Construction of the Daniel K. Inouye Solar Telescope (DKIST) is well underway on the Haleakalā summit on the Hawaiian island of Maui. Featuring a 4-m aperture and an off-axis Gregorian configuration, the DKIST will be the world’s largest solar telescope. It is designed to make high-precision measurements of fundamental astrophysical processes and produce large amounts of spectropolarimetric and imaging data. These data will support research on solar magnetism and its influence on solar wind, flares, coronal mass ejections, and solar irradiance variability. Because of its large aperture, the DKIST will be able to sense the corona’s magnetic field—a goal that has previously eluded scientists—enabling observations that will provide answers about the heating of stellar coronae and the origins of space weather and exo-weather. The telescope will cover a broad wavelength range (0.35 to 28 microns) and operate as a coronagraph at infrared (IR) wavelengths. Achieving the diffraction limit of the 4-m aperture, even at visible wavelengths, is paramount to these science goals. The DKIST’s state-of-the-art adaptive optics systems will provide diffraction-limited imaging, resolving features that are approximately 20 km in size on the Sun.
At the start of operations, five instruments will be deployed: a visible broadband imager (VTF), a visible spectropolarimeter (ViSP), a visible tunable filter (VTF), a diffraction-limited near-IR spectropolarimeter (DLNIRSP), and a cryogenic near-IR spectropolarimeter (cryo-NIRSP). At the end of 2017, the project finished its fifth year of construction and eighth year overall. Major milestones included delivery of the commissioning blank, the completed primary mirror (M1), and its cell. Commissioning and testing of the coudé rotator is complete and the installation of the coudé cleanroom is underway; likewise, commissioning of the telescope mount assembly (TMA) has also begun. Various other systems and equipment are also being installed and tested. Finally, the observatory integration, testing, and commissioning (IT&C) activities have begun, including the first coating of the M1 commissioning blank and its integration within its cell assembly. Science mirror coating and initial on-sky activities are both anticipated in 2018.
KEYWORDS: Solar telescopes, Systems engineering, Telescopes, Visualization, Astronomy, Geographic information systems, Coating, Optical alignment, Wavefronts, Systems modeling
The Daniel K. Inouye Solar Telescope (DKIST) has been in its construction phase since 2010, anticipating the onset of the integration, test, and commissioning (IT&C) phase in early 2017, and the commencement of science verification in 2019. The works on Haleakala are progressing at a phenomenal rate and many of the various subsystems are either through or about to enter their Factory (or Laboratory) acceptance. The delays in obtaining site planning permissions, while a serious issue for Project Management, has allowed the sub-systems to develop well ahead of their required delivery to site. We have benefited from the knowledge that many sub-systems will be on site and ready for integration well before affecting the critical path. Opportunities have been presented for additional laboratory/factory testing which, while not free, significantly reduce the risks of potential delays and rework on site. From the perspective of IT&C this has provided an opportunity to develop the IT&C plans and schedules free from the pressures of imminent deployment.
In this paper we describe the ongoing planning of the Integration, Testing and Commissioning (IT&C) phase of the project in particular the detailed planning phase that we are currently developing.
KEYWORDS: Systems engineering, Solar telescopes, Telescopes, Mirrors, Software development, Manufacturing, Control systems, Observatories, Sun, Astronomy
The Daniel K. Inouye Solar Telescope (DKIST), formerly the Advanced Technology Solar Telescope (ATST), is now in its sixth year of construction. During the two years that have elapsed since our last systems engineering update we have been through factory acceptance of several major subsystems including the enclosure, telescope mount assembly, and the primary mirror. With these major milestones behind us, site assembly in progress, and with the integration, test, and commissioning phase about to begin, we will discuss what has been working well in terms of DKIST systems engineering processes along with some things we could have done better and would do differently if given another chance. The paper examines examples of successes including full-scale factory assembly of major mechanical components and some less optimum outcomes. We explore the reasons for success or failure, including the early delivery and level of detail in factory acceptance test procedures.
The Daniel K. Inouye Solar Telescope (DKIST), formerly the Advanced Technology Solar Telescope (ATST), has
been in its construction phase since 2010, anticipating the onset of the integration, test, and commissioning (IT&C)
phase late in 2016, and the commencement of science verification in early 2019. In this paper we describe the
planning of the Integration, Testing and Commissioning (IT&C) phase of the project.
KEYWORDS: Systems engineering, Control systems, Databases, Chromium, Radio frequency weapons, Telescopes, Adaptive optics, Solar telescopes, Document management, Error analysis
The Daniel K. Inouye Solar Telescope (DKIST), formerly the Advanced Technology Solar Telescope (ATST), has been in its construction phase since 2010, anticipating the onset of integration, test, and commissioning (IT and C) phase late in 2016, and the commencement of science verification in early 2019. In this paper we describe the role of Systems Engineering during these final phases of the project, and present some of the tools, techniques, and methods in use for these purposes. The paper concludes with a brief discussion of lessons learned so far including things we might do differently next time.
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: 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.
Turbulence, which may exist along an optical path inside a telescope or laboratory setup such as the Dunn Solar
Telescope observing room, can negatively impact the imaging performance at the final detector plane. In order to derive
requirements and error budget terms for the Advanced Technology Solar Telescope (ATST) we performed
interferometric measurements with the goal to determine the amount of aberrations introduced by the air mass through
which the beam propagates and characterize temporal and spatial frequencies of these aberrations. We used a He-Ne
laser interferometer to measure aberrations along a 50m and 33m, collimated 150mm diameter laser beam. The
experiments were performed with both vertical and horizontal beam propagation. We investigated the impact on the
amount of self-induced turbulence of the difference in temperature between the top and the bottom of the optical
laboratory, the impact of heat sources, such as electronics racks, and the effect of a laminar air flow applied to parts of
the beam path. The analysis of the interferograms yields values of the rms wave front aberrations excluding tip/tilt in the
range of 1.45nm/m - 2nm/m (@632nm) for the vertical beam propagation and between 0.8nm/m - 1.6nm/m for the
horizontal beam. The spatial spectrum of the turbulence tends to decay faster than Kolmogorov turbulence. This is true,
in particular, for the horizontal beam path. The temporal frequencies are on the order of a few Hz (<10Hz).
Michael Jacobson, Ruth Kneale, Fred Gillett, Keith Raybould, John Filhaber, Charles Carniglia, Ronald Laird, Dennis Kitchens, Ric Shimshock, Donald Booth
Acting as a prime contractor to the Gemini Project, the Optical Data Associates (ODA), with its major subcontractors, BOC Coating Technologies (BOCCT) and Deposition Sciences, Inc. (DSI), developed options for depositing protected silver coatings on the 8-M primary mirrors. The project began with a study that identified sputtering as the preferred deposition technique, defined a set of candidate adhesor and protective coatings for the silver layer, and simulated stack performance. The next phase involved pilot magnetron sputtering studies by BOCCT and DSI of designs involving silicon nitride and hafnia, respectively. ODA also developed mid-IR reflectance standards at (lambda) equals 10.6 micrometers to control the silver coating measurements in the critical 8 - 12 micrometers atmospheric window. The study results were successful, with both BOCCT and DSI producing Ag coatings with R equals 0.9920 +/- 0.0001 and protected Ag coatings with R equals 0.9910 +/- 0.0001. The Gemini Project coating plants are designed to sputter bare and protected Al and Ag coatings.
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