A rhodium-emitted X-ray with a photon energy at 20 KeV was employed to irradiate CaF2 with different surface finishing. Color centers associated with the irradiation damage were determined by spectral measurements. The depth distribution of the color centers was calculated and confirmed in a wedge spot generated by magnetorheological finishing. The results suggest that the color center formation is directly associated with the damage resistance of the optics. Laser durable grade CaF2 demonstrates higher damage resistance to the X-ray irradiation when compared to excimer ArF laser grade CaF2. Subsurface-damage-free CaF2 surfaces further enhance the damage resistance.
This paper describes the manufacturing steps necessary to manufacture hemispherical concave aspheric mirrors for high- NA systems. The process chain is considered from generation to final figuring and includes metrology testing during the various manufacturing steps. Corning Incorporated has developed this process by taking advantage of recent advances in commercially available Satisloh and QED Technologies equipment. Results are presented on a 100 mm concave radius nearly hemispherical (NA = 0.94) fused silica sphere with a better than 5 nm RMS figure. Part interferometric metrology was obtained on a QED stitching interferometer. Final figure was made possible by the implementation of a high-NA rotational MRF mode recently developed by QED Technologies which is used at Corning Incorporated for production. We also present results from a 75 mm concave radius (NA = 0.88) Corning ULE sphere that was produced using sub-aperture tools from generation to final figuring. This part demonstrates the production chain from blank to finished optics for high-NA concave asphere.
Previously we established that the combination of new machining parameters for openbacked
monolithic lightweighted ZERODUR® mirror substrates, coupled with new methods for optical
finishing of aggressively lightweighted mirrors, have relieved classical mirror design constraints imposed
upon 1.2m diameter lightweight mirrors. We demonstrate that openback mirror substrates now offer
comparable mass, Eigenfrequency and substructure print-through performance to the sandwich-mirror
architecture, but with considerably less manufacturing effort than for sandwich mirrors. Here we extend
the analyses of the first paper from 1.2m diameter down to 0.6m in diameter and up to 2.4m diameter and
4m diameter mirrors.
Recent game-changing technology greatly extends the design possibilities and range of applications for aggressively lightweighted open-back Zerodur® mirrors. We have compared several lightweighting design approaches under this new technology. Analytic comparisons are for 1.2m mirrors, all constrained to have a free-free first Eigenfrequency of 200 Hz. Figures of merit include resulting mass, thickness and relative cost. Much more aggressive masses are now available in open-back mirrors, competitive with the more expensive closed-back sandwich mirrors. These breakthroughs are relevant to spaceborne implementation of lightweight mirrors ranging from a few tenths of a meter in diameter to up to 4 meters in diameter.
KEYWORDS: Telescopes, Image segmentation, Mirrors, Control systems, Domes, Simulation of CCA and DLA aggregates, Image quality, Cameras, Computing systems, Camera shutters
The HET is unique among 9-meter class telescopes in featuring an Arecibo-like design with a focal surface tracker. The focal surface tracker causes image quality and pointing/tracking performance to interact in a complex way that has no precedent in astronomical telescope system design and that has presented unusual demands upon commissioning. The fixed-elevation, segmented primary-mirror array offers some simplifications over traditional telescope design in principle, but has presented challenges in practice. The sky access characteristics of the HET also place unique demands on observational planning and discipline. The HET is distinguished by uniquely low construction and operating costs which affected commissioning. In this contribution, we describe those aspects of our commissioning experience that may impact how similar telescopes are designed, especially those with larger aperture, and review the challenges and lessons learned from commissioning a 9-meter class telescope with a small technical team.
COHSI was successfully commissioned at the United Kingdom IR Telescope on Mauna Kea during a seven night observing run which coincided with this conference. Here we briefly describe the instrument and give a preliminary report on its performance at this time. The suppression optics and masks worked extremely well and the instrument background was found to be very low.
This paper describes the results of a test program to evaluate four Rockwell HAWAII and two PICNIC near IR array detectors with a view to their application in imaging, spectroscopy and in fast telescope tracking and interferometer fringe detection. Results of the laboratory test of the arrays are presented, together with a guide for their general operation.
We are currently building a panoramic wide field near infrared imaging camera based on 4 Rockwell Hawaii HgCdTe 10242 detectors. The survey instrument will operate in the J and H bands and will be as scientifically versatile and as easy to use as a large format CCD camera. It is expected to be ready for astronomical use by late 1997. It will be particularly well-suited for surveys of star-forming regions, low mass stars, distant galaxies, clusters and QSOs. The camera will be commissioned at the prime focus of the 2.5 m Isaac Newton telescope, where the image scale is 0.45'/pixel, giving an effective field of view of 14.6 by 14.6 arc minutes. The field of view of this camera with 0.15' pixels is 5.1 by 5.1 arc minutes and is thus approximately 60 times larger than the current near-infrared imager on Keck (NIRC). When combined with a 4.0 m class telescope, the combination is approximately 10 times as powerful as the Keck 10.0 m, when the apertures are taken into account. The options for upgrading the camera into a wide field spectroscopic survey instrument are currently being investigated.
One of the main limitations to the study of faint objects in the near-infrared (1 to 2 micrometer) is the luminous, varying sky background from very narrow OH emission lines originating in the Earth's upper atmosphere. This source of background contributes 95% to 98% of the total sky counts in the J & H atmospheric windows. We present the optical layout of the Cambridge OH suppression instrument. COHSI is designed to deliver OH suppressed, R equals 500, spectroscopy for both J & H spectral bands simultaneously providing an integral field mode and a multi-object mode. COHSI also has an OH suppression imaging mode. A modular approach has been selected for COHSI with the instrument consisting of three components. The first section consists of simple re-imaging lenses and a lens array interfacing the telescope to a set of optical fibers. This decouples the design of COHSI's main components from the telescope allowing COHSI to be easily used with different telescopes and making it free from flexure problems. The second section of COHSI is the OH suppression 'filter' itself. The size of this section is significantly smaller than in other similarly planned instruments. The third and final module of COHSI is the cryogenic low-resolution imaging spectrograph.
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