Engineering topics
Publications and source records attributed to Fay, T. D..
System consists of television camera using 25 mm SEC vidicon, low dispersion spectrograph, and digital video image system used for buffer storage of video data during tube readout scanning. Six-bit ADC converts video to digital data which are stored on magnetic tape for future evaluation.
Explore the source record for details and available documents.
A 25-mm vidicon camera was previously modified to allow operation in an integration mode for low-light-level astronomical work. The camera was then mated to a low-dispersion spectrograph for obtaining spectral information in the 400 to 750 nm range. A high speed digital video image system was utilized to digitize the analog video signal, place the information directly into computer-type memory, and record data on digital magnetic tape for permanent storage and subsequent analysis.
Detailed comparison of a series of stellar atmospheric models at effective temperatures of 3800 and 3500 K with scanner observations of Betelgeuse (alpha Ori, M2 Iab). The atmospheres are hydrostatic, flux-constant, LTE atmospheres which include the opacity of H2O, CO, CN, and atomic line blanketing. To reduce the flux shortward of 6000 A enough to agree with observations requires either strong atomic line blanketing (or a similar opacity source) or significant reddening, or (likely) both. The visual extinction (an estimate of which depends strongly on the line blanketing, especially in the 1- to 2-micron region) lies between 0.4 and 2.0 mag. Comparison of predicted strengths of observed CO and CN features with observations and of predicted column densities of CO, OH, NH, and H2O with published column densities suggests that C/H may be less than its solar value by about a factor of 10 and C/O may be less than 0.6 in Betelgeuse.
Rotational lines of the (0, 0) and (1, 1) bands of the C2(-) ion are shown to be coincident with absorption features in the CH star HD 201626 (C1, 1). Of the 72 lines of the (0, 0) band studied, the coincidences are within 0.04 A in all but two cases. These two lines are obviously blends, but of unknown origin. The identification of C2(-) must still be considered uncertain because the spectrum of HD 201626 is complex and many of the coincident lines are blended.
Umbral line profiles of H-alpha, NaD2 and HeI 10830 have been observed photoelectrically with a pressure scanning spectrometer. The H-alpha line profile shows, in a medium-sized spot, a pronounced weakening in the wings but a persistence of the line core in agreement with the results of Fricke and Elsaesser (1965). The profile of the HeI 10830 line shows an unexpected strengthening over the umbra of the two spots which have been observed. The NaD2 line profile together with continuum observations at 4260, 5890, and 6530 A have been accounted for with an empirical (T, tau) relation by one of us (Yun, 1971). The wavelength dependence and the absolute values from 4000 to 14,000 A of the intensity curve generated by this relation shows very good agreement with the intensities observed by Woehl et al. (1970) in a spot of similar diameter.
Description of an oscillating magnetic analyzer (KDP crystal plus Glan-Thompson prism) coupled to an echelle-interferometer spectrograph, and of single-slit magnetometer which by pressure variations can be made to scan the entire profiles of the circularly and linearly polarized Zeeman components. Freon gas is used as the scanner gas with wavelength displacements of 0.02 A per 0.1 in. Hg pressure change at the NaD lines. The available scan range is 15 A in the visual spectral region.
Solar rotational line positions due to red band in IR continuum region to resolve blue-violet ambiguity
Spectrographic comparison of selected carbon and M stars, discussing atomic lines identifications