A. Quirrenbach, P. Amado, J. Caballero, R. Mundt, A. Reiners, I. Ribas, W. Seifert, M. Abril, J. Aceituno, F. Alonso-Floriano, H. Anwand-Heerwart, M. Azzaro, F. Bauer, D. Barrado, S. Becerril, V. J. Bejar, D. Benitez, Z. Berdinas, M. Brinkmöller, M. Cardenas, E. Casal, A. Claret, J. Colomé, M. Cortes-Contreras, S. Czesla, M. Doellinger, S. Dreizler, C. Feiz, M. Fernandez, I. Ferro, B. Fuhrmeister, D. Galadi, I. Gallardo, M. Gálvez-Ortiz, A. Garcia-Piquer, R. Garrido, L. Gesa, V. Gómez Galera, J. González Hernández, R. Gonzalez Peinado, U. Grözinger, J. Guàrdia, E. Guenther, E. de Guindos, H.-J. Hagen, A. Hatzes, P. Hauschildt, J. Helmling, T. Henning, D. Hermann, R. Hernández Arabi, L. Hernández Castaño, F. Hernández Hernando, E. Herrero, A. Huber, K. Huber, P. Huke, S. Jeffers, E. de Juan, A. Kaminski, M. Kehr, M. Kim, R. Klein, J. Klüter, M. Kürster, M. Lafarga, L. Lara, A. Lamert, W. Laun, R. Launhardt, U. Lemke, R. Lenzen, M. Llamas, M. Lopez del Fresno, M. López-Puertas, J. López-Santiago, J. Lopez Salas, H. Magan Madinabeitia, U. Mall, H. Mandel, L. Mancini, J. Marin Molina, D. Maroto Fernández, E. Martín, S. Martín-Ruiz, C. Marvin, R. Mathar, E. Mirabet, D. Montes, J. Morales, R. Morales Muñoz, E. Nagel, V. Naranjo, G. Nowak, E. Palle, J. Panduro, V. Passegger, A. Pavlov, S. Pedraz, E. Perez, D. Pérez-Medialdea, M. Perger, M. Pluto, A. Ramón , R. Rebolo, P. Redondo, S. Reffert, S. Reinhart, P. Rhode, H.-W. Rix, F. Rodler, E. Rodríguez, C. Rodríguez López, R. Rohloff, A. Rosich, M Sanchez Carrasco, J. Sanz-Forcada, P. Sarkis, L. Sarmiento, S. Schäfer, J. Schiller, C. Schmidt, J. H. M. M. Schmitt, P. Schöfer, A. Schweitzer, D. Shulyak, E. Solano, O. Stahl, C. Storz, H. Tabernero, M. Tala, L. Tal-Or, R.-G. Ulbrich, G. Veredas, J. I. Vico Linares, F. Vilardell, K. Wagner, J. Winkler, M.-R. Zapatero Osorio, M. Zechmeister, M. Ammler-von Eiff, G. Anglada-Escudé, C. del Burgo, M. Garcia-Vargas, A. Klutsch, J.-L. Lizon, M. Lopez-Morales, A. Ofir, A. Pérez-Calpena, M. A. C. Perryman, E. Sánchez-Blanco , J. B. P. Strachan, J. Stürmer, J. Suárez, T. Trifonov, S. Tulloch, W. Xu
The CARMENES instrument is a pair of high-resolution (R⪆80,000) spectrographs covering the wavelength range from 0.52 to 1.71 μm, optimized for precise radial velocity measurements. It was installed and commissioned at the 3.5m telescope of the Calar Alto observatory in Southern Spain in 2015. The first large science program of CARMENES is a survey of ~ 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.
The Waltz Spectrograph is a fiber-fed high-resolution échelle spectrograph for the 72 cm Waltz Telescope at the Landessternwarte, Heidelberg. It uses a 31.6 lines/mm 63.5° blaze angle échelle grating in white-pupil configuration, providing a spectral resolving power of R ~ 65,000 covering the spectral range between 450-800nm in one CCD exposure. A prism is used for cross-dispersion of échelle orders. The spectrum is focused by a commercial apochromat onto a 2k×2k CCD detector with 13.5μm per pixel. An exposure meter will be used to obtain precise photon-weighted midpoints of observations, which will be used in the computation of the barycentric corrections of measured radial velocities. A stabilized, newly designed iodine cell is employed for measuring radial velocities with high precision. Our goal is to reach a radial velocity precision of better than 5 m/s, providing an instrument with sufficient precision and sensitivity for the discovery of giant exoplanets. Here we describe the design of the Waltz spectrograph and early on-sky results.
With the steadily increasing complexity of scientific instruments, there is an ever-growing demand for improved control electronics. This is especially important for infrared instruments, where the challenging vacuum and cryogenic systems increase the demands on the overall control system. The control electronics must monitor and adjust many different subsystems in different locations, some mounted at the telescope and others placed inside the telescope building. To implement these different demands, a comprehensive Interlock system with process visualization and powerful diagnostics has been developed at the Calar Alto Observatory and the Zentrum für Astronomie Heidelberg (LS
MATISSE is the second-generation mid-infrared spectrograph and imager for the Very Large Telescope Interferometer (VLTI) at Paranal. This new interferometric instrument will allow significant advances by opening new avenues in various fundamental research fields: studying the planet-forming region of disks around young stellar objects, understanding the surface structures and mass loss phenomena affecting evolved stars, and probing the environments of black holes in active galactic nuclei. As a first breakthrough, MATISSE will enlarge the spectral domain of current optical interferometers by offering the L and M bands in addition to the N band. This will open a wide wavelength domain, ranging from 2.8 to 13 μm, exploring angular scales as small as 3 mas (L band) / 10 mas (N band). As a second breakthrough, MATISSE will allow mid-infrared imaging - closure-phase aperture-synthesis imaging - with up to four Unit Telescopes (UT) or Auxiliary Telescopes (AT) of the VLTI. Moreover, MATISSE will offer a spectral resolution range from R ∼ 30 to R ∼ 5000. Here, we present one of the main science objectives, the study of protoplanetary disks, that has driven the instrument design and motivated several VLTI upgrades (GRA4MAT and NAOMI). We introduce the physical concept of MATISSE including a description of the signal on the detectors and an evaluation of the expected performances. We also discuss the current status of the MATISSE instrument, which is entering its testing phase, and the foreseen schedule for the next two years that will lead to the first light at Paranal.
MATISSE is the mid-infrared spectrograph and imager for the Very Large Telescope Interferometer (VLTI) at Paranal. This second generation interferometry instrument will open new avenues in the exploration of our Universe. Mid-infrared interferometry with MATISSE will allow significant advances in various fundamental research fields: studies of disks around young stellar objects where planets form and evolve, surface structures and mass loss of stars in late evolutionary stages, and the environments of black holes in active galactic nuclei. MATISSE is a unique instrument. As a first breakthrough it will enlarge the spectral domain used by optical interferometry by offering the L & M bands in addition to the N band, opening a wide wavelength domain, ranging from 2.8 to 13 μm on angular scales of 3 mas (L/M band) / 10 mas (N band). As a second breakthrough, it will allow mid-infrared imaging – closure-phase aperture-synthesis imaging – with up to four Unit Telescopes (UT) or Auxiliary Telescopes (AT) of the VLTI. MATISSE will offer various ranges of spectral resolution between R~30 to ~5000. In this article, we present some of the main science objectives that have driven the instrument design. We introduce the physical concept of MATISSE including a description of the signal on the detectors and an evaluation of the expected performance and discuss the project status. The operations concept will be detailed in a more specific future article, illustrating the observing templates operating the instrument, the data reduction and analysis, and the image reconstruction software.
A. Quirrenbach, P. Amado, J. Caballero, R. Mundt, A. Reiners, I. Ribas, W. Seifert, M. Abril, J. Aceituno, F. J. Alonso-Floriano, M. Ammler-von Eiff, R. Antona Jiménez, H. Anwand-Heerwart, M. Azzaro, F. Bauer, D. Barrado, S. Becerril, V. J. Béjar, D. Benítez, Z. Berdiñas, M. Cárdenas, E. Casal, A. Claret, J. Colomé, M. Cortés-Contreras, S. Czesla, M. Doellinger, S. Dreizler, C. Feiz, M. Fernández, D. Galadí, M. Gálvez-Ortiz, A. García-Piquer, M. García-Vargas, R. Garrido, L. Gesa, V. Gómez Galera, E. González Álvarez, J. González Hernández, U. Grözinger, J. Guàrdia, E. Guenther, E. de Guindos, J. Gutiérrez-Soto, H.-J. Hagen, A. Hatzes, P. Hauschildt, J. Helmling, T. Henning, D. Hermann, L. Hernández Castaño, E. Herrero, D. Hidalgo, G. Holgado, A. Huber, K. Huber, S. Jeffers, V. Joergens, E. de Juan, M. Kehr, R. Klein, M. Kürster, A. Lamert, S. Lalitha, W. Laun, U. Lemke, R. Lenzen, Mauro López del Fresno, B. López Martí, J. López-Santiago, U. Mall, H. Mandel, E. Martín, S. Martín-Ruiz, H. Martínez-Rodríguez, C. Marvin, R. Mathar, E. Mirabet, D. Montes, R. Morales Muñoz, A. Moya, V. Naranjo, A. Ofir, R. Oreiro, E. Pallé, J. Panduro, V.-M. Passegger, A. Pérez-Calpena, D. Pérez Medialdea, M. Perger, M. Pluto, A. Ramón, R. Rebolo, P. Redondo, S. Reffert, S. Reinhardt, P. Rhode, H.-W. Rix, F. Rodler, E. Rodríguez, C. Rodríguez-López, E. Rodríguez-Pérez, R.-R. Rohloff, A. Rosich, E. Sánchez-Blanco, M. Sánchez Carrasco, J. Sanz-Forcada, L. Sarmiento, S. Schäfer, J. Schiller, C. Schmidt, J. H. M. M. Schmitt, E. Solano, O. Stahl, C. Storz, J. Stürmer, J. Suárez, R. Ulbrich, G. Veredas, K. Wagner, J. Winkler, M. Zapatero Osorio, M. Zechmeister, F. Abellán de Paco, G. Anglada-Escudé, C. del Burgo, A. Klutsch, J. Lizon, M. López-Morales, J. Morales, M. A. C. Perryman, S. Tulloch, W. Xu
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 (Y 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 - 1.7μm.
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 coud´e
laboratory of the 3.5m dome. Each vacuum tank is equipped with a temperature stabilization system capable
of keeping the temperature constant to within ±0.01°C 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.
Andreas Quirrenbach, Pedro Amado, Walter Seifert, Miguel Sánchez Carrasco, Holger Mandel, Jose Caballero, Reinhard Mundt, Ignasi Ribas, Ansgar Reiners, Miguel Abril, Jesus Aceituno, Javier Alonso-Floriano, Matthias Ammler-von Eiff, Guillem Anglada-Escude, Regina Antona Jiménez, Heiko Anwand-Heerwart, David Barrado y Navascués, Santiago Becerril, Victor Bejar, Daniel Benitez, Concepcion Cardenas, Antonio Claret, Josep Colome, Miriam Cortés-Contreras, Stefan Czesla, Carlos del Burgo, Michaela Doellinger, R. Dorda, Stefan Dreizler, Carmen Feiz, Matilde Fernandez, David Galadi, Rafael Garrido, Jonay González Hernández, Josep Guardia, Eike Guenther, Enrique de Guindos, Juan Gutiérrez-Soto, Hans Hagen, Artie Hatzes, Peter Hauschildt, Jens Helmling, Thomas Henning, Enrique Herrero, Armin Huber, Klaus Huber, Sandra Jeffers, Viki Joergens, Enrique de Juan, M. Kehr, Alexis Klutsch, Martin Kürster, S. Lalitha, Werner Laun, Ulrike Lemke, Rainer Lenzen, Jean-Louis Lizon, Mauro López del Fresno, Mercedes López-Morales, Javier López-Santiago, Ulrich Mall, Eduardo Martin, Susana Martín-Ruiz, Eduard Mirabet, David Montes, Juan Carlos Morales, Rafael Morales Muñoz, Andres Moya, Vianak Naranjo, Raquel Oreiro, David Pérez Medialdea, Michael Pluto, Ovidio Rabaza, Alejandro Ramon, Rafael Rebolo, Sabine Reffert, Petra Rhode, Hans-Walter Rix, Florian Rodler, Eloy Rodríguez, Cristina Rodríguez López, Emilio Rodríguez Pérez, A. Rodriguez Trinidad, Ralf-Reiner Rohloff, Ernesto Sánchez-Blanco, Jorge Sanz-Forcada, Sebastian Schäfer, Jörg Schiller, Christof Schmidt, Jürgen Schmitt, Enrique Solano, Otmar Stahl, Clemens Storz, Julian Stürmer, Juan Carlos Suarez, Ulrich Thiele, Rainer Ulbrich, Manuela Vidal-Dasilva, Karl Wagner, Johannes Winkler, Wenli Xu, Maria Rosa Zapatero Osorio, Mathias Zechmeister
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 échelle 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.
MATISSE is a mid-infrared spectro-interferometer combining the beams of up to four Unit Telescopes or Auxiliary
Telescopes of the Very Large Telescope Interferometer (VLTI) of the European Southern Observatory.
MATISSE will constitute an evolution of the two-beam interferometric instrument MIDI. New characteristics present in
MATISSE will give access to the mapping and the distribution of the material, the gas and essentially the dust, in the
circumstellar environments by using the mid-infrared band coverage extended to L, M and N spectral bands. The four
beam combination of MATISSE provides an efficient uv-coverage: 6 visibility points are measured in one set and 4
closure phase relations which can provide aperture synthesis images in the mid-infrared spectral regime.
We give an overview of the instrument including the expected performances and a view of the Science Case. We present
how the instrument would be operated. The project involves the collaborations of several agencies and institutes: the
Observatoire de la Côte d’Azur of Nice and the INSU-CNRS in Paris, the Max Planck Institut für Astronomie of
Heidelberg; the University of Leiden and the NOVA-ASTRON Institute of Dwingeloo, the Max Planck Institut für
Radioastronomie of Bonn, the Institut für Theoretische Physik und Astrophysik of Kiel, the Vienna University and the
Konkoly Observatory.
GRAVITY is an adaptive optics assisted Beam Combiner for the second generation VLTI instrumentation. The
instrument will provide high-precision narrow-angle astrometry and phase-referenced interferometric imaging in the
astronomical K-band for faint objects. We describe the wide range of science that will be tackled with this instrument,
highlighting the unique capabilities of the VLTI in combination with GRAVITY. The most prominent goal is to observe
highly relativistic motions of matter close to the event horizon of Sgr A*, the massive black hole at center of the Milky
Way. We present the preliminary design that fulfils the requirements that follow from the key science drivers: It includes
an integrated optics, 4-telescope, dual feed beam combiner operated in a cryogenic vessel; near-infrared wavefrontsensing
adaptive optics; fringe-tracking on secondary sources within the field of view of the VLTI and a novel metrology
concept. Simulations show that 10 μas astrometry within few minutes is feasible for a source with a magnitude of
mK = 15 like Sgr A*, given the availability of suitable phase reference sources (mK = 10). Using the same setup, imaging of mK = 18 stellar sources in the interferometric field of view is possible, assuming a full night of observations and the corresponding UV coverage of the VLTI.
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.
With steadily increasing telescope sizes and the growing complexity of scientific instruments, there is an ever-growing
demand for improved electronics, controlling all the different optical parts on moving mechanisms. Among competing
requirements are, on one hand, the increasing number of actuators, with high-precision positioning in closed and open
loop, and on the other hand, smaller sizes, low power and restricted heat emission. A specific challenge is
accommodating mechanisms that operate in infrared instrumentation at cryogenic temperatures down to 60 Kelvin. In
this area piezo motors offer promising solutions. To fulfill these different demands a competitive motion control system
has been developed at the Max-Planck-Institut für Astronomie (MPIA) in Heidelberg, Germany. A modular chassis with
standardized boards provides best solutions for extensive tasks. High and low power DC servo motors, brushless DC
servo motors, stepper motors and piezo motors with different technologies are supported. Diversity position feedback
capabilities, like incremental and absolute encoders for non cryogenic and capacitive sensors and resolvers for cryogenic
applications, are provided.
Two feasibility studies for spectrographs that can deliver at least 4000 MOS slits over a 1° field at the prime focuses of
the Anglo-Australian and Calar Alto Observatories have been completed. We describe the design and science case of the
Calar Alto eXtreme Multiplex Spectrograph (XMS) for which an extended study, half way between feasibility study and
phase-A, was made. The optical design is quite similar than in the AAO study for the Next Generation 1 degree Field
(NG1dF) but the mechanical design of XMS is quite different and much more developed. In a single night, 25000 galaxy
redshifts can be measured to z~0.7 and beyond for measuring the Baryon Acoustic Oscillation (BAO) scale and many
other science goals. This may provide a low-cost alternative to WFMOS for example and other large fibre spectrographs.
The design features four cloned spectrographs which gives a smaller total weight and length than a unique spectrograph
to makes it placable at prime focus. The clones use a transparent design including a grism in which all optics are about
the size or smaller than the clone rectangular subfield so that they can be tightly packed with little gaps between
subfields. Only low cost glasses are used; the variations in chromatic aberrations between bands are compensated by
changing a box containing the grism and two adjacent lenses. Three bands cover the 420nm to 920nm wavelength range
at 10A resolution while another cover the Calcium triplet at 3A. An optional box does imaging. We however also studied
different innovative methods for acquisition without imaging. A special mask changing mechanism was also designed to
compensate for the lack of space around the focal plane. Conceptual designs for larger projects (AAT 2º field, CFHT,
VISTA) have also been done.
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.
MATISSE is foreseen as a mid-infrared spectro-interferometer combining the beams of up to four UTs/ATs of the Very
Large Telescope Interferometer (VLTI) of the European Southern Observatory. The related science case study
demonstrates the enormous capability of a new generation mid-infrared beam combiner.
MATISSE will constitute an evolution of the two-beam interferometric instrument MIDI. MIDI is a very successful
instrument which offers a perfect combination of spectral and angular resolution. New characteristics present in
MATISSE will give access to the mapping and the distribution of the material (typically dust) in the circumstellar
environments by using a wide mid-infrared band coverage extended to L, M and N spectral bands. The four beam
combination of MATISSE provides an efficient UV-coverage : 6 visibility points are measured in one set and 4 closure
phase relations which can provide aperture synthesis images in the mid-infrared spectral regime.
PRIMA, the instrument for Phase-Referenced Imaging and Micro-arcsecond Astrometry at the VLTI, is currently being
developed at ESO. PRIMA will implement the dual-feed capability, at first for two UTs or ATs, to enable simultaneous
interferometric observations of two objects that are separated by up to 1 arcmin. PRIMA is designed to perform narrow-angle
astrometry in K-band with two ATs as well as phase-referenced aperture synthesis imaging with instruments like
Amber and Midi. In order to speed up the full implementation of the 10 microarcsec astrometric capability of the VLTI
and to carry out a large astrometric planet search program, a consortium lead by the Observatoire de Genève, Max
Planck Institute for Astronomy, and Landessternwarte Heidelberg, has built Differential Delay Lines for PRIMA and is
developing the astrometric observation preparation and data reduction software. When the facility becomes fully
operational in 2009, we will use PRIMA to carry out a systematic astrometric Exoplanet Search program, called ESPRI.
In this paper, we describe the narrow-angle astrometry measurement principle, give an overview of the ongoing hardand
software developments, and outline our anticipated astrometric exoplanet search program.
ESPRI is a project which aims at searching for and characterizing extra-solar planets by dual-beam astrometry with
PRIMA@VLTI. Differential Delay Lines (DDL) are fundamental for achieving the micro-arcseconds accuracy required
by the scientific objective. Our Consortium, consisting of the Geneva Observatory, the Max-Planck Institut for
Astronomy Heidelberg, and the Landessternwarte Heidelberg, in collaboration with ESO, has built and tested these
DDLs successfully and will install them in summer 2008 at the VLTI. These DDLs consist of high quality cat's eyes
displaced on a parallel beam-mechanics and by means of a two-stage actuation with a precision of 5 nm over a stroke
length of 70 mm. Over the full range, a bandwidth of about 400 Hz is achieved. The DDLs are operated in vacuum. We
shall present, in this paper, their design and their exceptional performances.
AstraLux is the Lucky Imaging camera for the Calar Alto 2.2-m telescope, based on an electron-multiplying
high speed CCD. By selecting only the best 1-10% of several thousand short exposure frames, AstraLux provides
nearly diffraction limited imaging capabilities in the SDSS i' and z' filters over a field of view of 24×24 arcseconds.
By choosing commercially available components wherever possible, the instrument could be built in short time
and at comparably low cost. We present the instrument design, the data reduction pipeline, and summarise the
performance and characteristics.
With the building of scientific camera systems for astronomical purposes in mind, the Max-Planck-Institut fuer
Astronomie (MPIA) has recently started developing new visual and infrared detector Read-out systems.
Due to the modular design, the electronics components can be configured for a wide range of currently available IR-detectors
and CCDs. The new Read-out Electronics are able to handle single or multiple detector systems with up to 144
input channels, feature high-speed data transfer and low power dissipation and additionally the system size is small and
lightweight.
The design is divided in four functional groups: controller board with variable Pattern Generator and fast fiber link,
clock/bias board, analog to digital converter board and the PCI data receiver board which writes the incoming data into
the computer memory. This design is highly versatile and allows for a wide variety of applications.
The high data transfer rate, small size and low heat dissipation makes these Read-out Electronics ideal for relatively
large focal plane arrays. The first instrument running with the new Read-out Electronics will be PANIC (Panoramic Near
Infrared Camera) at the 2.20 m telescope on Calar Alto.
PANIC is a wide-field NIR camera, which is currently under development for the Calar Alto observatory (CAHA) in
Spain. It uses a mosaic of four Hawaii-2RG detectors and covers the spectral range from 0.8-2.5 μm (z to K-band). The
field-of-view is 30×30 arcmin. This instrument can be used at the 2.2m telescope (0.45arcsec/pixel, 0.5×0.5 degree
FOV) and at the 3.5m telescope (0.23arcsec/pixel, 0.25×0.25 degree FOV).
The operating temperature is about 77K, achieved by liquid Nitrogen cooling. The cryogenic optics has three flat folding
mirrors with diameters up to 282 mm and nine lenses with diameters between 130 mm and 255 mm. A compact filter
unit can carry up to 19 filters distributed over four filter wheels. Narrow band (1%) filters can be used.
The instrument has a diameter of 1.1 m and it is about 1 m long. The weight limit of 400 kg at the 2.2m telescope
requires a light-weight cryostat design. The aluminium vacuum vessel and radiation shield have wall thicknesses of only
6 mm and 3 mm respectively.
In this paper we present an overview of the construction and implementation of the unmodulated infrared pyramid wavefront sensor PYRAMIR at the Calar Alto 3.5 m telescope. PYRAMIR is an extension of the existing visible Shack-Hartmann adaptive optics system ALFA, which allows wavefront sensing in the near-infrared wavefront regime. We describe the optical setup and the calibration procedure of the pyramid wavefront sensor. We discuss possible drawbacks of the calibration and show the results gained on Calar Alto.
A first generation of VLTI (Very Large Telescopes Interferometer) focal instruments, AMBER in the near-infrared and MIDI in the mid-infrared, has been already integrated and tested. New and important science results have been obtained. These instruments combine two (for MIDI) or three (for AMBER) beams coming from the eight telescopes installed at Cerro Paranal (four 8-meters and four 1.8-meters telescopes). In order to improve the capabilities of the interferometer and to engage a new scientific prospective, the second generation of VLTI instruments is currently under study. MATISSE belongs to this second generation. MATISSE objective is the image reconstruction. It will extend the astrophysical potential of the VLTI by overcoming the ambiguities existing in the interpretation of simple visibility measurements. It is a spectro-interferometer combining up to four beams with a large spectral coverage ranging from 3 to 25 μm (L, M, N and Q bands). Different spectral resolutions (between 30 and 1500) are foreseen. MATISSE will measure closure phase relations thus offering an efficient capability for image reconstruction. The concept of MATISSE is presented in this paper. The recombination mode of MATISSE is similar to the AMBER beam combination, but has been adapted to the constraints specific to the mid-infrared domain.
Our objective is the development of mid-infrared imaging at the VLTI. The related science case study demonstrates the enormous capability of a new generation mid-infrared beam combiner. MATISSE will constitute an evolution of the two-beam interferometric instrument MIDI by increasing the number of recombined beams up to four. MIDI is a very successful instrument which offers a perfect combination of spectral and angular resolution. New characteristics present in MATISSE will give access to the mapping and the distribution of the material (typically dust) in the circumstellar environments by using a wide mid-infrared band coverage extended to L, M, N and Q spectral bands. The four beam combination of MATISSE provides an efficient UV-coverage: 6 visibility points are measured in one set and 4 closure phase relations which can provide for the first time aperture synthesis images in the mid-infrared spectral regime. The mid-infrared spectral domain is very relevant for the study of the environment of various astrophysical sources. Our science case studies show the wide field of applications of MATISSE. They will be illustrated in the first part of this presentation through the perspective of imaging the circumstellar environments/discs of young stellar objects. The MATISSE characteristics will be given in a second part of the presentation.
KEYWORDS: Digital signal processing, Electronics, Mirrors, Actuators, Adaptive optics, Deformable mirrors, Control systems, Diagnostics, Digital micromirror devices, Power supplies
Full-custom electronics have been designed to drive Xinetics deformable mirrors, for use with the PYRAMIR (Calar Alto) and LINC/NIRVANA (Large Binocular Telescope) AO instruments, under contract to the Max-Planck-Institut fur Astronomie (MPIA). Significant enhancements to the original 1998 design for ALFA (Calar Alto) have been incorporated, including an embedded 2.1 Gb/s fiber link, temperature-controlled bias voltage, and multiple tip-tilt control outputs. Each 7U chassis with integral power supplies can drive mirrors of up to 349 actuators, and may be cascaded to support larger mirrors. A customized 600 MHz 'C6415 DSP module was specified to minimize latency, with frame rates above 7.5 KHz demonstrated for the 349-actuator DM. Power op-amps with 0.38 W/channel quiescent dissipation were chosen to reduce heat load, while supporting full-power (60 Vpp) bandwidth to above 300 Hz. These subsystems were successfully integrated in Heidelberg during November, 2003. The engineering firm responsible for the design, Cambridge Innovations, has since been awarded two additional contracts for DM electronics, including a new full-custom design for AURA (Gemini Observatory) to drive multiple high-voltage CILAS piezo bimorph DMs.
A new wavefront sensor based on the pyramid principle is being built at MPIA, with the objective of integration in the Calar Alto adaptive optics system ALFA. This sensor will work in the near-infrared wavelength range (J, H and K bands). We present here an update of this project, named PYRAMIR, which will have its first light in some months. Along with the description of the optical design, we discuss issues like the image quality and chromatic effects due to band sensing. We will show the characterization of the tested pyramidal components as well as refer to the difficulties found in the manufacturing process to meet our requirements. Most of the PYRAMIR instrument parts are kept inside a liquid nitrogen cooled vacuum dewar to reduce thermic radiation. The mechanical design of the cold parts is described here. To gain experience, a laboratory pyramid wavefront sensor was set up, with its optical design adapted to PYRAMIR. Different tests were already performed. The electronic and control systems were designed to integrate in the existing ALFA system. We give a description of the new components. An update on the future work is presented.
The PRIMA facility will implement dual-star astrometry at the VLTI. We have formed a consortium that will build the PRIMA differential delay lines, develop an astrometric operation and calibration plan, and deliver astrometric data reduction software. This will enable astrometric planet surveys with a target precision of 10μas. Our scientific goals include determining orbital inclinations and masses for planets already known from radial-velocity surveys, searches for planets around stars that are not amenable to high-precision radial-velocity observations, and a search for large rocky planets around
nearby low-mass stars.
KEYWORDS: Mirrors, James Webb Space Telescope, Actuators, Picture Archiving and Communication System, Optical components, Optical filters, Calibration, Electronics, Prisms, Spectrographs
The Mid-Infrared Instrument (MIRI) and the Near-Infrared Spectrograph (NIRSpec) of the JWST require various mechanisms for positioning optical elements in cryo-vacuum environment (7K resp. 35K): Wheels for exchanging filters, gratings and prisms, a flip mirror for switching between the sky and internal calibration sources and a linear actuator for refocusing purposes will have to be developed. In order to fulfill the stringent requirements of the mission, comprising to survive a warm ARIANE 5 launch, to guarantee high accuracy positioning in the cryovacuum with minimal power dissipation, to be operational with high reliability during 10 years of lifetime and to be testable under various environmental conditions, we propose a low cost and low schedule risk approach, based on the successful flight experience and qualification heritage from ESA’s infrared missions ISO and HERSCHEL.
CONICA has been developed by a German consortium under an ESO contract, to serve together with the VLT adaptive optics system NAOS as a high resolution multimode NIR camera and spectrograph. We report on final laboratory performance tests carried out during the integration period with the adaptive optics. Apart from an outline of the capabilities of this multimode instrument such as high resolution imaging, spectroscopy, Fabry-Perot and a sophisticated internal flexure compensation, we will turn our attention to a detailed examination of the detector characteristics to fully exploit the potential of the ALADDIN array.
Mechanisms operating in the cryovacuum are required to rotate filter and dichroic wheels, to tilt gratings and to flip in the beam of an internal calibration source. The design proposed here is based on similar mechanisms flown successfully on the liquid helium cooled European ISO-satellite and being presently under qualification for ESA's cooled HERSCHEL-satellite. Their main characteristics are high reliability during the 10 year lifetime in space, high precision and low heat dissipation in the cryovacuum.
The mid-infrared interferometric instrument MIDI is currently undergoing testing in preparation for commissioning on the Very Large Telescope Interferometer VLTI at the end of this year 2002. It will perform interferometric observations over the 8 μm - 13 μm wavelength range, with a spatial resolution of 20 milliarcsec, a spectral resolution of up to 250, and an anticipated point source sensitivity of N = 4 mag or 1 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 and the performance during laboratory tests, both for broadband and spectrally resolved observing modes. We also briefly outline the planned guaranteed time observations.
First laboratory test result of CONICA are presented for the variety of observation modes: using the final ALADDIN- Detector, IR images in direct, spectroscopic and polarimetric modes are compared to theoretically expected diffraction limited point spread functions. In long slit spectroscopy, wavelength calibration and spectral resolution is demonstrated for the different grism, slit and camera combinations.
MIDI is a two channel mid-infrared interferometric instrument developed for the Very Large Telescopes (VLT) Interferometer (VLTI). A control system with real-time capabilities integrates the various VLTI subsystems. Based on the VLTI control architecture and its interferometric extension, the VLTI control system, the MIDI control system will use synchronized VME computers running Tornado to control time critical subsystems such as delay lines and detector control electronics. Standard Unix workstations run high-level coordinating, monitoring, and data pre-processing tasks as well as graphical user interfaces. We describe the MIDI control architecture, the data flow and storage concept, and the self fringe tracking option. Furthermore we introduce a software package currently under development to simulate observations with MIDI.
The Max-Planck-Institutes for Astronomy and for Extraterrestrial Physics (MPE) have recently installed a laser guide star (LGS) adaptive optics (AO) system at the 3.5m telescope on Calar Alto in Spain. The AO system consists of a Shack-Hartmann sensor, a deformable mirror with 97 actuators, and a wave-front processor that allows closed loop operations of up to 1200 Hz. As a first step we closed the high order AO loop on bright natural guide stars. As a second step we closed the AO loop ALFA's design, operation, and upgrade plans.
The 3.8 m UK Infrared Telescope has been the focus of a program of upgrades intended to deliver images which are as close as possible to the diffraction limit at (lambda) equals 2.2 micrometers (FWHM equals 0.'12). This program is almost complete and many benefits are being seen. A high-bandwidth tip-tilt secondary mirror driven by a Fast Guider sampling at <EQ 100 Hz effectively eliminates image movement as long as a guide star with R < 16.m5 is available within +/- 3.'5 of the target. Low-order active control of the primary mirror and precision positioning of the secondary, using simple lookup tables, provide telescope optics which are already almost diffraction limited at (lambda) equals 2 micrometers . To reduce facility seeing the dome has been equipped with sixteen closable apertures to permit natural wind flushing, assisted in low winds by the building ventilation system. The primary mirror will soon be actively cooled and the concrete dome floor may be thermally insulated against daytime heating if fire safety concerns can be resolved. Delivered images in the K band now have FWHM which is usually <EQ 0.'8, frequently <EQ 0.'6 and quite often approximately 0.'3. Examples of the latter are shown: these approximate the resolution achieved by NICMOS on the HST. We estimate that the productivity of the telescope has approximately doubled, while its oversubscription factor has increased to > 4.
The 3.8 m UK infrared telescope (UKIRT) is currently the focus of an upgrades program to improve its imaging performance, ideally to approach its diffraction limit in the near-IR at 2.2 micrometer, with FWHM approximately 0.'12. This program is now in its late stages. All the new systems have been designed, most have been manufacture and many have been installed. A new top end carries an adaptive tip-tilt secondary mirror with active precision alignment, which, with low-order active control of the primary mirror, should provide the desired intrinsic optical performance. The adaptive tip- tilt system will correct image motion from telescope vibrations and drive errors and from atmospheric wavefront tilt; delivered images are expected regularly to be less than 0.'5 over wide fields, and within a factor 2 or so of the diffraction limit, at least inside an isoplanatic patch of order an arcmin radius. To reduce facility seeing the primary mirror has been equipped with a ventilation system and will receive a 5 kW cooling system; the dome is being equipped with sixteen closable apertures to permit natural wind flushing, which can be assisted by the building air handling system in low winds. It is hoped that facility seeing -- excluding boundary layer effects -- will be imperceptible during approximately 85% of observable time. The upgraded UKIRT should be well capable of exploiting fully the very best conditions on Mauna Kea.
This is a progress report on the development of the tip-tilt secondary mirror for the United Kingdom Infrared Telescope on Mauna Kea, Hawaii. The concept-- with emphasis on the electromechanical and optomechanical design--was published in an earlier paper. The reader is kindly requested to refer to the background information given there. Here, we present the electronics, system control and data handling considerations along with updated design drawings of the mirror and the combined piezoelectric/hexapod mirror mounts.
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