Engineering topics

Kazes, I.

Publications and source records attributed to Kazes, I..

3 records

NASA NTRS1989

Molecular gas in the powerful radio galaxies Perseus A and 4C 12.50

Perseus A, 4C 12.50, and Cygnus A have been observed in the CO(J = 1 to 0) line. In Perseus, an estimate of 3.2 x 10 to the 9th solar masses is found for the molecular gas in the giant galaxy in the cluster center. An upper limit of M(H2) = 9 x 10 to the 9th solar masses is obtained for the galaxy in the center of Cygnus A. The results suggest that large amounts of molecular gas, and thus high rates of star formation, are involved in the genesis of the central engines that power extragalactic radio sources.

Mirabel, I. F.↗

NASA NTRS1988

Detection of H I, OH, CO, and optical imaging of the distant galaxy IRAS 12112 + 0305

The detection of H I absorption and OH and CO emission from the galaxy IRAS 12112 + 0305, which is receding from the sun at about 7 percent of the speed of light is reported. This galaxy, which appears to be an ongoing merger, radiates about 2 x 10 to the 12th solar luminosities in the infrared. The H I, OH, and CO spectra are indicative of large turbulent motions. From the millimeter wave CO observations, a total mass of molecular gas of 4 x 10 to the 10th solar masses is inferred. The OH emission in the 1667 MHz line is the most luminous extragalactic OH maser reported so far, with an isotropic luminosity of 1800 solar luminosities.

Mirabel, I. F.↗

NASA NTRS1984

The Smallest Sizes of Diffuse Interstellar Clouds

By observing the difference in optical depths between absorption spectra toward the two components of double sources, the variations in opacity over lengths of less than 0.1 up to 10 pc inside diffuse interstellar clouds were measured. Significant variations were detected on scales larger than about 0.2 pc, but not less. This may represent the minimum size for diffuse cloud structure. By comparing the variations of Gaussian fitted line parameters, it was found that variations in the internal velocity field of diffuse clouds explain the data better than tiny independent cloudlets.

Dickey, J. M.↗