The warm calibration unit (WCU) is one of the subsystems of the future METIS instrument on the Extremely Large Telescope (ELT). Operating at room temperature, the WCU is mounted above the main cryostat of METIS. It will be employed as a calibration reference for science observations, as well as for verification and alignment purposes during the AIT phase. The WCU is designed and constructed at the University of Cologne, one of the partner in the METIS consortium. WCU recently went through a successful Optics Long Lead Items Review by ESO. Now, the WCU is entering the last phase of the project, the Final Design Review (FDR). In this paper, we present the current status of the WCU design and summarize the mechanical and system engineering work. We describe the design of the hexapod formed by six manually adjustable links and its interfaces with the METIS cryostat together with the CFRP-based optical bench and Invar-based optical mounts. Lab prototyping results of one actuator under a nominal load of 5 kN confirms the achievable high linear resolution (20 µm). We present the status of the WCU laser cabinet. We discuss the lastest progress in the laboratory testing of some WCU functionalities, such as the fibre-fed monochromatic sources for the spectral calibration of the LM-Spectrograph of METIS, and the spatial calibration sources using the integrating sphere. We detail the activities foreseen until FDR together with the preparation of the sub-system MAIT work.
METIS, the mid-infrared imager and spectrograph for the wavelength range 2.9 -13.5 µm (astronomical L-, MN- band), will be one of the three science instruments at the Extremely Large Telescope (ELT). It will provide diffraction-limited imaging, coronagraphy, high-resolution integral field spectroscopy, and low and medium resolution slit spectroscopy. Within the international METIS consortium, the University of Cologne is responsible for the design, manufacturing, integration, and qualification of the Warm Calibration Unit (WCU) of the instrument. In this contribution, we present the current status of the optical design and principle of optical operation of the WCU. The main train of the WCU optics is based on a modified F/17.75 Offner relay, with the optical output parameters matching the plate scale, F-number, as well as the exit-pupil position and size of that of the ELT. We discuss the optical design, and tolerance analysis of the WCU relay optics as part of the Optics FDR review by ESO. In addition, we present the concept and design of the Invar mechanical mounts for the WCU Zerodur mirrors, which are expected to undergo thermal and mechanical stresses. Finally, we present the optical design and analysis of the visible channel of the WCU that is aimed at alignment verification, as well as visualization of the METIS focal and pupil planes.
During the past years, the VLTI-instrument GRAVITY has made spectacular discoveries with phase-referenced interferometric imaging with milliarcsecond resolution and ten microarcsecond astrometry. Here, we report on the upgrade of the GRAVITY science spectrometer with two new grisms in October 2019, increasing the instrument throughput by a factor > 2. This improvement was made possible by using a high refractive index Germanium substrate, which reduces the grism and groove angles, and by successfully applying an anti-reflection coating to the ruled surface to overcome Fresnel losses. We present the design, manufacturing, and laboratory testing of the new grisms, as well as the results from the re-commissioning on sky.
The warm calibration unit (WCU) is one subsystem of the future METIS instrument on the European Extremely Large Telescope (E-ELT). Operating at daytime temperature, the WCU is mounted above the main cryostat of METIS and will be employed as calibration reference for science observations, as well as for verification and alignment purposes during the AIT phase. The WCU is designed and constructed at the University of Cologne, partner in the METIS consortium. The WCU, together with the full METIS instrument, went recently through a successful preliminary design review (PDR) phase at ESO and is entering now the Phase C of the project. In this paper, we present the current status of the WCU and summarize the mostly mechanical and optical engineering work. We adopted a hexapod unit to interface with the METIS cryostat and a CFRP-based optical bench to optimally cope with alignment flexure. We develop the case for fiber-fed laser sources feeding the integrating sphere for spectral calibration of the LM-Spectrograph of METIS. We detail the activity foreseen for Phase C including the optical tolerances analysis, the eigenfrequency and earthquake analysis and a preparation of the sub-system MAIT work, finishing the paper with a short overview of the WCU future plans.
We present the preliminary design of the calibration unit of the future E-ELT instrument METIS. This independent subunit is mounted externally to the main cryostat of METIS and will function both as calibration reference for science observations, as well as verification and alignment tool during the AIT phase. In this paper, we focus on describing its preliminary layout and foreseen functionalities, based on the performance requirements defined at system level and the constraints imposed by warm IR background. We discuss the advantage of employing an integrating sphere as common radiation emitter, leading to a novel and versatile design, where the source’s spatio-spectral properties can be varied with high fidelity and repeatability. By combining only few tuneable sources and mechanisms we show how a large instrument such as METIS can be calibrated and tested, without the need of a complex cold calibration unit.
METIS, a mid-infrared imager and spectrograph for the wavelength range 2.9–19μm (astronomical L-, M-, N- and Q-band), will be one of the first three science instruments at the European Extremely Large Telescope (E-ELT). It will provide diffraction limited imaging, coronagraphy, high resolution integral field spectroscopy and low and medium resolution slit spectroscopy. Within the international METIS consortium, the 1st Institute of Physics of the University of Cologne in Germany is responsible for the design, manufacturing, integration and qualification of the Warm Calibration Unit (WCU) of the instrument. The WCU will be a self-contained unit operating at ambient temperature outside of the voluminous METIS dewar, feeding a variety of optical calibration and alignment signals into the optical path of METIS. The functionalities of the WCU will be used for routine daily daytime calibrations after astronomical observing nights and verification of the internal alignment of METIS during assembly, integration and verification (AIV). In this contribution we present the preliminary optical design and principle of operation of the WCU in its current state of the preliminary design phase of METIS.
The work package of the University of Cologne within the GRAVITY consortium included the development and
manufacturing of two spectrometers for the beam combiner instrument. Both spectrometers are optimized for
different tasks. The science spectrometer provides 3 different spectral resolutions. In the highest resolution the
length of the spectral lines is close to the borders of the imaging area of the detector. Also the integration time
of these high resolution images is relative long. Therefor the optical pathes have to be controlled by the feedback
of a faster spectrometer. The fringe tracking spectrometer has only one low resolution to allow much shorter
integration times. This spectrometer provides a feedback for the control loops which stabilize the optical pathes
of the light from the telescope to the instrument. This is a new key feature of the whole GRAVITY instrument.
Based on the optical layout my work was the design of the mechanical structure, mountings, passive and
active adjustment mechanisms. This paper gives a short review about the active mechanisms and the compliant
lens mounts. They are used similarly in both spectrometers. Due to the observation and analysis of near-infrared
light the mechanisms have to run at cryogenic temperatures and in a high vacuum. Except the linear stages, the
motorized mechanisms will get used for several times per observation.
The LINC-NIRVANA Fringe and Flexure Tracking System has nearly completed assembly in the lab in Cologne, and will soon be ready for shipment and integration into the full LINC-NIRVANA system at MPIA Heidelberg. This paper provides an overview of the final assembly and testing phase in Cologne, concentrating on those aspects that directly affect instrument performance, including the detector performance and stability of the detector positioning system.
LINC-NIRVANA (LN) is an innovative Fizeau interferometric imager for the Large Binocular Telescope (LBT). LN uses Multi-Conjugate Adaptive Optics (MCAO) for high-sky-coverage single-eye imagery and interferometric beam combination. The last two years have seen both successes and challenges. On the one hand, final integration is proceeding well in the lab. We also achieved First Light at the LBT with the Pathfinder experiment. On the other hand, funding constraints have forced a significant re-planning of the overall instrument implementation. These laboratory, observatory, and financial “events” provide lessons for builders of complex interferometric instruments on large telescopes. This paper presents our progress and plans for bringing the instrument online at the telescope.
GRAVITY is a 2nd generation VLTI Instrument o which operates on 6 interferometric baselines by using all 4 Unit Telescopes. It will deliver narrow angle astrometry with 10μas accuracy at the infrared K-band. At the 1. Physikalische Institut of the University of Cologne, which is part of the international GRAVITY consortium, two spectrometers, one for the sciene object, and one for the fringe tracking object, have been designed, manufactured and tested. These spectrometers are two individual devices, each with own housing and interfaces. For a minimized thermal background, the spectrometers are actively cooled down to an operating temperature of 80K in the ambient temperature environment of the Beam Combiner Instrument (BCI) cryostat. The outer casings are mounted thermal isolated to the base plate by glass fiber reinforced plastic (GRP) stands, copper cooling structures conduct the cold inside the spectrometers where it is routed to components via Cu cooling stripes. The spectrometers are covered with shells made of multi insulation foil. There will be shown and compared 3 cooling installations: setups in the Cologne test dewar, in the BCI dewar and in a mock-up cad model. There are some striking differences between the setup in the 2 different dewars. In the Cologne Test dewar the spectrometers are connected to the coldplate (80K); a Cu cooling structure and the thermal isolating GRP stands are bolted to the coldplate. In the BCI dewer Cu cooling structure is connected to the bottom of the nitrogen tank (80K), the GRP stands are bolted to the base plate (240K). The period of time during the cooldown process will be analyzed.
Operating on 6 interferometric baselines, i.e. using all 4 unit telescopes (UTs) of the Very Large Telescope Interferometer (VLTI) simultaneously, the 2nd generation VLTI instrument GRAVITY will deliver narrow-angle astrometry with 10μas accuracy at the infrared K-band. At this angular resolution, GRAVITY will e.g. be able to detect the positional shift of the photo-center of a flare at the Galactic Center within its orbital timescale of about 20 minutes, using the observed motion of the flares as dynamical probes of the gravitational field around the supermassive black hole Sgr A*. Within the international GRAVITY consortium, the 1. Physikalische Institut of the University of Cologne is responsible for the development and construction of the two spectrometers of the camera system: one for the science object, and one for the fringe tracking object, both being operated in cryo-vacuum conditions. In this contribution we describe the basic functionality of the two units and present the final optical design of the two spectrometers as it got realised successfully until end of 2013 with minor changes to the Final Design Review (FDR) of October 2011. In addition we present some of the first light images of the two spectrometers, taken at the laboratory of the Cologne institute between Dec. 2012 and Oct. 2013 respectively. By the end of 2013 both spectrometers got transferred to the PI institute of GRAVITY, the Max-Planck-Institute for Extraterrestrial Physics, where at the time of writing they are undergoing system-level testing in combination with the other sub-systems of GRAVITY.
GRAVITY1 is a 2nd generation Very Large Telescope Interferometer (VLTI) operated in the astronomical K-band. In the Beam Combiner Instrument2 (BCI) four Fiber Couplers3 (FC) will feed the light coming from each telescope into two fibers, a reference channel for the fringe tracking spectrometer4 (FT) and a science channel for the science spectrometer4 (SC). The differential Optical Path Difference (dOPD) between the two channels will be corrected using a novel metrology concept.5 The metrology laser will keep control of the dOPD of the two channels. It is injected into the spectrometers and detected at the telescope level. Piezo-actuated fiber stretchers correct the dOPD accordingly. Fiber-fed Integrated Optics6 (IO) combine coherently the light of all six baselines and feed both spectrometers. Assisted by Infrared Wavefront Sensors7 (IWS) at each Unit Telescope (UT) and correcting the path difference between the channels with an accuracy of up to 5 nm, GRAVITY will push the limits of astrometrical accuracy to the order of 10 μas and provide phase-referenced interferometric imaging with a resolution of 4 mas. The University of Cologne developed, constructed and tested both spectrometers of the camera system. Both units are designed for the near infrared (1.95 - 2.45 μm) and are operated in a cryogenic environment. The Fringe Tracker is optimized for highest transmission with fixed spectral resolution (R = 22) realized by a double-prism.8 The Science spectrometer is more diverse and allows to choose from three different spectral resolutions8 (R = [22, 500, 4000]), where the lowest resolution is achieved with a prism and the higher resolutions are realized with grisms. A Wollaston prism in each spectrometer allows for polarimetric splitting of the light. The goal for the spectrometers is to concentrate at least 90% of the ux in 2 × 2 pixel (36 × 36 μm2) for the Science channel and in 1 pixel (24 × 24 μm) in the Fringe Tracking channel. In Section 1, we present the arrangement, direction of spectral dispersion and shift of polarization channels for both spectrometers, and the curvature of the spectra in the science spectrometer. In Section 2 we determine the best focus position of the detectors. The overall contrast of images at different positions of the detector stage is computed with the standard deviation of pixel values in the spectra containing region. In Section 3 we analyze high dynamic range images for each spectrometer and resolution obtained at the afore determined best focus positions. We deduce the ensquared energy from the FWHM of Gaussian fits perpendicular to the spectra.
We present an update on LINC-NIRVANA (LN), an innovative, high-resolution infrared imager for the Large Binocular
Telescope (LBT). LN uses Multi-Conjugate Adaptive Optics (MCAO) for high-sky-coverage diffraction-limited
imagery and interferometric beam combination. The last two years have seen both successes and challenges. On the one
hand, final integration is proceeding well in the lab. We also achieved First Light at the LBT with the Pathfinder
experiment. On the other hand, funding constraints have forced a significant re-planning of the overall instrument
implementation. This paper presents our progress and plans for bringing the instrument online at the telescope.
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.
Optical and opto-mechanical components in astronomical instruments are amongst the most expensive and
delicate single parts. Lenses made of special glasses or crystals are sometimes difficult to obtain (if at all),
especially with larger diameters and are figured and polished involving time-consuming and even risky procedures.
At infrared wavelengths (< 5μm), when the instrument is cooled to temperatures even below that of liquid
nitrogen, mechanical stress is induced between e.g. a glass lens and its metal mounting due to different heat
expansion coefficients of the materials involved. This can considerably degrade the performance of the whole
instrument. At infrared wavelengths the optical specifications considering surface roughness and form error
are less tight than in the optical due to the longer wavelengths involved. Hence metal mirrors with a surface
roughness and a form error of around 50 nm (RMS) may generally be favoured due to lower production costs then
lenses. Goal of the project described here is to manufacture plane, spherical or aspherical aluminum mirrors,
which are not hampered in the ways described above, in a cost effective procedure with optical specifications
(surface roughness and form error) of less than 100 nm (RMS) by means of direct diamond milling.
Operating on 6 interferometric baselines, i.e. using all 4 unit telescopes (UTs) of the Very Large Telescope
Interferometer (VLTI) simultaneously, the 2nd generation VLTI instrument GRAVITY will deliver narrow-angle
astrometry with 10μas accuracy at the infrared K-band. At this angular resolution, GRAVITY will be able to
detect the positional shift of the photo-center of a flare at the Galactic Center within its orbital timescale of
about 20 minutes, using the observed motion of the flares as dynamical probes of the gravitational field around
the supermassive black hole Sgr A*.
Within the international GRAVITY consortium, the 1. Physikalische Institut of the University of Cologne
is responsible for the development and construction of the two spectrometers of the camera system: one for
the science object, and one for the fringe tracking object, both being operated at cryo-vacuum. In this paper
we present the phase-C final optical design of the two spectrometers as it got derived from the scientific and
technical requirements and as it was presented and reviewed successfully at the Final Design Review (FDR) at
the European Southern Observatory (ESO) in October 2011.
LINC-NIRVANA is a near-Infrared homothetic, beam combining camera for the Large Binocular Telescope that offers Multi-Conjugate Adaptive Optics wavefront correction and fringe tracking to achieve a time-stable fringe pattern. Therefore, the trajectory of the reference source has to be followed as accurate as possible for a precise point spread function acquisition. The presented measurement campaign shows detector positioning errors exceeding the requirements significantly and indicates that these huge errors arise from the software, while the installed hardware matches the requirements.
We present the latest status of the control system of the LN (LINC-NIRVANA) FFTS (Fringe and Flexure Tracker
System) for the LBT. The software concept integrates the sensor data and control of the various subsystems
and provides the interaction with the whole LN instrument. Varying conditions and multiple configurations for
observations imply a flexible interconnection of the control loops for the hardware manipulators with respect
to the time-critical data analysis of the fringe detection. In this contribution details of the implementation of
the algorithms on a real-time Linux PC are given. By considering the results from simulations of the system
dynamics, lab experiments, atmospheric simulations, and telescope characterization the optimal parameter setup
for an observation can be chosen and basic techniques for adaption to changing conditions can be derived.
The Fringe and Flexure Tracking System (FFTS) is meant to monitor and correct atmospheric piston varia tion and instrumental vibrations and flexure during near-infrared interferometric image acquisition of LING NIRVANA. In close work with the adaptive optics system the FFTS enables homothetic imaging for the Large Binocular Telescope. One of the main problems we had to face is the connection between the cryogenic upper part of the instrument, e.g. detector head, and the lower ambient temperature part. In this ambient temperature part the moving stages are situated that move the detector head in the given field of view (FOV). We show how we solved this problem using the versatile material glass fiber reinforced plastics (GFRP's) and report in what way this material can be worked. We discuss in detail the exquisite characteristics of this material which we use to combine the cryogenic and ambient environments to a fully working system. The main characteristics that we focus on are the low temperature conduction and the tensile strength of the GFRP's. The low temperature conduction is needed to allow for a low heat-exchange between the cryogenic and ambient part whereas the tensile strength is needed to support heavy structures like the baffle motor and to allow for a minimum of flexure for the detector head. Additionally, we discuss the way we attached the GFRP to the remaining parts of the FFTS using a two component encapsulant.
GRAVITY belongs to the 2nd generation of the Very Large Telescope Interferometer (VLTI) and will operate inK-band on 6 baselines using all 4 Unit Telescopes of the VLT. With an unprecedented astrometrical accuracy of l0μas it will be, amongst others, capable of detecting the highly relativistic motion of the photocenter of a flare surrounding the supermassive black hole at the Galactic Centre, and thus probe General Relativity. The contribution of the University of Cologne within the international GRAVITY-Consortium is the design, manufacturing, qualification and assembly of the Fringe Tracking Spectrometer and the Science Spectrometer in the Beam Combiner Instrument (BCI). The BCI will be located in the interferometric lab of the VLTI. The spectrometers will be operated at 85K in a 200K environment in the BCI. We present the design and qualification of a linear displacement mechanism, which will be used at the focus stages of the detectors in both spectrometers and at the zoom stage in the Fringe Tracking Spectrometer. The mechanism consists of 4 double-hinged compliant joints which support the stage and provide a linear motion along the optical axis. The stage characterization at room and cryogenic conditions are presented.
The super-massive 4 million solar mass black hole (SMBH) SgrA* shows variable emission from the millimeter to the X-ray domain. A detailed analysis of the infrared light curves allows us to address the accretion phenomenon in a statistical way. The analysis shows that the near-infrared flux density excursions are dominated by a single state power law, with the low states of SgrA* are limited by confusion through the unresolved stellar background. We show that for 8-10m class telescopes blending effects along the line of sight will result in artificial compact star-like objects of 0.5-1 mJy that last for about 3-4 years. We discuss how the imaging capabilities of GRAVITY at the VLTI, LINC-NIRVANA at the LBT and METIS at the E-ELT will contribute to the investigation of the low variability states of SgrA*.
LINC-NIRVANA (LN) is a German /Italian interferometric beam combiner camera for the Large Binocular Telescope. Due to homothetic imaging, LN will make use of an exceptionally large field-of-view. As part of LN, the Fringe-and-Flexure-Tracker system (FFTS) will provide real-time, closed-loop measurement and correction of pistonic and flexure signals induced by the atmosphere and inside the telescope-instrument system. Such
compensation is essential for achieving coherent light combination over substantial time intervals (~10min.).
The FFTS is composed of a dedicated near-infrared detector, which can be positioned by three linear stages within the curved focal plane of LN. The system is divided into a cryogenic (detector) and ambient (linear stages) temperature environment, which are isolated from each other by a moving baffie. We give an overview of the current design and implementation stage of the FFTS opto-mechanical components. The optical components represent an update of the original design to assess slow image motion induced by the LN instrument separately.
We present an update on the LINC-NIRVANA (LN) instrument, an innovative Fizeau-mode beam combiner for the
Large Binocular Telescope (LBT). LN will deliver 10 mas spatial resolution in the near infrared over a 10 arcsec field of
view. In addition to optical-path-difference control, the instrument must correct a wide field of view on the sky using
multi-conjugated adaptive optics. This substantially increases sky coverage for fringe tracking reference stars.
Subsystem delivery and testing is almost complete, and final Assembly, Integration, and Verification are well advanced.
We report on closed-loop control of a number of subsystems, including fine-tuning and optimization of the delay line.
Measurement and remediation of instrument flexure are key to the success of LN. Several laboratory performance
experiments demonstrate that components are within specification. With several interacting subsystems, LN faces a
complexity challenge. A Pathfinder experiment at LBT will verify multiple aspects of LINC-NIRVANA and the
telescope starting in winter 2012-2013. Finally, we report on efforts to prepare for early science exploitation in "LINC"
mode, which uses single-conjugate adaptive optics.
Operating on 6 interferometric baselines, i.e. using all 4 UTs, the 2nd generation VLTI instrument GRAVITY will deliver narrow angle astrometry with 10μas accuracy at K-band.
We present the system design of the science and fringe tracking spectrometers of GRAVITY: The fringe tracking spectrometer is optimised for highest sensitivity, providing a fixed spectral resolution. The science spectrometer provides 3 different low - medium spectral resolutions. Both spectrometers provide detector focus stages and deployable Wollaston prisms. The two spectrometers also feed the beams of the metrology laser system of GRAVITY backwards into the integrated optics beam-combiner, propagating back to the M2 mirrors of the 4 telescopes.
A two stage blocking system is implemented in the GRAVITY science and the fringe tracking spectrometer optical
design. The blocking system consists of a dichroic beam splitter and two long wave band-pass filters with the top
level requirements of high transmission of the science light in the K-Band (1.95 - 2.45 μm) region and high blocking power optical density (OD) ≥ 8 for each filter at the metrology laser wavelength of 1.908 μm. The laser metrology blocking filters were identified as one critical optical component in the GRAVITY science and fringe tracker
spectrometer design. During the Phase-C study of GRAVITY all the filters were procured and individually tested in terms of spectral response at K-band, transmission, blocking (OD) and reflection at the metrology laser wavelength. We present the measurements results of the full metrology blocking system in its final configuration as to be implemented in the GRAVITY spectrometers.
Operating on 6 interferometric baselines, i.e. using all 4 UTs, the 2nd generation VLTI instrument GRAVITY will
deliver narrow angle astrometry with 10μas accuracy at the infrared K-band.
Within the international GRAVITY consortium, the Cologne institute is responsible for the development and
construction of the two spectrometers: one for the science object, and one for the fringe tracking object.
Optically two individual components, both spectrometers are two separate units with their own housing and interfaces
inside the vacuum vessel of GRAVITY. The general design of the spectrometers, however, is similar. The optical layout
is separated into beam collimator (with integrated optics and metrology laser injection) and camera system (with
detector, dispersive element, & Wollaston filter wheel). Mechanically, this transfers to two regions which are separated
by a solid baffle wall incorporating the blocking filter for the metrology Laser wavelength. The optical subunits are
mounted in individual rigid tubes which pay respect to the individual shape, size and thermal expansion of the lenses.
For a minimized thermal background, the spectrometers are actively cooled down to an operating temperature of 80K in
the ambient temperature environment of the GRAVITY vacuum dewar. The integrated optics beam combiner and the
metrology laser injection, which are operated at 200/240K, are mounted thermally isolated to the cold housing of the
spectrometers.
The optical design has shown that the alignment of the detector is crucial to the performance of the spectrometers.
Therefore, in addition to four wheel mechanisms, six cryogenic positioning mechanisms are included in the mechanical
design of the detector mount.
The dynamics of stars and gas undoubtedly shows the existence of a 4 million solar mass black hole at the
center of the Milky Way: Sagittarius A* (SgrA*). Violent flare emission allows us to probe the immediate
environment of the central mass. Near-infrared polarimetry now shows signatures of strong gravity that are
statistically significant against randomly polarized red noise. Using these signatures we can derive spin and
inclination information of SgrA*. A combined synchrotron self Compton (SSC) and adiabatic expansion model
with source components peaking in the sub-mm domain can fully account for the observed flare flux densities
and the time delays towards the (sub-)mm flares that have been reported in some cases. We discuss the expected
centroid paths of the NIR images and summarize how the geometrical structure of the emitting region (i.e.
spot shape, presence of a torus or spiral-arm pattern etc.) affects this centroid tracks. While most of the
mentioned geometries are able to fit the observed fluxes, future NIR interferometry with GRAVITY at the
VLT will break some of the degeneracies between different emission models. In this contribution we summarize
several GRAVITY science cases for SgrA*. Our simulations propose that focusing GRAVITY observations on
the polarimetry mode could reveal a clear centroid track of the spot(s). A non-detection of centroid shifts cannot
rule out the multi-component model or spiral arms scenarios. However, a clear wander between alternating
centroid positions during the flares will prove the idea of bright long-lived spots occasionally orbiting the central
black hole.
The Fringe and Flexure Tracker System (FFTS) of the LINC-NIRVANA instrument is designed to monitor and
correct the atmospheric piston variations and the instrumental vibrations and flexure at the LBT during the
NIR interferometric image acquisition. In this contribution, we give an overview of the current FFTS control
design, the various subsystems, and their interaction details. The control algorithms are implemented on a realtime
computer system with interfaces to the fringe and flexure detector read-out electronics, the OPD vibration
monitoring system (OVMS) based on accelerometric sensors at the telescope structure, the piezo-electric actuator
for piston compensation, and the AO systems for offloading purposes. The FFTS computer combines data from
different sensors with varying sampling rate, noise and delay. This done on the basis of the vibration data and the
expected power spectrum of atmospheric conditions. Flexure effects are then separated from OPD signals and
the optimal correcting variables are computed and distributed to the actuators. The goal is a 120 nm precision
of the correction at a bandwidth of about 50 Hz. An end-to-end simulation including models of atmospheric
effects, actuator dynamics, sensor effects, and on-site vibration measurements is used to optimize controllers and
filters and to pre-estimate the performance under different observation conditions.
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.
Operating on 6 interferometric baselines, i.e. using all 4 unit telescopes (UTs) of the Very Large Telescope
Interferometer (VLTI) simultaneously, the 2nd generation VLTI instrument GRAVITY will deliver narrow-angle
astrometry with 10μas accuracy at the infrared K-band. At this angular resolution, GRAVITY will be able to
detect the positional shift of the photo-center of a flare at the Galactic Center within its orbital timescale of
about 20 minutes, using the observed motion of the flares as dynamical probes of the gravitational field around
the supermassive black hole Sgr A*.
Within the international GRAVITY consortium, the 1. Physikalische Institut of the University of Cologne is
responsible for the development and construction of the two spectrometers of the camera system: one for the
science object, and one for the fringe tracking object. In this paper we present the phase-B optical design of the
two spectrometers as it got derived from the scientific and technical requirements and as it passed the preliminary
design review (PDR) at the European Southern Observatory (ESO) successfully in late 2009.
We present the latest status of the fringe detecting algorithms for the LINC-NIRVANA FFTS (Fringe and Flexure
Tracker System). The piston and PSF effects of the system from the top of the atmosphere through the telescopes and
multi-conjugate AO systems to the detector are discussed and the resulting requirements for the FFTS outlined.
LINC-NIRVANA is the near-infrared Fizeau interferometric imaging camera for the Large Binocular Telescope (LBT).
For an efficient interferometric operation of LINC-NIRVANA the Fringe and Flexure Tracking System (FFTS) is
mandatory: It is a real-time servo system that allows to compensate atmospheric and instrumental optical pathlength
differences (OPD). The thereby produced time-stable interference pattern at the position of the science detector enables
long integration times at interferometric angular resolutions.
As the development of the FFTS includes tests of control software and robustness of the fringe tracking concept in a
realistic physical system a testbed interferometer is set up as laboratory experiment.
This setup allows us to generate point-spread functions (PSF) similar to the interferometric PSF of the LBT via a
monochromatic (He-Ne laser) or a polychromatic light source (halogen lamp) and to introduce well defined, fast varying
phase offsets to simulate different atmospheric conditions and sources of instrumental OPD variations via dedicated
actuators.
Furthermore it comprises a piston mirror as actuator to counteract the measured OPD and a CCD camera in the focal
plane as sensor for fringe acquisition which both are substantial devices for a fringe tracking servo loop. The goal of the
setup is to test the performance and stability of different control loop algorithms and to design and optimize the control
approaches.
We present the design and the realization of the testbed interferometer and comment on the fringe-contrast behavior.
A two stage blocking system is implemented in the GRAVITY science and the fringe tracking spectrometer optical
design. The blocking system consists of a dichroic mirror and a long wave band-pass filter with the top level
requirements of high transmission of the science light in the K-Band (1.95 - 2.5 μm) region and high blocking power
optical density (OD) ≥ 8 for the metrology laser wavelength at 1.908 μm. The laser metrology blocking filters have been
identified as one critical optical component in the GRAVITY science and fringe tracker spectrometer design.
During the Phase-B study of GRAVITY we procured 3 blocking filter test samples for demonstration and qualification
tests. We present the measurements results of an effective blocking of the metrology laser wavelength with a long wave
band-pass filter at OD=12.
We present an update on the construction and integration of LINC-NIRVANA, a Fizeau-mode imaging interferometer
for the Large Binocular Telescope (LBT). The LBT is a unique platform for interferometry, since its two, co-mounted
8.4 meter primary mirrors present an orientation-independent entrance pupil. This allows Fizeau-mode beam
combination, providing 23-meter spatial resolution and 12-meter effective collecting area for panoramic imagery
LINC-NIRVANA will sit at one of the shared, bent focal stations, receiving light from both mirrors of the LBT. The
instrument uses visible wavelength radiation for wavefront control, and the near-infrared bands for science and fringe
tracking. LINC-NIRVANA employs a number of innovative technologies, including multi-conjugated adaptive optics,
state-of-the-art materials, low vibration mechanical coolers, active and passive control, and sophisticated software for
data analysis.
The instrument is in its final construction and integration phase. This paper reports on overall progress, including
insights gained on large instrument assembly, software integration, science planning, and vibration control. A number of
additional contributions to this conference focus on individual subsystems and integration-related issues.
LINC-NIRVANA is the NIR homothetic imaging camera for the Large Binocular Telescope (LBT). In close
cooperation with the Adaptive Optics systems of LINC-NIRVANA the Fringe and Flexure Tracking System
(FFTS) is a fundamental component to ensure a complete and time-stable wavefront correction at the position
of the science detector in order to allow for long integration times at interferometric angular resolutions. In this
contribution, we present the design and the realization of the ongoing FFTS laboratory tests, taking into account
the system requirements. We have to sample the large Field of View and to follow the reference source during
science observations to an accuracy of less than 2 microns. In particular, important tests such as cooling tests
of cryogenic components and tip - tilt test (the repeatability and the precision under the different inclinations)
are presented. The system parameters such as internal flexure and precision are discussed.
LINC-NIRVANA (LN) is a German/Italian interferometric beam combiner camera for the Large Binocular
Telescope. Due to homothetic imaging, LN will make use of an exceptionally large field-of-view. As part of LN,
the Fringe-and-Flexure-Tracker system (FFTS) will provide real-time, closed-loop measurement and correction
of pistonic and flexure signals induced by the atmosphere and inside the telescope-instrument system. Such
compensation is essential for achieving coherent light combination over substantial time intervals (~ 10min.).
The FFTS is composed of a dedicated near-infrared detector, which can be positioned by three linear stages
within the curved focal plane of LN. The system is divided into a cryogenic (detector) and ambient (linear
stages) temperature environment, which are isolated from each other by a moving baffle. We give an overview
of the current design and implementation stage of the FFTS opto-mechanical and electronic components. We
present recent important updates of the system, including the development of separated channels for the tracking
of piston and flexure. Furthermore, the inclusion of dispersive elements will allow for the correction of atmospheric
differential refraction, as well as the induction of artificial dispersion to better exploit the observational-conditions
parameter space (air mass, brightness).
GRAVITY is a 2nd generation VLTI Instrument which operates on 6 interferometric baselines by using all 4
UTs. It will offer narrow angle astrometry in the infrared K-band with an accuracy of 10 ìas.
The University of Cologne is part of the international GRAVITY consortium and responsible for the design
and manufacturing of the two spectrometers. One is optimized for observing the science object, providing three
different spectral resolutions and optional polarimetry, the other is optimized for a fast fringe tracking at a spectral
resolution of R=22 with optional polarimetry. In order to achieve the necessary image quality, the current
mechanical design foresees 5 motorized functions, 2 linear motions and 3 filter wheels. Additionally the latest
optical design proposal includes 20 degrees of freedom for manual adjustments distributed over the different
optical elements.
Both spectrometers require precise linear and rotational movements on micrometer or arcsecond scales. These
movements will be realized using custom linear stages based on compliant joints. These stages will be driven
by actuators based on a Phytron/Harmonic Drive combination. For dimensioning and in order to qualify the
reliability of these mechanisms, it is necessary to evaluate the mechanisms on the base of several prototypes. Due
to the cryogenic environment the wheel mechanisms will be driven by Phytron stepper motors, too. A ratchet
mechanism, which is currently in the beginning of his design phase, will deliver the required precision to the
filter wheels.
This contribution will give a first impression how the next mechanical prototypes will look like. Besides, advantages
of purchasing and integrating a distance sensor and a resolver are reported. Both are supposed to work
under cryogenic conditions and should achieve high resolutions for the measuring of movements inside the test
cryostat.
Laboratory and on-sky experience suggests that the integration of big astronomical instruments, specially of a
complex interferometric system, is a challenging process. LINC-NIRVANA is the Fizeau interferometric imager
for the Large Binocular Telescope (LBT). Simulating the final operating environment of every system component
has shown how critical is the presence of flexures, vibrations and thermal expansion. Assembling and aligning
the opto-mechanical sub-systems will require an absolute reference which is not affected by static displacements
or positioning errors.
A multi-purpose calibration unit has been designed to ensure the quality of the alignment of optics and
detectors and the reliability of the mechanical setup. This new compact and light-weighted unit is characterized
by sophisticated kinematics, simple mechanical design and composite materials. In addition, the reduced number
of motorized axis improves the stiffness and lowers the angular displacements due to moving parts. The modular
concept integrates several light sources to provide the proper calibration reference for the different sub-systems
of LINC-NIRVANA. For the standard alignment of the optics an absolute reference fiber will be used. For flatfielding
of the detectors the unit provides an integrating sphere, and a special rotating multi-fiber plate (infrared
and visible) is used to calibrate the advanced adaptive optics and the fringe-tracking systems. A module to
control non-common path aberrations (Flattening of Deformable Mirrors) is also provided.
The current results of our ongoing Galactic Center (GC) observations with optical long baseline interferometry (OLB-IF)
are presented. We achieved first IR-IF fringes in both available IR science regimes of the VLTI (MIDI: 10 μm) and
(AMBER: 2 μm), demonstrating the new capabilities provided by large aperture telescope arrays to the Galactic center
research. We show that the highest angular resolution only available through interferometric techniques is necessary
to observe the GC ISM production in the making and distinguish individual sources from its dusty surroundings. An
overview over the currently available IF-technology is given, biased towards the GC science case. The feasibility of
phase-referencing to the supergiant GCIRS 7, located only 5" away from SgrA*, to increase the sensitivity and spectral
resolution of the observations, is discussed, and supported by the first real data. The presentation will conclude with an
outlook to the near future about how the upcoming astrometric and off-axis phase-referencing capabilities of the Keck and
VLT Interferometers, nicknamed ASTRA and PRIMA, will greatly extend the currently existing capabilities to observe
astrophysical phenomena in the Galactic center at the borderline to General relativity in a yet uninvestigated regime.
GRAVITY is a 2nd generation VLTI instrument that operates in the K-band and uses up to 4 telescopes simultaneously.
GRAVITY will provide interferometric astrometry of two objects in a 2 arcsecond field of view at
an astrometric precision of 10 μas. Using all four UTs and six interferometric baselines, it will allow for phase-referenced
imaging at mas resolution in combination with spectroscopic and polarimetric observing capabilities.
The large field of view of the VLTI delay lines is worldwide unique on a 140 m baseline, and no other VLTI
instrument is taking advantage of that outstanding capability so far.
In this paper we present the optical and mechanical design of the two spectrometers of the instrument.
The presented design resulted from the successful Phase A study of the system and provides low-resolution
spectroscopy using grisms and Wollaston prisms for polarimetry.
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.
LINC-NIRVANA is an innovative imaging interferometer fed by dedicated multi-conjugated adaptive optics systems.
The instrument combines the light of the two, 8.4-meter primary mirrors of the Large Binocular Telescope (LBT) on a
single focal plane, providing panoramic imagery with 23-meter spatial resolution. LINC-NIRVANA is entering its final
integration phase, with the large adaptive-optics and imaging subsystems coming together in the clean room in
Heidelberg. Here, we report on progress, including insights gained on instrument assembly and vibration control.
LINC-NIRVANA is the NIR homothetic imaging camera for the Large Binocular Telescope (LBT). Its Fringe
and Flexure Tracking System (FFTS) is mandatory for an effcient interferometric operation of LINC-NIRVANA:
the task of this cophasing system is to assure a time-stable interference pattern in the focal plane of the camera.
A testbed interferometer, set up as laboratory experiment, is used to develop the FFTS control loop and
to test the robustness of the fringe tracking concept. The geometry of the resulting interferometric intensity
distribution in the focal plane of the implemented CCD corresponds to that of the LBT PSF. The setup allows to
produce monochromatic (He-Ne laser) and polychromatic (halogen lamp) PSFs and allows to actively introduce
well defined low-order phase perturbations, namely OPD and differential tip/tilt. Furthermore, all components
that are required in a fringe tracking servo loop are included: a sensor for fringe acquisition and an actuator
to counteract measured OPD. With this setup it is intended to determine the performance with which a fringe
tracking control loop is able to compensate defined OPD sequences, to test different control algorithms, and to
optimize the control parameters of an existing servo system.
In this contribution we present the design and the realization of the testbed interferometer. Key parameters
describing the white light testbed interferometer, such as fringe contrast and thermal sensitivity are discussed.
The effects of all controllable phase perturbations are demonstrated.
LINC-NIRVANA is the near-infrared homothetic imaging camera for the Large Binocular Telescope. Once
operational, it will provide an unprecedented combination of angular resolution, sensitivity and field of view. Its
Fringe and Flexure Tracking System (FFTS) is mandatory for an efficient interferometric operation of LINC-NIRVANA.
It is tailored to compensate low-order phase perturbations in real-time to allow for a time-stable
interference pattern in the focal plane of the science camera during the integration. Two independent control
loops are realized within FFTS: A cophasing loop continuously monitors and corrects for atmospheric and
instrumental differential piston between the two arms of the interferometer. A second loop controls common
and differential image motion resulting from changing orientations of the two optical axes of the interferometer.
Such changes are caused by flexure but also by atmospheric dispersion.
Both loops obtain their input signals from different quadrants of a NIR focal plane array. A piezo-driven
piston mirror in front of the beam combining optics serves as actuator in the cophasing loop. Differential piston
is determined by fitting a parameterized analytical model to the observed point spread function of a reference
target. Tip-tilt corrections in the flexure loop are applied via the secondary mirrors. Image motion is sensed for
each optical axis individually in out-of-focus images of the same reference target.
In this contribution we present the principles of operation, the latest changes in the opto-mechanical design,
the current status of the hardware development.
LINC-NIRVANA is the NIR homothetic imaging camera for the Large Binocular Telescope (LBT). Its Fringe
and Flexure Tracking System (FFTS) is mandatory for an efficient interferometric operation of LINC-NIRVANA:
the task of this cophasing system is to assure a time-stable interference pattern in the focal plane of the camera.
Differential piston effects will be detected and corrected in a real-time closed loop by analyzing the PSF of
a guide star at a frequency of 100Hz-200Hz. A dedicated piston mirror will then be moved in a corresponding
manner by a piezo actuator. The long-term flexure tip/tilt variations will be compensated by the AO deformable
mirrors.
A testbed interferometer has been designed to simulate the control process of the movement of a scaled
piston mirror under disturbances. Telescope vibration and atmospheric variations with arbitrary power spectra
are induced into the optical path by a dedicated piezo actuator. Limiting factors of the control bandwith are
the sampling frequency and delay of the detector and the resonance frequency of the piston mirror. In our setup
we can test the control performance under realistic conditions by considering the real piston mirrors dynamics
with an appropriate software filter and inducing a artificial delay of the PSF detector signal. Together with
the expected atmospheric OPD variations and a realistic vibration spectrum we are able to quantify the piston
control performance for typical observation conditions. A robust control approach is presented as result from
in-system control design as provided by the testbed interferometer with simulated dynamics.
As a near-infrared (NIR) wide field interferometric imager offering an angular resolution of about 10 milliarcseconds
LINC-NIRVANA at the Large Binocular Telescope will be an ideal instrument for imaging the center of the
Milky Way especially in conjunction with mm/sub-mm interferometers like CARMA, ATCA or, in the near
future, ALMA. Sagittarius A* (Sgr A*) is the electromagnetc manifestation of the ~4×106M super-massive
black hole (SMBH) at the Galactic Center. First results from a mult-wavelength campaign focused on Sgr A*,
based on the VLT
and on CARMA, ATCA, and the IRAM 30m-telescope, in May 2007 show that the NIR
data are consistent with partially depolarized non-thermal emission from confined hot spots in relativistic orbits
around SgrA*. A 3mm flare following a May 2007 NIR flare is consistent with SSC emission from adiabatically
expanding plasma in a wind or jet. With the LBT and ALMA we will be able to study the spectral evolution
of NIR/sub-mm/mm flare emission in order to constrain the emission mechanism, the jet/wind physics, and
possibly determine the angular momentum of the SMBH. LINC/NIRVANA will also serve to investigate the
stellar population and dynamics in the cluster surrounding Sgr A*. A particular emphasis will lie on examining
dust embedded and young stars and to unravel the star formation history in the cluster.
For the 0.3 parsec core radius central star cluster the investigation of will be investigated.
We present how it is achieved to mount a double prism in the filter wheel of MIRIM - the imager of JWST's Mid
Infrared Instrument. In order to cope with the extreme conditions of the prisms' surroundings, the low resolution
double prism assembly (LRSDPA) design makes high demands on manufacturing accuracy. The design and the
manufacturing of the mechanical parts are presented here, while 'Manufacturing and verification of ZnS and Ge
prisms for the JWST MIRI imager' are described in a second paper [1]. We also give insights on the astronomical
possibilities of a sensitive MIR spectrometer. Low resolution prism spectroscopy in the wavelength range from
5-10 microns will allow to spectroscopically determine redshifts of objects close to/at the re-ionization phase of
the universe.
LINC-NIRVANA is an innovative imaging interferometer fed by dedicated multi-conjugated adaptive optics systems.
The instrument combines the light of the two, 8.4-meter primary mirrors of the Large Binocular Telescope (LBT) on a
single focal plane, providing panoramic imagery with 23-meter spatial resolution. The instrument employs a number of
innovative technologies, including multi-conjugated adaptive optics, state-of-the-art materials, low vibration mechanical
coolers, active and passive control, and sophisticated software for data analysis. LINC-NIRVANA is entering its final
integration phase, with the large adaptive-optics and imaging subsystems coming together in the clean room in
Heidelberg. Here, we report on progress, including insights gained on integration of large instruments.
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 real-time. In the fringe tracking concept that we present, differential piston information is gathered in the image plane by analyzing the PSF of a reference star anywhere in the large field of view of the LBT. We have developed and tested a fast PSF analysis algorithm that allows to clearly identify differential piston even in the case of low S/N. We present performance estimates of the algorithm. Since the performance of the FFTS algorithm has a strong impact on the overall sky coverage of LINC-NIRVANA, we studied the required limiting magnitudes of the fringe tracking reference star for different scenarios. As the FFTS may not necessarily operate on the science target, but rather uses a suitable reference star at a certain angular distance to the science target, differences between piston values at the two positions add to the residual piston of the FFTS. We have dealt with the question of differential piston angular anisoplanatism and studied a possible improvement of the isopistonic patch size by the use of multi-conjugate adaptive optics (MCAO). In its final stage, LINC-NIRVANA will be equipped with such a system.
Current and future opportunities for interferometric observations of the Galactic Center in the near- and mid-infrared (NIR/MIR) wavelength domain are highlighted. Main emphasis is being put on the Large Binocular Telescope (LBT) and the Very Large Telescope Interferometer (VLTI). The Galactic Center measurements of stellar orbits and strongly variable NIR and X-ray emission from Sagittarius A* (SgrA*) at the center of the Milky Way have provided the strongest evidence so far that the dark mass concentration at this position is associated with a super massive black hole. Similar dark mass concentrations seen in many galactic nuclei are most likely super massive black holes as well. High angular resolution interferometric observations in the NIR/MIR will provide key information on the central massive black hole and the stellar cluster it is embedded in. These observations have already started: Recent results on the luminous dust enshrowded star IRS3 using MIDI at the VLTI are presented and future scientific possibilities in the GC using MIDI at the VLTI in the MIR and GRAVITY in the NIR are highlighted. As a NIR wide field interferometric imager offering an angular resolution of about 10 milliarcseconds LINC/NIRVANA at the Large Binocular Telescope will be an ideal instrument for imaging galactic nuclei including the center of the Milky Way.
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.
We present the adaptive optics assisted, near-infrared VLTI instrument - GRAVITY - for precision narrow-angle astrometry and interferometric phase referenced imaging of faint objects. Precision astrometry and phase-referenced interferometric imaging will realize the most advanced vision of optical/infrared interferometry with the VLT. Our most ambitious science goal is to study motions within a few times the event horizon size of the Galactic Center massive black hole and to test General Relativity in its strong field limit. We define the science reference cases for GRAVITY and derive the top level requirements for GRAVITY. The installation of the instrument at the VLTI is planned for 2012.
KEYWORDS: Computing systems, Image processing, Interferometry, Near infrared, Signal processing, Atmospheric corrections, Sensors, Control systems, Telescopes, Point spread functions
The correction of atmospheric differential piston and instrumental flexure effects is mandatory for optimum interferometric performance 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. On a timescale of milliseconds, image data of the order of 4K bytes has to be retrieved from the FFTS detector, analyzed, and the results have to be sent to the control system. The need for a reliable communication between several processes within a confined period of time calls for solutions with good real-time performance. We investigated two soft real-time options for the Linux platform. The design we present takes advantage of several features that follow the POSIX standard with improved real-time performance, which were implemented in the new Linux kernel (2.6.12). Several concepts, such as synchronization, shared memory, and preemptive scheduling are considered and the performance of the most time-critical parts of the FFTS software is tested.
LINC-NIRVANA is the interferometric near-infrared imaging camera for the Large Binocular Telescope (LBT). Being able to observe at wavelength bands from J to K (suppported by an adaptive optics system operating at visible light) LINC-NIRVANA will provide an unique and unprecedented combination of high angular resolution (~ 9 milliarcseconds at 1.25μm), wide field of view (~ 100 arcseconds2 at 1.25μm), and large collecting area (~ 100m2).
One of the major contributions of the 1. Physikalische Institut of the University of Cologne to this project is the development and provision of the Fringe and Flexure Tracking System (FFTS). In addition to the single-eye adaptive optics systems the FFTS is a crucial component to ensure a time-stable wavefront correction over the full aperture of the double-eye telescope, a mandatory pre-requisite for interferometric observations.
Using a independent HAWAII 1 detector array at a combined focus close to the science detector, the Fringe and Flexure Tracking System analyses the complex two-dimensional interferometric point spread function (PSF) of a suitably bright reference source at frame rates of up to several hundred Hertz. By fitting a parameterised theoretical model PSF to the preprocessed image-data the FFTS determines the amount of pistonic phase difference and angular misalignment between the wavefronts of the two optical paths of LINC-NIRVANA. For every exposure the corrective parameters are derived in real-time and transmitted to a dedicated piezo-electric fast linear mirror for simple path lengths adjustments, and/or to the adaptive optics systems of the single-eye telescopes for more complicated corrections.
In this paper we present the basic concept and currect status of the opto-mechanical design of the Fringe and Flexure Tracker, the operating principle of the fringe and flexure tracking loops, and the encouraging result of a laboratory test of the piston control loop.
The Fringe and Flexure Tracking System (FFTS) is designed to correct
the atmospheric piston variations and the instrumental flexure during the NIR interferometric image acquisition of the LINC-NIRVANA camera at the LBT. The interferometric image quality depends on the performance of these corrections.
Differential piston and flexure effects will be detected and corrected in a real-time closed loop by analyzing the PSF of a guide star at a frequency of up to several hundred Hz. A dedicated piston mirror will then be moved in a corresponding manner by a piezo actuator.
The FFTS is expected to provide a residual piston of better then 0.1 λ at the central wavelength of the science band. Thus, the required correction bandwidth is 10-20 Hz as differential piston simulations of different seeing conditions indicate. Therefore, a sampling frequency of 100-200 Hz is required to correct OPD variations. The upper limit for the loop frequency is the resonance frequency of the mirror and the response function respectively.
The piston mirror as the actuator and the FFTS detector as the sensor
feedback are embedded in a very complex system. Many control loop aspects like sampling frequencies, delays, controller algorithm and control bandwidth have to be identified. With accurate simulations of the system the limits of atmospheric and instrumental conditions for reliable closed loops can be determined against the respective control parameters. We present strategies for the closed-loop control of the piston correction which are suitable to achieve the 0.1 λ requirement and the optimal overall imaging performance with a sufficient "all-purpose" control stability.
MIRI, the Mid-InfraRed Instrument, is one of the 4 instruments currently under development for the NASA/ESA
James Webb Space Telescope. Together with the US, MIRI is built by a consortium of 28 European institutes
under the lead-management of ESA. The instrument consists of two main modules, a spectroscopic and an
imaging part. The imager will allow imaging, coronography and low resolution spectroscopy. The latter mode
will use a ZnS-Ge-double-prism assembly as dispersive element.
In this contribution, we present the design concept for the mounting of this double prism assembly which places
the prisms into the optical path of the imager via an interface to the imager's filterwheel. Despite the very
limited available space in the filterwheel and the high weight of the prisms (in comparison to the other filters
in the filterwheel), the kinematic mounting of the individual prisms guarantees exact placement with smallest
possible induced forces into the prisms. The here presented design of the development model of the double prism
assembly is based upon GEM calculation. Experimental thermal and vibrational tests will be performed by the
time of this conference.
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.
As a near-infrared (NIR) wide field interferometric imager offering an
angular resolution of about 10 milliarcseconds LINC/NIRVANA at the
Large Binocular Telescope will be an ideal instrument for
imaging of galactic nuclei including the center of the Milky Way.
Recent optical/IR imaging surveys can now quite successfully be used
to search for star-galaxy pairs that are suitable for interferometric
observation with LINC NIRVANA. These objects can then be used to efficiently investigate galaxy interaction, nuclear activity, and star formation in distant galaxies. In the NIR these investigations will be carried out at scales below 100~pc for z<0.05 and at scales
below 500~pc at z<2.
The Galactic Center measurements of stellar orbits and strongly
variable NIR and X-ray emission from Sagittarius A* at the center of the Milky Way have provided the strongest evidence so far that the dark mass concentrations seen in many galactic nuclei are most likely super massive black holes. Observations with LINC NIRVANA will allow to simultaneously investigate the stellar dynamics of the entire central cluster, the determination of the amount of extended mass within the cusp region, and to monitor the activity of the 3 million solar mass black hole at the position of Sagittarius A* at separations of only about 10 light hours or 15 Schwarzschild radii.
LINC-NIRVANA is the interferometric near-infrared imaging camera for the Large Binocular Telescope (LBT). Operating at JHK bands LINC-NIRVANA will provide an unique and unprecedented combination of high angular resolution (~9 milliarcseconds at 1.25 µm), wide field of view (~100 arcseconds2 at 1.25 µm), and large collecting area (~100 m2).
One of the major contributions of the I. Physikalische Institut of the University of Cologne to this project is the development of the Fringe and Flexure Tracking System (FFTS). In close cooperation with the Adaptive Optics systems of LINC-NIRVANA the FFTS is a fundamental component to ensure a complete and time-stable wavefront correction at the position of the science detector in order to allow for long integration times at interferometric angular resolutions.
Using a dedicated near-infrared detector array at a combined focus close to the science detector, the Fringe and Flexure Tracking System analyses the interferometric point spread function (PSF) of a suitably bright reference source at frame rates of several hundred Hertz up to 1 kHz. By fitting a parameterized theoretical model PSF to the preprocessed image-data the FFTS determines the amount of pistonic phase difference and the amount of an angular misalignment between the wavefronts of the two optical paths of LINC-NIRVANA. For every exposure the correcting parameters are derived in real-time and transmitted to the respective control electronics, or the Adaptive Optics systems of the single-eye telescopes, which will adjust their optical elements accordingly.
In this paper we present the opto-mechanical hardware design, the principle of operation of the software control algorithms, and the results of first numerical simulations and laboratory experiments of the performance of this Fringe and Flexure Tracking System.
The correction of atmospherical differential piston and instrumental flexure effects is mandatory for full interferometric performance of the LBT NIR interferometric imaging camera LINC-NIRVANA. This is the task of the Fringe and Flexure Tracking System (FFTS), which is part of the contribution of the I. Physikalische Institut of the University of Cologne to the project. Differential piston and flexure effects will be detected and corrected in a real-time closed loop by analyzing the PSF of a guide star at a frequency of up to several hundred Hz.
Numerous critical design parameters for both FFTS hardware and control loop have to be derived from simulations. Detailed knowledge of the special shape of the LBT interferometric PSF as a function of a variety of parameters is required to design the fringe tracking control loop. In this paper we will show the results of our software that allows us to generate polychromatic interferometric PSFs for a number of different scenarios.
Our fringe detection algorithm is based on an analytic model which is fitted to the acquired PSF. We present the results of the evaluation of the algorithm in terms of speed and residual piston, as well as the first successful implementation of the algorithm in a closed loop system.
Simulations of the time evolution of differential piston have been performed in order to investigate necessary correction frequencies and the variation of differential piston across the usable field of view. These simulations are based on the Layer Oriented Adaptive Optics performance simulator "LOST" of the Osservatorio Astriofisico di Arcetri.
Interferometry with the Very Large Telescope Interferometer (VLTI) will allow imaging of the Galactic Center and the nuclei of extragalactic sources at an angular resolution of a few milliarcseconds. VLTI will be a prime instrument to study the
immediate environment of the massive black hole at the center of the Milky Way. With the MID infrared Interferometric instrument (MIDI) for example the enigmatic compact dust embedded MIR-excess sources
within the central parsec should be resolvable. Further the observations of external galactic nuclei will allow unprecedented measurements of physical parameters (i.e. structure and luminosity) in these systems. With the exception of a few 'self-referencing' sources these faint-target observations will benefit from the available off-axis wavefront-correction system STRAP, working on suitable guide stars (GS).
To fully exploit the use of VLTI within this context, the following questions have to be addressed among others: How feasible is blind-pointing on (faint) science targets? Are VLTI observations still efficiently feasible if these faint science targets exceed the usual angular distance (≤1 arcmin) to a GS candidate, enabling a standard closed-loop tip-tilt correction? How is the fringe-tracking procedure affected in densely populated regions such as the Galactic Center? What preparatory steps have to be performed to successfully observe these non-standard targets with the VLTI?
In this contribution, we present aspects for the preparation of VLTI observations, which will be conducted in the near future. Considering these example observations of the Galactic Center region, several details of observing modes are discussed, which are necessary to observe such science targets. The final goal is the definition of observational strategies that are optimized for the discussed
classes of targets, which provide properties touching the limits of VLTI observability.
We describe LINC-NIRVANA, a 1-2.5 micron interferometric imaging instrument for the Large Binocular Telescope. Operating in Fizeau beam combination mode, LINC-NIRVANA will deliver the sensitivity of a 12-meter telescope and the angular resolution of a 23-meter telescope. Unlike traditional interferometers, LINC-NIRVANA will be a true imaging device, with a field of view of ten arcseconds on a single HAWAII-2 detector array. LINC-NIRVANA employs a number of state-of-the-art technologies, including multi-conjugated adaptive optics (MCAO), innovative cooling systems, and complex software for instrument control and data analysis. We report on overall project progress and highlight some unique aspects of LINC-NIRVANA that should be of wider interest to the near-infrared instrument-building community.
KEYWORDS: James Webb Space Telescope, Spectroscopy, Mirrors, Sensors, Electronics, Imaging systems, Optical components, Mid-IR, Optical filters, Picture Archiving and Communication System
MIRI is one of three focal plane instruments for the JWST covering the wavelengths region 5...28 μm. It is jointly developed by US and European institutes with the latter ones being responsible for the complete optical bench assembly, cryomechanisms, calibration source and the related electronics. MIRI is the combination of an imager with coronographic and low-resolution spectroscopic capabilities and a high-resolution integral-field spectrometer. These diverse options require several mechanisms to select a specific observing mode: (1) a filter wheel with bandpass filters, coronographic masks and a prism, (2) two grating/dichroic wheels with dispersing and order-sorting elements and (3) a flip mirror to direct the beam of an internal black body source into the spectrometer section. All mechanisms are required to operate under laboratory conditions (warm launch) as well as in the cryovacuum in space. The heat dissipation has to be small and the reliability and precision very high. Our low risk approach is the application of successfully qualified and flown components of the ISOPHOT (ISO) and PACS (HERSCHEL) instruments. We will report on the concept developed in phase B.
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.
The I. Physikalische Institut of the University of Cologne is participating in an international collaboration with the Max-Planck-Institut fur Astronomie in Heidelberg and the Osservatorio Astrofisico di Arcetri for the development of LINC/NIRVANA, the Near-Infrared/Visible Interferometric Camera for the Large Binocular Telescope (LBT). LINC/NIRVANA will be one of the two interferometric camera systems of the LBT and will operate at wavelengths from 0.6 μm to 2.4 μm, with the long wavelength regime between 1.0 μm and 2.5 μm being covered by LINC (LBT INterferometric Camera} and the shorter wavelengths part from 0.6 μm to 1.0 μm being processed by NIRVANA (Near-InfraRed/Visible Adaptive iNterferometer for Astronomy}.
The main contributions of the Cologne institute to this camera will be the 77K dewar and the Fringe and Flexure Tracker (FFT) for the near-infrared part on the system. Detecting and correcting the fast pistonic aberrations of the atmosphere and the slow flexure of the instrument in a closed-loop operation, the presence and proper function of the FFT is mandatory for a time-stable image quality at highest interferometic resolutions. In order to get the best possible image correction for LINC, the FFT will be located inside the camera dewar at an interferometric focus close the one of the near-infrared science detector. Using simple optical elements it will continuously monitor the time-variable phase difference and pupil locations of the incoming wavefronts from the two arms of the twin-telescope.
In this article we give a short overview of the camera concept of LINC and present the current status of the design and development of the FFT going on at our institute at the University of Cologne.
Fizeau interferometry at the Large Binocular Telescope (LBT) offers significant advantages over other facilities in terms of spatial resolution, field of view, and sensitivity. We provide an update of the LINC-NIRVANA project, which aims to bring a near-infrared and visible wavelength Fizeau beam combiner to the LBT by late 2005. As with any complex instrument, a number of detailed requirements drive the final design adopted.
Stellar proper motions, radial velocities and accelarations obtained with high angular resolution techniques over the past decade have convincingly proven the presence of a central compact dark mass of 3x106 M. This mass is most likely associated with the compact radio source Sagittarius A* and represents one of the best candidates for a super massive Black Hole.
This contribution summarizes some important observational facts and outlines the future possibilities for interferometric observations of the Galactic Center. In the near future interferometric observations of that region with the LBT, VLTI and the Keck Interferometer will be possible. Detailed measurements of the stellar orbits close to the center will allow us to precisely determine the compactness, extent and shape of any extended mass contribution e.g. due to a central stellar cusp. Emphasis will be put on the potential of the NIR LBT interferometric camera LINC. Given the combination of large telescope apertures, adaptive optics, and interferometry it is likely that stars with orbital time scales of the order of one year will be detected. Theses sources, however, will most likely not be on simple Keplerian orbits. The effects of measurable prograde relativistic and retrograde Newtonian periastron shifts will result in rosetta shaped orbits. An increased interferometric point source sensitivity will also allow for an effective search and monitoring of an IR counterpart of SgrA*.
Adaptive optics (AO) coupled to laser guide star systems is crucial to future ground based astronomical observations. It allows correction of image distortion caused by the Earth's turbulent atmosphere, over a hugely larger fraction of the sky than achieved by using only natural stars. Yet there are still very few such systems producing any sort of scientific results. ALFA, now offered on a shared risk basis as a user- instrument at Calar Alto Observatory in Spain, is continuing to improve its performance during closed loop operation on both natural and laser guide stars. The ability to close the loop on the LGS through thin cirrus cloud has the potential to increase the number of nights previously considered suitable for the laser by a factor of about two. In particular, science observations carried out on such a night are described. As part of the TMR network for Laser Guide Stars at Large Telescopes we are studying the distribution of atoms in the mesospheric sodium layer and its evolution over time. Additionally, a new experiment to provide an on- line monitor of the mesospheric sodium layer has been proposed and the results of a simulation are presented. This study will be of importance to large telescopes with laser stars at good astronomical sites where accurate statistics of the sodium layer are required, both for optimal scheduling of observations and for keeping the wavefront sensor focused on the LGS.
The ALFA-Laser of the MPE/MPIA adaptive optic system utilizes a 4W cw-laser for the creation of a sodium layer guide star. The artificial star serves as a reference source for the adaptive optics system installed at the Calar Alto observatory in souther Spain. Several distortion sources are affecting the laser beam and result in a laser guide star spot size too large on which to lock the adaptive optics loop properly. Therefore a number of analysis tools have been installed just before the laser beam expander and measurements of the beam quality have been performed. In this contribution we present parts of the experimental setup and results of these measurements. In addition we report on experimental studies of the guide star brightness when exciting the sodium layer with different polarization states of the laser radiation. A surprisingly large gain in response flux, when using circular polarization, has been measured. The complicated behavior of the polarization state with telescope position, due to phase changes at the beam relay mirrors, makes a control loop necessary to keep the projected beam optimal.
The sodium laser guide star adaptive optics system ALFA has been constructed at the Calar Alto 3.5m telescope. Following the first detection of the laser beacon on the wavefront sensor in 1997 the system is now being optimized for best performance. In this contribution we discuss the current status of the launch beam and the planned improvements and upgrades. We report on the performance level achieved when it is used with the adaptive optics system, and relate various aspects of our experience during operation of the system. We have begun to produce scientific result and mention two of these.
SHARP I and SHARP II are near infrared cameras for high-angular-resolution imaging. Both cameras are built around a 256 X 256 pixel NICMOS 3 HgCdTe array from Rockwell which is sensitive in the 1 - 2.5 micrometers range. With a 0.05"/pixel scale, they can produce diffraction limited K-band images at 4-m-class telescopes. For a 256 X 256 array, this pixel scale results in a field of view of 12.8" X 12.8" which is well suited for the observation of galactic and extragalactic near-infrared sources. Photometric and low resolution spectroscopic capabilities are added by photometric band filters (J, H, K), narrow band filters ((lambda) /(Delta) (lambda) approximately equals 100) for selected spectral lines, and a CVF ((lambda) /(Delta) (lambda) approximately equals 70). A cold shutter permits short exposure times down to about 10 ms. The data acquisition electronics permanently accepts the maximum frame rate of 8 Hz which is defined by the detector time constants (data rate 1 Mbyte/s). SHARP I has been especially designed for speckle observations at ESO's 3.5 m New Technology Telescope and is in operation since 1991. SHARP II is used at ESO's 3.6 m telescope together with the adaptive optics system COME-ON + since 1993. A new version of SHARP II is presently under test, which incorporates exchangeable camera optics for observations with scales of 0.035, 0.05, and 0.1"/pixel. The first scale extends diffraction limited observations down to the J-band, while the last one provides a larger field of view. To demonstrate the power of the cameras, images of the galactic center obtained with SHARP I, and images of the R136 region in 30 Doradus observed with SHARP II are presented.
We present interferograms and reconstructed images obtained with the MPE imaging beam combiner simulator COSI.The purpose of COSI is to simulate the imaging beam combiner at the coherent focus of the ESO VLTI in multi-speckle mode of under conditions of partial or full correction of the single telescope wave front by adaptive optics. The data discussed here were taken in multi-speckle and single speckle mode. COSI consists of a 1-m telescope and a near- IR continuum light source to simulate the radiation from astronomical objects. Two flat mirrors allow us to use one half of the telescope as a transmitter and the other half as a receiver. In the receiving focus we have installed the MPE speckle camera SHARP, which uses a HgCdTe 2562 NICMOS 3 array. A pupil mask over the aperture allows us to simulate various telescope configurations like the one with a beam compression factor of 100 as it will be used for the ESO VLT interferometer. COSI is used to explore NIR array detector properties and their suitability for interferometric measurements and to generate data to develop and test image reconstruction algorithms. First interferograms of single and multiple objects were taken early 1993. Employing various deconvolution and Fourier-inversion methods, a diffraction limited image of the pin-hole sources can be successfully recovered which experimentally demonstrates the feasibility of interferometric imaging with a large monolithic beam combiner. Thus, we have demonstrated that COSI is an excellent test bed to investigate methods of image recovery and to investigate how the methods are influenced by effects like atmospheric turbulence, expected optical imperfections and detector characteristics. Early this year (1994) we installed hot-air seeing simulators for individual subapertures. This allows us now to take interferograms in multi- speckle mode.
We present the layout and construction of main parts of the imaging beam combiner simulator experiment COSI, which has been set up at the Max Planck Institut fuer extraterrestrische Physik. The purpose of COSI is to simulate the imaging beam combiner at the coherent focus of the ESO VLTI. Main objectives of the experiment are to explore near-infrared array detector properties and to generate data for testing (developing) image reconstruction algorithms. COSI consists of a 1-m telescope and a near-infrared continuum light source to simulate the radiation from astronomical objects. Close to the focal plane, the beam is split into two foci. The beam is relayed between the two parts of the telescope by a roof mirror. Between the telescope and the retroreflector in the quasi-parallel beam, a pupil mask allows us to define a number of beams, thus simulating various telescope configurations with a beam compression factor of 100. The light from the pin-hole source is transmitted through the telescope system to the near-infrared camera placed in the receiving focus. The wavefront in the beams can be influenced by seeing simulators. Presently we use hot air devices, but for the final configuration we aim at deformable mirrors to have detailed control over the wavefront. Experimental results on image recovery achieved up to now are reported elsewhere in this conference.
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