Earl J. Spillar

Measurements of Binary Stars with the Starfire Optical Range Adaptive Optics Systems

To investigate the relative photometry produced by adaptive optics within the isoplanatic patch, we observed four binaries, 10 UMa, UMa, 81 Cnc, and κ UMa, with adaptive optics using natural guide stars on the 3.5 m telescope, as well as one binary, β Del, with adaptive optics using a laser guide star on the 1.5 m telescope at the Starfire Optical Range. Iterative blind deconvolution (IBD) and parametric blind deconvolution (PBD) techniques were used to postprocess the data, which produced consistent results for position angles, separations, and magnitude differences. We also conducted simulations that verify the agreement between IBD and PBD and compared their measurements to truth data. From the results of both observations and simulations, we conclude that adaptive optics is well suited for providing not only position angles and separations for close binaries, but also good relative magnitudes without quadrant ambiguity. From the observations, we find that the secondary of 81 Cnc (separation = 012) appears to be 0.12 mag brighter than the primary at 0.85 μm and is, therefore, cooler. We also derive a new orbit for κ UMa (separation = 0067). Our results for β Del (ADS 14073) have significantly improved precision compared with the 1998 analyses of the same data by ten Brummelaar and colleagues and by Roberts, ten Brummelaar, and Mason.

Near-infrared imaging of NGC 5195

NGC 5195, the near companion of M51, was imaged in the near infrared J, H, and K bands with the Wyoming Infrared Camera. The observations map a 3.5 by 3.5 arcmin field at a resolution of 2 arcsec. Data reduction are described and surface and aperture photometry presented. The obscuration which confuses optical classifications is unimportant in the infrared. For the first time, we have an unobstructed view of the galaxy from which to perform a morphological classification and make measurements. Three distinct components which are clearly visible in the images are discussed : a bulge, a bar, and a disk

THE WYOMING INFRARED OBSERVATORY TELESCOPE SOFTWARE SYSTEM

We describe the University of Wyoming telescope control and data acquisition software system. The software was designed to be maintainable, portable, and inexpensive. Moreover, the software was designed to allow rapid communication between the hardware, the data acquisition processes, and the tracking processes, while leaving each distinct. We show how the new realtime features embodies in the POSIX.4 standard and implemented in the Unix compatible LynxOS operating system allow us to perform all of our tasks on a single 80486 machine with a standard Unix-like environment, with outstanding real-time performance. We discuss our telesocpe pointing model, which allows us to point with a root mean square error of less than 5 arcseconds over the sky with the 2.3 meter telesopce. For more detailed investigation and use, we will make the software available through anonymous FTP.

Deconvolution of intensity correlation functions

Abstract not available.

Wyoming prime-focus near-infrared camera

the prime focus of the Wyoming Infrared Observatory (WIRO) 2.3-m telescope. The detector is a 64 x 64 element HgCdTe array. A microprocessor-based control board residing on the dewar clocks the CCD multiplexer, controls the double-correlated sampling, and digitizes the detector signal. All voltage levels and clocking sequences can be adjusted by software in real time. The data acquisition computer communicates with the control board over a modified RS-232 link at an adjustable rate (usually 50 kilobaud). This allows virtually any computer to be used for data acquisition with a minimum of difficulty. The optics are optimized for the study of extended sources of low surface brightness, with maximum optical throughput. The f/2 primary is followed by a liquid-nitrogen-cooled Wynne corrector and two cold-filter wheels with a capacity of 12 individual filters and a 90-degree CVF segment. The positions of the lens, the instrument, and the filter wheels are adjusted by stepper motors. The plate scale is 2.06 arcseconds per pixel.