TY - JOUR
T1 - IR heterodyne spectrometer MILAHI for continuous monitoring observatory of Martian and Venusian atmospheres at Mt. Haleakalā, Hawaii
AU - Nakagawa, Hiromu
AU - Aoki, Shohei
AU - Sagawa, Hideo
AU - Kasaba, Yasumasa
AU - Murata, Isao
AU - Sonnabend, Guido
AU - Sornig, Manuela
AU - Okano, Shoichi
AU - Kuhn, Jeffrey R.
AU - Ritter, Joseph M.
AU - Kagitani, Masato
AU - Sakanoi, Takeshi
AU - Taguchi, Makoto
AU - Takami, Kosuke
N1 - Funding Information:
The authors would like to thank all members of the Infrared Heterodyne spectroscopy group at Tohoku University/University of Cologne, and Theodor Kostuik, and Timothy A Livengood (NASA/GSFC) for their contributions to the work described in this paper. The authors gratefully thank all members of Institute for Astronomy (IfA), Maui, University of Hawaii (UH), for their supports to the operation at the top of Mt. Haleakalā, Hawaii. A Japanese planetary research observatory, T60, became operational and was installed at Haleakalā Observatory to replace a facility at Iitate, Fukushima, damaged by the destructive 2011 earthquake, owing to a long-standing cooperation of IfA/UH. HN expresses our thanks to Director and staff of Higashi-Hiroshima 1.5 m-telescope for their support of validation test of the instrument. This work was supported by Tohoku University Global Education and Research Center for Earth and Planetary Dynamics Program, Nagoya University , Strategic Young Researcher Overseas Visits Program for Accelerating Brain Circulation Program, Japan Aerospace Exploration Agency/Institute of Space and Astronautical Science (JAXA/ISAS) , Solar-Terrestrial Environment Laboratory in Nagoya University , the Japanese Society for the Promotion of Science (JPSP) ( #22740320 , #25800271 , #22340142 , and #24403007 ), European Union FP7 CrossDrive Project .
Publisher Copyright:
© 2016 Elsevier Ltd.
Copyright:
Copyright 2016 Elsevier B.V., All rights reserved.
PY - 2016/7/1
Y1 - 2016/7/1
N2 - A new Mid-Infrared Laser Heterodyne Instrument (MILAHI) with >106 resolving power at 7-12 μm was developed for continuous monitoring of planetary atmospheres by using dedicated ground-based telescopes for planetary science at Mt. Haleakalā, Hawaii. Room-temperature-type quantum cascade lasers (QCLs) that cover wavelength ranges of 7.69-7.73, 9.54-9.59, and 10.28-10.33 μm have been newly installed as local oscillators to allow observation of CO2, CH4, H2O2, H2O, and HDO. Modeling and predictions by radiative transfer code gave the following scientific capabilities and measurement sensitivities of the MILAHI. (1) Temperature profiles are achieved at altitudes of 65-90 km on Venus, and the ground surface to 30 km on Mars. (2) New wind profiles are provided at altitudes of 75-90 km on Venus, and 5-25 km on Mars. (3) Direct measurements of the mesospheric wind and temperature are obtained from the Doppler-shifted emission line at altitudes of 110 km on Venus and 75 km on Mars. (4) Detections of trace gases and isotopic ratios are performed without any ambiguity of the reproducing the terrestrial atmospheric absorptions in the observed wavelength range. A HDO measurement of twice the Vienna Standard Mean Ocean Water (VSMOW) can be obtained by 15-min integration, while H2O of 75 ppm is provided by 3.62-h integration. The detectability of the 100 ppb-CH4 on Mars corresponds to an integration time of 32 h.
AB - A new Mid-Infrared Laser Heterodyne Instrument (MILAHI) with >106 resolving power at 7-12 μm was developed for continuous monitoring of planetary atmospheres by using dedicated ground-based telescopes for planetary science at Mt. Haleakalā, Hawaii. Room-temperature-type quantum cascade lasers (QCLs) that cover wavelength ranges of 7.69-7.73, 9.54-9.59, and 10.28-10.33 μm have been newly installed as local oscillators to allow observation of CO2, CH4, H2O2, H2O, and HDO. Modeling and predictions by radiative transfer code gave the following scientific capabilities and measurement sensitivities of the MILAHI. (1) Temperature profiles are achieved at altitudes of 65-90 km on Venus, and the ground surface to 30 km on Mars. (2) New wind profiles are provided at altitudes of 75-90 km on Venus, and 5-25 km on Mars. (3) Direct measurements of the mesospheric wind and temperature are obtained from the Doppler-shifted emission line at altitudes of 110 km on Venus and 75 km on Mars. (4) Detections of trace gases and isotopic ratios are performed without any ambiguity of the reproducing the terrestrial atmospheric absorptions in the observed wavelength range. A HDO measurement of twice the Vienna Standard Mean Ocean Water (VSMOW) can be obtained by 15-min integration, while H2O of 75 ppm is provided by 3.62-h integration. The detectability of the 100 ppb-CH4 on Mars corresponds to an integration time of 32 h.
KW - Heterodyne
KW - High spectral resolution
KW - Infrared
KW - Planetary atmospheres
KW - Spectroscopy
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U2 - 10.1016/j.pss.2016.04.002
DO - 10.1016/j.pss.2016.04.002
M3 - Article
AN - SCOPUS:84992310985
VL - 126
SP - 34
EP - 48
JO - Planetary and Space Science
JF - Planetary and Space Science
SN - 0032-0633
ER -