interferometer (VLTI) at Paranal. This second generation interferometry instrument will open new avenues in the exploration of our Universe. Mid-infrared interferometry with MATISSE will allow significant advances in various fundamental research fields: studies of disks around young stellar objects where planets form and evolve, surface structures and mass loss of stars in late evolutionary stages, and the environments of black holes in active galactic nuclei. MATISSE is a unique instrument. As a first breakthrough it will enlarge the spectral domain used by optical interferometry by offering the L & M bands in addition to the N band, opening a wide wavelength domain, ranging from 2.8 to 13 μm on angular scales of 3 mas (L/M band) / 10 mas (N band). As a second breakthrough, it will allow mid-infrared imaging – closure-phase aperture-synthesis imaging – with up to four Unit Telescopes (UT) or Auxiliary Telescopes (AT) of the VLTI. MATISSE will offer various ranges of spectral resolution between R~30 to ~5000. In this article, we present some of the main science objectives that have driven the instrument design. We introduce the physical concept of MATISSE including a description of the signal on the detectors and an evaluation of the expected performance and discuss the project status. The operations concept will be detailed in a more specific future article, illustrating the observing templates operating the instrument, the data reduction and analysis, and the image reconstruction software.

Published
2014

17. PANIC in the lab: status before commissioning

Author

José Miguel Ibáñez, Clemens Storz, Julio Gómez, Ulrich Mall, Armin Huber, Matilde Fernández, Matthias Alter, Patrick Fopp, Antonio J. García Segura, Vianak Naranjo, Ralf-Rainer Rohloff, V. Terron, Irene Rodríguez, J. Fried, Richard J. Mathar, Klaus Meisenheimer, Peter Bizenberger, Bernhard Dorner, Johana Panduro, M. Concepcion Cárdenas Vázquez, and Werner Laun

Subjects
Pixel, Infrared, Computer science, Observatory, Project commissioning, Field of view, Spectral bands, Remote sensing
Abstract

PANIC is the new PAnoramic Near-Infrared camera for Calar Alto, a joint project by the MPIA in Heidelberg, Germany, and the IAA in Granada, Spain. It can be operated at the 2.2m or 3.5m CAHA telescopes to observe a field of view of 30'x30' or 15'x15' respectively, with a sampling of 4096x4096 pixels. It is designed for the spectral bands from Z to K, and can be equipped with additional narrow-band filters. The instrument is close to completion and will be delivered to the observatory in Spain in fall 2014. It is currently in the last stage of assembly, where the optical elements are being aligned, which will be followed by final laboratory tests of the instrument. This paper contains an update of the recent progress and shows results from the optical alignment and detector performance tests.

Published
2014

18. CARMENES Instrument Overview

Author

Mercedes Lopez-Morales, F. F. Bauer, Javier López-Santiago, Johana Panduro, E. Mirabet, M. Fernandez, J. Guàrdia, Ana Pérez-Calpena, H. Martínez-Rodríguez, Pedro J. Amado, P. Rhode, M. Kehr, Ansgar Reiners, Mauro López del Fresno, K. F. Huber, E. de Juan, Otmar Stahl, R. G. Ulbrich, David Barrado, M. A. C. Perryman, Enric Palle, Cristina Rodríguez-López, Víctor J. S. Béjar, J. Stürmer, R.-R. Rohloff, D. Benítez, A. Garcia-Piquer, J. Helmling, R. Antona Jiménez, E. Rodríguez-Pérez, B. López Martí, Clemens Storz, Josep Colomé, G. Holgado, D. Galadí, C. Feiz, Sebastian Schafer, W. Xu, R. Morales Muñoz, Ulrich Mall, Werner Laun, A. Ramón, E. de Guindos, R. Garrido, Simon Tulloch, F. J. Alonso-Floriano, A. P. Hatzes, Jesús Aceituno, J. I. González Hernández, S. Dreizler, C. Schmidt, V. Gómez Galera, C. J. Marvin, A. Rosich, A. Claret, Juan Carlos Morales, Mathias Zechmeister, J. H. M. M. Schmitt, Juan Carlos Suárez, S. Reinhardt, Walter Seifert, Rainer Lenzen, C. del Burgo, M. Doellinger, Miguel Abril, Florian Rodler, H. W. Rix, D. Montes, V. M. Passegger, Eike W. Guenther, M. C. Gálvez-Ortiz, Ernesto Sánchez-Blanco, P. Redondo, M. L. García-Vargas, S. Becerril, Holger Mandel, E. González Álvarez, A. Moya, H. Anwand-Heerwart, Vianak Naranjo, Martin Kürster, A. Quirrenbach, Susana Martín-Ruiz, J. Schiller, D. Hidalgo, M. Pluto, D. Hermann, A. Klutsch, D. Pérez Medialdea, Rafael Rebolo, Armin Huber, J. L. Lizon, M. Ammler-von Eiff, E. Rodriguez, M. R. Zapatero Osorio, M. Azzaro, A. Lamert, Guillem Anglada-Escudé, M. A. Sánchez Carrasco, Ralf Klein, Aviv Ofir, Karl Wagner, H. J. Hagen, Eduardo L. Martín, Z. M. Berdiñas, Sandra V. Jeffers, R. Oreiro, L. F. Sarmiento, M. C. Cárdenas, U. Lemke, Ulrich Grözinger, Sabine Reffert, Richard J. Mathar, Jorge Sanz-Forcada, Peter H. Hauschildt, E. Solano, J. Winkler, Manuel Perger, Ignasi Ribas, Th. Henning, S. Lalitha, Juan Gutiérrez-Soto, M. Cortés-Contreras, Lluis Gesa, Jose A. Caballero, L. Hernández Castaño, F. J. Abellán de Paco, E. Herrero, G. Veredas, E. Casal, Viki Joergens, Reinhard Mundt, and S. Czesla

Subjects
Physics, Astrofísica, business.industry, Cassegrain reflector, Dichroic glass, Stellar classification, Exoplanet, law.invention, Telescope, Astronomía, Optics, Observatory, law, Spectral resolution, business, Spectrograph
Abstract

This paper gives an overview of the CARMENES instrument and of the survey that will be carried out with it during the first years of operation. CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Echelle Spectrographs) is a next-generation radial-velocity instrument under construction for the 3.5m telescope at the Calar Alto Observatory by a consortium of eleven Spanish and German institutions. The scientific goal of the project is conducting a 600-night exoplanet survey targeting ∽ 300 M dwarfs with the completed instrument. The CARMENES instrument consists of two separate echelle spectrographs covering the wavelength range from 0.55 to 1.7 μm at a spectral resolution of R = 82,000, fed by fibers from the Cassegrain focus of the telescope. The spectrographs are housed in vacuum tanks providing the temperature-stabilized environments necessary to enable a 1 m/s radial velocity precision employing a simultaneous calibration with an emission-line lamp or with a Fabry-Perot etalon. For mid-M to late-M spectral types, the wavelength range around 1.0 μm (γ band) is the most important wavelength region for radial velocity work. Therefore, the efficiency of CARMENES has been optimized in this range. The CARMENES instrument consists of two spectrographs, one equipped with a 4k x 4k pixel CCD for the range 0.55 -1.05 μm, and one with two 2k x 2k pixel HgCdTe detectors for the range from 0.95 -1.7 μm. Each spectrograph will be coupled to the 3.5m telescope with two optical fibers, one for the target, and one for calibration light. The front end contains a dichroic beam splitter and an atmospheric dispersion corrector, to feed the light into the fibers leading to the spectrographs. Guiding is performed with a separate camera; on-axis as well as off-axis guiding modes are implemented. Fibers with octagonal cross-section are employed to ensure good stability of the output in the presence of residual guiding errors. The fibers are continually actuated to reduce modal noise. The spectrographs are mounted on benches inside vacuum tanks located in the coude laboratory of the 3.5m dome. Each vacuum tank is equipped with a temperature stabilization system capable of keeping the temperature constant to within ±0.01ºC over 24 hours. The visible-light spectrograph will be operated near room temperature, while the near-IR spectrograph will be cooled to ∽ 140 K. The CARMENES instrument passed its final design review in February 2013. The MAIV phase is currently ongoing. First tests at the telescope are scheduled for early 2015. Completion of the full instrument is planned for the fall of 2015. At least 600 useable nights have been allocated at the Calar Alto 3.5m Telescope for the CARMENES survey in the time frame until 2018. A data base of M stars (dubbed CARMENCITA) has been compiled from which the CARMENES sample can be selected. CARMENCITA contains information on all relevant properties of the potential targets. Dedicated imaging, photometric, and spectroscopic observations are underway to provide crucial data on these stars that are not available in the literature.

Published
2014

19. Standard modes of MPIA's current H2/H2RG-readout systems

Author

Clemens Storz, Ulrich Mall, Johana Panduro, Peter Bizenberger, Jose Ramos, and Vianak Naranjo

Subjects
chemistry.chemical_compound, Mode (computer interface), Current (mathematics), chemistry, business.industry, Observatory, Computer science, Detector, Electrical engineering, Electronics, Mercury cadmium telluride, business, Simulation
Abstract

Even though the last instruments built with the previous generation of MPIA-ROE are offering in the meantime most of the standard readout modes, the current generation ROE is based on the experience of the last years, and besides other properties like small volume, more channels, less power consumption, etc., it will also allow extended readout modes in the near future by using the detector engineering and data interfaces of GEIRS. The Hawaii-2-RG detector has a large amount of operational flexibilities to support extended readout modes. With special properties in the pattern generator of the ROE and in GEIRS, new extended readout modes can be implemented identically for the Hawaii-2 and the Hawaii-2RG in multichannel mode. This paper presents an overview of the standard readout schemes and describes additional selectable options, offered idle-modes, and some new extended modes available with this generation of MPIA-ROE for the next instruments and instrument updates using HgCdTe-detectors. During the last 15 years MPIA has built 8 sets of previous readout electronics (ROE) for 8 astronomical infrared instruments 1-8 . The generic infrared camera software GEIRS (spoken like 'cheers') is used in these instruments either as a pure readout software layer or as an overall control software for IR-instruments, the last case in particular with instruments for the Calar-Alto observatory in Spain.

Published
2012

20. The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems

Author

E. de Juan, Ralf Launhardt, M. Zechmeister, P. Rhode, Birgit Fuhrmeister, E. Díez-Alonso, Rafael Luque, H. J. Hagen, David Barrado, H. W. Rix, Ignasi Ribas, J. F. López Salas, L. M. Lara, Enric Palle, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, F. F. Bauer, Paula Sarkis, J. Stürmer, C. J. Marvin, Ovidio Rabaza, J. I. González Hernández, V. Wolthoff, Grzegorz Nowak, Jose Antonio Pascual, P. Schöfer, D. Maroto Fernández, Richard J. Mathar, Juan Gutiérrez-Soto, M. Cortés-Contreras, A. Claret, A. Kaminski, S. Grohnert, M. Lafarga, Walter Seifert, A. Guijarro, Susana Martín-Ruiz, I. Hermelo, A. Rosich, S. Sadegi, W. Xu, Holger Mandel, C. del Burgo, S. V. Jeffers, H. Magán Madinabeitia, Jorge Sanz-Forcada, M. Pluto, R.-R. Rohloff, D. Benítez, J. Klüter, M. Tala, Eike W. Guenther, D. Galadí-Enríquez, D. Montes, Ana Pérez-Calpena, Josep Colomé, Peter H. Hauschildt, M. Brinkmöller, Werner Laun, C. Feiz, A. Pavlov, E. Solano, J. Winkler, Eduardo L. Martín, Hugo M. Tabernero, U. Lemke, Ulrich Mall, Andreas Schweitzer, Manuel Perger, R. Hernández Arabí, Miguel Abril, A. Ramón, E. de Guindos, L. F. Sarmiento, Simon Tulloch, Karl Wagner, S. Pedraz, Fei Yan, J. B. P. Strachan, R. P. Hedrosa, A. P. Hatzes, Jesús Aceituno, P. Redondo, Guillem Anglada-Escudé, Johana Panduro, Rafael Rebolo, R. Oreiro, Philipp Huke, A. Sánchez-López, E. Rodriguez, E. Herrero, Evangelos Nagel, V. Gómez Galera, V. M. Passegger, Ralf Klein, M. E. Moreno-Raya, Otmar Stahl, H. Anwand-Heerwart, M. Azzaro, E. Casal, Luigi Mancini, M. A. C. Perryman, M. A. Sánchez Carrasco, J. Schiller, J. H. M. M. Schmitt, S. Reinhardt, M. Lampón, Z. M. Berdiñas, B. Arroyo-Torres, A. Klutsch, Ulrich Grözinger, S. Czesla, J. I. Vico Linares, M. J. López-González, M. López del Fresno, Reinhard Mundt, Sebastian Schafer, L. Hernández Castaño, Juan Carlos Suárez, Florian Rodler, D. Baroch, Lluis Gesa, Jose A. Caballero, M. Kürster, M. Blümcke, Emilio Marfil, Gilles Bergond, G. Veredas, C. Cifuentes, J. A. Marín Molina, F. J. Alonso-Floriano, Ernesto Sánchez-Blanco, S. Becerril, I. M. Ferro, Vianak Naranjo, Javier López-Santiago, E. Mirabet, J. Helmling, E. N. Johnson, Ansgar Reiners, R. Antona, M. L. García Vargas, A. Garcia-Piquer, Pedro J. Amado, A. Rodríguez Trinidad, J. Cano, M. Kim, Juan Carlos Morales, Trifon Trifonov, Lisa Nortmann, Andreas Quirrenbach, A. Moya, Th. Henning, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, Manuel López-Puertas, M. Ammler-von Eiff, M. R. Zapatero Osorio, Francesc Vilardell, M. C. Cárdenas Vázquez, Aviv Ofir, Rainer Lenzen, R. González-Peinado, Sabine Reffert, D. Pérez Medialdea, Armin Huber, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, German Research Foundation, Junta de Andalucía, Universidad Complutense de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), Comisión Nacional de Investigación Científica y Tecnológica (Chile), and German Centre for Air and Space Travel

Subjects
Astrofísica, FOS: Physical sciences, Context (language use), Stars: late-type, Astrophysics, 7. Clean energy, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, low-mass [Stars], Planet, 0103 physical sciences, Stars: low-mass, 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Orbital elements, Physics, Planets and satellites: dynamical evolution and stability, 010308 nuclear & particles physics, Astronomy and Astrophysics, Planetary system, dynamical evolution and stability [Planets and satellites], Exoplanet, Radial velocity, Astronomía, Planetary systems, Stars, 13. Climate action, Space and Planetary Science, late-type [Stars], Terrestrial planet, Astrophysics - Earth and Planetary Astrophysics
Abstract

The appendix tables are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/609/A117, Context. The main goal of the CARMENES survey is to find Earth-mass planets around nearby M-dwarf stars. Seven M dwarfs included in the CARMENES sample had been observed before with HIRES and HARPS and either were reported to have one short period planetary companion (GJ 15 A, GJ 176, GJ 436, GJ 536 and GJ 1148) or are multiple planetary systems (GJ 581 and GJ 876). Aims. We aim to report new precise optical radial velocity measurements for these planet hosts and test the overall capabilities of CARMENES. Methods. We combined our CARMENES precise Doppler measurements with those available from HIRES and HARPS and derived new orbital parameters for the systems. Bona-fide single planet systems were fitted with a Keplerian model. The multiple planet systems were analyzed using a self-consistent dynamical model and their best fit orbits were tested for long-term stability. Results. We confirm or provide supportive arguments for planets around all the investigated stars except for GJ 15 A, for which we find that the post-discovery HIRES data and our CARMENES data do not show a signal at 11.4 days. Although we cannot confirm the super-Earth planet GJ 15 Ab, we show evidence for a possible long-period (P = 7030 d) Saturn-mass (msini = 51.8M) planet around GJ 15 A. In addition, based on our CARMENES and HIRES data we discover a second planet around GJ 1148, for which we estimate a period P = 532.6 days, eccentricity e = 0.342 and minimum mass msini = 68.1M. Conclusions. The CARMENES optical radial velocities have similar precision and overall scatter when compared to the Doppler measurements conducted with HARPS and HIRES. We conclude that CARMENES is an instrument that is up to the challenge of discovering rocky planets around low-mass stars.© ESO, 2018., CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Insitut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation (DFG), the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, the DFG Research Unit FOR2544 >Blue Planets around Red Stars>, and by the Junta de Andalucia. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work used the Systemic Console package (Meschiari et al. 2009) for cross-checking our Keplerian and Dynamical fits and the python package astroML (VanderPlas et al. 2012) for the calculation of the GLS periodogram. The IEEC-CSIC team acknowledges support by the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grant ESP2016-80435-C2-1-R, as well as the support of the Generalitat de Catalunya/CERCA programme. The IAA-CSIC team acknowledges support by the Spanish Ministry of Economy and Competitiveness (MINECO) through grants AYA2014-54348-C03-01 and AYA2016-79425-C3-3-P as well as FEDER funds. The UCM team acknowledges support by the Spanish Ministry of Economy and Competitiveness (MINECO) from projects AYA2015-68012-C2-2-P and AYA2016-79425- C3-1,2,3-P and the Spanish Ministerio de Educacion, Cultura y Deporte, programa de Formacion de Profesorado Universitario, under grant FPU15/01476. T. T. and M.K. thank to Jan Rybizki for the very helpful discussion in the early phases of this work. V.J.S.B. is supported by grant AYA2015-69350-C3-2-P from the Spanish Ministry of Economy and Competiveness (MINECO). J.C.S. acknowledges funding support from Spanish public funds for research under project ESP2015-65712-C5-5-R (MINECO/FEDER), and under Research Fellowship program >Ramon y Cajal> with reference RYC2012-09913 (MINECO/FEDER). The contributions of M.A. were supported by DLR (Deutsches Zentrum fur Luft- und Raumfahrt) through the grants 50OW0204 and 50OO1501. J.L.-S. acknowledges the Office of Naval Research Global (award No. N62909-15- 1-2011) for support. C.d.B. acknowledges that this work has been supported by Mexican CONACyT research grant CB-2012-183007 and the Spanish Ministry of Economy and Competitivity through projects AYA2014-54348-C3-2-R. J.I.G.H., and R.R. acknowledge financial support from the Spanish Ministry project MINECO AYA2014-56359-P. J.I.G.H. also acknowledges financial support from the Spanish MINECO under the 2013 Ramon y Cajal program MINECO RYC-2013-14875. V. Wolthoff acknowledges funding from the DFG Research Unit FOR2544 >Blue Planets around Red Stars>, project No. RE 2694/4-1.We thank the anonymous referee for the excellent comments that helped to improve the quality of this paper.

21. The CARMENES search for exoplanets around M dwarfs - HD 147379b: A nearby Neptune in the temperate zone of an early-M dwarf

Author

Lluis Gesa, A. Lamert, Jose A. Caballero, Fei Yan, M. Blümcke, Karl Wagner, J. H. M. M. Schmitt, E. de Juan, E. Casal, V. Gómez Galera, Simon Tulloch, R. Oreiro, David Barrado, P. Schöfer, M. Lampón, Eike W. Guenther, A. P. Hatzes, Jesús Aceituno, A. Rosich, Rainer Lenzen, Enric Palle, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, B. Arroyo-Torres, H. Anwand-Heerwart, U. Lemke, J. B. P. Strachan, Miguel Abril, J. Schiller, J. Helmling, Evangelos Nagel, M. Lafarga, E. N. Johnson, Walter Seifert, R. P. Hedrosa, Rafael Rebolo, A. Guijarro, Sebastian Schafer, C. del Burgo, J. Klüter, M. Tala, S. Czesla, M. E. Moreno-Raya, A. Sánchez-López, Grzegorz Nowak, D. Montes, F. Labarga, L. Hernández Castaño, Juan Carlos Suárez, A. Claret, Ulrich Mall, J. F. López Salas, J. I. Vico Linares, E. Herrero, Florian Rodler, Manuel López-Puertas, M. Ammler-von Eiff, D. Baroch, Philipp Huke, R. González-Peinado, C. Feiz, M. J. López-González, S. V. Jeffers, S. Becerril, H. Magán Madinabeitia, I. M. Ferro, M. Brinkmöller, P. Rhode, M. R. Zapatero Osorio, I. Hermelo, Francesc Vilardell, C. J. Marvin, Ralf Launhardt, Gilles Bergond, M. López del Fresno, Reinhard Mundt, M. Zechmeister, Jorge Sanz-Forcada, M. C. Cárdenas Vázquez, G. Veredas, D. Pérez Medialdea, Aviv Ofir, Andreas Schweitzer, Armin Huber, Ansgar Reiners, R. Antona, A. Garcia-Piquer, Ana Pérez-Calpena, D. Maroto Fernández, D. Galadí-Enríquez, S. Reinhart, R. G. Ulbrich, H. W. Rix, Javier López-Santiago, E. Mirabet, C. Cifuentes, Johana Panduro, L. M. Lara, J. A. Marín Molina, A. Pavlov, M. Azzaro, M. A. Sánchez Carrasco, Susana Martín-Ruiz, Birgit Fuhrmeister, V. M. Passegger, A. Kaminski, M. Pluto, Richard J. Mathar, F. F. Bauer, Otmar Stahl, L. F. Sarmiento, Z. M. Berdiñas, Eduardo L. Martín, Hugo M. Tabernero, A. Rodríguez Trinidad, M. Kim, Peter H. Hauschildt, E. Solano, J. Winkler, Manuel Perger, R. Hernández Arabí, J. Cano, Lisa Nortmann, Andreas Quirrenbach, Trifon Trifonov, A. Klutsch, Ulrich Grözinger, S. Sadegi, Luigi Mancini, A. Moya, Holger Mandel, Ovidio Rabaza, Werner Laun, M. A. C. Perryman, J. I. González Hernández, W. Xu, F. J. Alonso-Floriano, A. Ramón, Ignasi Ribas, Ernesto Sánchez-Blanco, E. de Guindos, S. Pedraz, Vianak Naranjo, Sabine Reffert, M. Kürster, V. Wolthoff, H. J. Hagen, Emilio Marfil, Juan Gutiérrez-Soto, E. Díez-Alonso, M. Cortés-Contreras, Jose Antonio Pascual, Guillem Anglada-Escudé, Rafael Luque, Paula Sarkis, J. Stürmer, P. Redondo, S. Grohnert, E. Rodriguez, Ralf Klein, R.-R. Rohloff, D. Benítez, Josep Colomé, Th. Henning, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, M. L. García Vargas, Pedro J. Amado, Juan Carlos Morales, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, Comisión Nacional de Investigación Científica y Tecnológica (Chile), German Centre for Air and Space Travel, European Research Council, and Ministerio de Ciencia, Innovación y Universidades (España)

Subjects
Rotation period, Stars: activity, Astrofísica, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Stars: late-type, 01 natural sciences, Planets and satellites: individual: HD 147379 b, Settore FIS/05 - Astronomia e Astrofisica, Neptune, Planet, low-mass [Stars], 0103 physical sciences, Stars: low-mass, Eccentricity (behavior), individual: HD 147379 [Stars], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Stars: rotation, Stars: individual: HD 147379, Astronomy and Astrophysics, Exoplanet, individual: HD147379 [Stars], Radial velocity, Astronomía, rotation [Stars], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [Stars], individual: HD147379 b [Planets and satellites], individual: HD 147379 b [Planets and satellites], activity [Stars], Astrophysics - Earth and Planetary Astrophysics
Abstract

We report on the first star discovered to host a planet detected by radial velocity (RV) observations obtained within the CARMENES survey for exoplanets around M dwarfs. HD 147379 (V = 8.9 mag, M = 0.58 ± 0.08 M⊙), a bright M0.0 V star at a distance of 10.7 pc, is found to undergo periodic RV variations with a semi-amplitude of K = 5.1 ± 0.4 m s−1 and a period of P = 86.54 ± 0.06 d. The RV signal is found in our CARMENES data, which were taken between 2016 and 2017, and is supported by HIRES/Keck observations that were obtained since 2000. The RV variations are interpreted as resulting from a planet of minimum mass mP sin i = 25 ± 2 M⊕, 1.5 times the mass of Neptune, with an orbital semi-major axis a = 0.32 au and low eccentricity (e < 0.13). HD 147379 b is orbiting inside the temperate zone around the star, where water could exist in liquid form. The RV time-series and various spectroscopic indicators show additional hints of variations at an approximate period of 21.1 d (and its first harmonic), which we attribute to the rotation period of the star., FEDER/ERF FICTS-2011-02 funds, Major Research Instrumentation Programme and DFG Research Unit FOR2544 “Blue Planets around Red Stars, European Research Council (ERC-279347), Deutsche Forschungsgemeinschaft (RE 1664/12-1, RE 2694/4-1), Bundesministerium für Bildung und Forschung (BMBF-05A14MG3, BMBF-05A17MG3), Spanish Ministry of Economy and Competitiveness (MINECO, grants AYA2015-68012-C2-2-P, AYA2016-79425-C3-1,2,3-P, AYA2015-69350-C3-2-P, AYA2014-54348-C03- 01, AYA2014-56359-P, AYA2014-54348-C3-2-R, AYA2016-79425-C3-3-P and 2013 Ramòn y Cajal program RYC-2013-14875), Fondo Europeo de Desarrollo Regional (FEDER, grant ESP2016-80435-C2-1-R, ESP2015-65712-C5- 5-R), Generalitat de Catalunya/CERCA programme, Spanish Ministerio de Educación, Cultura y Deporte, programa de Formación de Profesorado Universitario (grant FPU15/01476), Deutsches Zentrum für Luft- und Raumfahrt (grants 50OW0204 and 50OO1501), Office of Naval Research Global (award no. N62909-15-1-2011), Mexican CONACyT grant CB-2012-183007.

22. The wind and the magnetospheric accretion onto the T Tauri star S Coronae Australis at sub-au resolution

Author

Tom Ray, Jason Dexter, T. Ott, Catherine Dougados, Frank Eisenhauer, Karine Perraut, A. Buron, A. Caratti o Garatti, Christian Straubmeier, Th. Henning, Johana Panduro, F. Haussmann, Pierre Léna, Gérard Rousset, Frederic H. Vincent, Yann Clénet, Stefan Hippler, Silvia Scheithauer, Antoine Mérand, Pierre Kervella, Wolfgang Brandner, Oliver Pfuhl, Magdalena Lippa, R. Genzel, C. Rau, Marcus Haug, Z. Hubert, E. F. van Dishoeck, V. Coudé du Foresto, Guy Perrin, W. J. de Wit, Imke Wank, Senol Yazici, Idel Waisberg, Sylvestre Lacour, J. Sanchez-Bermudez, Stefan Gillessen, J.-B. Le Bouquin, C. E. Garcia Dabo, Ekkehard Wieprecht, Eckhard Sturm, Casey Deen, Laurent Jocou, R.-R. Rohloff, Martin Kulas, Markus Schöller, António Amorim, Wing-Fai Thi, Gérard Zins, Johann Kolb, Andreas Eckart, R. Garcia Lopez, A. Ramirez, Jean-Phillipe Berger, Paulo J. V. Garcia, Lucas Labadie, Matthew Horrobin, Myriam Benisty, S. Kellner, F. Delplancke-Ströbele, Erich Wiezorrek, Julien Woillez, Christian A. Hummel, Ewald Müller, Roberto Abuter, Bernard Lazareff, Paola Caselli, Eric Gendron, Xavier Haubois, M. Wiest, Thibaut Paumard, Narsireddy Anugu, H. Bonnet, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, inconnu, Inconnu, Institut Jean Le Rond d'Alembert (DALEMBERT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), SIM/IDL Faculdade de Ciências da Universidade de Lisboa (FCUL), University of Lisboa, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max-Planck-Institut für Radioastronomie (MPIFR), Max Planck Institute for Extraterrestrial Physics (MPE), Mayo Clinic [Rochester], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Transport et Environnement (INRETS/LTE), Institut National de Recherche sur les Transports et leur Sécurité (INRETS), European Southern Observatory, Swedish Space Corporation (SSC), Departamento de Control Automático (CINVESTAV-IPN), Center for Research and Advanced Studies of the National Polytechnic Institute (CINVESTAV-IPN), Diamond Light Source, Harwell, Berks, England, 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), Universität zu Köln, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], AUTRES, 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]), Institut Jean le Rond d'Alembert (DALEMBERT), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, Universiteit Leiden, GRAVITY Collaboration, Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Binary number, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, circumstellar matter, Binary component, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Binary system, Spectral resolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Physics, infrared: ISM, [PHYS]Physics [physics], stars: formation, 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Accretion (astrophysics), T Tauri star, ISM: jets and outflows, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, techniques: interferometric, ISM: individual objects: S CrA, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

To investigate the inner regions of protoplanetary disks, we performed near-infrared interferometric observations of the classical TTauri binary system S CrA. We present the first VLTI-GRAVITY high spectral resolution ($R\sim$4000) observations of a classical TTauri binary, S CrA (composed of S CrA N and S CrA S and separated by $\sim$1.4"), combining the four 8-m telescopes in dual-field mode. Our observations in the near-infrared K-band continuum reveal a disk around each binary component, with similar half-flux radii of about 0.1 au at d$\sim$130 pc, inclinations ($i=$28$\pm$3$^o$\ and $i=$22$\pm$6$^o$), and position angles (PA=0$^o\pm$6$^o$ and PA=-2$^o\pm$12$^o$), suggesting that they formed from the fragmentation of a common disk. The S CrA N spectrum shows bright HeI and Br$\gamma$ line emission exhibiting inverse P-Cygni profiles, typically associated with infalling gas. The continuum-compensated Br$\gamma$ line visibilities of S CrA N show the presence of a compact Br$\gamma$ emitting region the radius of which is about $\sim$0.06 au, which is twice as big as the truncation radius. This component is mostly tracing a wind. Moreover, a slight radius change between the blue- and red-shifted Br$\gamma$ line components is marginally detected. The presence of an inverse P-Cygni profile in the HeI and Br$\gamma$ lines, along with the tentative detection of a slightly larger size of the blue-shifted Br$\gamma$ line component, hint at the simultaneous presence of a wind and magnetospheric accretion in S CrA N., Comment: Accepted by A&A

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