Martian Moons eXplorer (MMX) is a sample-return mission of Phobos, the larger moon of Mars. To achieve the mission, a high-resolution 3D model of Phobos is essential, which requires a large number of high-resolution images to be sent back to Earth with enough quality before carrying out the landing activity. To realize this, the data transfer bandwidth is the bottleneck, and we adopt CCSDS 122.0-B-1 image compression, a variation of data compression based on the DWT method. This method allows us to select only one output quality for one image compression. On the other hand, the data transfer strategy shall be to transfer minimum-quality images first for quick looks and full-quality ones later. To realize this with the least computing power, we modified the method to output a low-quality full image and two supplemental data sets to better quality. This work is based on the CCSDS 122.0-B-1 implementation by a group of the University of Nebraska Lincoln.
Understanding the origin of the Martian moons is the main objective of the JAXA MMX (Martian Moons eXploration) mission, that will be launched in October 2026. Among the 13 instruments composing the payload, MIRS is an infrared imaging spectrometer that will map the mineralogy and search for organic compounds on the moons’ surfaces. MIRS will also study the Martian atmosphere, focusing on the spatial and temporal variations of water, dust and clouds. MIRS is operating in the 0.9-3.6 μm spectral range with a spectral resolution varying from 22 nm to 32 nm. The field of view covers 3.3° whereas the instantaneous field of view is 0.35 mrad. This presentation will detail the design and present the end-to-end performance obtained during the final instrument test in a representative thermal environment.
Ultraviolet (UV) spectroscopy is one of the most powerful tools used in a wide range of scientific fields from planetary science to astronomy. We propose a future UV space telescope, LAPYUTA (Life-environmentology, Astronomy, and PlanetarY Ultraviolet Telescope Assembly), selected as a candidate for JAXA’s 6th M-class mission in 2023. Launch is planned for the early 2030s. LAPYUTA will accomplish the following four objectives related to two scientific goals: understanding (1) the habitable environment and (2) the origin of structure and matter in the universe. Objective 1 focuses on the subsurface ocean environments of Jupiter's icy moons and the atmospheric evolution of terrestrial planets. Objective 2 characterizes the atmosphere of the exoplanets around the habitable zone and estimates their surface environment by detecting their exospheric atmosphere. In cosmology and astronomy, Objective 3 tests whether the structures of presentday galaxies contain ubiquitous Ly-α halos and reveals the physical origins of Ly-α halos. Objective 4 elucidates the synthesis process of heavy elements based on observations of ultraviolet radiation from hot gas immediately after neutronstar mergers. LAPYUTA will perform spectroscopic and imaging observations in the far-UV range of 110-190 nm with an effective area of >300 cm2 and a high spatial resolution of 0.1 arcsec. The apogee is 2,000 km, and the perigee is 1,000 km to avoid the influence of the geocorona when observing oxygen and hydrogen atoms and the Earth's radiation belt.
MIRS (MMX InfraRed Spectrometer) is an imaging spectrometer onboard of MMX (Martian Moon eXploration) mission. MMX is a JAXA sample return mission that will be launched in September 2024 to Martian system, to bring back to Earth sample from Phobos, to observe in detail Phobos and Deimos and to monitor Mars’s atmosphere with observations of dust storm, clouds, and distributions of total amount of water vapor. The main objectives of the mission are to understand the origin of Martian moons, to constrain the processes for planetary formation and to understand the evolutionary processes of the Martian system. MIRS is a push-broom imaging spectrometer working in the range from 0.9 to 3.6 micron.
We report on the development of the liquid nitrogen cooled hollow core waveguide (HCW) applicable for guiding midinfrared light from telescopes to the cryogenically cooled instruments with high transmittance. We employed a commercially available HCW, 2-m in length, transmitting 8 < λ < 13 μm in wavelength (astronomical N-band), made of polyimide tube with inner diameter of 0.8mmφ coated with a thin glass clad with Ag coated with AgI. In the present study, we designed and fabricated a flexible triple tube capable of cooling the HCW with liquid nitrogen flow, preventing ambient water vapor condensation on both inner and outer surface. One end of the HCW was sealed with 2mmφ and 1mm thick AR-coated Ge window employed with a vacuum adhesive, while another end left open for evacuation inside the HCW. The transmittance of the liquid nitrogen cooled HCW was measured by using the light source: quantum cascade laser continuously oscillating at 10.4 μm in wavelength with ~50 mW, and a thermopile detector. We have found ~10% improvement of the transmittance at 77 K compared with the room temperature condition. The observed increase of HCW transmittance is in reasonable accordance with a theoretical prediction based on the Drude model and the experimental data for electrical conductivity of thin Ag film at low temperature.
We demonstrate a new design hollow optical fiber suitable for use on IR heterodyne spectroscopy in mid-infrared wavelength region. The spectral feature of the laser emission line and the system noise temperature obtained by heterodyne detection with hollow optical fiber is confirmed by a laboratory measurement. The system noise temperature less than 3000 K obtained by the experimental setup with the CO2 laser-based heterodyne system led by a hollow optical fiber is only ~100 % above the quantum limit. The hollow optical fiber allows heterodyne detection with a sufficient efficiency. This permits simplified fabrication, provides even more weight reduction. Further investigation is required for use of hollow optical fiber on the target source.
We present concept and laboratory demonstration of high-contrast apodization baffle for instruments to be carried on exploration missions of the solar system. The primary science objective of the high-contrast baffle is to reveal escape of atmosphere on Mars, while other faint objects around blight sources are potential targets. We diverted heritages studied for exoplanet science and instrumentation to this work. The apodization in this work is realized by edge with microscopic Gaussian shaped structure. A simulation to confirm the concept and design of the high-contrast apodization baffle was carried out. Then, a baffle which was consisting of transparent flat substrate and thin film of aluminum on it was manufactured. The experiment was executed with He-Ne laser with wavelength of 633 nm. As the result, it was demonstrated that the apodization by the Gaussian edge is significantly working to improve the contrast. Achieved contrast is better than 10-6.5 and 10-8 in θ > 0.5 degree and θ > 1 degree, respectively. These results satisfy the requirement for remote sensing of the atmospheric less on Mars.
We report the current status of small-telescope activities and the 1.8-m aperture telescope PLANETS project at Haleakala dedicated to planetary and exoplanetary observations. Continuous monitoring is essential to understand the planetary atmospheric phenomena, and therefore, own facilities with even small- and medium sized telescopes and instruments are important. On the summit of Mt. Haleakala, Hawaii, we are operating a 40 cm (T40) and 60 cm (T60) telescopes for measuring faint atmospheric features such as Io torus, Mercury, and so on. It has uniquely provided long-term Io torus activities for more than ten years. T60 is now observing planetary atmospheres in visible and infrared ranges. The polarization imager DIPOL-2 is also installed to measure the weak polarization of exoplanetary light. In addition, we are carrying out a 1.8-m off-axis telescope project PLANETS at Haleakala. This project is managed by the PLANETS Foundation (www.planets.life) is an international collaboration of several institutes from Japan, USA, Germany, Brazil, and France. This off-axis optical system enables very low-stray light contamination and high-contrast in data, i.e., "high dynamic range". It will achieve unrivaled scientific capabilities on coronagraphy and polarimetry, aimed at detecting exoplanet reflected light and tenuous planetary exo-atmospheres in the Solar system. The main mirror is Clearceram ZHS with a diameter of 1850 mm, which is now on the final polishing process. We completed the telescope design and wind analysis of the mechanical support and tracking. The "split-ring" mount is so stiff that it has a first vibration mode above 50 Hz.
We report the development of infrared Echelle spectrograph covering 1 - 4 micron and mid-infrared heterodyne
spectrometer around 10 micron installed on the 60-cm telescope at the summit of Haleakala, Hawaii (alt.=3000m). It is
essential to carry out continuous measurement of planetary atmosphere, such as the Jovian infrared aurora and the
volcanoes on Jovian satellite Io, to understand its time and spatial variations. A compact and easy-to-use high resolution
infrared spectrometer provide the good opportunity to investigate these objects continuously. We are developing an
Echelle spectrograph called ESPRIT: Echelle Spectrograph for Planetary Research In Tohoku university. The main
target of ESPRIT is to measure the Jovian H3+ fundamental line at 3.9 micron, and H2 nu=1 at 2.1 micron. The 256x256
pixel CRC463 InSb array is used. An appropriate Echelle grating is selected to optimize at 3.9 micron and 2.1 micron for
the Jovian infrared auroral observations. The pixel scale corresponds to the atmospheric seeing (0.3 arcsec/pixel). This
spectrograph is characterized by a long slit field-of-view of ~ 50 arcsec with a spectral resolution is over 20,000. In
addition, we recently developed a heterodyne spectrometer called MILAHI on the 60 cm telescope. MILAHI is
characterized by super high-resolving power (more than 1,500,000) covering from 7 - 13 microns. Its sensitivity is 2400
K at 9.6 micron with a MCT photo diode detector of which bandwidth of 3000 MHz. ESPRIT and MILAHI is planned to
be installed on 60 cm telescope is planned in 2014.
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