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.
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.
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.
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.
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).
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 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.
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.
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.
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.
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.
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.
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