Noise Temperature and Gain Loss Due to Paints and Primers: A Case Study of DSN Antennas
In achieving high performance for reflector antennas, it has been noted that it is essential to carefully assess the roles of surface paints and primers.
Engineering topics
Publications and source records attributed to Otoshi, T..
In achieving high performance for reflector antennas, it has been noted that it is essential to carefully assess the roles of surface paints and primers.
This article presents the derivation of equations necessary to calculate noise temperature of a lossy flat plate reflector. Reflector losses can be due to metallic surface resistivity and multi-layer dielectric sheets including thin layer of plating, paint, and primer on the reflector surface.
A new 34-m research and development antenna was fabricated and tested as a precursor to introducing beam waveguide (BWG) antennas and Ka-band (32 GHz) frequencies into the NASA/JPL Deep Space Network. For deep space use, system noise temperature is a critical parameter. There are thought to be two major contributors to noise temperature in a BWG system: the spillover past the mirrors, and the conductivity loss in the walls. However, to date, there are no generally accepted methods for computing noise temperatures in a beam waveguide system. An extensive measurement program was undertaken to determine noise temperatures in such a system along with a correspondent effort in analytic prediction. Utilizing a very sensitive radiometer, noise temperature measurements were made at the Cassegrain focus, an intermediate focal point, and the focal point in the basement pedestal room. Several different horn diameters were used to simulate different amounts of spillover past the mirrors. Two analytic procedures were developed for computing noise temperature, one utilizing circular waveguide modes and the other a semiempirical approach. The results of both prediction methods are compared to the experimental data.
A new 34-meter research and development antenna was fabricated and tested as a precursor to introducing beamwaveguide antennas and Ka-band frequencies into the NASA/JPL Deep Space Network. For deep space use, system noise temperature is a critical parameter. There are thought to be two major contributors to noise temperature in a BWG system: the spillover past the mirrors and the conductivity loss in the walls. However, to date, there are no generally accepted methods for computing noise temperatures in a beamwaveguide system. An extensive measurement program was undertaken to determine noise temperatures in such a system along with a correspondent effort in analytic prediction. Utilizing a very sensitive radiometer, noise temperature measurements were made at the cassegrain focus, an intermediate focal point, and the focal point in the basement pedestal room...
This paper presents a new way to design a low-loss couipler for high- or low-dielectric constant, dielectric waveguide for optical or millimeter/submillimeter waves.
This paper presents an analytical method for determining the exact distance a load is required to be offset from a passive two-port network to obtain maximum or miunimum return losses from the terminated two-port network.
This paper describes the errors associated with measuring time delays of signals propagating through the primary path of a large Cassegrain antenna.
Insertion loss and reflection coefficient measurements and changes on waveguide system of Venus deep space station cone