IEEE - Aerospace and Electronic Systems - February 2023 - 22
Review of Terahertz Antenna Technology for Science Missions in Space
Figure 7.
Structure schematic of the AMSU-B instrument [12].
Sweden, Canada, France, and Finland. It operates at a
height of 552 km (LEO) above the Earth and carries two
instruments: the submillimeter and millimeter radiometer
(SMR) and the optical spectrograph and infrared imager
system (OSIRIS). The design of the OSIRIS instrument is
beyond the scope of THz antenna technology. The main
purpose of the SMR instrument shown in Figure 8 is to
study the upper atmosphere, including temperature, pressure,
and species like ClO, H2O, H2O2, HNO3, HO2,
N2O, and O3. The radiometer has five channels: A1 (541-
558 GHz), A2 (486-504 GHz), B1 (563-581 GHz), B2
(547-564 GHz), and C1 (118.25-119.25 GHz). The
antenna system consists of an offset Gregorian telescope
and a quasi-optical network.
THEGREGORIANANTENNA
The SMR instrument uses a 1.1-m dual reflector offset
Gregorian telescope with shaped surfaces, which could
ensure both high gain and low sidelobe levels. The reflectors
are made from carbon-fiber-reinforced-plastics
(CFRP), and the front surfaces are coated with vacuum
deposited aluminum. The measured surface accuracy is 8
mm rms for the primary mirror and 5 mm rms for the secondary.
The beam size and efficiencies of the Gregorian
antenna are shown in Table 3.
THEQUASI-OPTICALNETWORK
The incoming radiation from the telescope or the cold sky is
directed to the following quasi-optical network shown in
Figure 9. The network consists of a switching mirror, a
dichroic filter, polarization grids, elliptical mirrors, and corner
22
Figure 8.
Photograph and Block diagram of the SMR instrument [14].
IEEE A&E SYSTEMS MAGAZINE
FEBRUARY 2023
cube reflectors. The switching mirror directs the radiation
from the telescope, the internal load, or the cold sky to the
receivers. A dichroic filter separates the millimeter channel
C1 from the submillimeter channels B1 and B2, and a lensmirror
combination directs the millimeterwave into the Potter
horn. Within the submillimeter bands, the frequency separation
is achieved using two polarization grids. Then, the separated
signals are sent to the Martin-Pulpett interferometers
for single sideband filtering and feeding the Schottkymixers.
Also the inherently low-loss QO front-ends was chosen
and designed to meet the broadband need in this mission,
four submillimeter channels and one mm wave channel was
separated using two polarization grids and a planar dichroic
filter.
IEEE - Aerospace and Electronic Systems - February 2023
Table of Contents for the Digital Edition of IEEE - Aerospace and Electronic Systems - February 2023
Contents
IEEE - Aerospace and Electronic Systems - February 2023 - Cover1
IEEE - Aerospace and Electronic Systems - February 2023 - Cover2
IEEE - Aerospace and Electronic Systems - February 2023 - Contents
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