Presented are the results of in-situ computational fluid dynamics (CFD) modeling of the air knife assembly, associated grid-convergence study, and factory acceptance test results. The air knife assembly, a key thermal systems component of the Daniel K. Inouye Solar Telescope (DKIST), serves the dual purpose of ventilating the ceiling of the Coudé laboratory and as the interface between laboratory and ambient environments using an air curtain. During factory acceptance testing, flow visualization of the air curtain revealed that the flow was deflected upwards, suggesting that an unexpected pressure gradient had developed. Installed filter pressure sensors between the bottom of the air knife and the factory floor, indicated that a significant positive pressure had developed, 0.77 in w.c. above ambient. Outflow from the air knife, measured using a hot wire anemometer, exceeded the expected flow rate by a factor of approximately 1.5. It is hypothesized that large-scale eddies, generated by air knife outflow reversing at the floor, may have induced false downward velocity readings causing the increased pressure and flow rate. In-situ CFD modeling suggests that the air knife will meet or exceed all performance requirements. Outflow is predicted to be unidirectional, with an average velocity of 0.28 m/s and temperature within the 20 ± 0.5 C˚ margins. Maximum wavefront error introduced at the interface is predicted to be 84.3 nm root mean square (RMS).
Implementation of an air curtain at the thermal boundary between conditioned and ambient spaces allows for observation over wavelength ranges not practical when using optical glass as a window. The air knife model of the Daniel K. Inouye Solar Telescope (DKIST) project, a 4-meter solar observatory that will be built on Haleakalā, Hawai’i, deploys such an air curtain while also supplying ventilation through the ceiling of the coudé laboratory. The findings of computational fluid dynamics (CFD) analysis and subsequent changes to the air knife model are presented. Major design constraints include adherence to the Interface Control Document (ICD), separation of ambient and conditioned air, unidirectional outflow into the coudé laboratory, integration of a deployable glass window, and maintenance and accessibility requirements. Optimized design of the air knife successfully holds full 12 Pa backpressure under temperature gradients of up to 20°C while maintaining unidirectional outflow. This is a significant improvement upon the .25 Pa pressure differential that the initial configuration, tested by Linden and Phelps, indicated the curtain could hold. CFD post- processing, developed by Vogiatzis, is validated against interferometry results of initial air knife seeing evaluation, performed by Hubbard and Schoening. This is done by developing a CFD simulation of the initial experiment and using Vogiatzis’ method to calculate error introduced along the optical path. Seeing error, for both temperature differentials tested in the initial experiment, match well with seeing results obtained from the CFD analysis and thus validate the post-processing model. Application of this model to the realizable air knife assembly yields seeing errors that are well within the error budget under which the air knife interface falls, even with a temperature differential of 20°C between laboratory and ambient spaces. With ambient temperature set to 0°C and conditioned temperature set to 20°C, representing the worst-case temperature gradient, the spatial rms wavefront error in units of wavelength is 0.178 (88.69 nm at λ = 500 nm).
We provide an update on the construction status of the Daniel K. Inouye Solar Telescope. This 4-m diameter facility is designed to enable detection and spatial/temporal resolution of the predicted, fundamental astrophysical processes driving solar magnetism at their intrinsic scales throughout the solar atmosphere. These data will drive key research on solar magnetism and its influence on solar winds, flares, coronal mass ejections and solar irradiance variability. The facility is developed to support a broad wavelength range (0.35 to 28 microns) and will employ state-of-the-art adaptive optics systems to provide diffraction limited imaging, resolving features approximately 20 km on the Sun. At the start of operations, there will be five instruments initially deployed: Visible Broadband Imager (VBI; National Solar Observatory), Visible SpectroPolarimeter (ViSP; NCAR High Altitude Observatory), Visible Tunable Filter (VTF (a Fabry-Perot tunable spectropolarimeter); Kiepenheuer Institute for Solarphysics), Diffraction Limited NIR Spectropolarimeter (DL-NIRSP; University of Hawaii, Institute for Astronomy) and the Cryogenic NIR Spectropolarimeter (Cryo-NIRSP; University of Hawaii, Institute for Astronomy).
As of mid-2016, the project construction is in its 4th year of site construction and 7th year overall. Major milestones in the off-site development include the conclusion of the polishing of the M1 mirror by University of Arizona, College of Optical Sciences, the delivery of the Top End Optical Assembly (L3), the acceptance of the Deformable Mirror System (Xinetics); all optical systems have been contracted and are either accepted or in fabrication. The Enclosure and Telescope Mount Assembly passed through their factory acceptance in 2014 and 2015, respectively. The enclosure site construction is currently concluding while the Telescope Mount Assembly site erection is underway. The facility buildings (Utility and Support and Operations) have been completed with ongoing work on the thermal systems to support the challenging imaging requirements needed for the solar research.
Finally, we present the construction phase performance (schedule, budget) with projections for the start of early operations.
KEYWORDS: Solar telescopes, Observatories, Telescopes, Thermal analysis, Systems modeling, Solar radiation models, Cooling systems, Data modeling, Solar radiation, MATLAB
The climate of Haleakalā requires the observatories to actively adapt to changing conditions in order to produce the best possible images. Observatories need to be maintained at a temperature closely matching ambient or the images become blurred and unusable. The Daniel K. Inouye Solar Telescope is a unique telescope as it will be active during the day as opposed to the other night-time stellar observatories. This means that it will not only need to constantly match the ever-changing temperature during the day, but also during the night so as not to sub-cool and affect the view field of other telescopes while they are in use.
To accomplish this task, plate coil heat exchanger panels will be installed on the DKIST enclosure that are designed to keep the temperature at ambient temperature +0°C/-4°C. To verify the feasibility of this and to validate the design models, a test rig has been installed at the summit of Haleakalā. The project’s purpose is to confirm that the plate coil panels are capable of maintaining this temperature throughout all seasons and involved collecting data sets of various variables including pressures, temperatures, coolant flows, solar radiations and wind velocities during typical operating hours. Using MATLAB, a script was written to observe the plate coil’s thermal performance. The plate coil did not perform as expected, achieving a surface temperature that was generally 2ºC above ambient temperature. This isn’t to say that the plate coil does not work, but the small chiller used for the experiment was undersized resulting in coolant pumped through the plate coil that was not supplied at a low enough temperature. Calculated heat depositions were about 23% lower than that used as the basis of the design for the hillers to be used on the full system, a reasonable agreement given the fact that many simplifying assumptions were used in the models. These were not carried over into the testing.
The test rig performance showing a 23% margin provides a high degree of confidence for the performance of the full system when it is installed. If time allows, additional testing could be done that includes additional incident angles and times of day. This would allow a more complete analysis. If additional testing were to be performed, it’s recommended to use a larger chiller capable of reaching lower temperatures. The test rig design could also be optimized in order to bring the plate coil up to its maximum efficiency. In the future, the script could be rewritten in a different computer language, so that the data could be solved for quicker. Further analysis could also include different types of coolants.
KEYWORDS: Solar telescopes, Systems engineering, Observatories, Content addressable memory, Chromium, Control systems, Neodymium, Databases, Phase modulation, Process control
We provide a brief update on the construction status of the Daniel K. Inouye Solar Telescope, a $344M, 10-year construction project to design and build the world's largest solar physics observatory. We review the science drivers along with the challenges in meeting the evolving scientific needs over the course of the construction period without jeopardizing the systems engineering and management realization. We review the tools, processes and performance measures in use in guiding the development as well as the risks and challenges as the project transitions through various developmental phases. We elaborate on environmental and cultural compliance obligations in building in Hawai'i. We discuss the broad "lessons learned". Finally, we discuss the project in the context of the evolving management oversight within the US (in particular under the NSF).
KEYWORDS: Solar telescopes, Control systems, System integration, Fourier transforms, Cooling systems, Telescopes, Fermium, Frequency modulation, Fluorescence correlation spectroscopy, Fluctuations and noise
The Daniel K. Inouye Solar Telescope (DKIST) Observatory is under construction at Haleakalā, Maui, Hawai’i. When complete, the DKIST will be the largest solar telescope in the world. The Facility Management System (FMS) is a subsystem of the high-level Facility Control System (FCS) and directly controls the Facility Thermal System (FTS). The FMS receives operational mode information from the FCS while making process data available to the FCS and includes hardware and software to integrate and control all aspects of the FTS including the Carousel Cooling System, the Telescope Chamber Environmental Control Systems, and the Temperature Monitoring System. In addition it will integrate the Power Energy Management System and several service systems such as heating, ventilation, and air conditioning (HVAC), the Domestic Water Distribution System, and the Vacuum System. All of these subsystems must operate in coordination to provide the best possible observing conditions and overall building management. Further, the FMS must actively react to varying weather conditions and observational requirements. The physical impact of the facility must not interfere with neighboring installations while operating in a very environmentally and culturally sensitive area. The FMS system will be comprised of five Programmable Automation Controllers (PACs). We present a pre-build overview of the functional plan to integrate all of the FMS subsystems.
KEYWORDS: Solar radiation models, Cooling systems, Systems modeling, Thermal modeling, Solar telescopes, Control systems, Cladding, Atmospheric modeling, Safety, Data modeling
Analyses have shown that even a white-painted enclosure requires active exterior skin-cooling systems to mitigate dome seeing which is driven by thermal nonuniformities that change the refractive index of the air. For the Daniel K. Inouye Solar Telescope (DKIST) Enclosure, this active surface temperature control will take the form of a system of water cooled plate coils integrated into the enclosure cladding system. The main objective of this system is to maintain the surface temperature of the enclosure as close as possible to, but always below, local ambient temperature in order to mitigate this effect. The results of analyses using a multi-layer cladding temperature model were applied to predict the behavior of the plate coil cladding system and ultimately, with safety margins incorporated into the resulting design thermal loads, the detailed designs. Construction drawings and specifications have been produced. Based on these designs and prior to procurement of the system components, a test system was constructed in order to measure actual system behavior. The data collected during seasonal test runs at the DKIST construction site on Haleakalā are used to validate and/or refine the design models and construction documents as appropriate. The test fixture was also used to compare competing hardware, software, components, control strategies, and configurations. This paper outlines the design, construction, test protocols, and results obtained of the plate coil thermal test bench for the DKIST carousel cooling system.
We present the details on an experiment to investigate the behavior of an air curtain that is subjected to a transverse
pressure gradient. The setup simulates the conditions that will be present in the Advanced Technology Solar Telescope
(ATST), a 4-meter solar observatory that will be built on Haleakala, Hawaii. A test rig was built to replicate the region at
which the optical path crosses a temperature and pressure boundary between the telescope mount region, which is at the
ambient temperature and pressure, and a warmer, pressurized lab space directly below. Use of an air curtain in place of
an optically-transmitting window at the interface would allow science observations at a wider range of scientific
wavelengths. With the air curtain exhibiting transitional flow behavior across the boundary, and applied pressure
gradients of up to 6.5 Pa, we found that the air curtain was able to hold a pressure gradient of 0.25 Pa. As the applied
pressure was increased, transient turbulent regions formed at the interface, and predictable flow behavior only occurred
in the region closest to the air curtain blower. Computer modeling is used to validate the test data, identify laminar
regions of the air curtain where minimal image distortion would occur, and explore the relationship between the applied
pressure, effective pressure difference, and air curtain profile.
KEYWORDS: Telescopes, Control systems, Computing systems, Fluctuations and noise, Cooling systems, Wind energy, Energy efficiency, Solar telescopes, Space telescopes, Coating
The management and control of the local aero-thermal environment is critical for success of the Advanced Technology
Solar Telescope (ATST). In addition to minimizing disturbances to local seeing, the facility thermal systems must meet
stringent energy efficiency requirements to minimize impact on the surrounding environment and meet federal
requirements along with operational budgetary constraints. This paper describes the major facility thermal equipment
and systems to be implemented along with associated energy management features. The systems presented include the
central plant, the climate control systems for the computer room and coudé laboratory, the carousel cooling system
which actively controls the surface temperature of the rotating telescope enclosure, and the systems used for active and
passive ventilation of the telescope chamber.
KEYWORDS: Camera shutters, Solar radiation models, Telescopes, Thermal modeling, Control systems, Systems modeling, Solar telescopes, Observatories, Sun, Skin
The Advanced Technology Solar Telescope (ATST) is a 4-m class solar telescope to be built in Haleakala Observatory
in Maui (HI). It will be the largest solar telescope in the world, with unprecedented abilities to view details of the Sun.
Using adaptive optics technology, ATST will be able to provide the sharpest views ever taken of the solar surface. It is
expected that the 4-meter class telescope will have a significant impact on the study of stellar magnetic fields, plasma
physics and astronomy, allowing scientists to learn even more about the Sun and solar-terrestrial interactions.
Apart from the traditional weather protection functions, ATST Enclosure supports the telescope Aperture Stop which
must be accurately positioned to fully illuminate the primary mirror, while preventing insolation of any other system
components. This positioning is performed by the enclosure shutter (altitude) and azimuth mechanisms. In order to
evaluate the positioning capabilities of both mechanisms and verify the structure-mechanism-control interaction of the
involved systems a dynamic coupled model has been created.
On the other hand, the skin of the enclosure is thermally controlled to avoid the "enclosure seeing" by rejecting solar
radiation and keeping its surface temperature as close as possible below the ambient temperature. The thermal control is
achieved by a set of water cooled plate coils. The cooling fluid flow is controlled to achieve the desired reference
temperature. The performance of the system is being analyzed by means of mathematical model with couples the
thermal radiation analysis and the control system performances.
The ATST scientific instruments are located on benches installed on a large diameter rotating coud lab floor. The light path from the telescope to the instruments is greater than 38 meters and passes from external ambient conditions to the 'shirt-sleeve' environment of the coudé lab. In order to minimize any contribution to local seeing or wavefront distortion, two strategies are implemented. First, an air curtain is installed where the beam passes from ambient conditions to the lab space and second, the coudé lab environmental conditions are tightly controlled. This paper presents the design parameters of the environmental conditions, the basis of each design parameter, an overview of the equipment and components of the system planned to control those conditions, and the thermal and computational fluid dynamic analyses that have been performed in support of the system as designed.
The 4m Advance Technology Solar Telescope (ATST) will be the most powerful solar telescope and the world's leading
ground-based resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and
variability in the Sun's output. The project has successfully passed its final design review and the Environmental Impact
Study for construction of ATST on Haleakala, Maui, HI has been concluded in December of 2009. The project is now
entering its construction phase. As its highest priority science driver ATST shall provide high resolution and high
sensitivity observations of the dynamic solar magnetic fields throughout the solar atmosphere, including the corona at
infrared wavelengths. With its 4 m aperture, ATST will resolve features at 0."03 at visible wavelengths and obtain 0."1
resolution at the magnetically highly sensitive near infrared wavelengths. A high order adaptive optics system delivers a
corrected beam to the initial set of state-of-the-art, facility class instrumentation located in the coudé laboratory facility.
The initial set of first generation instruments consists of five facility class instruments, including imagers and spectropolarimeters.
The high polarimetric sensitivity and accuracy required for measurements of the illusive solar magnetic
fields place strong constraints on the polarization analysis and calibration. Development and construction of a fourmeter
solar telescope presents many technical challenges, including thermal control of the enclosure, telescope structure
and optics and wavefront control. A brief overview of the science goals and observational requirements of the ATST
will be given, followed by a summary of the design status of the telescope and its instrumentation, including design
status of major subsystems, such as the telescope mount assembly, enclosure, mirror assemblies, and wavefront
correction
KEYWORDS: Mirrors, Prototyping, Thermal modeling, Control systems design, Solar telescopes, Performance modeling, Convection, Observatories, Telescopes, Control systems
The Advanced Technology Solar Telescope (ATST) project plans to implement thermal control of the primary mirror
using jet impingement of temperature controlled air on the backside of the meniscus mirror. This technique will be used
to minimize temperature rise of the optical surface due to coating absorption, minimizing mirror seeing effects. The
performance of this system has been evaluated using numerical modeling techniques and weather data recorded at the
proposed observatory site. To aid in the design of the M1 thermal control system for the ATST, a prototype test bed was
designed, fabricated and tested. This paper reviews the progress and results of this development program.
KEYWORDS: Telescopes, Control systems, Wavefronts, Adaptive optics, Observatories, Mirrors, Buildings, Control systems design, Solar telescopes, Optical instrument design
The four-meter Advanced Technology Solar Telescope (ATST) will be the most powerful solar telescope and the
world's leading resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and
variability in the Sun's output. Development of a four-meter solar telescope presents many technical challenges (e.g.,
thermal control of the enclosure, telescope structure and optics). We give a status report of the ATST project (e.g.,
system design reviews, PDR, Haleakalä site environmental impact statement progress) and summarize the design of the
major subsystems, including the telescope mount assembly, enclosure, mirror assemblies, wavefront correction, and
instrumentation.
The derived heat loads from thermal models are used to size the equipment that controls exterior enclosure seeing for the
Advanced Technology Solar Telescope. These loads are highly dependent on the radiative properties assumed for the
surface coatings of the enclosure. The properties of traditional white coatings and paints are known to degrade with time
as they are exposed to the elements, but not by how much or how quickly. The solar reflectance and thermal emissivity
of coatings considered for use on the enclosure, in a weathered condition, are not readily available from coatings
manufacturers or in the scientific literature. The results from a one-year test of nine different coatings that were
weathered at the summit of Haleakala on the island of Maui, Hawaii are reported and discussed.
The exterior of the Advanced Technology Solar Telescope enclosure requires cooling to eliminate so-called external
dome seeing caused by solar loading during the observing day. This is achieved by way of coolant circulation through
external plate coil panels, thereby maintaining the exterior surfaces of the enclosure at or just below ambient air
temperature. As the distance from the optical path increases (e.g., on the surface of the lower enclosure), the stringency
of the temperature requirement is diminished, thereby allowing a greater difference between the surface temperature and
the ambient air temperature. This paper presents a comparison of the modeled performance of an active thermal control
strategy on the lower enclosure to a passive strategy that employs concrete panels. A life-cycle cost analysis of each
option is also presented.
KEYWORDS: Thermal modeling, Telescopes, Systems modeling, Convection, Solar radiation models, Solar telescopes, Cooling systems, Control systems, Camera shutters, Observatories
Telescope enclosure design is based on an increasingly standard set of criteria. Enclosures must provide failsafe protection in a harsh environment for an irreplaceable piece of equipment; must allow effective air flushing to minimize local seeing while still attenuating wind-induced vibration of the telescope; must reliably operate so that the dome is never the reason for observatory down time; must provide access to utilities, lifting devices and support facilities; and they must be affordable within the overall project budget. The enclosure for the Advanced Technology Solar Telescope (ATST) has to satisfy all these challenging requirements plus one more. To eliminate so-called external dome seeing, the exterior surfaces of the enclosure must be maintained at or just below ambient air temperature while being subjected to the full solar loading of an observing day. Further complicating the design of the ATST enclosure and support facilities are the environmental sensitivities and high construction costs at the selected site - the summit of Haleakala on the island of Maui, Hawaii. Previous development work has determined an appropriate enclosure shape to minimize solar exposure while allowing effective interior flushing, and has demonstrated the feasibility of controlling the exterior skin temperature with an active cooling system. This paper presents the evolution of the design since site selection and how the enclosure and associated thermal systems have been tailored to the particular climatic and terrain conditions of the site. Also discussed are load-reduction strategies that have been identified through thermal modeling, CFD modeling, and other analyses to refine and economize the thermal control systems.
KEYWORDS: Telescopes, Control systems, Mirrors, Wavefronts, Adaptive optics, Observatories, Control systems design, Buildings, Interfaces, Solar telescopes
The four-meter Advanced Technology Solar Telescope (ATST) will be the most powerful solar telescope and the world's leading resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and variability in the Sun's output. Development of a four-meter solar telescope presents many technical challenges (e.g., thermal control of the enclosure, telescope structure and optics). We give a status report of the ATST project (e.g., system design reviews, instrument PDR, Haleakala site environmental impact statement progress) and summarize the design of the major subsystems, including the telescope mount assembly, enclosure, mirror assemblies, wavefront correction, and instrumentation.
The four-meter Advanced Technology Solar Telescope (ATST) will be the most powerful solar telescope and the world's leading resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and variability in the Sun's output. Development of a four-meter solar telescope presents many technical challenges, which include: thermal control of optics and telescope structure; contamination control of the primary mirror to achieve low scattered light levels for coronal observations; control of instrumental polarization to allow accurate and precise polarimetric observations of solar magnetic fields; and high-order solar adaptive optics that uses solar granulation as the wavefront sensing target in order to achieve diffraction limited imaging and spectroscopy. We give a status report of the ATST project focusing on the substantial progress that has been made with the design of the ATST. We summarize the design of the major subsystems, including the enclosure, the primary and secondary mirror assemblies, the coude and Nasmyth focal stations, adaptive optics and instrumentation. The site selection has been successfully concluded and we discuss areas where the site selection impacts the design.
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