Spectrophotometry of Ton 524a, b.
Spectra of Ton 524a, b show that these two compact emission-line galaxies have nearly identical redshifts. This is the first pair of Seyfert-like galaxies that appear to form a physical pair.
Robinson, L. B.↗
SEARCH · Engineering Papers
Results for “spectrophotometry”
Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.
Spectrophotometry of the supernova in NGC 5253 from 0.33 to 2.2 microns.
Explore the source record for details and available documents.
Kirshner, R. P.↗
Minor planets and related objects. XI - 0.4-0.8 micron spectrophotometry of /1685/ Toro.
Explore the source record for details and available documents.
Johnson, T. V.↗
Infrared photometry and spectrophotometry of Titan
The wide variation in infrared brightness temperature of Titan is explained in terms of a greenhouse effect. Radiometric observations in the infrared and microwave frequencies indicate an alternate hot atmospheric model. Methane, ammonia, hydrogen atoms, and nitrogen atoms are suggested as main constituents for the Titan atmosphere.
Morrison, D.↗
Photoelectric spectrophotometry of OQ 172 and OH 471
Absolute spectral energy distributions for the large redshift quasars OQ 172 and OH 471 are discussed along with similar data for two other quasars 4C05.34 and PHL 957. Assuming cosmological redshifts, OQ 172 and OH 471 are not as luminous as PHL 957. If these quasars are basically similar and if radiative processes dominate, the strength of Ly alpha and the behavior of the continuum at the Lyman limit strongly suggest that these objects consist of a central ionizing source surrounded by discrete clouds, filaments or a gaseous structure such as a disk. This gaseous matter does not cover the whole solid angle surrounding the source.
Oke, J. B.↗
Spectrophotometry of comets
Photoelectric spectrophotometric- and image tube equipped spectrographic-studies on comets are used to formulate a new model for the cometary nucleus that is physically similar to the icy-conglomerate. Absolute flux distributions of the principal spectral features for five comets of different compositions and heliocentric distances were evaluated. Comparison of visible and infrared brightnesses was used to calculate the optical albedos of observed particles.
Odell, C. R.↗
IR spectrophotometry of Jupiter and Saturn
High spatial resolution spectrophotometric observations (from 0.6 to 2.0 microns) are used to study the Jovian and Saturnian limb darkening at 0 deg phase angle. The limb-darkening coefficients (k) of the Minnaert function are 1.0 over Jupiter's entire disk and between 0.75 and 0.90 for different latitudes on Saturn. These data are used to derive geometric albedoes (G) for the various belts, zones, spots, and regions observed on Jupiter and Saturn. These values of G and k are in turn used to show that an isotropic scattering model is invalid for Jupiter and that at least an asymmetric scattering function, such as the Euler function, is needed to fit the Jovian data. The Jovian scattering function is found to generally vary between 0.960 (1 + 0.85 cos theta) and 0.994 (1 + 0.42 cos theta) as a function of wavelength and the feature observed. The Saturn geometric albedoes and values of k indicate that Euler's function fails to adequately model the scattering properties of Saturnian clouds; they may be better represented by a cumulus cloud model.
Binder, A. B.↗
Photoelectric spectrophotometry of OQ 172 and OH 471
Absolute spectral energy distributions for the large-redshift quasars OQ 172 and OH 471 are discussed along with similar data for two other quasars: 4C 05.34 and PHL 957. If the redshift are assumed to be cosmological, OQ 172 and OH 471 are not as luminous as PHL 957. If these quasars are basically similar and if radiative processes dominate, the strength of alpha and the behavior of the continuum at the Lyman limit strongly suggest that these objects consist of a central ionizing source surrounded by discrete clouds, filaments, or a gaseous structure such as a disk. This gaseous matter does not cover the whole solid angle surrounding the source.
Oke, J. B.↗
Rocket ultraviolet spectrophotometry of Comet Kohoutek /1973f/
On January 5, 1974, the ultraviolet emissions from Comet Kohoutek (1973f) in the spectral range from 1200 to 3200 A were studied with the aid of a rocket carrying two spectrophotometers. In addition to the Lyman alpha line of atomic hydrogen at 1216 A and the (0,0) and (1,1) bands of OH at 3090 and 3142 A, both atomic oxygen (1304 A) and atomic carbon (1657 and 1561 A) were detected.
Feldman, P. D.↗
Developments in spectrophotometry I: An instrument for high-resolution measurements of optical intensity and polarization
Device has resolution required to analyze polarization of the spectra of unknown gases, liquids, or solids (or a mixture of these phases). Such resolution has not been available on conventional instruments.
Fymat, A. L.↗
Developments in spectrophotometry II: A multiple-frequency particle-size spectrometer
Instrument can be used to remotely determine complete spectrum of sizes of particles of unknown composition suspended in gas or liquid. Device does not required direct physical sample of particles.
Fymat, A. L.↗
Developments in spectrophotometry III: Multiple-field-of-view spectrometer to determine particle-size distribution and refractive index
Instrument is based on inverse solution ot equations for light scattered by a transparent medium. Measurements are taken over several angles of incidence rather than over several frequencies. Measurements can be used to simultaneously determine chemical and physical properties of particles in mixed gas or liquid.
Fymat, A. L.↗
Absolute spectrophotometry in M31 and M32
For a number of places in the bulge of M31 and for two places in M32 photometric scans from 3300 A to 10,600 A have been obtained with the multichannel spectrometer on the 5-meter Hale telescope. The scans show that in both objects the color temperature (particularly shortwards of 5000 A) decreases towards the center and that the strength of the CN bands increases towards the center in both objects in agreement with earlier observations. The new data can all be interpreted in terms of an increase of heavy element abundance towards the center in both objects by a factor probably less than 2 and by an excess of heavy elements in M31 compared to M32 by a factor probably greater than 2, in qualitative agreement with earlier conclusions.
Oke, J. B.↗
Photoelectric spectrophotometry of Wolf-Rayet stars
Photoelectric spectrum scans of five southern Wolf-Rayet stars in the spectral range lambda lambda 4600-4720 were analyzed to study the variability of brightness and of emission line strengths. No variations of any kind in short time scale were found. However, in WC stars night-to-night variations of three to four percent were detected in the emission line strengths.
Bahng, J. D. R.↗
Ultraviolet stellar spectrophotometry from a balloon platform
A 40 centimeter diameter aperture, balloon-borne telescope and ultraviolet spectrometer is described and selected scientific results are briefly reviewed. The general configuration of the 0.4 angstrom resolution instrument is shown and the utilization of servo-controlled secondary mirror, image dissector detector, and special mirror coatings are discussed. An outlook for astronomical research in the mid-ultraviolet from balloon-borne telescopes is presented together with future development plans for JSC's balloon-borne payload.
Kondo, Y.↗
Spectrophotometry of prominences in the phase preceding decay
The results are presented of spectrophotometric processing of prominence spectra in both the quiet and the decay phases. A catalog was compiled of equivalent widths, central intensities, Doppler half-widths, and half-widths of emission lines. The reduced Doppler half-widths of D3 and of the H, K Ca(+) lines obtained in a prominence active phase are much larger than those obtained during a quiet phase. Comparison of the equivalent widths and central intensities of H sub alpha, H sub beta hydrogen and D3 helium lines shows that the values increase in the active phase for the D3 lines and decrease for the H sub alpha, H sub beta lines.
Rakhubovskiy, A. S.↗
Optical and infrared spectrophotometry of 18 Markarian galaxies
Slit spectra, spectrophotometric scans and infrared broad band observations are presented. Eight of the program galaxies can be classified as Seyfert galaxies. Arguments are given that thermal, nonthermal and stellar radiation components were present. One group of Seyfert galaxies was characterized both by the presence of a high density region of gas and by a continuum dominated by nonthermal radiation. The continua of the remaining program Seyferts, which did not have a high density region of gas, were dominated by thermal radiation from dust and a stellar continuum. Ten of the galaxies, which are not Seyfert galaxies, are shown to be examples of extragalactic H 2 regions.
Becklin, E. E.↗
Ultraviolet spectrophotometry of Sirius from Gemini 12
The spectral energy distribution of Sirius between 2500 and 3700 A at a resolution of 7 A is obtained from plates taken on Gemini 12. The agreement with other observations and the most recent line-blanketed model atmospheres is good. The equivalent width of the Mg II doublet near 2800 A is 6.0 A, if the continuum level is represented by regions near 2650 and 2910 A. This is consistent with expectations for a hot Am star and implies line blocking of up to 15% in this wavelength region.
Spear, G. G.↗