Japan Geoscience Union Meeting 2016

Presentation information


Symbol P (Space and Planetary Sciences) » P-CG Complex & General

[P-CG21] Planetary atmosphere, ionosphere and magnetosphere

Wed. May 25, 2016 3:30 PM - 5:00 PM 101A (1F)

Convener:*Takeshi Imamura(Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science), Yukihiro Takahashi(Department of Cosmosciences, Graduate School of Science, Hokkaido University), Yoshiyuki O. Takahashi(Graduate School of Science, Kobe University), Keiichiro Fukazawa(Academic Center for Computing and Media Studies, Kyoto University), Hiromu Nakagawa(Planetary Atmosphere Physics Laboratory, Department of Geophysics, Graduate School of Science, Tohoku University), Chair:Hiromu Nakagawa(Planetary Atmosphere Physics Laboratory, Department of Geophysics, Graduate School of Science, Tohoku University)

4:15 PM - 4:30 PM

[PCG21-04] Initial results of IR2 camera on board Akatsuki

*Takehiko Satoh1, Makoto Suzuki1, Yasumasa Kasaba3, Munetaka UENO2, George HASHIMOTO4, Takao M. Sato1, Takayuki Enomoto5 (1.Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 2.Kobe University, 3.Tohoku University, 4.Okayama University, 5.SOKENDAI)

Keywords:Venus atmosphere, near-infrared, cloud property, CO

Akatsuki, after its successful orbit insertion on 7 Dec 2015, is under the initial check-out phase. IR2, a 2-um camera on board Akatsuki, is to investigate the Venusian atmospheric dynamics, distribution of the trace gas, aerosol properties and mechanisms of their production and maintenance.
The detector of IR2 is a 1024x1024 pixels PtSi (17-um pixel pitch), combined with the f=84.2 mm lens (F/4, Nikon). The field of view is a square of 12 degrees on a side. To suppress the dark current in PtSi, it is cooled to ~65 K, while the optics including filters are < 190 K to reduce the infrared radiation. Such cooling is achieved by a single-stage Stirling cooler from Sumitomo Heavy Industries, the company responsible to the entire IR2 system.
IR2 has 4 Venus filters: 1.735, 2.26, and 2.32 um are for the night-side of Venus. These "windows" are wavelength regions where CO2 absorption is relatively weak and the thermal emissions originating the lower atmosphere can leak to the space. Therefore, these windows allow imaging of lower clouds as silhouette and enable measurements of atmospheric dynamics in deeper levels. The 2.32-um filter, in CO absorption band, allows to map the distribution of CO in the lower atmosphere. We de-cloud by differentiating 2.32-um image from nearly-simultaneous 2.26-um image.
The 2.02-um filter for the day-side allows the cloud top altimetry by utilizing the stron CO2 absorption.
In this paper, we present initial results of data analysis acquired during the check-out phase, and will present the latest data from the orbit.