W. M. Keck Observatory's next-generation adaptive optics facility

Wizinowich, Peter; Adkins, Sean M.; Dekany, Richard; Gavel, Donald T.; Max, C. E.; Bartos, Randy; Bell, J.; Bouchez, Antonin H.; Chin, Jason C. Y.; Conrad, Albert; Delacroix, Alex; Johansson, Erik M. J.; Kupke, Renate; Lockwood, Chris; Lyke, James E.; Marchis, Franck; McGrath, Elizabeth J.; Medeiros, D.; Morris, Mark; Morrison, D. R. O.; Neyman, C.; Panteleev, Sergey; Pollard, M.; Reinig, Marc; Stalcup, Thomas; Thomas, Sandrine; Troy, Mitchell; Tsubota, K.; Velur, V.; Wallace, J. Kent; Wetherell, Edward

doi:10.1117/12.857628

Cited by 16 publications

(9 citation statements)

References 20 publications

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“…An alternative approach, being pursued by the W. M. Keck Observatory Next-Generation Adaptive Optics (NGAO) team [16], [17], [18], [19] is to combine MOAO sharpening with pupil-conjugated deformable mirror correction based on laser tomography AO (LTAO). In this hybrid approach, the first LTAO stage applies a relatively low-order correction to the entire field of view, using a moderate format DM in a common pupil plan.…”

Section: Moao Sharpening With Ltaomentioning

confidence: 99%

Sharpening of natural guide stars for low-order wavefront sensing using patrolling laser guide stars

2008

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A laser guide star (LGS) adaptive optics (AO) system generally requires additional tip/tilt information derived using a natural guide star (NGS), while multi-LGS systems will benefit from measurement of additional low-order wavefront modes using one or more NGS's. If we use AO sharpened NGS's, we can improve both the measurement accuracy and accessible sky fraction while also minimizing the observational overhead of faint NGS acquisition. Multi-object adaptive optics (MOAO) sharpening of NGS is possible where a good estimate of the NGS wavefront can be made, for example where tomographic wavefront information is available. We describe a new approach for high Strehl ratio sharpening, based on additional patrolling laser beacons, to eliminate generalized anisoplanatism and minimize tomography error in the NGS direction.

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Section: Moao Sharpening With Ltaomentioning

confidence: 99%

Sharpening of natural guide stars for low-order wavefront sensing using patrolling laser guide stars

2008

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“…3 3. The current and planned adaptive optics systems (hereafter LGSAO & NGAO; [37], [38], respectively) at the W.M.Keck Observatory are chosen to represent current and upcoming AO performance on 8-10m class telescopes. We consider the current instrument NIRC2, although further gains might be possible with an instrument upgrade in conjuction with the AO system upgrade.…”

Section: Summary Of Simulated Instrumental Setupsmentioning

confidence: 99%

Precision cosmology with time delay lenses: high resolution imaging requirements

Meng

Treu

Agnello

et al. 2015

J. Cosmol. Astropart. Phys.

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Abstract. Lens time delays are a powerful probe of cosmology, provided that the gravitational potential of the main deflector can be modeled with sufficient precision. Recent work has shown that this can be achieved by detailed modeling of the host galaxies of lensed quasars, which appear as "Einstein Rings" in high resolution images. The distortion of these arcs and counter-arcs, as measured over a large number of pixels, provides tight constraints on the difference between the gravitational potential between the quasar image positions, and thus on cosmology in combination with the measured time delay. We carry out a systematic exploration of the high resolution imaging required to exploit the thousands of lensed quasars that will be discovered by current and upcoming surveys with the next decade. Specifically, we simulate realistic lens systems as imaged by the Hubble Space Telescope (HST), James Webb Space Telescope (JWST), and ground based adaptive optics images taken with Keck or the Thirty Meter Telescope (TMT). We compare the performance of these pointed observations with that of images taken by the Euclid (VIS), Wide-Field Infrared Survey Telescope (WFIRST) and Large Synoptic Survey Telescope (LSST) surveys. We use as our metric the precision with which the slope γ of the total mass density profile ρ tot ∝ r −γ for the main deflector can be measured. Ideally, we require that the statistical error on γ be less than 0.02, such that it is subdominant to other sources of random and systematic uncertainties. We find that survey data will likely have sufficient depth and resolution to meet the target only for the brighter gravitational lens systems, comparable to those discovered by the SDSS survey. For fainter systems, that will be discovered by current and future surveys, targeted follow-up will be required. However, the exposure time required with upcoming facilitites such as JWST, the Keck Next Generation Adaptive Optics System, and TMT, will only be of order a few minutes per system, thus making the follow-up of hundreds of systems a practical and efficient cosmological probe.arXiv:1506.07640v2 [astro-ph.CO] 1 Sep 2015

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“…In 2014 we are nearing completion of two upgrades to our AO systems and we are in the detailed design phase of a third upgrade. All of these upgrades also pave the way for our plans to design and build our next generation adaptive optics system (NGAO) [4] .…”

Section: Adaptive Opticsmentioning

confidence: 99%

New developments in instrumentation at the W. M. Keck Observatory

et al. 2014

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The W. M. Keck Observatory continues to develop new capabilities in support of our science driven strategic plan which emphasizes leadership in key areas of observational astronomy. This leadership is a key component of the scientific productivity of our observing community and depends on our ability to develop new instrumentation, upgrades to existing instrumentation, and upgrades to supporting infrastructure at the observatory. In this paper we describe the as measured performance of projects completed in 2014 and the expected performance of projects currently in the development or construction phases. Projects reaching completion in 2014 include a near-IR tip/tilt sensor for the Keck I adaptive optics system, a new center launch system for the Keck II laser guide star facility, and NIRES, a near-IR Echelle spectrograph for the Keck II telescope. Projects in development include a new seeing limited integral field spectrograph for the visible wavelength range called the Keck Cosmic Web Imager, a deployable tertiary mirror for the Keck I telescope, upgrades to the spectrograph detector and the imager of the OSIRIS instrument, and an upgrade to the telescope control systems on both Keck telescopes.

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W. M. Keck Observatory's next-generation adaptive optics facility

Cited by 16 publications

References 20 publications

Sharpening of natural guide stars for low-order wavefront sensing using patrolling laser guide stars

Sharpening of natural guide stars for low-order wavefront sensing using patrolling laser guide stars

Precision cosmology with time delay lenses: high resolution imaging requirements

New developments in instrumentation at the W. M. Keck Observatory

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