125 results on '"Rainer Lenzen"'
Search Results
2. Vorwort
- Author
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Thomas Jäger and Rainer Lenzen
- Published
- 2021
3. The CARMENES search for exoplanets around M dwarfs: High-resolution optical and near-infrared spectroscopy of 324 survey stars
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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)
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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.
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- 2018
4. Detection of the gravitational redshift in the orbit of the star S2 near the Galactic centre massive black hole
- Author
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R.-R. Rohloff, Andreas Eckart, Sarah Kendrew, Maryam Habibi, Joany Andreina Manjarres Ramos, S. Kellner, Nicolas Blind, D. Ziegler, Wolfgang Brandner, Casey Deen, Bernard Lazareff, Jean-Philippe Berger, Gérard Zins, M. Haug, A. Ramirez, Eric Gendron, F. Haußmann, Thomas Ott, E. Müler, Silvia Scheithauer, Jason Spyromilio, Andreas Kaufer, Xavier Haubois, Markus Schöller, Eckhard Sturm, C. Collin, Stefan Hippler, Laurent Jocou, Myriam Benisty, Julien Woillez, Linda J. Tacconi, A. Buron, Imke Wank, S. von Fellenberg, M. Wiest, Paulo Gordo, Luca Pasquini, Pierre Kervella, L. Palanca, Magdalena Lippa, Martin Kulas, Roderick Dembet, Gilles Duvert, Z. Hubert, Jason Dexter, Yann Clénet, P. T. de Zeeuw, C. Rau, A. Jimenez Rosales, H. Bonnet, Sylvestre Lacour, Guy Perrin, Odele Straub, P. Fédou, J.-B. Le Bouquin, Christian Straubmeier, S. Yazici, Ekkehard Wieprecht, Gérard Rousset, V. Lapeyrère, N. M. Förster Schreiber, Sebastian Rabien, Felix Widmann, Th. Henning, F. Delplancke-Ströbele, M. Bauböck, F. Chapron, Frank Eisenhauer, Gert Finger, R. Garcia Lopez, G. Rodríguez-Coira, Reinhard Genzel, Frederic H. Vincent, Pierre Léna, Thibaut Paumard, Narsireddy Anugu, Idel Waisberg, J. Sanchez-Bermudez, N. Schuler, Karine Perraut, P. M. Plewa, Paulo J. V. Garcia, António Amorim, Yitping Kok, Oliver Pfuhl, Lieselotte Jochum, V. dCoudé u Foresto, Matthew Horrobin, Udo Neumann, Rainer Lenzen, Erich Wiezorrek, Antoine Mérand, Konrad R. W. Tristram, Norbert Hubin, Feng Gao, Stefan Gillessen, Roberto Abuter, 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]), 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), GRAVITY, 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), 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)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and 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)
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General relativity ,black hole physics ,FOS: Physical sciences ,Astrophysics ,Physics - Classical Physics ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,General Relativity and Quantum Cosmology ,Gravitation ,Gravitational field ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,Very Large Telescope ,Galaxy: center ,010308 nuclear & particles physics ,Classical Physics (physics.class-ph) ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,[PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph] ,Black hole ,Space and Planetary Science ,gravitation ,Astrophysics of Galaxies (astro-ph.GA) ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Schwarzschild radius ,Gravitational redshift - Abstract
The highly elliptical, 16-year-period orbit of the star S2 around the massive black hole candidate Sgr A* is a sensitive probe of the gravitational field in the Galactic centre. Near pericentre at 120 AU, ~1400 Schwarzschild radii, the star has an orbital speed of ~7650 km/s, such that the first-order effects of Special and General Relativity have now become detectable with current capabilities. Over the past 26 years, we have monitored the radial velocity and motion on the sky of S2, mainly with the SINFONI and NACO adaptive optics instruments on the ESO Very Large Telescope, and since 2016 and leading up to the pericentre approach in May 2018, with the four-telescope interferometric beam-combiner instrument GRAVITY. From data up to and including pericentre, we robustly detect the combined gravitational redshift and relativistic transverse Doppler effect for S2 of z ~ 200 km/s / c with different statistical analysis methods. When parameterising the post-Newtonian contribution from these effects by a factor f, with f = 0 and f = 1 corresponding to the Newtonian and general relativistic limits, respectively, we find from posterior fitting with different weighting schemes f = 0.90 +/- 0.09 (stat) +\- 0.15 (sys). The S2 data are inconsistent with pure Newtonian dynamics., Comment: Accepted for publication in A&A Letters, 29 June 2018, 10 pages, 6 figures, corresponding author: F. Eisenhauer
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- 2018
5. GRAVITY chromatic imaging of η Car's core. Milliarcsecond resolution imaging of the wind-wind collision zone (Brγ, He I)
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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
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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.
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- 2018
6. CARMENES: high-resolution spectra and precise radial velocities in the red and infrared
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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
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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.
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- 2018
7. CARMENES: an overview six months after first light
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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
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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
8. Mid-Infrared Instrumentation for the European Extremely Large Telescope
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Sarah Kendrew, Hans Ulrich Käufl, Remko Stuik, Gert Finger, Bernhard R. Brandl, Rainer Lenzen, Lars Venema, and Alistair Glasse
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Physics ,business.industry ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Context (language use) ,Astrophysics ,law.invention ,Telescope ,Conceptual design ,law ,Calibration ,Extremely Large Telescope ,Instrumentation (computer programming) ,Aerospace engineering ,Adaptive optics ,business ,Spectrograph - Abstract
MIDIR is the proposed thermal/mid-IR imager and spectrograph for the European Extremely Large Telescope (E-ELT). It will cover the wavelength range of 3 to at least 20 microns. Designed for diffraction-limited performance over the entire wavelength range, MIDIR will require an adaptive optics system; a cryogenically cooled system could offer optimal performance in the IR, and this is a critical aspect of the instrument design. We present here an overview of the project, including a discussion of MIDIR's science goals and a comparison with other infrared (IR) facilities planned in the next decade; top level requirements derived from these goals are outlined. We describe the optical and mechanical design work carried out in the context of a conceptual design study, and discuss some important issues to emerge from this work, related to the design, operation and calibration of the instrument. The impact of telescope optical design choices on the requirements for the MIDIR instrument is demonstrated., Comment: for publication in SPIE Proceedings vol. 6692, Cryogenic Optical Systems and Instrumentation XII, eds. J.B. Heaney and L.G. Burriesci, San Diego, Aug 2007
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- 2016
9. METIS: System engineering and optical design of the mid-infrared E-ELT instrument
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Rik ter Horst, Wolfgang Brandner, Laurent Jolissaint, Christopher M. Wright, Alistair Glasse, Ad Oudenhuysen, Hans Ulrich Käufl, Toby J. T. Moore, Bernhard R. Brandl, Thomas Henning, Christoffel Waelkens, Stefan Hippler, Maarten Baes, Lars Venema, Frank Molster, Paul van der Werf, Ewine F. van Dishoeck, Ralf Siebenmorgen, Eric Pantin, Joris Blommaert, Pierre-Olivier Lagage, Sarah Kendrew, Hermann Böhnhardt, Rainer Lenzen, and Remko Stuik
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Physics ,business.industry ,Optical polarization ,law.invention ,Telescope ,Grism ,Optics ,law ,Metis ,Spectral resolution ,Extremely large telescope ,business ,Adaptive optics ,Spectrograph ,Remote sensing - Abstract
METIS is a mid-infrared instrument proposed for the European Extremely Large Telescope (E-ELT). It is designed to provide imaging and spectroscopic capabilities in the 3μm to 14μm region up to a spectral resolution of 100.000. Here the technical concept of METIS is described which has been developed based on an elaborated science case which is presented elsewhere in this conference. There are five main opto-mechanical modules all integrated into a common cryostat: The fore-optics is re-imaging the telescope focal plane into the cryostat, including a chopper, an optical de-rotator and an un-dispersed pupil stop. The imager module provides diffraction limited direct imaging, low-resolution grism spectroscopy, polarimetry and coronagraphy. The high resolution IFU spectrograph offers a spectral resolution of 100.000 for L- and M-band and optional 50.000 for the N-band. In addition to the WFS integrated into the E-ELT, there is a METIS internal on-axis WFS operating at visual wavelengths. Finally, a cold (and an external warm) calibration unit is providing all kinds of spatial and spectral calibrations capabilities. METIS is planned to be used at one of the direct Nasmyth foci available at the E-ELT. This recently finished Phase-A study carried out within the framework of the ESO sponsored E-ELT instrumentation studies has been performed by an international consortium with institutes from Germany, Netherlands, France, United Kingdom and Belgium. © 2010 Copyright SPIE - The International Society for Optical Engineering.
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- 2016
10. Correcting METIS spectra for telluric absorption to maximize spectral fidelity
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Rainer Lenzen, Lars Venema, Metis team, Frank Molster, Klaus M. Pontoppidan, Ralf Siebenmorgen, Bernhard R. Brandl, S. Uttenthaler, Eric Pantin, Andreas Seifahrt, Phil Parr-Burman, Joris Blommaert, Sarah Kendrew, McLean, Ian S., Ramsay, Suzanne K., and Takami, Hideki
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Physics ,Absorption spectroscopy ,business.industry ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Field of view ,Stellar classification ,Spectral line ,Integral field spectrograph ,Optics ,Metis ,Astrophysics::Earth and Planetary Astrophysics ,Spectral resolution ,Astrophysics - Instrumentation and Methods for Astrophysics ,business ,Spectrograph ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics - Abstract
METIS is a mid-infrared instrument proposed for the European Extremely Large Telescope (E-ELT). It is designed to provide imaging and spectroscopic capabilities in the 3 - 14 micron region up to a spectral resolution of 100000. One of the novel concepts of METIS is that of a high-resolution integral field spectrograph (IFS) for a diffraction-limited mid-IR instrument. While this concept has many scientific and operational advantages over a long-slit spectrograph, one drawback is that the spectral resolution changes over the field of view. This has an impact on the procedures to correct for telluric absorption lines imprinted on the science spectra. They are a major obstacle in the quest to maximize spectral fidelity, the ability to distinguish a weak spectral feature from the continuum. The classical technique of division by a standard star spectrum, observed in a single IFS spaxel, cannot simply be applied to all spaxels, because the spectral resolution changes from spaxel to spaxel. Here we present and discuss possible techniques of telluric line correction of METIS IFS spectra, including the application of synthetic model spectra of telluric transmission, to maximize spectral fidelity., Comment: 11 pages, 3 figures; Copyright (2010) Society of Photo-Optical Instrumentation Engineers. One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited
- Published
- 2016
11. VLT diffraction-limited imaging and spectroscopy in the NIR: Weighing the black hole in Centaurus A with NACO
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H. W. Rix, Klaus Meisenheimer, Rainer Lenzen, M. A. Prieto, Markus Hartung, N. Haering-Neumayer, and Michele Cappellari
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Diffraction ,Physics ,Stellar mass ,Centaurus A ,Astrophysics (astro-ph) ,Velocity dispersion ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Spectral line ,law.invention ,Black hole ,Space and Planetary Science ,law ,0103 physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Hydrostatic equilibrium ,010306 general physics ,Spectroscopy ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We present high spatial resolution near-infrared spectra and images of the nucleus of Centaurus A (NGC 5128) obtained with NAOS-CONICA at the VLT. The adaptive optics corrected data have a spatial resolution of 0.06" (FWHM) in K- and 0.11" in H-band, four times higher than previous studies. The observed gas motions suggest a kinematically hot disk which is orbiting a central object and is oriented nearly perpendicular to the nuclear jet. We model the central rotation and velocity dispersion curves of the [FeII] gas orbiting in the combined potential of the stellar mass and the (dominant) black hole. Our physically most plausible model, a dynamically hot and geometrically thin gas disk, yields a black hole mass of M_bh = (6.1 +0.6/-0.8) 10^7 M_sun. As the physical state of the gas is not well understood, we also consider two limiting cases: first a cold disk model, which completely neglects the velocity dispersion; it yields an M_bh estimate that is almost two times lower. The other extreme case is to model a spherical gas distribution in hydrostatic equilibrium through Jeans equation. Compared to the hot disk model the best-fit black hole mass increases by a factor of 1.5. This wide mass range spanned by the limiting cases shows how important the gas physics is even for high resolution data. Our overall best-fitting black hole mass is a factor of 2-4 lower than previous measurements. With our revised M_bh estimate, Cen A's offset from the M_bh-sigma relation is significantly reduced; it falls above this relation by a factor of ~2, which is close to the intrinsic scatter of this relation. (Abridged), Comment: 12 pages, 14 figures, including minor changes following the referee report; accepted for publication in The Astrophysical Journal
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- 2016
12. Adaptive optics challenges for mid-IR ELT instrumentation
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Rainer Lenzen, Sarah Kendrew, Lars Venema, Alistair Glasse, Bernhard R. Brandl, Remko Stuik, and Ulli Kaeufl
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Physics ,business.industry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Physics::Optics ,Context (language use) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Optics ,Astrophysics::Earth and Planetary Astrophysics ,Instrumentation (computer programming) ,business ,Focus (optics) ,Adaptive optics ,Astrophysics::Galaxy Astrophysics ,Remote sensing - Abstract
Adaptive optics issues particular to a system operating at mid-infrared wavelengths are discussed in the context of MIDIR, the mid-IR instrument for the European ELT. Particular focus is on atmospheric properties at these wavelengths. © 2011 OSA.
- Published
- 2016
13. CIAO: wavefront sensors for GRAVITY
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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)
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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.
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- 2016
14. System tests and on-sky commissioning of the GRAVITY-CIAO wavefront sensors
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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)
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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
15. FIRST RESULTS FROM VERY LARGE TELESCOPE NACO APODIZING PHASE PLATE: 4 μm IMAGES OF THE EXOPLANET β PICTORIS b
- Author
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Julien Girard, Daniel Apai, Gael Chauvin, Mickael Bonnefoy, Rainer Lenzen, Anthony Boccaletti, Anne-Marie Lagrange, Sascha P. Quanz, Michael Meyer, Markus Kasper, Matthew A. Kenworthy, and Philip M. Hinz
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Physics ,Very Large Telescope ,Astronomy and Astrophysics ,Astrophysics ,Effective temperature ,Surface gravity ,Position angle ,Exoplanet ,law.invention ,Photometry (optics) ,Space and Planetary Science ,law ,Planet ,Coronagraph - Abstract
Direct imaging of exoplanets requires both high contrast and high spatial resolution. Here, we present the first scientific results obtained with the newly commissioned apodizing phase plate coronagraph (APP) on VLT/NACO. We detected the exoplanet β Pictoris b in the narrowband filter centered at 4.05 μm (NB4.05). The position angle (20913 ± 212) and the projected separation to its host star (0354 ± 0012, i.e., 6.8 ± 0.2 AU at a distance of 19.3 pc) are in good agreement with the recently presented data from Lagrange et al. Comparing the observed NB4.05 magnitude of 11.20 ± 0.23 mag to theoretical atmospheric models, we find a best fit with a 7-10 M Jupiter object for an age of 12 Myr, again in agreement with previous estimates. Combining our results with published L' photometry, we can compare the planet's [L' – NB4.05] color to that of cool field dwarfs of higher surface gravity suggesting an effective temperature of ~1700 K. The best-fit theoretical model predicts an effective temperature of ~1470 K, but this difference is not significant given our photometric uncertainties. Our results demonstrate the potential of NACO/APP for future planet searches and provide independent confirmation as well as complementary data for β Pic b.
- Published
- 2010
16. An Imaging Survey for Extrasolar Planets around 45 Close, Young Stars with the Simultaneous Differential Imager at the Very Large Telescope and MMT
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Laird M. Close, Douglas L. Miller, Thomas Henning, Elena Masciadri, Beth Biller, S. Kellner, Rainer Lenzen, Craig Kulesa, Eric E. Mamajek, Eric L. Nielsen, Wolfgang Brandner, Matthew A. Kenworthy, Donald W. McCarthy, and Markus Hartung
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Physics ,Very Large Telescope ,education.field_of_study ,Population ,Kepler-37d ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Planetary system ,Exoplanet ,Stars ,Space and Planetary Science ,Planet ,education - Abstract
Wepresent theresultsof asurveyof 45young(P250Myr), close(P50pc) starswiththeSimultaneous Differential Imager (SDI) implemented at the VLT and the MMT for the direct detection of extrasolar planets. As part of the survey, we observed 54 objects, consisting of 45 close, young stars; two more distant ( 2 � which behaved consistently like a real object. From our survey null result,we can rule out (with 93% confidence) a model planet population where N(a) / constant out to a distance of 45 AU.
- Published
- 2007
17. AB Doradus C: age, spectral type, orbit, and comparison to evolutionary models
- Author
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Markus Hartung, Laird M. Close, Wolfgang Brandner, Rainer Lenzen, Eric L. Nielsen, J. C. Guirado, Beth Biller, and Christopher Lidman
- Subjects
Physics ,Solar mass ,Hertzsprung–Russell diagram ,Astrophysics (astro-ph) ,Brown dwarf ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Type (model theory) ,Orbit ,symbols.namesake ,Stars ,Space and Planetary Science ,symbols ,Low Mass - Abstract
We expand upon the results of Close et al. 2005 regarding the young, low-mass object AB Dor C and its role as a calibration point for theoretical tracks. We present an improved spectral reduction and a new orbital solution with two additional epochs. Our improved analysis confirms our spectral type of M8 (+/- 1) and mass of 0.090+/-0.003 solar masses for AB Dor C. Comparing the results for AB Dor C with other young, low-mass objects with dynamical masses we find a general trend where current evolutionary models tend to over-predict the temperature (or under-predict the mass) for low mass stars and brown dwarfs. Given our precision, there is a ~99% chance that the mass of AB Dor C is underestimated by the DUSTY tracks in the HR diagram., 7 pages, 10 figures, proceedings for the workshop "Ultralow-mass star formation and evolution", to be published in Astronomische Nachrichten - Astronomical Notes
- Published
- 2005
18. The science case for exoplanets and star formation using mid-IR instrumentation at the OWL telescope
- Author
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Wolfgang Brandner, B. Brandl, and Rainer Lenzen
- Subjects
Physics ,Telescope ,Space and Planetary Science ,law ,Star formation ,Astronomy ,Astronomy and Astrophysics ,Instrumentation (computer programming) ,Exoplanet ,law.invention ,Astrobiology ,Discoveries of exoplanets - Published
- 2005
19. A Survey of Close, Young Stars with SDI at the VLT and MMT
- Author
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Thomas Henning, Markus Hartung, Elena Masciadri, Wolfgang Brandner, Rainer Lenzen, Eric L. Nielsen, Donald W. McCarthy, Laird M. Close, and Beth Biller
- Subjects
Physics ,Stars ,Space and Planetary Science ,Astronomy ,Astronomy and Astrophysics ,Astrophysics - Published
- 2005
20. On the Age, Spectral Type, Orbit, and Comparison to Evolutionary Models of AB Dor C
- Author
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Christopher Lidman, Wolfgang Brandner, Laird M. Close, Beth Biller, Rainer Lenzen, Markus Hartung, Eric L. Nielsen, and J. C. Guirado
- Subjects
Physics ,T Tauri star ,Space and Planetary Science ,K-type main-sequence star ,Brown dwarf ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Orbit (control theory) ,Type (model theory) ,Stellar classification ,Main sequence - Published
- 2005
21. Suppressing Speckle Noise for Simultaneous Differential Extrasolar Planet Imaging (SDI) at the VLT and MMT
- Author
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Donald W. McCarthy, Laird M. Close, Rainer Lenzen, Beth Biller, Eric L. Nielsen, S. Kellner, Wolfgang Brandner, and Markus Hartung
- Subjects
Physics ,Astrophysics (astro-ph) ,Brown dwarf ,FOS: Physical sciences ,Astronomy and Astrophysics ,Speckle noise ,Filter (signal processing) ,H band ,Astrophysics ,Exoplanet ,Reduction (complexity) ,Stars ,Space and Planetary Science ,Data reduction - Abstract
We discuss the instrumental and data reduction techniques used to suppress speckle noise with the Simultaneous Differential Imager (SDI) implemented at the VLT and the MMT. SDI uses a double Wollaston prism and a quad filter to take 4 identical images simultaneously at 3 wavelengths surrounding the 1.62 um methane bandhead found in the spectrum of cool brown dwarfs and gas giants. By performing a difference of images in these filters, speckle noise from the primary can be significantly attenuated, resulting in photon noise limited data past 0.5''. Non-trivial data reduction tools are necessary to pipeline the simultaneous differential imaging. Here we discuss a custom algorithm implemented in IDL to perform this reduction. The script performs basic data reduction tasks but also precisely aligns images taken in each of the filters using a custom shift and subtract routine. In our survey of nearby young stars at the VLT and MMT (see Biller et al., this conference), we achieved H band contrasts >25000 (5 sigma Delta F1(1.575 um) > 10.0 mag, Delta H > 11.5 mag for a T6 spectral type object) at a separation of 0.5" from the primary star. We believe that our SDI images are among the highest contrast astronomical images ever made from ground or space for methane rich companions., 5 pages, 3 figures, 1 table. Presented at IAU Colloquium 200, Direct Imaging of Exoplanets: Science and Techniques
- Published
- 2005
22. Search and investigation of extra-solar planets with polarimetry
- Author
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J. Tinbergen, Rainer Lenzen, F. Joos, M. Kasper, Th. Henning, Hans Martin Schmid, R. G. Gratton, Markus Feldt, Daphne Stam, Andreas Quirrenbach, D. Gisler, R. Wolstencroft, Jean-Luc Beuzit, Rens Waters, Christophe Verinaud, David Mouillet, C. Thalmann, and C. Moutou
- Subjects
Physics ,Solar System ,business.industry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Polarimetry ,Astronomy ,Astronomy and Astrophysics ,Polarimeter ,Exoplanet ,law.invention ,Stars ,Optics ,Space and Planetary Science ,Planet ,law ,Astrophysics::Solar and Stellar Astrophysics ,Terrestrial planet ,Astrophysics::Earth and Planetary Astrophysics ,business ,Coronagraph ,Astrophysics::Galaxy Astrophysics - Abstract
Light reflected from planets is polarized. This basic property of planets provides the possibility for detecting and characterizing extra-solar planets using polarimetry. The expected polarization properties of extra-solar planets are discussed that can be inferred from polarimetry of “our” solar system planets. They show a large variety of characteristics depending on the atmospheric and/or surface properties. Best candidates for a polarimetric detection are extra-solar planets with an optically thick Rayleigh scattering layer.Even the detection of highly polarized extra-solar planets requires a very sophisticated instrument. We present the results from a phase A (feasibility) study for a polarimetric arm in the ESO VLT planet finder instrument. It is shown that giant planets around nearby stars can be searched and investigated with an imaging polarimeter, combined with a powerful AO system and a coronagraph at an 8 m class telescope.A similar type of polarimeter is also considered for the direct detection of terrestrial planets using an AO system on one of the future Extremely Large Telescopes.
- Published
- 2005
23. A dynamical calibration of the mass–luminosity relation at very low stellar masses and young ages
- Author
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J. C. Guirado, Chris Lidman, Wolfgang Brandner, Eric E. Mamajek, Rainer Lenzen, Laird M. Close, Eric L. Nielsen, Markus Hartung, and Beth Biller
- Subjects
Physics ,Solar mass ,Multidisciplinary ,Stellar mass ,Young stellar object ,Mass–luminosity relation ,Brown dwarf ,Astronomy ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Luminosity ,Stars ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Planetary mass ,Astrophysics::Galaxy Astrophysics - Abstract
Mass is the most fundamental parameter of a star, yet it is also one of the most difficult to measure directly. In general, astronomers estimate stellar masses by determining the luminosity and using the 'mass-luminosity' relationship, but this relationship has never been accurately calibrated for young, low-mass stars and brown dwarfs. Masses for these low-mass objects are therefore constrained only by theoretical models. A new high-contrast adaptive optics camera enabled the discovery of a young (50 million years) companion only 0.156 arcseconds (2.3 au) from the more luminous (> 120 times brighter) star AB Doradus A. Here we report a dynamical determination of the mass of the newly resolved low-mass companion AB Dor C, whose mass is 0.090 +/- 0.005 solar masses. Given its measured 1-2-micrometre luminosity, we have found that the standard mass-luminosity relations overestimate the near-infrared luminosity of such objects by about a factor of approximately 2.5 at young ages. The young, cool objects hitherto thought to be substellar in mass are therefore about twice as massive, which means that the frequency of brown dwarfs and planetary mass objects in young stellar clusters has been overestimated.
- Published
- 2005
24. A new VLT surface map of Titan at 1.575 microns
- Author
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Rainer Lenzen, Laird M. Close, Tom Herbst, Christopher Lidman, Markus Hartung, Wolfgang Brandner, and O. Marco
- Subjects
Physics ,Solar System ,Haze ,business.industry ,Surface map ,Astronomy ,Astronomy and Astrophysics ,Methane ,chemistry.chemical_compound ,Wavelength ,symbols.namesake ,Optics ,chemistry ,Space and Planetary Science ,symbols ,Longitude ,business ,Titan (rocket family) ,Adaptive optics - Abstract
We present a first high contrast 1.575 micron surface map of Titan, that is haze corrected by simultaneously imaging the stratospheric layer. At visible and most near-infrared wavelengths, the methane rich atmosphere completely obscures the surface; only in a few narrow wavelength windows does the atmosphere become optically thin. One of the most convenient windows (Griffith et al. 2003) lies at 1.58 μm, adjacent to the methane absorption feature at 1.62 μm. Our data span seven consecutive nights, resulting in phase coverage of 275° in longitude. The images were taken with NAOS-CONICA adaptive optics system at the VLT, using the recently commissioned Simultaneous Differential Imager mode (SDI). The combination of adaptive optics and simultaneous imaging through three filters sampling the methane absorption at 1.6 micron reveals extraordinary details of Titan's surface. Providing views of Titan's surface at high resolution (60 mas) is of particular topical importance, since the Cassini-Huygens mission is currently approaching the Saturn system and the Huygens probe will enter Titan's atmosphere in early 2005.
- Published
- 2004
25. ε Indi Ba,Bb: The nearest binary brown dwarf
- Author
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Wolfgang Brandner, Mark J. McCaughrean, Rainer Lenzen, Markus Hartung, Ralf-Dieter Scholz, Laird M. Close, Beth Biller, and N. Lodieu
- Subjects
Physics ,Space and Planetary Science ,Angular distance ,Orbital motion ,Brown dwarf ,Binary number ,Astronomy and Astrophysics ,Astrophysics ,Binary system ,Orbital period ,Stellar classification ,Spectral line - Abstract
We have carried out high angular resolution near-infrared imaging and low-resolution (R~1000) spectroscopy of the nearest known brown dwarf, Eps Indi B, using the ESO VLT NAOS/CONICA adaptive optics system. We find it to be a close binary (as also noted by Volk et al. 2003) with an angular separation of 0.732 arcsec, corresponding to 2.65AU at the 3.626pc distance of the Eps Indi system. In our discovery paper (Scholz et al. 2003), we concluded that Eps Indi B was a ~50Mjup T2.5 dwarf: our revised finding is that the two system components (Eps Indi Ba and Eps Indi Bb) have spectral types of T1 and T6, respectively, and estimated masses of 47 and 28Mjup, respectively, assuming an age of 1.3Gyr. Errors in the masses are +/-10 and +/-7Mjup, respectively, dominated by the uncertainty in the age determination (0.8-2Gyr range). This uniquely well-characterised T dwarf binary system should prove important in the study of low-mass, cool brown dwarfs. The two components are bright and relatively well-resolved: Eps Indi B is the only T dwarf binary in which spectra have been obtained for both components. They have a well-established distance and age. Finally, their orbital motion can be measured on a fairly short timescale (nominal orbital period 15 yrs), permitting an accurate determination of the true total system mass, helping to calibrate brown dwarf evolutionary models.
- Published
- 2004
26. Discovery of a Candidate for the Central Star of the Ultracompact H <scp>ii</scp> Region G5.89-0.39
- Author
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Wolfgang Brandner, Elena Puga, Rainer Lenzen, Th. Henning, Eric Gendron, Bringfried Stecklum, Anne-Marie Lagrange, Gérard Rousset, Markus Feldt, 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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
- Subjects
Physics ,Very Large Telescope ,H II region ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Star (graph theory) ,Space and Planetary Science ,Primary (astronomy) ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Exact location ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Adaptive optics ,Astrophysics::Galaxy Astrophysics - Abstract
We present high-resolution, near-infrared images of the ultracompact H II region G5.89-0.39 that were taken during a commissioning run of the NACO adaptive optics/near-infrared camera system at the Very Large Telescope. For the first time, these data reveal the exact location of a very promising candidate for the primary, ionizing star of this region and provide a good estimate of its spectral type. We very briefly discuss the morphology of the region and the implications of finding the star at a location where it was quite unexpected, namely, off-center of a shell.
- Published
- 2003
27. Calibration of NAOS and CONICA static aberrations
- Author
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Gérard Rousset, Thierry Fusco, Rainer Lenzen, Laurent M. Mugnier, Markus Hartung, A. Blanc, Francois Lacombe, 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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
- Subjects
Physics ,Very Large Telescope ,biology ,business.industry ,Zernike polynomials ,Near-infrared spectroscopy ,Astrophysics::Instrumentation and Methods for Astrophysics ,Physics::Optics ,Astronomy and Astrophysics ,Wavefront sensor ,biology.organism_classification ,law.invention ,symbols.namesake ,Optics ,[SDU]Sciences of the Universe [physics] ,Space and Planetary Science ,law ,Calibration ,symbols ,Conica ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Adaptive optics ,business ,Beam splitter - Abstract
NAOS is the first adaptive optics (AO) system of the Very Large Telescope and will provide CONICA with diffraction-limited images. CONICA is a near infrared camera that offers a variety of imaging and spectroscopic observing modes. A technique will be described to benefit of the AO system to correct not only for atmospheric turbulence but also for the internal optical aberrations of the high-resolution camera and the beam splitters of NAOS. The aberrant optical components in the light path of CONICA as well as the beam splitters are outside of the AO loop and therefore no self-acting correction is possible. Independently of the AO wavefront sensor, a separate measurement of these aberrations using a method called phase diversity allows one to predict for a certain instrument configuration the corresponding aberrations. They are quantified by sets of Zernike coefficients that are rendered to the adaptive optics. This technique turns out to be very flexible and results in a further improvement of the optical overall performance. The application of phase diversity to the instrument is investigated in a preceding paper (Blanc et al. 2003). In the present paper we present in detail the instrumental implementation of phase diversity, the obtained calibration results, and the achieved gain in optical performance.
- Published
- 2003
28. [Untitled]
- Author
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W Morr, Johannes de Jong, R.-R. Rohloff, E. J. Bakker, Sebastien Morel, W. D. Cotton, Olivier Chesneau, Richard J. Mathar, Udo Neumann, H. Hanenburg, Bernard Grimm, S Damstra, Rainer Lenzen, Jan-Willem Pel, Uwe Graser, Peter Schuller, Guy Perrin, O. von der Lühe, A. Böhm, B. Stecklum, J. Meisner, Sebastiano Ligori, L. B. F. M. Waters, Karl Wagner, Frank Przygodda, Christoph Leinert, Bruno Lopez, AW Glazenborg-Kluting, Clemens Storz, Werner Laun, and Walter Jaffe
- Subjects
Physics ,Very Large Telescope ,MIDI ,Point source ,business.industry ,Astronomy and Astrophysics ,computer.file_format ,Tracking (particle physics) ,Interferometry ,Optics ,Space and Planetary Science ,Broadband ,Spectral resolution ,business ,Image resolution ,computer ,Remote sensing - Abstract
After more than five years of preparation, the mid-infrared interferometric instrument MIDI has been transported to Paranal where it will undergo testing and commissioning on the Very Large Telescope Interferometer VLTI from the end of 2002 through large part of this year 2003. Thereafter it will be available as a user instrument to perform interferometric observations over the 8 μm-13 μm wavelength range, with a spatial resolution of typically 20 milliarcsec, a spectral resolution of up to 250, and an anticipated point source sensitivity of N = 3−4 mag or 1−2.5 Jy for self — fringe tracking, which will be the only observing mode during the first months of operation. We describe the layout of the instrument, laboratory tests, and expected performance, both for broadband and spectrally resolved observing modes. We also briefly outline the planned guaranteed time observations.
- Published
- 2003
29. Integration and bench testing for the GRAVITY Coudé IR adaptive optics (CIAO) wavefront sensor
- Author
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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
30. METIS: the mid-infrared E-ELT imager and spectrograph
- Author
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Eva Schmalzl, Remko Stuik, Matthew A. Kenworthy, Christoffel Waelkens, Sander Paalvast, Alistair Glasse, S. Heikamp, Manuel Guedel, Frank Molster, Markus Feldt, Michael Meyer, Lars Venema, Bernhard R. Brandl, Sascha P. Quanz, Rainer Lenzen, and Eric Pantin
- Subjects
Physics ,business.industry ,Exoplanet ,law.invention ,Telescope ,Optics ,law ,Metis ,Angular resolution ,Spectral resolution ,business ,Adaptive optics ,Spectrograph ,Long-slit spectroscopy - Abstract
METIS will be among the first generation of scientific instruments on the E-ELT. Focusing on highest angular resolution and high spectral resolution, METIS will provide diffraction limited imaging and coronagraphy from 3-14μm over an 20x20° field of view, as well as integral field spectroscopy at R ~ 100,000 from 2.9-5.3μm. In addition, METIS provides medium-resolution (R ~ 5000) long slit spectroscopy, and polarimetric measurements at N band. While the baseline concept has already been discussed at previous conferences, this paper focuses on the significant developments over the past two years in several areas: The science case has been updated to account for recent progress in the main science areas circum-stellar disks and the formation of planets, exoplanet detection and characterization, Solar system formation, massive stars and clusters, and star formation in external galaxies. We discuss the developments in the adaptive optics (AO) concept for METIS, the telescope interface, and the instrument modelling. Last but not least we provide an overview of our technology development programs, which ranges from coronagraphic masks, immersed gratings, and cryogenic beam chopper to novel approaches to mirror polishing, background calibration and cryo-cooling. These developments have further enhanced the design and technology readiness of METIS to reliably serve as an early discovery machine on the E-ELT.
- Published
- 2014
31. CARMENES Instrument Overview
- Author
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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
32. Characterizing Exoplanets in the Visible and Infrared: A Spectrometer Concept for the EChO Space Mission
- Author
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F. Müller, Manuel Güdel, Ian J. M. Crossfield, Roland Ottensamer, Etienne Renotte, Sascha P. Quanz, Rainer Lenzen, Udo J. Wehmeier, B. Vandenbussche, Patricio E. Cubillos, Oliver Krause, Th. Henning, Kay Justtanont, Björn Benneke, Hans Martin Schmid, Ansgar Reiners, Ulrich Grözinger, Ö. H. Detre, Michael R. Meyer, Jan-Rutger Schrader, J.-Y. Plesseria, Jeroen Bouwman, Ulrich Klaas, Silvia Scheithauer, Ralf-Rainer Rohloff, Ulf Seemann, Christoph Mordasini, Joseph Harrington, M. Ebert, R. van Boekel, Daphne Stam, Nikku Madhusudhan, and Adrian M. Glauser
- Subjects
Cosmic Vision ,FOS: Physical sciences ,01 natural sciences ,7. Clean energy ,Space exploration ,010309 optics ,0103 physical sciences ,010303 astronomy & astrophysics ,Instrumentation ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Remote sensing ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Spectrometer ,Spacecraft ,business.industry ,Echo (computing) ,Observational techniques ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy and Astrophysics ,instruments ,instrumentation: spectrographs. [Planetary systems ,space vehicles] ,Exoplanet ,13. Climate action ,Astrophysics::Earth and Planetary Astrophysics ,business ,Astrophysics - Instrumentation and Methods for Astrophysics ,Space environment ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Transit-spectroscopy of exoplanets is one of the key observational techniques to characterize the extrasolar planet and its atmosphere. The observational challenges of these measurements require dedicated instrumentation and only the space environment allows an undisturbed access to earth-like atmospheric features such as water or carbon-dioxide. Therefore, several exoplanet-specific space missions are currently being studied. One of them is EChO, the Exoplanet Characterization Observatory, which is part of ESA's Cosmic Vision 2015-2025 program, and which is one of four candidates for the M3 launch slot in 2024. In this paper we present the results of our assessment study of the EChO spectrometer, the only science instrument onboard this spacecraft. The instrument is a multi-channel all-reflective dispersive spectrometer, covering the wavelength range from 400 nm to 16 microns simultaneously with a moderately low spectral resolution. We illustrate how the key technical challenge of the EChO mission - the high photometric stability - influences the choice of spectrometer concept and drives fundamentally the instrument design. First performance evaluations underline the fitness of the elaborated design solution for the needs of the EChO mission., 20 pages, 8 figures, accepted for publication in the Journal of Astronomical Instrumentation
- Published
- 2013
33. Characterization of the transmitted near-infrared wavefront error for the GRAVITY/VLTI Coudé Infrared Adaptive Optics System
- Author
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Sarah Kendrew, Thomas Henning, Wolfgang Brandner, Stefan Hippler, Yann Clénet, Rainer Lenzen, Pengqian Yang, Armin Huber, Oliver Pfuhl, Casey Deen, Jianqiang Zhu, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Max Planck Institute for Extraterrestrial Physics (MPE), 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), and Shandong University
- Subjects
Infrared Rays ,Phase (waves) ,01 natural sciences ,010309 optics ,Optics ,0103 physical sciences ,Adaptive optics ,Image resolution ,ComputingMilieux_MISCELLANEOUS ,Lenses ,010302 applied physics ,Physics ,[PHYS]Physics [physics] ,Very Large Telescope ,business.industry ,Stray light ,Astrophysics::Instrumentation and Methods for Astrophysics ,Equipment Design ,Wavefront sensor ,Atomic and Molecular Physics, and Optics ,Metrology ,Equipment Failure Analysis ,Interferometry ,Artifacts ,business ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Telescopes - Abstract
The adaptive optics system for the second-generation VLT-interferometer (VLTI) instrument GRAVITY consists of a novel cryogenic near-infrared wavefront sensor to be installed at each of the four unit telescopes of the Very Large Telescope (VLT). Feeding the GRAVITY wavefront sensor with light in the 1.4 to 2.4 micrometer band, while suppressing laser light originating from the GRAVITY metrology system, custom-built optical components are required. In this paper, we present the development of a quantitative near-infrared point diffraction interferometric characterization technique, which allows measuring the transmitted wavefront error of the silicon entrance windows of the wavefront sensor cryostat. The technique can be readily applied to quantitative phase measurements in the near-infrared regime. Moreover, by employing a slightly off-axis optical setup, the proposed method can optimize the required spatial resolution and enable real time measurement capabilities. The feasibility of the proposed setup is demonstrated, followed by theoretical analysis and experimental results. Our experimental results show that the phase error repeatability in the nanometer regime can be achieved.
- Published
- 2013
34. Surface figure measurement of flat mirrors based on the subaperture stitching interferometry
- Author
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Thomas Henning, Stefan Hippler, Wolfgang Brandner, Pengqian Yang, Rainer Lenzen, Sarah Kendrew, Armin Huber, Zhaojun Yan, Casey Deen, and Jianqiang Zhu
- Subjects
Physics ,Wavefront ,Surface (mathematics) ,business.industry ,law.invention ,Image stitching ,Interferometry ,Optics ,Planar ,law ,Astronomical interferometer ,Optical flat ,business ,Adaptive optics - Abstract
Large flat mirrors can be characterized using a standard interferometer coupled with stitching the subaperture measurement data. Such systems can measure the global full map of the optical surface by minimizing the inconsistency of data in the adjacent regions. We present a stitching technique that makes use of a commercial phase-shifting Twyman- Green interferometer in combination with an iterative optimized stitching algorithm. The proposed method has been applied to determine the surface errors of planar mirrors with an accuracy of a few nanometers. Moreover, the effect of reference wavefront error is explored. The feasibility and the performance of the proposed system are also demonstrated, along with a detailed error analysis and experimental results. © 2012 SPIE.
- Published
- 2012
35. CARMENES. I: instrument and survey overview
- Author
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Rainer Ulbrich, Thomas Henning, Susana Martín-Ruiz, Jorge Sanz-Forcada, A. Klutsch, Rafael Morales Muñoz, David Barrado y Navascués, Martin Kürster, Enrique de Guindos, Guillem Anglada-Escudé, M. Pluto, Eike W. Guenther, Jean-Louis Lizon, Ovidio Rabaza, Cristina López, Sabine Reffert, Ralf-Reiner Rohloff, E. Herrero, Peter H. Hauschildt, E. Solano, Johannes Winkler, Rainer Lenzen, Clemens Storz, Miguel A. Sánchez Carrasco, Carlos del Burgo, Klaus Huber, Jesús Aceituno, H. Anwand-Heerwart, Regina Antona Jiménez, Maria Rosa Zapatero Osorio, Ansgar Reiners, C. Feiz, Ignasi Ribas, Otmar Stahl, D. Galadí, Emilio Rodríguez Pérez, E. Rodriguez, Ricardo Dorda, Werner Laun, Petra Rhode, A. Ramón, Jürgen H. M. M. Schmitt, S. Lalitha, W. Xu, Juan Gutiérrez-Soto, Hans Hagen, Javier Alonso-Floriano, Matilde Fernández, M. Cortés-Contreras, J. Guàrdia, A. Moya, Concepcion Cardenas, Reinhard Mundt, U. Lemke, Javier López-Santiago, Ernesto Sánchez-Blanco, Enrique de Juan, Mercedes Lopez-Morales, Sebastian Schafer, Juan Carlos Suárez, Florian Rodler, Viki Joergens, D. Montes, A. Rodríguez Trinidad, Jörg Schiller, Julian Stürmer, Vianak Naranjo, Karl Wagner, Andreas Quirrenbach, Artie P. Hatzes, Ulrich Thiele, Rafael Rebolo, R. Oreiro, S. Czesla, Miguel Abril, Stefan Dreizler, Eduardo L. Martín, Jose A. Caballero, Antonio Claret, Josep Colomé, Michaela Doellinger, Jonay I. González Hernández, Armin Huber, Pedro J. Amado, Juan Carlos Morales, Hans-Walter Rix, Mauro López del Fresno, Mathias Zechmeister, Walter Seifert, S. Becerril, Eduard Mirabet, V. J. S. Béjar, M. Kehr, J. Helmling, R. Garrido, Daniel Benitez, C. Schmidt, Sandra V. Jeffers, Matthias Ammler-von Eiff, David Pérez Medialdea, Ulrich Mall, Manuela Vidal-Dasilva, and Holger Mandel
- Subjects
Physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Cassegrain reflector ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Exoplanet ,law.invention ,Telescope ,Observatory ,law ,Planet ,Astrophysics::Solar and Stellar Astrophysics ,Terrestrial planet ,Astrophysics::Earth and Planetary Astrophysics ,Spectral resolution ,Circumstellar habitable zone ,Astrophysics::Galaxy Astrophysics - Abstract
CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs) is a next-generation instrument for the 3.5m telescope at the Calar Alto Observatory, built by a consortium of eleven Spanish and German institutions. The CARMENES instrument consists of two separate echelle spectrographs covering the wavelength range from 0.55 μm to 1.7 μm at a spectral resolution of R = 82, 000, fed by fibers from the Cassegrain focus of the telescope. Both spectrographs are housed in temperature-stabilized vacuum tanks, to enable a long-term 1 m/s radial velocity precision employing a simultaneous calibration with Th-Ne and U-Ne emission line lamps. CARMENES has been optimized for a search for terrestrial planets in the habitable zones (HZs) of low-mass stars, which may well provide our first chance to study environments capable of supporting the development of life outside the Solar System. With its unique combination of optical and near-infrared ´echelle spectrographs, CARMENES will provide better sensitivity for the detection of low-mass planets than any comparable instrument, and a powerful tool for discriminating between genuine planet detections and false positives caused by stellar activity. The CARMENES survey will target 300 M dwarfs in the 2014 to 2018 time frame.
- Published
- 2012
36. An end-to-end instrument model for the proposed E-ELT instrument METIS
- Author
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Rainer Lenzen, Joris Blommaert, Lars Venema, Bernhard R. Brandl, Eric Pantin, J. Meisner, Eva Schmalzl, Michael Meyer, Alistair Glasse, Frank Molster, and Sarah Kendrew
- Subjects
Cryostat ,business.industry ,Computer science ,Measure (physics) ,First light ,law.invention ,Telescope ,Wavelength ,Software ,law ,Metis ,Aerospace engineering ,business ,Spectrograph ,Simulation - Abstract
The optimal performance of an instrument relies critically on accurate performance estimates during its design phase. They need to be modeled to give the science and engineering teams a preview of the performance of the instrument, to guide the design process, to prove the capabilities of the instrument and to prepare science ready software tools before the instrument is operational. METIS, the Mid-infrared E-ELT Imager, is an instrument concept for the E-ELT that covers the thermal infrared wavelengths from 2.9-14μm (L, M and N band). It contains a diffraction limited imager and an integral field high resolution spectrograph. The instrument consists of two independent units, the imager and the spectrograph, and is entirely encased in a cryostat to maintain the stable low temperatures required for good performance at mid-infrared wavelengths. METIS was identified in the instrument roadmap as the third instrument for the E-ELT, after two first light instruments. Because in the mid-infrared the Earth's atmosphere and the telescope mirrors radiate and produce a very high thermal background, it is crucial to develop techniques and mechanisms to measure and reduce this background, to achieve the desired performance of an E-ELT. To demonstrate the capabilities of METIS, years before the actual instrument is built and can be tested, we are developing an end-to-end instrument model, which will simulate the full capacity of METIS. The structure of the model and first results of the performance evaluation are shown. © 2012 SPIE.
- Published
- 2012
37. METIS: the thermal infrared instrument for the E-ELT
- Author
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Michael Meyer, Eric Pantin, Eva Schmalzl, Manuel Guedel, Frank Molster, Stefan Hippler, Emeric Le Floc'h, Joris Blommaert, Remko Stuik, Klaus M. Pontoppidan, Ignas Snellen, Rainer Lenzen, Lars Venema, J. Meisner, Bernhard R. Brandl, Alistair Glasse, and Wolfgang Brandner
- Subjects
Physics ,business.industry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Polarimetry ,Astronomy ,Optics ,Integral field spectrograph ,Metis ,Angular resolution ,Astrophysics::Earth and Planetary Astrophysics ,Spectral resolution ,business ,Extremely large telescope ,Spectrograph ,Long-slit spectroscopy - Abstract
The ‘Mid-infrared ELT Imager and Spectrograph’ (METIS) will be the third instrument on the European Extremely Large Telescope (E-ELT). METIS will provide diffraction limited imaging in the atmospheric L/M and N-band from 3 to 14 μm over an 18˝×18˝ field of view, as well as high contrast coronagraphy, medium-resolution (R ≤ 5000) long slit spectroscopy, and polarimetry. In addition, an integral field spectrograph will provide a spectral resolution of R ~ 100,000 at L/M band. Focusing on highest angular resolution and high spectral resolution, METIS will deliver unique science, in particular in the areas of exo-planets, proto-planetary-disks and high-redshift galaxies, which are illustrated in this paper. The reduction of the E-ELT aperture size had little impact on the METIS science case. With the recent positive developments in the area of detectors, the METIS instrument concept has reached a high level of technology readiness. For some key components (cryogenic chopping mirror, immersed grating, sorption cooler and cryogenic derotator) a development and test program has been launched successfully.
- Published
- 2012
38. CARMENES. V: non-cryogenic solutions for YJH-band NIR instruments
- Author
-
S. Becerril, Ignasi Ribas, Ansgar Reiners, Rainer Lenzen, Holger Mandel, M. A. Sánchez-Carrasco, A. Quirrenbach, Ernesto Sánchez-Blanco, Jose A. Caballero, M. C. Cárdenas, Pedro J. Amado, and Walter Seifert
- Subjects
Physics ,business.industry ,Detector ,Near-infrared spectroscopy ,Astrophysics::Instrumentation and Methods for Astrophysics ,Exoplanet ,Radial velocity ,chemistry.chemical_compound ,Optics ,chemistry ,Heat flux ,K band ,Water cooling ,Mercury cadmium telluride ,business - Abstract
Currently, every single instrument using NIR detectors is cooled down to cryogenic temperatures to minimize the thermal flux emitted by a warm instrument. Cryogenization, meaning reaching very low operating temperatures, is a must when the K band is needed for the science case. This results in more complex and more expensive instruments. However, science cases that do not benefit from observing in the K band, like the detection of exoplanets around M dwarfs through the radial velocity technique, can make use of non-cryogenic instruments. The CARMENES instrument is implementing a cooling system which could allow such a solution. It is being built by a consortium of eleven Spanish and German institutions and will conduct an exoplanet survey around M dwarfs. Its concept includes two spectrographs, one equipped with a CCD for the range 550-950 nm, and one with HgCdTe detectors for the range from 950-1700 nm, covering therefore the YJH bands. In this contribution, different possibilities are studied to reach the final cooling solution to be used in CARMENES, all of them demonstrated to be feasible, within the requirements of the SNR requested by the science case.
- Published
- 2012
39. Designing the METIS adaptive optics system
- Author
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Michael Meyer, Stefan Hippler, Remko Stuik, Joris Blommaert, Frank Molster, A. Stolte, Eric Pantin, Rainer Lenzen, A. Glasse, Lars Venema, and Bernhard R. Brandl
- Subjects
Wavelength ,Spectrometer ,Computer science ,Electronic engineering ,Metis ,Metre ,Sensitivity (control systems) ,Adaptive optics ,Spectroscopy ,Extremely large telescope ,Remote sensing - Abstract
METIS, the Mid-infrared E-ELT Imager and Spectrometer is foreseen to be the third instrument on the European Extremely Large Telescope (E-ELT) and the only instrument to provide high sensitivity mid-IR imaging and spectroscopy to the E-ELT. In order to reach the maximum resolution and sensitivity, an adaptive optics system is required. Since the operational wavelength of METIS is the longest of all E-ELT instruments and the field is relatively small, the complexity of the AO system is significantly reduced, both in required speed as well as order of the AO system. Adaptive Optics has been demonstrated to deliver consistently high performance for the current generation of 6-10 meter class telescopes at mid-infrared wavelengths, and similar performance is expected for METIS on the E-ELT. But in order to provide a reliable system on the E-ELT, several effects which have a minor impact on 6-8 meter class telescopes will need to be investigated for their impact on METIS AO. These effects include refractivity, atmospheric composition variations, but also the operation in a complex operational environment given by both METIS as well as the E-ELT. In this paper we describe the scientific requirements on the METIS AO system, the specific issues related to Adaptive Optics in the mid-IR and expected performance of the METIS AO system on the E-ELT.
- Published
- 2012
40. Optimizing the transmission of the GRAVITY/VLTI near-infrared wavefront sensor
- Author
-
Jianqiang Zhu, Oliver Pfuhl, Thomas Henning, Stefan Hippler, A. Böhm, Rainer Lenzen, Constanza Araujo-Hauck, Y. Clénet, Sarah Kendrew, Wolfgang Brandner, Armin Huber, Ralf-Rainer Rohloff, Pengqian Yang, Casey Deen, 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
Physics ,Wavefront ,Cryostat ,Gravity (chemistry) ,Physics::Instrumentation and Detectors ,business.industry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Physics::Optics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Wavefront sensor ,Laser ,Deformable mirror ,Metrology ,law.invention ,Optics ,law ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Adaptive optics ,business ,Astrophysics::Galaxy Astrophysics - Abstract
The GRAVITY instrument's adaptive optics system consists of a novel cryogenic near-infrared wavefront sensor to be installed at each of the four unit telescopes of the VLT. Feeding the GRAVITY wavefront sensor with light in the 1.4 - 2.4 micrometer band, while suppressing laser light originating from the GRAVITY metrology system, custom-built optical components are required. Here we report on optical and near-infrared testing of the silicon entrance windows of the wavefront sensor cryostat and other reflective optics used in the warm feeding optics. © 2012 SPIE.
- Published
- 2012
41. LINC-NIRVANA: optical elements of the fringe and flexure tracker
- Author
-
Semir Smajic, Andreas Eckart, Udo Beckmann, Bettina Lindhorst, Evangelia Tremou, Jens Zuther, Imke Wank, Rainer Lenzen, Matthew Horrobin, Steffen Rost, C. Rauch, Jörg-Uwe Pott, Thomas Bertram, Christian Straubmeier, and Uwe Lindhorst
- Subjects
Physics ,business.industry ,Detector ,Astrophysics::Instrumentation and Methods for Astrophysics ,Large Binocular Telescope ,Compensation (engineering) ,Homothetic transformation ,law.invention ,Interferometry ,Optics ,Cardinal point ,law ,Periscope ,business ,Beam (structure) - Abstract
LINC-NIRVANA (LN) is a German /Italian interferometric beam combiner camera for the Large Binocular Telescope. Due to homothetic imaging, LN will make use of an exceptionally large field-of-view. As part of LN, the Fringe-and-Flexure-Tracker system (FFTS) will provide real-time, closed-loop measurement and correction of pistonic and flexure signals induced by the atmosphere and inside the telescope-instrument system. Such compensation is essential for achieving coherent light combination over substantial time intervals (~10min.). The FFTS is composed of a dedicated near-infrared detector, which can be positioned by three linear stages within the curved focal plane of LN. The system is divided into a cryogenic (detector) and ambient (linear stages) temperature environment, which are isolated from each other by a moving baffie. We give an overview of the current design and implementation stage of the FFTS opto-mechanical components. The optical components represent an update of the original design to assess slow image motion induced by the LN instrument separately.
- Published
- 2012
42. Visible/infrared spectrometer for EChO
- Author
-
Manuel Güdel, Adrian M. Glauser, Roland Ottensamer, Th. Henning, Etienne Renotte, H. M. Schmid, R. van Boekel, Oliver Krause, Michael Meyer, Ulrich Klaas, Ulrich Grözinger, Rainer Lenzen, Jan-Rutger Schrader, Sascha P. Quanz, Udo J. Wehmeier, Daphne Stam, R.-R. Rohloff, Bart Vandenbussche, and F. Müller
- Subjects
Physics ,Cosmic Vision ,Spectrometer ,Observatory ,Planet ,Infrared ,Echo (computing) ,Hot Jupiter ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astrophysics::Earth and Planetary Astrophysics ,Exoplanet - Abstract
The Exoplanet Characterisation Observatory (EChO) is a medium class mission candidate within ESA's Cosmic Vision 2015-2025 program on space science. EChO will be equipped with a visible to infrared spectrometer covering the wavelength range from 0.4 - 11 μm (goal: 16 μm) at a spectral resolving power between 30 and 300 in order to characterize the atmospheres of known transiting extrasolar planets ranging from Hot Jupiters to Super Earths. In this paper we will present first results from the dedicated study of the EChO science payload carried out by our EChO Instrument Consortium during the assessment phase of the mission.
- Published
- 2012
43. A star in a 15.2-year orbit around the supermassive black hole at the centre of the Milky Way
- Author
-
Eric Gendron, Wolfgang Brandner, Reiner Hofmann, Tal Alexander, Nelly Mouawad, Anne-Marie Lagrange, Daniel Rouan, Karl M. Menten, Markus Hartung, Andreas Eckart, Reinhard Genzel, Jason Spyromilio, Gérard Rousset, Christopher Lidman, Matt Lehnert, Francois Lacombe, T. Ott, Rainer Schödel, A. F. M. Moorwood, N. Ageorges, Rainer Lenzen, Norbert Hubin, Mark J. Reid, 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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
- Subjects
Physics ,Supermassive black hole ,Multidisciplinary ,Astrophysics::High Energy Astrophysical Phenomena ,Milky Way ,Galactic Center ,Astronomy ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astrometry ,Quasi-star ,General Relativity and Quantum Cosmology ,Intermediate-mass black hole ,Stellar black hole ,Astrophysics::Earth and Planetary Astrophysics ,Orbit (control theory) ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics::Galaxy Astrophysics - Abstract
Many galaxies are thought to have supermassive black holes at their centres-more than a million times the mass of the Sun. Measurements of stellar velocities and the discovery of variable X-ray emission have provided strong evidence in favour of such a black hole at the centre of the Milky Way, but have hitherto been unable to rule out conclusively the presence of alternative concentrations of mass. Here we report ten years of high-resolution astrometric imaging that allows us to trace two-thirds of the orbit of the star currently closest to the compact radio source (and massive black-hole candidate) Sagittarius A*. The observations, which include both pericentre and apocentre passages, show that the star is on a bound, highly elliptical keplerian orbit around Sgr A*, with an orbital period of 15.2 years and a pericentre distance of only 17 light hours. The orbit with the best fit to the observations requires a central point mass of (3.7 +/- 1.5) x 10(6) solar masses (M(*)). The data no longer allow for a central mass composed of a dense cluster of dark stellar objects or a ball of massive, degenerate fermions.
- Published
- 2002
44. Black Hole Mass Estimates Based on C IV are Consistent With Those Based on the Balmer Lines
- Author
-
Vianak Naranjo, S. Mathur, Rainer Lenzen, R. Lederer, Ulrich Mall, Dong Zhang, J. van Saders, Hans Gemperlein, Christopher S. Kochanek, Anna Pasquali, M. Dietrich, Roberto J. Assef, Walter Seifert, Bradley M. Peterson, Mukremin Kilic, C. Feiz, Reiner Hofmann, M. Lehmitz, Peter Buschkamp, Clemens Storz, Werner Laun, P. Mueller, Marcus Juette, Holger Mandel, Rubab Khan, Catherine J. Grier, E. E. Falco, R. W. Pogge, K. K. Madsen, P. Weiser, A. Quirrenbach, K. Mogren, B. J. Shappee, S. Kozłowski, Kelly D. Denney, A. Germeroth, D. Stern, Volker Knierim, Kai Lars Polsterer, Nancy Ageorges, Paul Martini, and R. S. Barrows
- Subjects
Physics ,Supermassive black hole ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Balmer series ,Sigma ,FOS: Physical sciences ,Astronomy and Astrophysics ,Quasar ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,medicine.disease_cause ,Spectral line ,symbols.namesake ,Full width at half maximum ,Space and Planetary Science ,medicine ,symbols ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,Ultraviolet ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Using a sample of high-redshift lensed quasars from the CASTLES project with observed-frame ultraviolet or optical and near-infrared spectra, we have searched for possible biases between supermassive black hole (BH) mass estimates based on the CIV, Halpha and Hbeta broad emission lines. Our sample is based upon that of Greene, Peng & Ludwig, expanded with new near-IR spectroscopic observations, consistently analyzed high S/N optical spectra, and consistent continuum luminosity estimates at 5100A. We find that BH mass estimates based on the FWHM of CIV show a systematic offset with respect to those obtained from the line dispersion, sigma_l, of the same emission line, but not with those obtained from the FWHM of Halpha and Hbeta. The magnitude of the offset depends on the treatment of the HeII and FeII emission blended with CIV, but there is little scatter for any fixed measurement prescription. While we otherwise find no systematic offsets between CIV and Balmer line mass estimates, we do find that the residuals between them are strongly correlated with the ratio of the UV and optical continuum luminosities. Removing this dependency reduces the scatter between the UV- and optical-based BH mass estimates by a factor of approximately 2, from roughly 0.35 to 0.18 dex. The dispersion is smallest when comparing the CIV sigma_l mass estimate, after removing the offset from the FWHM estimates, and either Balmer line mass estimate. The correlation with the continuum slope is likely due to a combination of reddening, host contamination and object-dependent SED shapes. When we add additional heterogeneous measurements from the literature, the results are unchanged., Accepted for publication in The Astrophysical Journal. 37 text pages + 8 tables + 23 figures. Updated with comments by the referee and with a expanded discussion on literature data including new observations
- Published
- 2011
45. LUCIFER1 commissioning at the LBT
- Author
-
L. Schäffner, Peter Buschkamp, Werner Laun, Peter Müller, Marcus Jütte, Clemens Storz, Hans Gemperlein, C. Feiz, Anna Pasquali, John M. Hill, Walter Seifert, M. Lehmitz, Holger Mandel, A. Quirrenbach, Ulrich Mall, Kai Lars Polsterer, A. Germeroth, P. Weiser, Nancy Ageorges, Volker Knierim, Rainer Lenzen, R. Lederer, Vianak Naranjo, and Reiner Hofmann
- Subjects
Physics ,Pixel ,biology ,business.industry ,Near-infrared spectroscopy ,Large Binocular Telescope ,biology.organism_classification ,law.invention ,Telescope ,Narrow band ,Optics ,law ,business ,Lucifer - Abstract
LUCIFER 1 is the rst of two identical camera-spectrograph units installed at the LBT (Large Binocular Telescope) on Mount Graham in Arizona. Its commissioning took place between September 2008 and November 2009 and has immediately been followed by science operations since December 2009. LUCIFER has a 4x4 arcminute eld of view. It is equipped with a 2048x2048 pixel HAWAII-2 array, suitable lters (broad-band z, J, H, K & Ks plus 12 medium and narrow band near-infrared lters) and three gratings for spectroscopy for a resolution of up to 15000. LUCIFER has 3 cameras: two specic for seeing limited imaging (the N3.75 camera, with 0.12"/pixel) and spectroscopy (the N1.8 camera, with 0.25"/pixel) and one for diraction limited observations (the N30 camera). We report here about the completed seeing-limited commissioning, thus using only two of the cameras.
- Published
- 2010
46. Status and new operation modes of the versatile VLT/NaCo
- Author
-
Nicolas Huerta, Antoine Mérand, Jared O'Neal, Gérard Zins, Sridharan Rengaswamy, Sascha P. Quanz, Stefan Gillessen, Rainer Lenzen, Guillaume Montagnier, Markus Kasper, Nick Kornweibel, Julien Girard, Alexandre Gallenne, Pierre Kervella, Matthew A. Kenworthy, Rainer Schödel, Naco Iot, 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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
- Subjects
Very Large Telescope ,business.industry ,Computer science ,media_common.quotation_subject ,Frame (networking) ,FOS: Physical sciences ,Wavefront sensor ,Sextant (astronomical) ,law.invention ,Tilt (optics) ,Laser guide star ,Sky ,law ,Planet ,Astrophysics - Instrumentation and Methods for Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,business ,Adaptive optics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Computer hardware ,media_common - Abstract
This paper aims at giving an update on the most versatile adaptive optics fed instrument to date, the well known and successful NACO . Although NACO is only scheduled for about two more years at the Very Large Telescope (VLT), it keeps on evolving with additional operation modes bringing original astronomical results. The high contrast imaging community uses it creatively as a test-bench for SPHERE and other second generation planet imagers. A new visible wavefront sensor (WFS) optimized for Laser Guide Star (LGS) operations has been installed and tested, the cube mode is more and more requested for frame selection on bright sources, a seeing enhancer mode (no tip/tilt correction) is now offered to provide full sky coverage and welcome all kind of extragalactic applications, etc. The Instrument Operations Team (IOT) and Paranal engineers are currently working hard at maintaining the instrument overall performances but also at improving them and offering new capabilities, providing the community with a well tuned and original instrument for the remaining time it is being used. The present contribution delivers a non-exhaustive overview of the new modes and experiments that have been carried out in the past months., Comment: 10 pages, 7 figures, SPIE 2010 Astronomical Instrumentation Proceeding
- Published
- 2010
47. The METIS AO system: bringing extreme adaptive optics to the mid-IR
- Author
-
Stefan Hippler, Rainer Lenzen, A. Glasse, Joris Blommaert, Lars Venema, Eric Pantin, Sarah Kendrew, Laurent Jolissaint, Remko Stuik, and Bernhard R. Brandl
- Subjects
Physics ,Spectrometer ,business.industry ,Instrumentation ,Strehl ratio ,law.invention ,Telescope ,Interferometry ,Optics ,law ,Metis ,Adaptive optics ,Extremely large telescope ,business ,Remote sensing - Abstract
METIS (Mid-infrared E-ELT Imager and Spectrometer) is the mid-infrared instrument proposed for the European Extremely Large Telescope (E-ELT). METIS will be the first instrument in the mid-IR that will actually require an Adaptive Optics system in order to reach a performance close to the diffraction limit. Extending Adaptive Optics for the mid-IR from the current generation of telescopes to 30-42 meter telescopes is technically challenging, but appears at first sight significantly easier than at visible and near infrared wavelengths. Adaptive Optics has been demonstrated to deliver Strehl Ratios exceeding 95% on 6-8 meter class telescopes at 10 microns, but achieving this performance on E-ELTs under normal observation conditions, requires that several higher order effects are taken into account. The performance of a mid-IR AO system drops significantly if refractivity effects and atmospheric composition variations are not compensated. Reaching Strehl Ratios of over 90% in the L, M and N band will require special considerations and will impact the system design and control scheme of AO systems for mid-IR on ELTs. The METIS instrument has finalized its preliminary design phase and in this paper we present the results of our performance estimates of the METIS AO system. We have included the effects of refractivity and composition fluctuations on the performance of the AO system and we have investigated how these effects impact the science cases for mid-IR instrumentation on an ELT.
- Published
- 2010
48. Characterization and performance of the 4k x 4k Hawaii-2RG Mosaic for PANIC
- Author
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Karl Wagner, J. Helmling, M. C. Cárdenas, Vianak Naranjo, Rainer Lenzen, Ralf-Rainer Rohloff, Harald Baumeister, Clemens Storz, Matilde Fernández, Jose Ramos, Matthias Alter, Armin Huber, Werner Laun, J. Fried, Peter Bizenberger, Ulrich Mall, J. M. Ibáñez Mengual, Antonio J. García Segura, and Julio Gómez
- Subjects
Optics ,Computer science ,Observatory ,business.industry ,Computer graphics (images) ,medicine ,Panic ,Field of view ,Mosaic (geodemography) ,medicine.symptom ,business - Abstract
PANIC, the PAnoramic Near-Infrared Camera for Calar Alto, is one of the next generation instruments for this observatory. In order to cover a field of view of approximately 30 arcmin, PANIC uses a mosaic of four 2k x 2k HAWAII-2RG arrays from Teledyne. This document presents the preliminary results of the basic characterization of the mosaic. The performance of the system as a whole, as well as the in-house readout electronics and software capabilities will also be briefly discussed.
- Published
- 2010
49. LUCIFER1: performance results
- Author
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Marcus Jütte, Rainer Lenzen, Holger Mandel, Clemens Storz, A. Germeroth, Ulrich Mall, Anna Pasquali, C. Feiz, Hans Gemperlein, Peter Buschkamp, P. Weiser, Peter Müller, Walter Seifert, L. Schäffner, Kai Lars Polsterer, Werner Laun, Andreas Quirrenbach, M. Lehmitz, Reiner Hofmann, R. Lederer, Volker Knierim, Nancy Ageorges, and Vianak Naranjo
- Subjects
Physics ,business.industry ,System of measurement ,Optical instrument ,Near-infrared spectroscopy ,Large Binocular Telescope ,law.invention ,Telescope ,Optics ,Software ,law ,Calibration ,business ,Spectrograph - Abstract
LUCIFER1 is a NIR camera and spectrograph installed at the Large Binocular Telescope (LBT). Working in the wavelength range of 0.9-2.5micron, the instrument is designed for direct imaging and spectroscopy with 3 different cameras. A set of longslit masks as well as up to 23 user defined (MOS) masks are available. The set of user defined masks can be exchanged while the instrument is at operating temperature. Extensive tests have been done on the electro-mechanical functions, image motion due to flexure, optical quality, instrument software, calibration and especially on the multi-object spectroscopy. Also a detailed characterization of the instrument's properties in the different observing modes has been carried out. Results are presented and compared to the specifications.
- Published
- 2010
50. CARMENES: Calar Alto high-resolution search for M dwarfs with exo-earths with a near-infrared Echelle spectrograph
- Author
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J. Helmling, F. Rodler, A. Rodríguez Trinidad, R. Garrido, G. Wiedemann, Stefan Dreizler, Víctor J. S. Béjar, Karl Wagner, F. Gutiérrez-Soto, Ignasi Ribas, E. Herrero, S. Becerril, E. Rodriguez, Andrés Moya, Cristina Afonso, Th. Henning, A. Böhm, W. Xu, Walter Seifert, Miguel Abril, Johny Setiawan, Rainer Lenzen, Ernesto Sánchez-Blanco, Eric Martin, Jacob L. Bean, Ovidio Rabaza, M. C. Cárdenas, Vianak Naranjo, Reinhard Mundt, Enrique Solano, E. Mirabet, J. I. González Hernández, M. A. Sánchez Carrasco, Clemens Storz, D. Barrado y Navascués, A. Claret, R. Morales Muñoz, R.-R. Rohloff, C. Schmidt, Ansgar Reiners, Martin Kürster, Josep Colomé, M. R. Zapatero Osorio, M. Fernandez, J. Guàrdia, Sabine Reffert, C. del Burgo, Holger Mandel, D. Galadí, Juan Carlos Suárez, Pedro J. Amado, X. Francisco, U. Thiele, A. Quirrenbach, Juan Carlos Morales, Otmar Stahl, Eike W. Guenther, Werner Laun, A. Ramón, Ulrich Mall, L. P. Costillo, D. Montes, Susana Martín-Ruiz, Rafael Rebolo, A. P. Hatzes, Jesús Aceituno, Jose A. Caballero, and Viki Joergens
- Subjects
Physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Cassegrain reflector ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Exoplanet ,law.invention ,010309 optics ,Telescope ,Radial velocity ,Stars ,law ,Observatory ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Spectral resolution ,010303 astronomy & astrophysics ,Spectrograph ,Astrophysics::Galaxy Astrophysics - Abstract
CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs) is a next-generation instrument to be built for the 3.5m telescope at the Calar Alto Observatory by a consortium of Spanish and German institutions. Conducting a five-year exoplanet survey targeting ~ 300 M stars with the completed instrument is an integral part of the project. The CARMENES instrument consists of two separate spectrographs covering the wavelength range from 0.52 to 1.7 μm at a spectral resolution of R = 85, 000, fed by fibers from the Cassegrain focus of the telescope. The spectrographs are housed in a temperature-stabilized environment in vacuum tanks, to enable a 1m/s radial velocity precision employing a simultaneous ThAr calibration.
- Published
- 2010
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