GMTIFS: The Giant Magellan Telescope integral fields spectrograph and imager

Sharp, Robert; Bloxham, Gabe; Boz, Robert; Bundy, Dave; Davies, J.; Espeland, Brady; Fordham, Bartholomew; Hart, John; Herrald, Nicholas; Nielsen, Jon; Vaccarella, Annino; Vest, Colin; Young, P.; McGregor, Peter

doi:10.1117/12.2231561

Cited by 12 publications

(8 citation statements)

References 17 publications

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“…1.9, [49]: multi-object spectrograph for Astrophysics, inter galactic medium, and cosmology. G-CLEF [50]: GMT consortium large earth finder; GMTIFS [51]: GMT integral-field spectrograph; GMACS [52]: GMT multi-object astronomical and cosmological spectrograph; GMTNIRS [53]: GMT near-infrared spectrograph. NFIRAOS [54]: narrow-field infrared AO system; IRIS [55]:infrared imager and spectrograph; IRMS [56]:infrared multi-object spectrograph; TMT-AGE [57]: TMT analyzer for galaxies in the early universe; WFOS: wide-field optical spectrometer.…”

Section: Error Budget In Aomentioning

confidence: 99%

Projected Pupil Plane Pattern: an alternative LGS wavefront sensing technique

Yang

Bharmal

Myers

2018

Monthly Notices of the Royal Astronomical Society

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any wayThe full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Abstract For the next generation of extremely large telescopes, Focal Anisoplanatism (FA) renders single Laser Guide Star AO useless. Here we analyze a novel LGS alternative configuration with corresponding wavefront sensing and reconstruction method, termed Projected Pupil Plane Pattern, to solve the problem of Focal Anisoplanatism. With PPPP, turbulence is sensed during uplink by a laser beam projected as a collimated beam from the whole telescope primary mirror. Phase changes due to the turbulence introduce intensity variations that then increase in amplitude with propagation distance. By observing the distribution of intensity at two distant planes, the Transport-of-Intensity equation can be used to determine the phase aberration encountered during the uplink path. A simple imaging camera can then be used to measure the wavefront by imaging the backscattered light patterns. We have successfully demonstrated PPPP works both by simulation and laboratory experiment, where we find that PPPP can achieve equivalent performance to a SH WFS associated with a NGS. However it is shown that the main problem of PPPP is its low Signal-to-Noise Ratio if a 20 W laser is used. To reduce the requirement for high laser power, an alternative reconstructor based upon nonlinear Artificial Neural Networks has been developed, and provides a wavefront with measurement error around 160 nm RMS with a single 200 W laser on a 4-m diameter telescope. PPPP is therefore ready for a practical onsky test, which we are currently undertaking at Electro Optical Systems (EOS) Debris Laser Ranging (DLR) system, Australia. Supervisors: Nazim Bharmal and Richard Myers ii Acknowledgements I acknowledge financial support from China Scholarship Council (CSC) for covering the living expenses during my first three years of study, and from Durham University for my last year, as well as the funding of STFC for my PhD project.

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Section: Error Budget In Aomentioning

confidence: 99%

Projected Pupil Plane Pattern: an alternative LGS wavefront sensing technique

Yang

Bharmal

Myers

2018

Monthly Notices of the Royal Astronomical Society

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“…Beyond MOAO and the MOSAIC instrument, the same approach can be generalized to support other AO concepts relying on multiple wavefront sensing directions and turbulence tomography [6]. For instance, one can cite the MAORY MCAO instrument on the E-ELT [25] but also the GMTIFS and associated Laser Tomography AO (LTAO) module on the GMT [26] or the future MCAO module for the TMT [27]. Hence, this work is meant to have a critical impact on both the design phases of most ELTs AO instrumentation programs as well as their future operations on-sky.…”

Section: Understanding the Origin Of The Universementioning

confidence: 99%

Mixed-Precision Tomographic Reconstructor Computations on Hardware Accelerators

Doucet

Ltaief

Gratadour

et al. 2019

2019 IEEE/ACM 9th Workshop on Irregular Applications: Architectures and Algorithms (IA3)

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“…In this paper, we present an overview of those developments for the first generation instrument suite. Details of the individual instrument designs and their status can be found elsewhere in these procedings 3,4,5,6,7 . We also describe a modest optical imager that recently has been added to the first generation of instruments, as well as several early ideas for future instruments.…”

Section: Introductionmentioning

confidence: 99%

Instrumentation progress at the Giant Magellan Telescope project

Jacoby

Bernstein

Bouchez³

et al. 2016

SPIE Proceedings

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Instrument development for the 24m Giant Magellan Telescope (GMT) is described: current activities, progress, status, and schedule. One instrument team has completed its preliminary design and is currently beginning its final design (G-CLEF, an optical 350-950 nm, high-resolution and precision radial velocity echelle spectrograph). A second instrument team is in its conceptual design phase (GMACS, an optical 350-950 nm, medium resolution, 6-10 arcmin field, multiobject spectrograph). A third instrument team is midway through its preliminary design phase (GMTIFS, a near-IR YJHK diffraction-limited imager/integral-field-spectrograph), focused on risk reduction prototyping and design optimization. A fourth instrument team is currently fabricating the 5 silicon immersion gratings needed to begin its preliminary design phase (GMTNIRS, a simultaneous JHKLM high-resolution, AO-fed, echelle spectrograph). And, another instrument team is focusing on technical development and prototyping (MANIFEST, a facility robotic, multifiber-feed, with a 20 arcmin field of view). In addition, a medium-field (6 arcmin, 0.06 arcsec/pix) optical imager will support telescope and AO commissioning activities, and will excel at narrow-band imaging. In the spirit of advancing synergies with other groups, the challenges of running an ELT instrument program and opportunities for cross-ELT collaborations are discussed.

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GMTIFS: The Giant Magellan Telescope integral fields spectrograph and imager

Cited by 12 publications

References 17 publications

Projected Pupil Plane Pattern: an alternative LGS wavefront sensing technique

Projected Pupil Plane Pattern: an alternative LGS wavefront sensing technique

Mixed-Precision Tomographic Reconstructor Computations on Hardware Accelerators

Instrumentation progress at the Giant Magellan Telescope project

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