The telescope structure of the Stratospheric Observatory for Infrared Astronomy (SOFIA) was subject to vibration excitation due to aircraft motions and airflow. To contribute to the efforts to meet pointing requirements and improve image stability, an active mass damping system for the primary mirror suspension has been designed and implemented during the early years of observatory operation phase. Various reasons had prevented further development for some time, but we were able to reactivate and operate the damping system for a set of selected missions before the premature decommissioning of the observatory. We present analyses from gathered engineering data and from astronomical observations about the effectiveness of the system during those missions and offer a projection on how future SOFIA campaigns would have benefited.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) employs an airborne telescope with a 2.7m primary mirror. The telescope structure is composed of carbon fibre with major parts of steel for the suspension and balancing components. It is exposed to harsh environmental conditions and subject to vibration excitation due to aircraft motions and turbulence from the airflow coming into the telescope cavity. To meet pointing requirements and improve image stability there are ongoing efforts on various components of the telescope system, one of which is the implementation of an Active Mass Damping (AMD) control system: Based on accelerometer signals, reaction mass actuators impose forces onto the support structure to dampen the vibration of optical components. The system has been designed, implemented and preliminary tested in the early years of SOFIA’s scientific operation, but concerns about the structural integrity of the primary mirror and new requirements regarding software qualification have prevented the activation and further development for several years. These concerns being addressed, we are now in the process of reactivating the AMD system on the support structure of the primary mirror. Recent ground tests and in-flight jitter measurements indicate that the damping system is very efficient at eliminating the excitation of targeted structural modes of the telescope structure at 40 to 80 Hz and the first bending modes of the primary mirror at 175 Hz, resulting in a significantly improved image quality. This paper presents the analysis of those measurements and discusses options for future development.
The telescope structure of the Stratospheric Observatory for Infrared Astronomy (SOFIA) is subject to vibration excitation due to aircraft motions and turbulence from the airflow coming into the telescope cavity. A proper understanding of the dynamical behavior of the telescope structure under operational loads is crucial for pointing control and measures against higher order optical aberrations. During design and construction a Finite Element model of the telescope assembly has been created in order to assess the structural integrity and the early performance. This legacy model used conservative assumptions and had a coarse approach on the approximation of some structural features. We present an updated Finite Element model of the SOFIA Primary Mirror Assembly, which represents support members as well as the primary mirror itself in greater detail, in order to support ongoing development for performance optimization. An iterative approach employing structural optimization was used to tune the model in order to fit modal parameters of the Primary Mirror Assembly which were measured in a test campaign prior to integration into the full telescope structure. The updated and tuned model is used to calculate deformations due to gravity, thermal loads and dynamic excitation. These deformations serve as input for ray-tracing analyses to investigate alterations in the light path in order to evaluate pointing errors and higher order optical aberrations.
The Stratospheric Observatory For Infrared Astronomy (SOFIA) reached its full operational capability in 2014 and takes off from the NASA Armstrong Flight Research Center to explore the universe about three times a week. Maximizing the program's scientific output naturally leaves very little flight time for implementation and test of improved soft- and hardware. Consequently, it is very important to have a comparable test environment and infrastructure to perform troubleshooting, verifications and improvements on ground without interfering with science missions. SOFIA's Secondary Mirror Mechanism is one of the most complex systems of the observatory. In 2012 a first simple laboratory mockup of the mechanism was built to perform basic controller tests in the lower frequency band of up to 50Hz. This was a first step to relocate required engineering tests from the active observatory into the laboratory. However, to test and include accurate filters and damping methods as well as to evaluate hardware modifications a more precise mockup is required that represents the system characteristics over a much larger frequency range. Therefore the mockup has been improved in several steps to a full test environment representing the system dynamics with high accuracy. This new ground equipment allows moving almost the entire secondary mirror test activities away from the observatory. As fast actuator in the optical path, the SMM also plays a major role in SOFIA's pointing stabilization concept. To increase the steering bandwidth, hardware changes are required that ultimately need to be evaluated using the telescope optics. One interesting concept presented in this contribution is the in- stallation of piezo stack actuators between the mirror and the chopping mechanism. First successful baseline tests are presented. An outlook is given about upcoming performance tests of the actively controlled piezo stage with local metrology and optical feedback. To minimize the impact on science time, the laboratory test setup will be expanded with an optical measurement system so that it can be used for the vast majority of testing.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) uses its compact and highly integrated Secondary Mirror Mechanism (SMM) to switch between target positions on the sky in a square wave pattern. This chopping motion excites eigenmodes of the mechanism structure, which limit controller and observatory performance. We present the setup and results of experimental modal tests performed on different building stages of a test-bench model as well as on the original flight hardware. Test results were correlated to simulations employing a finite element model in order to identify excited mode shapes and contributing flexible components of the Secondary Mirror Mechanism. It was possible to isolate the motion of the compensation ring and its elastic mounts as the vibration mode inducing the main disturbance at about 300 Hz, which is currently the main mode shape limiting the performance of the chopping controller.
The Stratospheric Observatory for Infrared Astronomy SOFIA consists of a B747-SP aircraft, which carries aloft a 2.7-meter reflecting telescope. The image stability goal for SOFIA is 0:2 arc-seconds rms. The performance of the telescope structure is affected by elastic vibrations induced by aeroacoustic and suspension disturbances. Active compensation of such disturbances requires a fast way of estimating the structural motion. Integrated navigation systems are examples of such estimation systems. However they employ a rigid body assumption. A possible extension of these systems to an elastic structure is shown by different authors for one dimensional beam structures taking into account the eigenmodes of the structural system. The rigid body motion as well as the flexible modes of the telescope assembly, however, are coupled among the three axes. Extending a special mathematical approach to three dimensional structures, the aspect of a modal observer based on integrated motion measurement is simulated for SOFIA. It is in general a fusion of different measurement methods by using their benefits and blinding out their disadvantages. There are no mass and stillness properties needed directly in this approach. However, the knowledge of modal properties of the structure is necessary for the implementation of this method. A finite-element model is chosen as a basis to extract the modal properties of the structure.
In this paper we present a novel highly sensitive detection system for diagnostic applications. The system is designed to
meet the needs of medical diagnostics for reliable measurements of pathogens and biomarkers in the low concentration
regime. It consists of a confocal detection unit, micro-structured sampling cells, and a "Virtual lab" analysis software.
The detection unit works with laser induced fluorescence and is designed to provide accurate and highly sensitive
measurement at the single molecule level. Various sampling cells are micro-structured in glass, silicon or polymers to
enable measurements under flow and nonflow conditions. Sampling volume is below one microliter. The "Virtual lab"
software analyzes the light intensity online according to the patent pending "Accurate Stochastic Fluorescence
Spectroscopy" (ASFS) developed by FluIT Biosystems GmbH. Tools for simulation and experiment optimization are
included as well. Experimental results for various applications with relevance for in vitro diagnostics will be presented.
The interdisciplinary project IMIKRID targets the "proof of concept" of a novel technological platform for the development of customised complete diagnostic systems of ultra high sensitivity for in-vitro diagnostics. For this purpose, an integrated microfluidic diagnostic platform is developed and its application concerning diagnostic problems in the area of oncology and cardiovascular diseases as well as in environmental applications will be demonstrated.
This paper presents a stochastic theory for the interpretation of photon counting histograms in fluorescence fluctuation spectroscopy (FFS). New concepts of an effective volume and a single molecule probability distribution are introduced to characterize a molecular species. Whereas the effective volume corresponds to the visibility of a molecular species in a given confocal setup, the single molecule probability distribution gives the signal measured for a single visible molecule. Specific properties of the effective volume and the single molecule probability distribution are discussed. Advantages arise for the high precision measurements of concentrations, mixtures, and binding constants especially for complex molecular environment, e.g. in flow systems and cell compartments.
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