Mr. Barry Poe Profile

Barry Poe

at National Solar Observatory

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Publications (2)

Proceedings Article | 11 September 2024 Presentation + Paper

The US National Science Foundation Daniel K. Inouye Solar Telescope operations commissioning: results and lessons learned

Thomas Rimmele, Alexandra Tritschler, Andres Parraguez, Friedrich Wöger, Bret Goodrich, Luke Johnson, Heather Marshall, Paul Jeffers, Alisdair Davey, Robert Tawa, Gary Candido, David Boboltz, Tetsu Anan, Christian Beck, Gianna Cauzzi, Serena Criscuoli, André Fehlmann, Catherine Fischer, David Harrington, Sarah Jaeggli, Maxim Kramar, David Kuridze, Thomas Schad, Dirk Schmidt, Joao Manuel da Silva Santos, Lucas Tarr, Han Uitenbroek, James Arnow, Joel Davidow, Dale Deibert, Alysa Derks, Arthur Eigenbrot, Tony Hays, Erik Johansson, Daniel Spiess, Frazer Watson, Scott Wiant, Hillary Hope Head, David Morris, Manuel Díaz Alfaro, Nuria Wright-Garba, Anthony Santini, Andrew Beard, David Berst, Bryan Cummings, Andrew Ferayorni, Stephen Guzzo, John Hubbard, Jon Munoz, Isabell Scholl, Eric Cross, Colleen Donnelly, Steve O'Brien, Rodell Agdinaoay, Wade Bortz, Christopher Foster, Gary Foster, Chriselle Ann Galapon, Brian Gregory, Stephanie Guzman, Marco Guzman, James Hoag, Mary Liang, Karl Newman, Brialyn Onodera, Sebastien Poupar, Myles Puentes, Lukas Rimmele, Erik Starman, Stacey Sueoka, Richard Summers, Aimee Szabo, Louis Szabo, Timothy Williams, Charles White, Chad Bader, James Barry, Eric Bio, Terran Carter, Linda Evans, Bruce Keahi, Kealli Koki, Michael Lay, Aidan Lay, Justin Lay, Barry Poe, Norman Tong, Roberto Casini, Alfred deWijn, Jeffrey Kuhn, Haosheng Lin, Thomas Kentischer, Clemens Halbgewachs

Proceedings Volume 13094, 130940Y (2024) https://doi.org/10.1117/12.3022760

KEYWORDS: Equipment, Magnetism, Calibration, Adaptive optics, Tunable filters, Polarization, Solar telescopes, Solar processes, Optical filters, Sun

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Proceedings Article | 29 August 2022 Presentation + Paper

A follow-up survey and mitigation of the DKIST telescope mount vibrations

Sebastien Poupar, Brialyn Onodera, Paul Jeffers, Barry Poe

Proceedings Volume 12182, 121820S (2022) https://doi.org/10.1117/12.2630477

KEYWORDS: Telescopes, Mirrors, Solar telescopes, MATLAB, Vibrometry

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The NSF's Daniel K. Inouye Solar Telescope (DKIST) is the largest solar telescope in the world, with a 4-m off-axis primary mirror and 16-m rotating coudé laboratory within the telescope pier. Due to its off-axis design, the mount size is equivalent to an on-axis 8-m class telescope. Like other large, complex telescopes, DKIST is affected by vibrations related to its size and several important rotating entities (e.g. enclosure, coudé, telescope mount). However, the DKIST must also disperse a solar heat load of 13kW, using a complex thermal design supplemented by several additional vibration sources. The diffraction limit of the telescope makes the optical error budget very tight, with the allotted budget for vibrations jitter set as low as 70 milli-arcsec. This translates to a few hundred nanometers RMS on certain mirrors, with the impact of jitter on on-sky image motion varying relative to the mirror position in the optical path. The DKIST recently celebrated the end of its construction phase in November 2021, enabling the start of operations and allowing science programs to be started. Vibrations data recording and management has become part of the telescope verification during observing, enabling early detection of new frequency peaks and amplitude increases in known frequencies. Previous vibrations surveys at DKIST were conducted by William McBride who has proposed and presented an allocations budget per location in 2018, implemented and measured various paths analyses, and linked those results to the AO system. As the transition to operations progressed and operations continues, several vibration sources have been activated. Comparisons of current vibration levels to the previous budget is ongoing in order to identify where solutions to improve performance and facilitate AO correction are required. We were notified of two strong frequencies (40 Hz and 80 Hz) contributing significantly to image motion, identified within the High Order Adaptive Optics (HOAO) performance report. Presented herein is the process used to identify the source of that vibration by building a knowledge base of the telescope’s vibration signature, and using data identification of the problematic peaks to find the vibration hardware’s source. An improved design was then engineered, tested and implemented. Finally, by comparing results to prior HOAO measurements, the improvement in performance can be quantified.

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