# The first diffraction-limited images from the W.M. Keck Telescope

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The Physical Object ID Numbers Other titles First diffraction limited images from the W.M. Keck Telescope. Statement K. Matthews ... [et al.]. Series NASA-TM -- 112894., NASA technical memorandum -- 112894. Contributions Matthews, K., United States. National Aeronautics and Space Administration. Format Microform Pagination 1 v. Open Library OL18118467M

### Details The first diffraction-limited images from the W.M. Keck Telescope FB2

ABSTRACT. The first diffraction limited, resolution, images on the W. Keck Telescope have been obtained at a wavelength of /zm. These images were part of an experiment to test the suitability of the Keck Telescope for speckle imaging.

In order to conduct this test, it was necessary to modify the pixelFile Size: KB. Get this from a library. The first diffraction-limited images from the W.M.

Keck Telescope. [K Matthews; United States. National Aeronautics and Space Administration.;]. Adaptive optics have been used on smaller telescopes, but this is the first time it’s been employed on a telescope as large as the mighty Keck II; it took nine years to adapt the observatory.

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Keck Telescope SCIENCE KIT Fact Sheet. Part 1. Highlights of The Keck Telescopes The Largest Telescope in the World It took almost years from the time Galileo first examined the heavens with his small telescope inuntil an astronomical observatory was built on a mountain top: inthe largest telescope in the world was a refractor featuring a inch diameter objective lens, on.

Keck NGS AO first light paper: Wizinowich, P., et al.PASPThe AO system was locked on a V= star and images were taken of the guide star.

Then the telescope was offset to four off-axis stars and images were taken at each star. The Strehl ratio as a. We present the first diffraction-limited K-band image of the Red Rectangle with 76 mas resolution, an H-band image with 75 mas resolution, and an RG filter image (∼ nm wavelength) with.

The first diffraction-limited images from the W. Keck Telescope. Publications of the Astronomical Society of the Pacific– A set of faint JHK standards for UKIRT The 0. turbulence and telescope aberrations.1–3 At the W. Keck Observatory there are identical AO sys-tems on the Keck I and Keck II telescopes.4 Keck I is used only for interferometry and hence does not have a science camera, whereas Keck II supports a number of instruments.

In this paper we character-ize the performance of the Keck II AO system. Abstract. Four years ago, we initiated a proper motion study of the Galaxy’s central stellar cluster using diffraction-limited K[$$\mu m$$]-band images obtained with the W.M.

Keck I m relative positional accuracies of $$\sim 3$$ milliarcsec, we have been able to measure stars moving with velocities up to km s-1 and, for the first time ever, accelerations of mas. A laser guide star is an artificial star image created for use in astronomical adaptive optics systems, which are employed in large telescopes in order to correct atmospheric distortion of light (called astronomical seeing).Adaptive optics (AO) systems require a wavefront reference source of light called a guide l stars can serve as point sources for this purpose, but sufficiently.

An optical telescope is a telescope that gathers and focuses light, mainly from the visible part of the electromagnetic spectrum, to create a magnified image for direct view, or to make a photograph, or to collect data through electronic image sensors.

There are three primary types of optical telescope: refractors, which use lenses (); reflectors, which use mirrors (). @article{osti_, title = {Near infra-red astronomy with adaptive optics and laser guide stars at the Keck Observatory}, author = {Max, C E and Gavel, D T and Olivier, S S}, abstractNote = {A laser guide star adaptive optics system is being built for the W.

Keck Observatory`s meter Keck II telescope. Two new near infra-red instruments will be used with this system: a high-resolution Cited by: 1. Gerry Neugebauer Bibliography.

Papers, etc. Neugebauer’s papers and a oral history interview by Timothy Moy are at the Caltech archives also contain a lengthy oral history interview with James A. Westphal. which discusses Neugebauer. Other References: Historical. Low, Frank J., G.H.

Rieke, & R.D. Gehrz, “The Beginning of Modern Infrared Astronomy— to ,” Ann. Abstract. Images of point-like astronomical sources formed on a CCD camera will be represented by a point spread function.

In the absence of other degrading effects, the spreading of the image is determined by the diffraction of light. Adaptive optics (AO) is a technique that removes the atmospheric disturbance and allows a telescope to achieve diffraction-limited imaging from the ground.

This is critical in achieving the maximum S/N given in equation (1).The basic idea of AO is to first measure the amount of atmospheric disturbance, then correct for it before the light reaches the camera. The Celestron CPCis a ″ diffraction limited Schmidt-Cassegrain telescope and off-the-shelf sells for $2, including the mount, (just the inch optical tube sells for$1,).

This book provides a unified treatment of the characteristics of telescopes of all types, both those whose performance is set by geometrical aberrations and the effect of the atmosphere, and those diffraction-limited telescopes designed for observations from above the atmosphere.

The celebration of the th anniversary of Galileo’s first use of an astronomical telescope provides a fitting context for planning new goals and directions for ground-based optical and infrared (OIR) astronomy in the 21st century. The revolutionary improvement over the unaided eye that Galileo.

At the Keck Observatory, these instruments include all four of the currently operational infrared science instruments; NIRSPEC (McLean ) - the first cryogenic infrared echelle spectrometer on a m telescope; NIRC2 (McLean and Larkin )- a diffraction-limited AO infrared camera built jointly with Caltech; OSIRIS (Larkin ) – a.

Peter Wizinowich is the Optical Systems Manager at the W. Keck Observatory (WMKO). He has been at WMKO sinceand has led the telescope optics installation and alignment, the adaptive optics development program and the Keck interferometer development activities.

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Overview of W. Keck Observatory The W. Keck Observatory (WMKO) operates twin 10 meter optical/infrared telescopes on the excellent site of Mauna Kea. Keck I achieved first light in and Keck II in The two telescopes feature a highly capable suite of advanced.

PROCEEDINGS OF SPIE Volume Proceedings of SPIE X, V SPIE is an international society advancing an interdisciplinary approach to the science and application of light. Optical and Infrared Interferometry III Françoise Delplancke Jayadev K. Rajagopal Fabien Malbet Editors 1 6 July Amsterdam, Netherlands.

The W. Keck Observatory is a two-telescope astronomical observatory at an elevation of 4, meters (13, ft) near the summit of Mauna Kea in the U.S. state of Hawaii. Both telescopes have 10 m (33 ft) aperture primary mirrors, and when completed in and were the largest astronomical telescopes in the world.

As we cross the threshold of the new millennium, astronomy with ground-based optical and infrared (O/IR) telescopes will continue to play its fundamental role in shaping our understanding of the workings of the universe, enriching the golden era of discovery that astronomy has enjoyed in the last decades.

) (c) The m Keck telescope.

### Description The first diffraction-limited images from the W.M. Keck Telescope PDF

This image shows one of the two Keck telescopes. The primary mirror consists of 36 hexagonal segments that are aligned to optical precision. The instruments are located on a platform on two sides of the telescope facing the declination bearings. The segmented mirror design approach was first used with the Keck Cited by: 4.

Figure 2 shows spot diagrams at the center of the field and at a field radius of 1 arcminute. The optical design is nearly diffraction-limited in the infrared over this size of field. The linear diameter of a 2- arcminute diameter field at the Cassegrain focus is m.

Figure 3 shows spot diagrams for a field radius of arcminutes. Instrumentation development at the W.M. Keck Observatory Author(s): Status of the Southern African Large Telescope (SALT) first-generation instruments Author(s): OSIRIS: a diffraction limited integral field spectrograph for Keck Author(s).

LSST Science Collaborations and LSST ProjectLSST Science Book, VersionarXiv Zoltán Haiman, “The Origin and Detection of High-Redshift Supermassive Black Holes”, Proceedings of "The First Stars and Galaxies: Challenges for the Next Decade", Austin, TX, March, arXiv Ghez was the first to deliver images from Keck observatory that were corrected for the blurring effects of the Earth’s atmosphere, breaking a fundamental barrier and deliver-ing images sharper than those from Hubble Space Telescope by more than a factor of By tracking the motions of stars, Ghez, Morris and Becklin.

Adaptive optics (AO) is essential for many elements of the science case for the Thirty Meter Telescope (TMT). The initial requirements for the observatory's facility AO system include diffraction-limited performance in the near IR, with 50 per cent sky coverage at the galactic pole.

Point spread function uniformity and stability over a 30 arc sec field-ofview are also required for precision.W. M. Keck Observatory Adaptive Optics Science Capabilities W. M. Keck Observatory Keck AO First TAC-allocated Science Milestones.

0 1 K2 NGAO + K2 Center Launch Camera. Future. AAS June Keck I LGS AO • LGS AO for Keck I telescope ().W. M. Keck Observatory adaptive optics program p. Performance predictions for the Keck telescope adaptive optics system p.

Near-infrared astronomy with adaptive optics and laser guide stars at the Keck Observatory p. Table of Contents provided by Blackwell's Book Services and R.R.

Bowker. Used with permission.