4MOST is a versatile spectroscopic facility soon to be installed on the ESO VISTA Telescope at Paranal. Prior to shipment to Chile, our team is conducting a comprehensive characterization of the instrument in a controlled laboratory setting. This preparatory phase is crucial for ensuring the fulfilment of both technical specifications and some key user requirements. The goal of this verification campaign is to obtain characterization data which will benchmark the performance of the spectrographs and the calibration unit against established metrics. The data primarily tests the spectral performance of the three spectrographs, the stability of the system, including the calibration unit, as well as the fiber throughput, which are pivotal for the success of 4MOST’s ambitious science goals. Additionally, the verification contains a selection of user requirements, ensuring the instrument’s readiness for the diverse scientific objectives it aims to enable. The results from these tests inform the observational strategy for future normal science operations. In this paper we outline the undertaken preparatory work, the applied testing procedures, and the anticipated implications of these tests, and their results, in the context of the final verification at the telescope, commissioning and normal science operations. This initial test phase marks a critical juncture in the 4MOST project timeline, setting the stage for a successful commissioning.
ANDES is a high resolution spectrograph for the ELT, with the goal of providing simultaneous spectra with R 100000 from 0.35 to 2.4 micrometer. The baseline of the instrument covers 0.4 - 1.8 micron. Here we present the study on the extension into the K-band (1.95 to 2.45 micron) with its scientific motivation and the technical solution. The spectrograph design is constrained by external limits, but a solution is found that enables key science cases in this wavelength range and closes the gap in ELT high resolution spectroscopy between the ANDES baseline and the METIS instrument. The spectrograph design is throughput-optimized and is fed by the diffraction-limited input from the ANDES SCAO system. We summarize the preliminary optical and cryo-mechanical design. But, as the available mass is one of the critical parameters, we also look into an alternative implementation of the spectrograph with carbon fiber.
We describe the instrument’s design and architecture, emphasizing its unique features. The design is driven by requirements on resolving power, slit area, spectral coverage and stability. The instrument can operate in seeinglimited or SCAO modes, with options for sky and/or calibration measurements. In SCAO mode, it can use a small Integral Field Unit (IFU) with different spaxel scales. The light from the telescope reaches the Front-End on the Nasmyth platform, which has four insertable modules: two seeing-limited arms, one SCAO arm and one IFU arm. They are connected by fibres or fibre bundles to the Spectrographs in different locations: the Nasmyth Platform and the Coud´e room. The wavelength splitting depends on the fibre transparency. The subsystems are placed at different distances from the telescope. In Phase-B-one, we performed analyses to define the best trade-off for the budgets and architecture. We extended the spectrographs toward the goal ranges as much as possible. ANDES is complex, but its sophisticated and modular design will enable next-generation astronomy research.
4MOST (4-meter Multi-Object Spectroscopic Telescope) is a wide-field, fiber-fed, high-multiplex spectroscopic survey facility to be installed on the 4-meter ESO telescope VISTA in Chile. The back-end consists of one high-resolution spectrograph (HRS) and two identical low-resolution spectrographs. 4MOST will afford with the HRS simultaneous observations of up to 812 targets on a hexagonal 4.4 square degrees field of view at a spectral resolution R<18,000 covering 392.6 to 679 nm in three channels. It is expected to be fully operational early 2024. In this paper, we present the integration and alignment applied for the HRS optics. The results of the tests of the fully integrated sub-system in our integration facility are discussed. The instrument schedule is outlined and the actual timeline of the previous procurement and manufacturing phase is given
4MOST (4-meter Multi-Object Spectroscopic Telescope) is a wide-field, fiber-feed, high-multiplex spectroscopic survey facility to be installed on the 4-meter ESO telescope VISTA in Chile. Its backend consists of one high resolution spectrograph and two identical low resolution spectrographs. The instrument is presently in the final design phase (review in May 2018) and is expected to enter full operations at the beginning of 2023 ([1] and [2]). The high resolution spectrograph (HRS) will afford simultaneous observations of up to 812 targets – over a hexagonal field of view of ~ 4.1 square degrees on sky – with a spectral resolution R>18,000 covering wavelength ranges between 393 and 679 nm in three channels. The optical design of the instrument is described in detail in [5]. In February 2017 the final design review for the optics was held and passed successfully. The final design review for the mechanics and all other parts of the instrument was held in May 2018. A summary and update of the optical and mechanical design of the HRS are presented in this paper. The detailed status of the manufacturing of the optics is given. The procedures and tools used during the AIT phase for the optical alignment of the HRS system, as well as the performance tests and characterizations are described.
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.
4MOST (4-meter Multi-Object Spectroscopic Telescope) is a wide-field, fiber-feed, high-multiplex spectroscopic survey facility to be installed on the 4-meter ESO telescope VISTA in Chile. It consists of two identical low resolution spectrographs and one high resolution spectrograph. The instrument is presently in the preliminary design phase and expected to get operational end of 2022. The high resolution spectrograph will afford simultaneous observations of up to 812 targets - over a hexagonal field of view of ~ 4.1 sq.degrees on sky - with a spectral resolution R>18,000 covering a wavelength range from 393 to 679nm in three channels. In this paper we present the optical and mechanical design of the high resolution spectrograph (HRS) as prepared for the review at ESO, Garching. The expected performance including the highly multiplexed fiber slit concept is simulated and its impact on the optical performance given. We show the thermal and finite element analyses and the resulting stability of the spectrograph under operational conditions.
CARMENES is a fiber-fed high-resolution Echelle spectrograph for the Calar Alto 3.5m telescope. The instrument is built by a German-Spanish consortium under the lead of the Landessternwarte Heidelberg. The search for planets around M dwarfs with a radial velocity of 1 m/s is the main focus of the planned science. Two channels, one for the visible, another for the near-infrared, will allow observations in the complete wavelength range from 550 to 1700 nm. To ensure the stability, the instrument is working in vacuum in a thermally controlled environment. The VIS channel spectrograph is covering the visible wavelength range from 0.55 to 0.95 μm with a spectral resolution of R=93,400 in a thermally and pressure-wise very stable environment. The VIS channel spectrograph started science operation in January 2016. Here we present the opto-mechanical and system design of the channel with the focus on the (re-)integration phase at the observatory and the measured performance during the testing and commissioning periods, including the lessons learned.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation Very Large Telescope (VLT) integral field
spectrograph developed for the European Southern Observatory (ESO). It combines a 1’ x 1’ field of view sampled at 0.2
arcsec for its Wide Field Mode (WFM) and a 7.5"x7.5" field of view for its Narrow Field Mode (NFM). Both modes will
operate with the improved spatial resolution provided by GALACSI (Ground Atmospheric Layer Adaptive Optics for
Spectroscopic Imaging), that will use the VLT deformable secondary mirror and 4 Laser Guide Stars (LGS) foreseen in
2015. MUSE operates in the visible wavelength range (0.465-0.93 μm). A consortium of seven institutes is currently
commissioning MUSE in the Very Large Telescope for the Preliminary Acceptance in Chile, scheduled for September,
2014.
MUSE is composed of several subsystems which are under the responsibility of each institute. The Fore Optics derotates
and anamorphoses the image at the focal plane. A Splitting and Relay Optics feed the 24 identical Integral Field Units
(IFU), that are mounted within a large monolithic instrument mechanical structure. Each IFU incorporates an image
slicer, a fully refractive spectrograph with VPH-grating and a detector system connected to a global vacuum and
cryogenic system. During 2012 and 2013, all MUSE subsystems were integrated, aligned and tested to the P.I. institute at
Lyon. After successful PAE in September 2013, MUSE instrument was shipped to the Very Large Telescope in Chile
where it was aligned and tested in ESO integration hall at Paranal. After, MUSE was directly transferred in monolithic
way onto VLT telescope where the first light was achieved.
This paper describes the MUSE main optical component: the Field Splitter Unit. It splits the VLT image into 24
subfields and provides the first separation of the beam for the 24 Integral Field Units. This talk depicts its manufacturing
at Winlight Optics and its alignment into MUSE instrument. The success of the MUSE alignment is demonstrated by the
excellent results obtained onto MUSE positioning, image quality and throughput onto the sky. MUSE commissioning at
the VLT is planned for September, 2014.
TOAD, the “Top Of the Atmosphere to Detector” simulator, is a primary engineering tool that accompanies the development of the 4MOST instrument. The ultimate goal is to provide a detailed, end-to-end performance model of 4MOST by providing the detector image for an artificial target field with less then 5% error. TOAD will be able to create a realistic output for any reasonable input. The input can be anything, from point sources through extended sources, calibration lamps or stray-light, entering the system at virtually any point in a optical path. During the development of the 4MOST facility, the TOAD simulator will give invaluable insight into the interaction of various parts of the instrument and the impact of engineering design decisions on the system performance.
The 4MOST[1] instrument is a concept for a wide-field, fibre-fed high multiplex spectroscopic instrument facility on the
ESO VISTA telescope designed to perform a massive (initially >25x106 spectra in 5 years) combined all-sky public
survey. The main science drivers are: Gaia follow up of chemo-dynamical structure of the Milky Way, stellar radial
velocities, parameters and abundances, chemical tagging; eROSITA follow up of cosmology with x-ray clusters of
galaxies, X-ray AGN/galaxy evolution to z~5, Galactic X-ray sources and resolving the Galactic edge;
Euclid/LSST/SKA and other survey follow up of Dark Energy, Galaxy evolution and transients. The surveys will be
undertaken simultaneously requiring: highly advanced targeting and scheduling software, also comprehensive data
reduction and analysis tools to produce high-level data products. The instrument will allow simultaneous observations of
~1600 targets at R~5,000 from 390-900nm and ~800 targets at R<18,000 in three channels between ~395-675nm
(channel bandwidth: 45nm blue, 57nm green and 69nm red) over a hexagonal field of view of ~ 4.1 degrees. The initial
5-year 4MOST survey is currently expect to start in 2020. We provide and overview of the 4MOST systems: optomechanical,
control, data management and operations concepts; and initial performance estimates.
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.
The foundation of the MUSE instrument with its high multiplexing factor of twenty-four spectrographs is formed
through its central main structure that accommodates all instrumental subsystems and links them with the telescope. Due
to instrument's dimension and complexity, the requirements on structural performance are demanding. How its
performance was tested and optimized through reverse engineering is addressed. Intimately mated with this central
structure is an optical relay system that splits the single telescopic field into twenty-four subfields. Each of those is
individually directed along three dimensions across the structure through a folding and imaging setup of an optical relay
system that at the end feeds one of the twenty-four spectrographs. This opto-mechanical relay system was tested when
mounted onto the main structure. The results obtained so far are given here.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation VLT integral field spectrograph (1x1arcmin² Field of View) developed for the European Southern Observatory (ESO), operating in the visible wavelength range (0.465-0.93 μm). A consortium of seven institutes is currently assembling and testing MUSE in the Integration Hall of the
Observatoire de Lyon for the Preliminary Acceptance in Europe, scheduled for 2013.
MUSE is composed of several subsystems which are under the responsibility of each institute. The Fore Optics derotates
and anamorphoses the image at the focal plane. A Splitting and Relay Optics feed the 24 identical Integral Field Units
(IFU), that are mounted within a large monolithic instrument mechanical structure. Each IFU incorporates an image
slicer, a fully refractive spectrograph with VPH-grating and a detector system connected to a global vacuum and
cryogenic system. During 2011, all MUSE subsystems were integrated, aligned and tested independently in each
institute. After validations, the systems were shipped to the P.I. institute at Lyon and were assembled in the Integration
Hall
This paper describes the end-to-end optical alignment procedure of the MUSE instrument. The design strategy, mixing
an optical alignment by manufacturing (plug and play approach) and few adjustments on key components, is presented.
We depict the alignment method for identifying the optical axis using several references located in pupil and image
planes. All tools required to perform the global alignment between each subsystem are described. The success of this
alignment approach is demonstrated by the good results for the MUSE image quality.
MUSE commissioning at the VLT (Very Large Telescope) is planned for 2013.
CARMENES is a fiber-fed high-resolution échelle spectrograph for the Calar Alto 3.5m telescope. The instrument is
built by a German-Spanish consortium under the lead of the Landessternwarte Heidelberg. The search for planets around
M dwarfs with a radial velocity accuracy of 1 m/s is the main focus of the planned science. Two channels, one for the
visible, another for the near-infrared, will allow observations in the complete wavelength range from 550 to 1700 nm. To
ensure the stability, the instrument is working in vacuum in a thermally controlled environment. The optical design of
both channels of the instrument and the front-end, as well as the opto-mechanical design, are described.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation VLT panoramic integral field spectrograph developed
for the European Southern Observatory (ESO), operating in the visible and Near Infrared wavelength range (0.465-0.93
μm) with a 1 arcmin square FoV sampled at 0.2arcsec. It is composed of a Calibration unit, a Fore-optics and a Splitting
and relay system that feeds 24 identical Integral Field Units (IFU); each one incorporates an advanced image slicer
associated with a classical spectrograph. This article will present the optical design choices that have been done to
optimize the costs, size and performances of the instrument as well as a detailed ghost images analysis of the whole
instrument.
The Multi Unit Spectroscopic Explorer (MUSE) is a second generation instrument in development for the Very Large
Telescope (VLT) of the European Southern Observatory (ESO). The MUSE splitting and relay optics splits the
corresponding telescope 1'x1' adaptive optics corrected field of view into 24 sub-fields and feeds each sub-field into a
spectrograph. The design of the field splitter and separator unit and the performance of its prototype are described in
detail in this paper. The relay optics builds a 24-channel fan-shaped bridge between the sub-fields and the corresponding
spectrographs. An overview of the alignment procedure is given.
The Multi Unit Spectroscopic Explorer MUSE is a second-generation VLT instrument. With its high multiplexing factor
of twenty-four individual spectrographs, it requires rather complex opto-mechanics to split the field of 1x1 arcminute on
the sky into twenty-four sub-fields and guide them along the central instrument structure to the feeding point of each
spectrograph. The requirements on the underlying mechanical structure are quite demanding in terms of opto-mechanical
stability under thermal loads and thermal mismatch, warping of its basement and excessive earthquake loads. In total
seven individual load cases and combinations of them have been analyzed in extensive finite-element analyses (within
Nastran) with subsequent optical analyses (within Zemax). These two types of analyses will be addressed here and their
combined output will be set into relation with the requirements.
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.
The Multi Unit Spectroscopic Explorer MUSE is an integral field device containing 24 spectrographs at the Nasmyth
focus of the VLT unit telescope. The total field size of 1'x1' needs to be split and separated into 24 sub-fields which are
relayed along a central structure into the entrance aperture of the individual spectrographs. The realization of the optics
for field splitting and separation as well as the relay optics to direct the light of the individual fields to the spectrographs
is described here. A very tight link exists between the relay optics system layout and the mechanical arrangement of the
spectrographs in the common central structure. A compact mounting is essential due to the restricted space for such a
large instrument even on the VLT Nasmyth platform. A suitable arrangement of vertical and horizontal stacking of the
spectrographs was found enabling their feeding from the unobstructed front side of the instrumental structure. The
central instrument mount was designed as a stiff structure absorbing print-through effects due to thermal mismatch with
the telescope platform but rigid enough to withstand earthquakes.
Combining the two 8.4 m telescopes of the Large Binocular Telescope 1(LBT) offers the unique possibility to achieve diffraction limited images with 23 m spatial resolution. This requires an interferometric superposition of the two telescope beams in a Fizeau-type interferometer. LINC-NIRVANA delivers a 10 arcsec x 10 arcsec panoramic field of view with 5 mas pixel size. In addition to delivering diffraction limited, single-telescope images, the optics have several additional constraints imposed by interferometric operation. In this paper, we describe the evolution of the optical design and how the individual optical subsystems were developed in parallel to provide optimal combined performance. We also present an alignment strategy to setup the optics and to achieve zero optical path difference.
LINC-NIRVANA is an imaging interferometer for the Large Binocular Telescope (LBT) and will make use of multi-conjugated adaptive optics (MCAO) with two 349 actuators deformable mirrors (DM), two 672 actuator deformable secondary mirrors and a total of 4 wavefront sensors (WFS) by using 8 or 12 natural guide stars each. The goal of the MCAO is to increase sky coverage and achieve a medium Strehl-ratio over the 2 arcmin field of view. To test the concepts and prototypes, a laboratory setup of one MCAO arm is being built. We present the layout of the MCAO prototype, planned and accomplished tests, especially for the used Xinetics DMs, and a possible setup for a test on sky with an existing 8m class telescope.
On the way to the Extremely Large Telescopes (ELT) the Large Binocular
Telescope (LBT) is an intermediate step. The two 8.4m mirrors create a masked aperture of 23m. LINC-NIRVANA is an instrument taking advantage of this opportunity. It will get, by means of Multi-Conjugated Adaptive Optics (MCAO), a moderate Strehl Ratio over a 2 arcmin field of view, which is used for Fizeau (imaging) interferometry in J,H and K. Several MCAO concepts, which are
proposed for ELTs, will be proven with this instrument. Studies of sub-systems are done in the laboratory and the option to test them on sky are kept open. We will show the implementation of the MCAO concepts and control aspects of the instrument and present the road map to the final installation at LBT. Major milestones of LINC-NIRVANA, like preliminary design review or final design review are already done or in preparation. LINC-NIRVANA is one of the
few MCAO instruments in the world which will see first light and go into operation within the next years.
Several multi-conjugate adaptive optics (MCAO) systems using the layer-oriented approach are under construction and will soon be tested at different facilities in several instruments. One of these instruments is LINC-NIRVANA, a Fizeau interferometer for the Large Binocular Telescope (LBT). This instrument uses a ground layer wavefront sensor (GWS) and a combined mid-high layer wavefront sensor (MHWS) with different fields of view (concept of multiple field of view), a 2-6 arcmin annular ring for the GWS and a 2 arcmin diameter central field of view for the MHWS. Both sensors are Pyramid wavefront sensors which optically co-add light from multiple natural guide stars.
The opto-mechanical problems concerning these sensors are related to the fast focal ratio of the beam on the pyramids coupled with the available pixelscale of detectors. This leads to very tight requirements on the moving systems (linear stages) for the star enlargers (SE) used to pick off the light of individual stars.
As there are 40 star enlargers in the overall system, additional efforts were put into the alignment system of the optics of the star enlargers and the reduction in size of the star enlargers to minimize the distance between available guide stars.
LUCIFER (LBT NIR Spectrograph Utility with Camera and Integral-Field
Unit for Extragalactic Research) is a NIR spectrograph and imager for
the LBT (Large Binocular Telescope) working in the wavelength range from 0.9 to 2.5 microns. The instrument is to be built by a consortium of five german institutes (Landessternwarte Heidelberg (LSW), Max Planck Institut for Astronomy (MPIA), Max Planck Institut for Extraterrestric Physics (MPE), Astronomical Institut of the Ruhr-University Bochum (AIRUB) and Fachhochschule for Technics and Design Mannheim (FHTG)). LUCIFER will be one of the first light instruments of the LBT and will be available to the community at the end of 2005. A copy of the instrument for the second LBT mirror follows about one year later.
The paper presents a brief status report of the procured and built
hardware, of the workpackages already carried out and summarizes the ongoing work in progress.
LINC-NIRVANA is a Fizeau interferometer which will be built for the Large Binocular Telescope (LBT). The LBT exists of two 8.4m mirrors on one mounting with a distance of 22.8m between the outer edges of the two mirrors. The interferometric technique used in LINC-NIRVANA provides direct imaging with the resolution of a 23m telescope in one direction and 8.4m in the other. The instrument uses multi-conjugated adaptive optics (MCAO) to increase the sky coverage and achieve the diffraction limit in J, H, K over a moderate Field of View (2 arcmin in diameter). During the preliminary design phase the team faced several problems similar to those for an instrument at a 23m telescope. We will give an overview of the current design, explain problems related to 20m class telescopes and present solutions.
Layer Oriented represented in the last few years a new and promising aproach to solve the problems related to the limited field of view achieved by classical Adaptive Optics systems. It is basically a different approach to multi conjugate adaptive optics, in which pupil plane wavefront sensors (like the pyramid one) are conjugated to the same altitudes as the deformable mirrors. Each wavefront sensor is independently driving its conjugated deformable mirror thus simplifying strongly the complexity of the wavefront computers used to reconstruct the deformations and drive the mirror themselves, fact that can become very important in the case of extremely large telescopes where the complexity is a serious issue. The fact of using pupil plane wavefront sensors allow for optical co-addition of the light at the level of the detector thus increasing the SNR of the system and permitting the usage of faint stars, improving the efficiency of the wavefront sensor. Furthermore if coupled to the Pyramid wavefront sensor (because of its high sensitivity), this technique is actually peforming a very efficient usage of the light leading to the expectation that, even by using only natural guide stars, a good sky coverage can be achieved, above all in the case of giant telescopes. These are the main reasons for which in the last two years several projects decided to make MCAO systems based on the Layer Oriented technique. This is the case of MAD (an MCAO demonstrator that ESO is building with one wavefront sensing channel based on the Layer Oriented concept) and NIRVANA (an instrument for LBT). Few months ago we built and successfully tested a first prototype of a layer oriented wavefront sensor and experiments and demonstrations on the sky are foreseen even before the effective first light of the above mentioned instruments. The current situation of all these projects is presented, including the extensive laboratory testing and the on-going experiments on the sky.
We are currently working on four projects employing Multi Conjugate Adaptive Optics in a Layer-Oriented fashion. These ranges from experimental validations, to demonstration facility or full instrument to be offered to an astronomical community and involves telescopes in the range of 4m to 24m equivalent telescope aperture. The current status of these projects along with their brief description is here given.
LUCIFER (LBT NIR-Spectroscopic Utility with Camera and Integral-Field Unit for Extragalactic Research) is a NIR spectrograph and imager for the Large Binocular Telescope (LBT) on Mt. Graham, Arizona. It is built by a consortium of five German institutes and will be one of the first light instruments for the LBT. Later, a second copy for the second mirror of the telescope will follow.
Both instruments will be mounted at the bent Gregorian foci of the two individual telescope mirrors. The final design of the instrument is presently in progress.
LUCIFER will work at cryogenic temperature in the wavelength range from 0.9 μm to 2.5 μm. It is equipped with three exchangeable cameras for imaging and spectroscopy: two of them are optimized for seeing-limited conditions, the third camera for the diffraction-limited
case with the LBT adaptive secondary mirror working. The spectral resolution will allow for OH suppression. Up to 33 exchangeable masks will be available for longslit and multi-object spectroscopy (MOS) over the full field of view (FOV). The detector will be a Rockwell HAWAII-2 HgCdTe-array.
In order to achieve moderate Field of View (2 arcmin in diameter) and nearly diffraction limited capabilities, at the reddest portion of the visible spectrum in the interferometric mode of LBT, two sophisticated MCAO channels are required. These are being designed to perform a detailed correction of the atmospheric turbulence through three deformable mirrors per telescope arm: the secondary adaptive mirror and two commercial piezostack mirrors, leading to an overall number of degree of freedom totaling ~ 3000. A combination of numerical and optical coaddition of light collected from natural reference stars located inside the scientific Field of View and in an annular region, partially vignetted, and extending up to ≈ 6 arcmin in diameter, allows for such a performance with individual loops characterized by a much smaller number of degree of freedom, making the real-time computation, although still challenging, to more reasonable levels. We implement in the MCAO channel the dual Field of View layer-oriented approach using natural guide stars, only allowing for limited, but significant, sky coverage.
In this paper, we review the salient facts for a range of available atmosphere emulation technologies, and in the framework of the ESO Multi-Conjugate-AO demonstrator project, aptly called MAD, we present our phase screen test results for silver-sodium ion-exchange, transmissive phase screens. We find (a) that the measured power spectrum of phase fluctuations is consistent with the input Von Karman spectrum and (b) that by tracking the best focus of ten spots formed by a silver-sodium ion-exchange micro-lens array, it was found that the wavelength dependence of 1.266μm of phase-shift is 1.5±2.5% relative to air in the wavelength range 550nm to 800μm.
Additionally, we present our optical design and specifications for MAPS, the Multi-Atmospheric Phase screens and Stars instrument that will be used to test MAD before shipment to the VLT. It includes glass screens conjugate to the 0.25km, 3.0km, and 9.0km atmospheric layers above the telescope. We explain the reasoning behind the choice of pupil size and implications for phase screen proximity, footprint sizes, and wind speed gradients. Our design mimics the VLT Nasmyth F/15 focal plane in terms of plate scale, field of view, high Strehl, and field curvature.
For dioptic instruments working in the near-infrared (NIR), the choice of materials for lenses is mostly limited to special glasses or crystals. Most commonly used are CaF2, BaF2, infrared fused silica, ZnS and ZnSe. Those materials can in general not provide good chromatic correction for fast systems. Moreover, the high index materials, as well as infrared glass like Schott IRG, are quite limited with regard to availability in larger sizes and thicknesses and/or optical quality.
An investigation was made for optical glasses from the Schott and Ohara catalogues with high transmission up to a wavelength of 2.4 μm. For the most promising materials, the transmission from λ0.35μm to λ3.0μm, was measured in the lab with high spectral resolution. A systematic analysis of combinations of those optical glasses with the infrared materials was performed and the combinations with extremely good chromatic correction in the NIR are presented. There were several combinations found which are well corrected even from λ0.55μm to λ2.5μm, as needed for some designs of adaptive optics systems.
LUCIFER is a full cryogenic NIR spectrograph and imager to be built by a consortium of fiber institutes, Max Planck Institut fuer Astronomie in Heidelberg, Max Planck Institut fuer Extraterrestrische Physik in Garching, Astronomisches Institut der Ruhr Universitaet Bochum and Fachhochschule fuer Technik und Gestaltung in Mannheim. The instrument has been selected as one of three first-light instruments for the Large Binocular Telescope on Mt. Graham, Arizona which first mirror becomes available to the community in early 2003. The second mirror and a second more or less identical spectrograph/imager follows 18 months later. Both LUCIFER instruments will be mounted dat the bent Gregorian foci of the two individual LBT-mirrors and include six observing six observing modes: seeing and diffraction limited imaging, seeing and diffraction limited longslit spectroscopy, seeing limited multi-object spectroscopy and integral-field spectroscopy. The detector will be a Rockwell HAWAII-2 HgCdTe-array with a pixel-size of 18(mu) .
LAMOST is a special Schmidt telescope of 4 meters aperture. It will be located in Xinglong station at Beijing Astronomical Observatory, China. The start of science operation is expected in 2004. There are 4000 optical fibers on the telescope focal surface that will feed 16 low resolution spectrographs (LRS) and one or more medium resolution spectrograph and one high resolution spectrograph. Here we present a description of the LRS specification and its optical design. LRS is a multi object fiber spectrograph that is optimized for galaxy red shift surveys. The output bema with f-ratio of 4 from fiber are collimated by a spherical mirror and then are split to red and blue band by a dichroic filter. We use reflective grating as dispersion elements. Spectra are focused onto 2048 by 2048 CCD using fast Schmidt camera with f-ratio of 1. Spectral coverage per exposure is from 370nm to 900nm. The beam size is 200mm resulting resolution 1000 with 3.3 arcsecond fiber slit. The slit with 130mm length picks up 250 fibers, so we need 16 low-resolution spectrograph to observe spectra of 4000 celestial objects in single exposure.
FORS is an all dioptric focal reducer designed for direct imaging, low-dispersion multi-object spectroscopy, imaging polarimetry and spectropolarimetry of faint objects. Two almost identical copies of the instrument were built by a consortium of three astronomical institutes under contract and in cooperation with ESO. FORS1 was installed in September 1998 and FORS2 in October 1999 at the Cassegrain foci of the ESO VLT unit telescope nos. 1 and 2. FORS1 is in regular operation since April 1999. Regular observation with FORS2 are scheduled to begin in April 2000.
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