Abstract
Compact and lightweight sensors with a high-frequency resolution are required for the passive observation of atmospheric water and oxygen emission lines at a reduced cost and power consumption. A molecular assessment high-resolution observation spectrometer (MAHOS) is developed as a compact, low power, digital fast Fourier transform spectrometer to be installed on a microsatellite. MAHOS has a compact design with dimensions of <inline-formula> <tex-math notation="LaTeX">$0.154\times 0.125\times0.040$ </tex-math></inline-formula> m<sup>3</sup> and mass of 0.7 kg. It uses only a few materials including a field-programmable gate array (FPGA) module with a lightweight aluminum alloy box. The highly stable spectrometer exhibits a sampling speed of 2.6624 GS/s and 16 384 frequency channels. The stability of the spectrometer is longer than 1200 s within the 1-GHz bandwidth. Thermal dissipation is achieved through a heat conductive gel filled in the gap between the most heat-generating component, the FPGA, and the aluminum alloy case. Results of a finite element analysis indicate that the design is stiff and stable enough to survive in the launch environment. Thermal analysis indicates the durability of the system during operation. Even in space where heat dissipation is not possible, self-heating temperatures are not a problem for the FPGA. In the future, the performance of the spectrometer will be verified by conducting environmental tests.
Highlights
Altitude of the middle atmosphere, which is yet unknown from actual measurements, we will learn how the water environment is changing on Mars [4]–[5]
To analyze the emission line spectrum of gaseous components of the atmosphere for remote sensing, various spectrometers have been developed for atmospheric remote sensing, of which the three main types are acousto-optic spectrometers (AOSs), chirp transform spectrometers (CTSs), and digital fast Fourier transform (FFT) spectrometers [10]
The AOS employed in submillimeter wave astronomy satellite (SWAS), which operated in spectral regions at approximately 487, 492, 548, 551, and 557 GH on the Odin satellite, had a mass of 7.5 kg and power consumption of 5.5 W with full operation [12]–[13]
Summary
Altitude of the middle atmosphere (about 80–130 km), which is yet unknown from actual measurements, we will learn how the water environment is changing on Mars [4]–[5]. The AOS employed in SWAS, which operated in spectral regions at approximately 487, 492, 548, 551, and 557 GH on the Odin satellite, had a mass of 7.5 kg and power consumption of 5.5 W with full operation [12]–[13] These AOSs needed to be installed on a large payload bus, and could not be mounted on a microsatellite. A CTS, utilizing a chirp filter to the spectrum using chirp waveforms in pulse-compression radar, is developed for the submillimeter wave instrument (SWI) of the ESA microsatellite Jupiter ICy moons Explorer [14]–[16] It is integrated into several trays containing other individual electronics subsystems as a component of the electronic unit and provides 1 GHz bandwidth at 100 kHz resolution.
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