The Mid-infrared ELT Imager and Spectrograph (METIS) is one of the first-light scientific instruments for the ELT with over 75 optical components. The science cases of METIS impose tight stability requirements on the optical performance. To assess whether the optical performance is harmed by micro-vibrations, the effect of numerous vibration sources on the optical stability are analyzed. We present the analysis approach and results for METIS. This includes finite element analysis to obtain transfer functions, compute rigid body motion response of optical elements and assess the optical impact by ray-tracing.
METIS, the Mid-infrared ELT Imager and Spectrograph for the Extremely Large Telescope (ELT), is one of the three firstgeneration science instruments, it has passed final design [1],[2] and is midway the Manufacturing, Assembly, Integration and verification (MAIV) phase. The Imager will be completely assembled and tested at MPIA in Heidelberg, Germany, before integration into the METIS instrument in Leiden, Netherlands. The Imager sub-system provides diffraction-limited imaging capabilities and low-resolution grism spectroscopy in two channels: the first covers the atmospheric L&M bands with a field of view of 11x11 arcsec, the second covers the N band, with a field of view of 14x14 arcsec. The two channels are equipped with a HAWAII-2RG detector for LM band and a GeoSnap detector for the N band, respectively [3],[5]. Challenging requirements suitable for high contrast imaging require a thorough integration and verification, particularly considering the size, complexity and the operating temperature of the instrument. Virtually, all components and units are in production or are already finished. The integration and verification of these units follow an MAIV plan including a detailed alignment scheme. The AIV part consists of three different phases: acceptance tests of components, alignment tasks, and verification of requirements. A dedicated test cryostat has been developed for the end-to-end verification to guarantee a smooth integration into the METIS instrument. Here, we present this MAIV process and describe in detail exemplary individual tasks of each phase to demonstrate the complexity of this stage of development and the managing of the challenging procedures. We also describe the tools and the corresponding setups used in the laboratory to execute the various tests, and the application of interferometric measurements at cryogenic conditions.
The Imager subsystem of METIS, the Mid-infrared ELT Imager and Spectrograph for the Extremely Large Telescope (ELT) in Chile, provides diffraction-limited imaging capabilities and medium-resolution spectroscopy over the full wavelength range 3 to 13 microns. This Imager has a collimator that feeds two cameras: LM bands and N band. A dichroic splits the bands into two camera optics and to the corresponding detectors. It also incorporates a precise pupil re-imaging optics for each channel, allowing the positioning of high contrast imaging masks for coronographic applications. The collimator and the two cameras are Three-Mirror Anastigmat systems (TMA). All mirrors' surfaces are freeform defined as Zernike surfaces directly polished onto bare aluminium. This optics permits diffraction-limited performance and allows diffraction-limited spectroscopy in the complete wavelength range as well as the required pupil performance. The Imager works at 40 Kelvin to provide detector-limited performance in both bands, while the fore optics of METIS operates at 70 Kelvin. Therefore, a kinematic mounting has been implemented to allow the temperature difference but at the same time keeps the optics aligned to the challenging accuracy required for high contrast imaging. We will present the optics design, the final opto-mechanics and their ongoing manufacturing at Fraunhofer Institute for Applied Optics and Precision Engineering (IOF).
METIS, the Mid-infrared Imager and Spectrograph for the Extremely Large Telescope (ELT), is one of the three first generation science instruments and about to complete its final design phase [1]. The Imager sub-system provides diffraction-limited imaging capabilities and low-resolution grism-spectroscopy in two channels: one covers the atmospheric LM bands with a field of view of 11x11 arcsec, and the second covers the N band, with a field of view of 14x14 arcsec. Both channels have a common collimator and a dichroic beam splitter dividing the light into two dedicated cameras and the corresponding detectors. In addition, the Imager provides a precise pupil re-imaging implementation allowing the positioning of high-contrast imaging masks for coronagraphic applications. The two channels are equipped with a HAWAII-2RG detector for LM-band and a GeoSnap detector for the N-band. We present the final optical design of the Imager in a summary, as well as the cryo-mechanical concept. The mechanical design gives an overview of the general design aspects and the analyses that demonstrate the approach how to deal with demanding stability and alignment requirements for high-contrast imaging. It further focuses on the design of individual units as e.g., on the GeoSnap detector mount and on the pupil re-imager. In addition, we exemplarily outline some of the key alignment and verification tasks, essential to guarantee the performance of the Imager.
LINC–NIRVANA (LN) is a MCAO module currently mounted on the Rear Bent Gregorian focus of the Large Binocular Telescope (LBT). It mounts a camera originally design to realize the interferometric imaging focal station of the LBT. LN follows the LBT strategy having two twin channels: a double Layer Oriented multi-conjugate adaptive optics system assists the two arms, supplying high order wave-front correction. In order to counterbalance the field rotation a mechanical derotation is applied for the two ground wave-front sensors, and an optical (K-mirror) one for the two high layers sensors, fixing the positions of the focal planes with respect to the pyramids aboard the wavefront sensors. The derotation introduces a pupil images rotation on the wavefront sensors changing the projection of the deformable mirrors on the sensor consequently. The soft real-time computer load the matrix corresponding to the needed at one degree step. Calibrations were performed in daytime only and using optical fibers.
The LBT (Large Binocular Telescope), located at about 3200m on Mount Graham (Tucson, Arizona) is an innovative project undertaken by institutions from Europe and USA. LINC-NIRVANA is an instrument which provides MCAO (Multi-Conjugate Adaptive Optics) and interferometry, combining the light from the two 8.4m telescopes coherently. This configuration offers 23m-baseline optical resolution and the sensitivity of a 12m mirror, with a 2 arc-minute diffraction limited field of view. The integration, alignment and testing of such a big instrument requires a well-organized choreography and AIV planning which has been developed in a hierarchical way. The instrument is divided in largely independent systems, and all of them consist of various subsystems. Every subsystem integration ends with a verification test and an acceptance procedure. When a certain number of systems are finished and accepted, the instrument AIV phase starts. This hierarchical approach allows testing at early stages with simple setups. The philosophy is to have internally aligned subsystems to be integrated in the instrument optical path, and extrapolate to finally align the instrument to the Gregorian bent foci of the telescope. The alignment plan was successfully executed in Heidelberg at MPIA facilities, and now the instrument is being re-integrated at the LBT over a series of 11 campaigns along the year 2016. After its commissioning, the instrument will offer MCAO sensing with the LBT telescope. The interferometric mode will be implemented in a future update of the instrument. This paper focuses on the alignment done in the clean room at the LBT facilities for the collimator, camera, and High-layer Wavefront Sensor (HWS) during March and April 2016. It also summarizes the previous work done in preparation for shipping and arrival of the instrument to the telescope. Results are presented for every step, and a final section outlines the future work to be done in next runs until its final commissioning.
We present descriptions of the alignment and calibration tests of the Pathfinder, which achieved first light during our 2013 commissioning campaign at the LBT. The full LINC-NIRVANA instrument is a Fizeau interferometric imager with fringe tracking and 2-layer natural guide star multi-conjugate adaptive optics (MCAO) systems on each eye of the LBT. The MCAO correction for each side is achieved using a ground layer wavefront sensor that drives the LBT adaptive secondary mirror and a mid-high layer wavefront sensor that drives a Xinetics 349 actuator DM conjugated to an altitude of 7.1 km. When the LINC-NIRVANA MCAO system is commissioned, it will be one of only two such systems on an 8-meter telescope and the only such system in the northern hemisphere. In order to mitigate risk, we take a modular approach to commissioning by decoupling and testing the LINC-NIRVANA subsystems individually. The Pathfinder is the ground-layer wavefront sensor for the DX eye of the LBT. It uses 12 pyramid wavefront sensors to optically co-add light from natural guide stars in order to make four pupil images that sense ground layer turbulence. Pathfinder is now the first LINC-NIRVANA subsystem to be fully integrated with the telescope and commissioned on sky. Our 2013 commissioning campaign consisted of 7 runs at the LBT with the tasks of assembly, integration and communication with the LBT telescope control system, alignment to the telescope optical axis, off-sky closed loop AO calibration, and finally closed loop on-sky AO. We present the programmatics of this campaign, along with the novel designs of our alignment scheme and our off-sky calibration test, which lead to the Pathfinder’s first on-sky closed loop images.
The LINC-NIRVANA Pathfinder1 (LN-PF), a ground-layer adaptive optics (AO) system recently commissioned at the Large Binocular Telescope (LBT), is one of 4 sensors that provide AO corrected images to the full LINC-NIRVANA instrument. With first light having taken place on November 17, 2013,2, 3 the core goals for the LN-PF have been accomplished. In this report, we look forward to one of the LN-PF extended goals. In particular, we review the acquisition mechanism required to place each of several star probes on its corresponding star in the target asterism. For emerging AO systems in general, co-addition of light from multiple stars stands as one of several methods being pursued to boost sky coverage. With 12 probes patrolling a large field of view (an annulus 6-arcminutes in diameter), the LN-PF will provide a valuable testbed to verify this method.
The LINC-NIRVANA Pathfinder experiment is a test-bed to verify a very complex sub-system: the Ground-layer Wavefront Sensor, or GWS. Pathfinder will test the GWS in its final working environment and demonstrate on-sky the performance achievable with a multiple natural guide star, ground-layer adaptive optics system with a very wide FoV. The GWS uses up to 12 natural guide stars within a 2.8'-6' annular field of view and drives the LBT adaptive secondary mirror to correct the lower layers of atmospheric turbulence. This paper will trace the path of the instrument on its way to First Light on-sky in November 2013, from its installation on the telescope to the calibrations to its final operation, focusing in particular on opto-mechanical and software aspects and how they lead to the main achieved results.
The LBT (Large Binocular Telescope) located in Mount Graham near Tucson/Arizona at an altitude of about
3200m, is an innovative project being undertaken by institutions from Europe and USA. The structure of the
telescope incorporates two 8.4-meter telescopes on a 14.4 center-to-center common mount. This configuration
provides the equivalent collecting area of a 12m single-dish telescope.
LINC-NIRVANA is an instrument to combine the light from both LBT primary mirrors in an imaging Fizeau
interferometer. Many requirements must be fulfilled in order to get a good interferometric combination of the
beams, being among the most important plane wavefronts, parallel input beams, homotheticity and zero optical path
difference (OPD) required for interferometry. The philosophy is to have an internally aligned instrument first, and
then align the telescope to match the instrument.
The sum of different subsystems leads to a quite ambitious system, which requires a well-defined strategy for
alignment and testing. In this paper I introduce and describe the followed strategy, as well as the different solutions,
procedures and tools used during integration. Results are presented at every step.
LINC-NIRVANA is an instrument combining the two 8.4 m telescopes of the Large Binocular Telescope (LBT)
coherently, in order to achieve the optical resolution of the 23 meter baseline. For this interferometric instrument
concept, the common beam combination requires diffraction limited optical performance. The optics, realized as a
Cassegrain telescope design, consists of aluminum mirrors, designed and manufactured to fulfill the challenging
specifications required for interferometric imaging. Due to the science wavelength range from 1 μm to 2.4 μm, covering
the J, H and K band of the atmosphere, the complete beam combiner including the optics is operated in cryogenic
environment at 60 Kelvin. Here, we demonstrate the verification of the optical performance at this temperature for
classical in-coherent and coherent illumination. We outline the test setup and present the achieved results of wavefront
error for the individual beams and fringe contrast for the interferometric point spread function.
This paper continues the already presented integration of the interferometric camera with the focus on the performance
of the cryogenic optics.
LINC-NIRVANA (LN) is the near-infrared, Fizeau-type imaging interferometer for the large binocular telescope (LBT) on Mt. Graham, Arizona (elevation of 3267 m). The instrument is currently being built by a consortium of German and Italian institutes under the leadership of the Max Planck Institute for Astronomy in Heidelberg, Germany. It will combine the radiation from both 8.4 m primary mirrors of LBT in such a way that the sensitivity of a 11.9 m telescope and the spatial resolution of a 22.8 m telescope will be obtained within a 10.5×10.5 arcsec 2 scientific field of view. Interferometric fringes of the combined beams are tracked in an oval field with diameters of 1 and 1.5 arcmin. In addition, both incoming beams are individually corrected by LN’s multiconjugate adaptive optics system to reduce atmospheric image distortion over a circular field of up to 6 arcmin in diameter. A comprehensive technical overview of the instrument is presented, comprising the detailed design of LN’s four major systems for interferometric imaging and fringe tracking, both in the near infrared range of 1 to 2.4 μm, as well as atmospheric turbulence correction at two altitudes, both in the visible range of 0.6 to 0.9 μm. The resulting performance capabilities and a short outlook of some of the major science goals will be presented. In addition, the roadmap for the related assembly, integration, and verification process are discussed. To avoid late interface-related risks, strategies for early hardware as well as software interactions with the telescope have been elaborated. The goal is to ship LN to the LBT in 2014.
LINC-NIRVANA (LN) is the near-infrared, Fizeau-type imaging interferometer for the Large Binocular Telescope
(LBT) on Mt. Graham, Arizona, USA (3267m of elevation). The instrument is currently being built by a consortium of
German and Italian institutes under the leadership of the Max Planck Institute for Astronomy (MPIA) in Heidelberg,
Germany. It will combine the radiation from both 8.4m primary mirrors of LBT in such a way that the sensitivity of a
11.9m telescope and the spatial resolution of a 22.8m telescope will be obtained within a 10.5arcsec x 10.5arcsec
scientific field of view. Interferometric fringes of the combined beams are tracked in an oval field with diameters of 1
and 1.5arcmin. In addition, both incoming beams are individually corrected by LN’s multi-conjugate adaptive optics
(MCAO) system to reduce atmospheric image distortion over a circular field of up to 6arcmin in diameter.
This paper gives a comprehensive technical overview of the instrument comprising the detailed design of LN’s four
major systems for interferometric imaging and fringe tracking, both in the NIR range of 1 - 2.4μm, as well as
atmospheric turbulence correction at two altitudes, both in the visible range of 0.6 - 0.9μm. The resulting performance
capabilities and a short outlook of some of the major science goals will be presented. In addition, the roadmap for the
related assembly, integration and verification (AIV) process will be discussed. To avoid late interface-related risks,
strategies for early hardware as well as software interactions with the telescope have been elaborated. The goal is to ship
LN to the LBT in 2014.
LINC-NIRVANA is an interferometric imaging camera, which combines the two 8.4 m telescopes of the Large
Binocular Telescope (LBT). The instrument operates in the wavelength range from 1.1 μm to 2.4 μm, covering the J, H
and K-band, respectively. The beam combining camera (NIRCS) offers the possibility to achieve diffraction limited
images with the special resolution of a 23 m telescope. The optics are designed to deliver a 10 arcsec × 10 arcsec field of
view with 5 mas resolution. In this paper we describe the evolution of the cryogenic optics, from design and
manufacturing to verification. Including the argumentation for decisions we made in order to present a sort of guideline
for large cryo-optics. We also present the alignment and testing strategies at a detailed level.
LINC-NIRVANA is an interferometric imaging camera, which combines the two 8.4 m telescopes of the Large
Binocular Telescope (LBT). The instrument operates in the wavelength range from 1.1 μm to 2.4 μm, covering the J, H and K-bands. The beam combining camera (NIRCS) offers the possibility to achieve diffraction limited images with the
spatial resolution of a 23 m telescope.
This camera, which combines the AO corrected beams of both telescopes, is designed to deliver a 10 arcsec x 10 arcsec
diffraction limited field of view. The optics and cryo-mechanics are designed for operation at 60 Kelvin. Equipped with a
HAWAII-2 detector mounted on a rotation stage in order to compensate for the sky rotation, a filter wheel and a dichroic
wheel to split the light into the science channel and the fringe tracking channel, the camera is fairly large and complex
and requires certain features to be considered and tested.
The verification of all these components follows a challenging AIV plan. We describe this AIV phase from initial
integration of individual units to the final verification tests of the complete system. We report the performance of the
cryogenic opto-mechanics and of the science detector. We also demonstrate the functionality of the cryo-mechanics and
the cryo-cooling at sub-system level, which represents the current state of integration. Finally, we discuss key elements
of our design and potential pros and cons.
LINC-NIRVANA will employ four wave front sensors to realize multi-conjugate correction on both arms of a Fizeau interferometer for LBT. Of these, one of the two ground-layer wave front sensors, together with its infrared test camera, comprise a stand-alone test platform for LINC-NIRVANA. Pathfinder is a testbed for full LINC-NIRVANA intended to identify potential interface problems early in the game, thus reducing both technical, and schedule, risk. Pathfinder will combine light from multiple guide stars, with a pyramid sensor dedicated to each star, to achieve ground-layer AO correction via an adaptive secondary: the 672-actuator thin shell at the LBT. The ability to achieve sky coverage by optically coadding light from multiple stars has been previously demonstrated; and the ability to achieve correction with an adaptive secondary has also been previously demonstrated. Pathfinder will be the first system at LBT to combine both of these capabilities.
Since reporting our progress at A04ELT2, we have advanced the project in three key areas: definition of specific goals for Pathfinder tests at LBT, more detail in the software design and planning, and calibration. We report on our progress and future plans in these three areas, and on the project overall.
LINC-NIRVANA[1] (LN) is an instrument for the Large Binocular Telescope[2] (LBT). Its purpose is to combine the light
coming from the two primary mirrors in a Fizeau-type interferometer. In order to compensate turbulence-induced
dynamic aberrations, the layer oriented adaptive optics system of LN[3] consists of two major subsystems for each side:
the Ground-Layer-Wavefront sensor (GLWS) and the Mid- and High-Layer Wavefront sensor (MHLWS). The MHLWS
is currently set up in a laboratory at the Max-Planck-Institute for Astronomy in Heidelberg. To test the multi-conjugate
AO with multiple simulated stars in the laboratory and to develop the necessary control software, a dedicated light
source is needed. For this reason, we designed an optical system, operating in visible as well as in infrared light, which
imitates the telescope's optical train (f-ratio, pupil position and size, field curvature). By inserting rotating surface etched
glass phase screens, artificial aberrations corresponding to the atmospheric turbulence are introduced. In addition,
different turbulence altitudes can be simulated depending on the position of these screens along the optical axis. In this
way, it is possible to comprehensively test the complete system, including electronics and software, in the laboratory
before integration into the final LINC-NIRVANA setup. Combined with an atmospheric piston simulator, also this effect
can be taken into account. Since we are building two identical sets, it is possible to feed the complete instrument with
light for the interferometric combination during the assembly phase in the integration laboratory.
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.
PANIC, the Panoramic Near-Infrared Camera, is a new instrument for the Calar Alto Observatory. A 4x4 k detector
yields a field of view of 0.5x0.5 degrees at a pixel scale of 0.45 arc sec/pixel at the 2.2m telescope. PANIC can be used
also at the 3.5m telescope with half the pixel scale. The optics consists of 9 lenses and 3 folding mirrors. Mechanical
tolerances are as small as 50 microns for some elements. PANIC will have a low thermal background due to cold
stops. Read-out is done with MPIA's own new electronics which allows read-out of 132 channels in parallel. Weight
and size limits lead to interesting design features. Here we describe the opto-mechanical design.
We present the second-generation VLTI instrument GRAVITY, which currently is in the preliminary design phase.
GRAVITY is specifically designed 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 have identified the key design features needed to achieve this
goal and present the resulting instrument concept. It includes an integrated optics, 4-telescope, dual feed beam combiner
operated in a cryogenic vessel; near infrared wavefront sensing adaptive optics; fringe tracking on secondary sources
within the field of view of the VLTI and a novel metrology concept. Simulations show that the planned design matches
the scientific needs; in particular that 10µas astrometry is feasible for a source with a magnitude of K=15 like Sgr A*,
given the availability of suitable phase reference sources.
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.
The last step in designing and building instruments are the verification and acceptance tests of the assembled units and of
the final instrument. For instruments, which are engineered to work at the limit of feasibility, these tests must be accurate
and stable at a level much better than the expected performance of the instrument. Particularly for interferometric
instruments, this requires special care for the test planning and implementation in order to achieve the necessary
performance. This paper describes the verification and acceptance tests of the PRIMA DDL optics in terms of wavefront
error and tilt requirements as well as the assembling and aligning accuracy. We demonstrate the conformity of the optics
and point out the limitations of the test methods.
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.
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. Two instruments are 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).
All major components for the first instrument have been manufactured or are in the final stage of procurement. While integration and testing of LUCIFER 1 started in spring 2006 at the MPIA in Heidelberg, the cryostat for LUCIFER 2 has been sent to the MPE in Garching for system integration tests of the MOS-unit and testing of the mask cabinet exchange. The control electronics for the basic instrument has been manufactured, the MOS control electronics has been integrated and is being debugged. The MOS control software is under development by AIRUB. Fabrication and integration of components for LUCIFER 2 have started.
LAIWO is a new CCD wide-field camera for the 40-inch Ritchey-Chretien telescope at Wise Observatory in Mitzpe Ramon/Israel. The telescope is identical to the 40-in. telescope at Las Campanas Observatory, Chile, which is described in [2]. LAIWO was designed and built at Max-Planck-Institute for Astronomy in Heidelberg, Germany.
The scientific aim of the instrument is to detect Jupiter-sized extra-solar planets around I=14-15 magnitude stars with the transit method, which relies on the temporary drop in brightness of the parent star harboring the planet.
LAIWO can observe a 1.4 x 1.4 degree field-of-view and has four CCDs with 4096*4096 pixels each The Fairchild Imaging CCDs have a pixel size of 15 microns. Since they are not 2-side buttable, they are arranged with spacings between the chips that is equal to the size of a single CCD minus a small overlap.
The CCDs are cooled by liquid nitrogen to a temperature of about -100 °C. The four science CCDs and the guider CCD are mounted on a common cryogenic plate which can be adjusted in three degrees of freedom. Each of these detectors can also be adjusted independently by a similar mechanism. The instrument contains large shutter and filter mechanisms, both designed in a modular way for fast exchange and easy maintenance.
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.
The correction of atmospheric differential piston and instrumental flexure effects is mandatory for interferometric operation of the LBT NIR interferometric imaging camera LINC-NIRVANA. The task of the Fringe and Flexure Tracking System (FFTS) is to detect and correct these effects in a real-time closed loop. Being a Fizeau-Interferometer, the LBT provides a large field of view (FoV). The FFTS can make use of the large FoV and increase the sky coverage of the overall instrument if it is able to acquire the light of a suitable fringe tracking reference star within the FoV. For this purpose, the FFTS detector needs to be moved to the position of the reference star PSF in the curved focal plane and needs to precisely follow its trajectory as the field rotates. Sub-pixel (1 pixel = 18.5 micron) positioning accuracy is required over a travel range of 200mm x 300mm x 70mm. Strong are the constraints imposed by the need of a cryogenic environment for the moving detector. We present a mechanical design, in which the Detector Positioning Unit (DPU) is realized with off-the-shelf micro-positioning stages, which can be kept at ambient temperature. A moving baffle will prevent the intrusion of radiation from the ambient temperature environment into the cryogenic interior of the camera. This baffle consists of two nested disks, which synchronously follow any derotation - or repositioning trajectory of the DPU. The detector, its fanout board and a filter wheel are integrated into a housing that is mounted on top of the DPU and that protects the FFTS detector from stray light. Long and flexible copper bands allow heat transfer from the housing to the LINC-NIRVANA heat exchanger.
The MPIA is leading an international consortium of institutes building an instrument called LINC-NIRVANA. The instrument will combine the light from the two 8.4 m primary mirrors of the LBT. The beam combiner will operate at wavelengths between 1.1 and 2.4 microns, using a Hawaii2 detector. A volume of about 1.6 m high with a diameter of about 0.65 m is required for the cold optics. The size of the instrument and the high requirements on vibrations brought us to a new approach for the cooling of the cryostat, which has never been tried in astronomy. The cryostat will be cooled by a flow of Helium gas. The cooler which cools the gas will be placed far away on a different level in the telescope building. The cold helium will be fed through long vacuum isolated transfer lines to the instrument cryostat. Inside the cryostat a tube will be wrapped around the mounting structure of the cold optics. The first hardware arrived at the MPIA in 2005 and the system will soon be tested in our labs.
This paper describes the whole process of designing, manufacturing and assembling the optics for an infrared pyramid wavefront sensor, called PYRAMIR. This sensor is built to work with the adaptive optical system at the 3.5 m telescope of the Calar Alto Observatory, Spain, which controls a 97 actuator deformable mirror. PYRAMIR is working in combination with an infrared science camera, which is used for observations. Since the wavefront sensor works in the near infrared (1.0 μm to 2.4 μm), the detector, the optics and all the mechanics are cooled to liquid nitrogen temperature. For this cryogenic condition, special care has to be taken for the optical design and the mounting of the lenses. We describe in detail the process from infrared optical design and cryo-mechanical engineering, to the final assembly of the opto-mechanical units and testing in the lab. Technical solutions are illustrated and the final performance is demonstrated.
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.
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.
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.
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.
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.
The MPIA in Heidelberg has built many instruments for IR observation over the years. While the previous instruments were moderate in size and could easily be enclosed in a liquid nitrogen dewar, future instruments will require different cooling concepts. The use of Gifford McMahon coolers was chosen for some instruments, but has the disadvantage of low frequency vibrations. The recently-developed pulse tube coolers have lower vibrations but other disadvantages. For the LINC-NIRVANA cryostat, we plan to build a cooling system with a constant flow of Helium through a heat exchanger inside the cryostat. This cooling concept could also be expanded to future instrumentation for the next generation of telescopes.
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.
The LINC-NIRVANA instrument is a 1-2.5 micron Fizeau interferometric imager, which combines the light of the two 8.4 m mirrors of the Large Binocular Telescope on Mt. Graham in Arizona. The cryogenic camera forms the heart of the science channel of this instrument, delivering a 1 arcmin diameter field of view with 5 mas spatial resolution. The center 10x10 arcseconds, initially limited by the size of the 2048x2048 Hawaii-2 detector, are used for science observations. For simplicity, the camera has a fixed, F/32 optical path of the combined beams, leading to wavelength-dependent sampling. We describe the main components of the camera, as well as present the calculations of interferometric performance and the required opto-mechanical tolerances. We demonstrate that specially designed components can reach these specifications.
In the last few years, astronomical instruments with infrared detectors have become increasingly important. These detectors as well as the mechanical mechanisms inside the instruments are operated in high vacuum at cryogenic temperature. Since ready-for-use cryogenic actuators are often not available from stock, the Max-Planck-Institut fur Astronomie (MPIA) in Heidelberg has developed actuators for both linear and circular movement. Information about the use of materials, dry film lubricants, and components like motors, micro switches and resolvers for this temperature region is hard to find in literature. Thus, large-scale experiments and tests were made to gain experience and to qualify the actuators for their use at cryogenic temperatures.
Omega2000 is the first near infrared (NIR) wide field camera installed on the 3.5 m telescope at Calar Alto which operates with a 2kx2k HAWAII-2 FPA. Each component of the camera system must suit high requirements to exploit the facilities provided by the imaging sensor. To meet these requirements was a great challenge in design and realization of the optics, the mechanical part and the electronics. The cryogenic optical system with a warm mirror baffle can produce excellent optical quality and high sensitivity over the whole 15.4x15.4 arcmin field of view. The readout electronics together with the camera control software provide multi functional data acquisition and the camera control software can perform the readout and on-line data reduction simultaneously at a high data rate. Different operational and readout modes of the data acquisition of the detector both for engineering and scientific purpose were implemented, tested and optimized and the characteristics of three HAWAII-2 detectors were also determined
in their hardware and software environment. Initial astronomical
observations were carried out successfully in autumn 2003.
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.
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.
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.
Omega2000 is a prime focus near infrared (NIR) wide-field camera for the 3.5 meter telescope at Calar Alto/Spain. Having a large field of view and an excellent optical quality, the instrument is particularly designed for survey observations. A cryogenic four lens focal reducer delivers a 15.4 x 15.4 arcminute field of view (FOV) with a pixel scale of 0.45"/pixel. The lenses are made of various optical materials, including CaF2 and BaF2 with diameters of up to 150 mm. They must be specially mounted to survive cooling and to follow the tight tolerances (± 0.05 mm for lens centricity and ± 30 arcsec for lens tilt) required by the optical design. For a wide range of observing applications, a filter mechanism can hold up to 17 filters of 3 inch diameter in 3 filter wheels. For exact and reproducible filter positions, a mechanical locking mechanism has been developed which also improves the cool-down performance of the filter wheels and filters. This mechanism allows a minimum distance of about 3 mm between the filter wheels. A Rockwell HAWAII-2 FPA is used to cover the wavelength range from 0.85 μm to 2.4 μm. Special care has been taken with regard to the thermal coupling of the detector. The thermal connection is made by gold layers on the fanout board and an additional spring-loaded mechanism. A warm mirror baffle system has been developed, in order to minimize the thermal background for K band observations. The camera is a focal reducer only and has no cold pupil stop.
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.
The imaging photometer and spectroscopic camera PACS, one of the three scientific instruments aboard the European 3.5 m infrared space telescope FIRST, will apply a tilting mirror mechanism for optical beam switching. The development of this focal plane chopper, capable of operation under cryovacuum conditions, is reported here. In order to meet the stringent requirements with respect to power dissipation and positional accuracy, special drive coils and a new position sensor had to be developed. A simulation model including electromagnetic analysis by the 3D code MAFIA, verified by extensive cold testing of the prototype hardware, was used for the optimization of the system and led to the advanced prototype of the chopper. Closed loop control of the mirror deflection allows square wave modulation in the frequency range 0 - 15 Hz (80% duty cycle) with amplitudes of +/- 9 degree(s) with high positional accuracy of less than 30'. The power dissipation at operating temperature of 4 K is below 500 (mu) W.
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