The Giant Magellan Telescope adaptive optics program

Antonin H. Bouchez, D. Scott Acton, Guido Agapito, Carmelo Arcidiacono, Francis Bennet, Valdemaro Biliotti, Marco Bonaglia, Runa Briguglio, Guido Brusa-Zappellini, Lorenzo Busoni, Luca Carbonaro, Johanan L. Codona, Rodolphe Conan, Thomas Connors, Oliver Durney, Brady Espeland, Simone Esposito, Luca Fini, Rusty Gardhouse, Thomas M. GauronMichael Hart, Phillip M. Hinz, Srikrishna Kanneganti, Edward J. Kibblewhite, Russell P. Knox, Brian A. McLeod, Thomas McMahon, Manny Montoya, Timothy J. Norton, Mark P. Ordway, Celine D'Orgeville, Simon Parcell, Piotr K. Piatrou, Enrico Pinna, Ian Price, Alfio Puglisi, Fernando Quiros-Pacheco, Armando Riccardi, John B. Roll, Gelys Trancho, Kristina Uhlendorf, Vidhya Vaitheeswaran, Marcos A. Van Dam, Dave Weaver, Marco Xompero

Research output: Chapter in Book/Report/Conference proceedingConference contribution

18 Scopus citations

Abstract

The Giant Magellan Telescope adaptive optics system will be an integral part of the telescope, providing laser guide star generation, wavefront sensing, and wavefront correction to most of the currently envisioned instruments. The system will provide three observing modes: Natural Guidestar AO (NGSAO), Laser Tomography AO (LTAO), and Ground Layer AO (GLAO). Every AO observing mode will use the telescope's segmented adaptive secondary mirror to deliver a corrected beam directly to the instruments. High-order wavefront sensing for the NGSAO and LTAO modes is provided by a set of wavefront sensors replicated for each instrument and fed by visible light reflected off the cryostat window. An infrared natural guidestar wavefront sensor with open-loop AO correction is also required to sense tip-tilt, focus, segment piston, and dynamic calibration errors in the LTAO mode. GLAO mode wavefront sensing is provided by laser guidestars over a ∼5 arcminute field of view, and natural guidestars over wider fields. A laser guidestar facility will project 120 W of 589 nm laser light in 6 beacons from the periphery of the primary mirror. An off-axis phasing camera and primary and secondary mirror metrology systems will ensure that the telescope optics remain phased. We describe the system requirements, overall architecture, and innovative solutions found to the challenges presented by high-order AO on a segmented extremely large telescope. Further details may be found in specific papers on each of the observing modes and major subsystems.

Original languageEnglish (US)
Title of host publicationAdaptive Optics Systems III
DOIs
StatePublished - Dec 1 2012
EventAdaptive Optics Systems III - Amsterdam, Netherlands
Duration: Jul 1 2012Jul 6 2012

Publication series

NameProceedings of SPIE - The International Society for Optical Engineering
Volume8447
ISSN (Print)0277-786X

Other

OtherAdaptive Optics Systems III
CountryNetherlands
CityAmsterdam
Period7/1/127/6/12

Keywords

  • Adaptive optics
  • Extremely large telescopes
  • Laser guidestar
  • Tomography
  • Wavefront sensing

ASJC Scopus subject areas

  • Electronic, Optical and Magnetic Materials
  • Condensed Matter Physics
  • Computer Science Applications
  • Applied Mathematics
  • Electrical and Electronic Engineering

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