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NASA NTRS1979

Infrared and optical measurements of the ionized gas in K3-50

Results are reported for optical, near-IR, and mid-IR spectrophotometry of the compact H II region K3-50A. The emission-line observations imply an electron density of about 100,000 per cu cm; the consistency of density measurements in the optical, IR, and radio sources suggests that the optical counterpart of K3-50A is a reflection nebula. Previous measurements of the anomalous extinction law in K3-50A are confirmed, this law is extended out to B-alpha at 4 microns, and a 9-micron optical depth of about 2.5 is obtained. Elemental abundances are derived from measurements of emission lines of several dominant ions of the same element and found to be in close agreement (50%) with mean cosmic abundances. Individual ionic ratios are compared with model H II region calculations to determine the nature of the ionizing radiation. It is concluded that if nongray UV dust absorption does not modify the spectrum appreciably, the radiation temperature can be associated with a stellar surface temperature of about 37,000 K, corresponding to an O6 supergiant.

Lester, D. F.↗

NASA NTRS1979

Space Telescope optics

The paper reviews the optical technology that has been developed over the last decade for the Space Telescope. The optical design of the telescope, the optical performance control system, and the anticipated optical performance are all presented. Consideration is also given to the initial complement of focal plane instruments.

Jones, C. O.↗

NASA NTRS1979

A model for testing centerfinding algorithms for automated optical navigation

An efficient software simulation of the imaging process for optical navigation is presented, illustrating results using simple examples. The problems of image definition and optical system modeling, including ideal image containing features and realistic models of optical filtering performed by the entire camera system, are examined. A digital signal processing technique is applied to the problem of developing methods of automated optical navigation and the subsequent mathematical formulation is presented. Specific objectives such as an analysis of the effects of camera defocusing on centerfinding of planar targets, addition of noise filtering to the algorithm, and implementation of multiple frame capability were investigated.

Griffin, M. D.↗

NASA NTRS1979

Forecast analysis of optical waveguide bus performance

Elements to be considered in the design of a data bus include: architecture; data rate; modulation, encoding, detection; power distribution requirements; protocol, work structure; bus reliability, maintainability; interterminal transmission medium; cost; and others specific to application. Fiber- optic data bus considerations for a 32 port transmissive star architecture, are discussed in a tutorial format. General optical-waveguide bus concepts, are reviewed. The electrical and optical performance of a 32 port transmissive star bus, and the effects of temperature on the performance of optical-waveguide buses are examined. A bibliography of pertinent references and the bus receiver test results are included.

Ledesma, R.↗

NASA NTRS1980

Method of forming a sharp edge on an optical device

A sharp edge is formed on an optical device by placing the optical device in a holding mechanism; grinding one surface so that it and a surface of the holding mechanism are co-planar; and polishing both the surface of the optical device and the surface of the holding mechanism with felt until an edge on the surface of the optical device adjacent to the surface of the holding mechanism obtains a desired sharpness.

Fleetwood, C. M.↗

NASA NTRS1980

Integrated optic waveguide devices

Integrated optic waveguide circuits with a phase bias and modulator on the same chip were designed, fabricated, and tested for use in a fiber-optic rotation sensor (gyro) under development. Single mode fiber-optic pigtails were permanently coupled to the four ports of the chip. The switch format was based on coherent coupling between waveguides formed in Z-cut LiNbO3. The control of the coupling was achieved by electro-optically varying the phase propagation constants of each guide. Fiber-to-chip interfacing required the development of appropriate fixturing and manipulation techniques to achieve the close tolerance needed for high coupling efficiency between a fiber with an approximately 5 micron m core and a channel guide with a roughly 2 micron m by 5 micron m cross section. Switch and chip performance at 0.85 micron m is discussed as well as potential improvements related to insertion loss reduction, switching voltages, and suppression of Li2O out-diffusion.

Ramer, O. G.↗

NASA NTRS1980

Spatial frequency response of an optical heterodyne receiver

The principles of transfer function analysis are applied to a passive optical heterodyne receiver to obtain the modulation transfer function (MTF). MTF calculations are performed based on an optical platform which is imaging vertically varying profiles at worst case shuttle orbit altitudes. An analysis of the derogatory effects of sampling (aliasing) and central obscurations on both resolution and heterodyne efficiency is given. It is found that the cascading property of MTF analysis must be carefully applied since the coherent transfer function of the optical receiver and that due to the local oscillator-detector combination are not separable but are related by the convolution of their products. Application of these results to the specific case of a space-lab type optical heterodyne receiver shows that resolutions of the order of 1.5-2.0 Km are possible for worst-case type orbital scenarios. Further, comparison of obscured-type receivers (e.g., Cassegrains) with unobscured receivers shows that both resolution and efficiency are severely degraded in an obscured-type receiver and consequently should not be used for a passive heterodyne detection scheme.

Fales, C. L.↗

NASA NTRS1980

Spatial acquisition of optical sources in the presence of intense interference

The problem of spatially acquiring an optical beacon in the presence of intense optical interference is considered. It is demonstrated that conventional acquisition procedures cannot establish acceptable levels of acquisition probability when competing with strong optical interference without requiring unreasonable amounts of prime power. As a possible solution, it is shown that a more sophisticated acquisition scheme can virtually eliminate the effects of optical interference while requiring only a modest increase in system complexity.

Vilnrotter, V. A.↗

NASA NTRS1979

A precise position and optical identification for 4U 2129+47 - X-ray heating and a 5.2 hour binary period

A precise (20 arcsec) position and an optical counterpart are presented for the weak X-ray source 4U 2129+47. The optical counterpart shows weak but distinct He II 4686-A and C III-N III 4640-4650-A emission. Both H-beta and Ca II H and K are sometimes visible in absorption. Numerous plates and spectrophotometric observations from the 1978 observing season show that the blue magnitude varies from 16.7 to 18.0 in a period of 5.2382 hours. The light curve is sinusoidal in appearance, but with sharply defined V-shaped minima. It is proposed that most of the optical emission from this system originates at the X-ray heated face of the normal star and hence that this system is analogous to HZ Her/Her X-1. This is one of the few intrinsically faint optical counterparts of X-ray sources that show clear evidence of binary nature. The observations suggest a distance of 1.2-1.6 kpc for the source, and a consequent X-ray luminosity of approximately 10 to the 34.8 ergs/s.

Thorstensen, J.↗

NASA NTRS1979

Television optics for the Voyager mission to Jupiter and Saturn

This paper is concerned with the optical portion of the Voyager spacecraft imaging science subsystem (ISS). After a brief description of the Voyager mission and its photographic aspects, the functional requirements for the television optics are outlined. Environmental considerations that constrained the design are summarized. One section of the paper is devoted to radiation testing and its impact on the design of the wide-angle optics. The main portion of this report, however, is devoted to a description of the Voyager television optics. Finally, Voyager imagery results that are current with the preparation of this paper are presented.

Snyder, L.↗

NASA NTRS1979

Quest for ultrahigh resolution in X-ray optics

A program of solar X-ray astronomy using grazing incidence optics has culminated in X-ray images of the corona having one arc second spatial resolution. These images have demonstrated that, in general, X-ray optics can be fabricated to their specifications and can provide the level of resolution for which they are designed. Several aspects of these programs relating to the performance of X-ray optics in regard to resolution, including the point response function, the variation of resolution with off-axis position and the recognition that nearly all solar X-ray images have been film limited, are discussed. By extending the experience gained on this and other programs it is clearly possible to design and fabricate X-ray optics with sub arc sec resolution. The performance required to meet the scientific objectives for the remainder of the century are discussed in relation to AXIO, an Advanced X-Ray Imaging Observatory for solar observations which is proposed for flight on the Space Shuttle. Several configurations of AXIO are described, each of which would be a major step in the quest for ultrahigh-resolution observations.

Davis, J. M.↗

NASA NTRS1979

Optical analysis of Cassegrainian concentrator systems

Cone optics procedures have been developed to treat optical systems employing multiple reflectors. The objective of the procedures is to develop efficient techniques to treat multiple reflections of cones when the secondary reflecting surface is curved - in fact, curved differently in different directions. The particular optical system under consideration is the Cassegrainian Concentrator System - a system consisting of a paraboloidal primary reflector and a confocal hyperboloidal secondary reflector. Multiple reflection cone optics methodology as well as preliminary results for the flux distributions and intercept factors based on it are presented in this paper. It is shown that neglecting local curvature effects of the secondary reflector, i.e. even in the differential solid angle within the sun's cone, may overestimate the peak of the flux distribution at the receiver aperture by a factor of two or more.

Bass, A. H., Jr.↗

NASA NTRS1980

The optically thin dust shell of Nova Cygni 1978

Nova Cygni 1978 was monitored photometrically from V to 19.5 microns for 120 days after the eruption. Following the initial expansion of the hot gas shell, an optically thin dust shell formed and reached a maximum visual optical depth of about 0.1 by day 60. No visible transition phase of the type observed in the very dusty DQ Herculis novae occurred in Nova Cygni 1978. It is argued that dust grain growth was inhibited because of the low mass of condensable atoms in the shell. Although the dust shell in Nova Cygni 1978 was optically thin at visual and infrared wavelengths, the grains grew to a radius of 0.3 micron which is comparable to the radius of the grains which grow in the optically thick shells of the DQ Herculis type novae.

Gehrz, R. D.↗

NASA NTRS1981

Optical fibers for the distribution of frequency and timing references

An optical fiber communications link was installed for the purpose of evaluating the applicability of optical fiber technology to the distribution of frequency and timing reference signals. It incorporated a 1.5km length of optical fiber cable containing two multimode optical fibers. The two fibers were welded together at one end of the cable to attain a path length of 3km. Preliminary measurements made on this link, including Allan variance and power spectral density of phase noise are reported.

Lutes, G. F.↗

NASA NTRS1981

Optical deep space communication via relay satellite

The possible use of an optical for high rate data transmission from a deep space vehicle to an Earth-orbiting relay satellite while RF links are envisioned for the relay to Earth link was studied. A preliminary link analysis is presented for initial sizing of optical components and power levels, in terms of achievable data rates and feasible range distances. Modulation formats are restricted to pulsed laser operation, involving bot coded and uncoded schemes. The advantage of an optical link over present RF deep space link capabilities is shown. The problems of acquisition, pointing and tracking with narrow optical beams are presented and discussed. Mathematical models of beam trackers are derived, aiding in the design of such systems for minimizing beam pointing errors. The expected orbital geometry between spacecraft and relay satellite, and its impact on beam pointing dynamics are discussed.

Gagliardi, R. M.↗

NASA NTRS1980

Acousto-optic spectrometer for radio astronomy

Recent developments in acousto-optic techniques and in photodetector arrays have made feasible a new type of RF spectrometer, offering the advantages of wide bandwidth, high resolution, large number of channels in compact, lightweight, energy efficient, and relatively low cost systems. Such a system employs an acousto-optic diffraction cell which serves the key role of converting RF signals to ultrasonic traveling-waves modulating the optical index of the cell. The cell is illuminated across its aperture by a monochromatic laser beam. A fraction of the light is diffracted by the acoustic waves. A focusing lens follows the cell and essentially performs a Fourier transform of the RF signal into a far-field intensity pattern. CSIRO in Australia and the Tokyo Astronomical Observatory in Japan have taken the lead in using acousto-optic techniques in astronomical applications. The first practical device was successfully made at CSIRO for obtaining dynamical spectrographs of solar radio emission.

Chin, G.↗

NASA NTRS1981

Multiwavelength monolithic integrated fiber optics terminal - An update

This paper serves as an update for the Multiwavelength Monolithic Integrated Fiber Optic Terminal (MMIFOT) being developed by MDAC-St. Louis for NASA's Johnson Space Center. The program objective is to utilize guided wave optical technology to develop a passive optical wavelength multiplexing subsystem with a single mode optical fiber serving as the transmission medium.

Spear-Zino, J. D.↗

NASA NTRS1981

Detection of acoustic emission in composites by optical fiber interferometry

Acoustic emission in prestressed composite panels using embedded single mode optical fiber was detected. Static loading of the composite matrix produces acoustic emission events, pulsed ultrasonic waves, which mechanically modulate the embedded fiber geometry and phase modulate the transmitted optical field. The modulation is detected by optical interferometry and Fourier optical processing techniques to produce an electronic signal proportional to acoustic field amplitude integrated along the length of the fiber in the specimen. Static and dynamic calibration of the detection system is discussed and frequency domain characterization of the acoustic field interaction with the fiber is presented.

Wade, J. C.↗