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Observation of the Airglow from the ISS by the IMAP Mission *Y

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Observation of the Airglow from the ISS by the IMAP Mission *Y 2013/3/13(ANGWIN workshop, Tachikawa) Observation of the airglow from the ISS by the IMAP mission *Y. Akiya [1], A. Saito [1], T. Sakanoi [2], Y. Hozumi [1], A. Yamazaki [3], Y. Otsuka [4] [1] Graduation School of Science, Kyoto University , [2] PPARC, Tohoku University, [3] ISAS/JAXA, [4] STE Laboratory, Nagoya University ----- Outline ----- Introduction of the IMAP mission Visible and near-infrared spectrographic imager Samples of airglow observation by VISI Summary “ISS-IMAP” mission Ionosphere, Mesosphere, Upper atmosphere and Plasmasphere Imagers of the ISS-IMAP mapping mission from the mission International Space Station (ISS) Observational imagers were installed on the Exposure Facility of Japanese Experimental Module: August 9th, 2012. Initial checkout: August and September, 2012 Nominal observations: October, 2012 - [Pictures: Courtesy of JAXA/NASA] [this issue]. According to characteristics of airglow emissions, wavelength range from 630 to 762 nm. Typical total intensity of such as intensity, emission height, background continuum, etc., we airglow is 100 1000 R as listed in Table 1, and 10 % variation of selected the airglow emissions which will be measured with VISI, the total intensity must be detected in order to investigate the and determined the requirements for instrumental design. The airglow variation pattern. In addition, short exposure cycle less targets and requirements are summarized in Table 1. than several seconds is necessary to measure small-scale airglow Table 1. Scientific Targets of VISI signatures (see Table 1) considering the orbital speed of ISS (~8 km/s). Airglow Required Region Scientific Typical A sectional view of VISI and its specifications are given in (waele- spatial (height) target intensity Figure 4 and Table 2, respectively. A grism imaging spectrometer ngth) resolution that consists of fast and distortion-free objective lens (F/0.96), upper- gravity two-line-slits, collimator and CCD sensor is designed to meet the O thermosphere wave, 50 km 100 R* high sensitivity, the wide wavelength coverage, the spatial (630nm)“ISS-IMAP” and ionosphere ionospheric mission resolution requirements, and the wide field-of-view (90 degrees). (250 km) disturbances The optical system of VISI is optimized at the off-axis gravity OH mesopause field-of-view, not around the optical center axis. In normal optics, Two imagerswave, are 32set km in1000 MCE R and (730nm) (85 km) image quality is the best around the optical axis, and it is degraded temperature EUVI toward the edge of field-of-view. However, both forward and observelower- from the Exposure O2 400 field-of-views of VISI are 45 degrees off-axis separated from the thermospehre gavity wave 32 km (762nm)Facility of Japanese ExperimentR/nm optical center axis, and incident light around the optical axis is not (95km) used. Thus, we gained the sensitivity at the off-axis field-of-views 6 2 Module*R: Rayleigh (10 /4/ on photons/cm the/str/s) ISS. by using some aspherical lenses in the optics. In addition, a distortion-fee optical system is adopted to minimize distortions. Smile distortion is estimated to be better than 5 pixels. All VISI (Visible and near-infrared surfaces of optical material are space qualified anti-reflection spectrographic imager) observes(AR) coated. Total throughputs of this optics including a bend mirror and a grims (absolute efficiency of VISI~0.63) are 0.47 at 630 airglow emission with line nm and 0.53 at 762 nm. scanningFig. 2. (left) Kibo in Exposedthe module.nadir MCE direction. will be mounted to the port at top-right. (right) Constituents of MCE. EUVI (Extreme ultraviolet 2.1 Mission Overview Kibo EF has several ports to install imager)payloads, and MCE observes will be mounted resonance to one of them as shown in Figure 1. MCE is a complex module consisting of five instruments.scattering VISI is installed lightat the bottom from of MCE plasma to look down in to the earth. ISS is orbiting at an altitude range of 350 450 km with a theperiod ofupper ~90 min and atmosphere an inclination of 52 degrees in rangingthe from +51.6 to 51.6 degrees in geographical latitude. As shown in limb direction. Figure 3, VISI has two field-of-views pointing 45 degrees forward Fig. 3. Schematic drawing of the field-of-of vies and 45 degrees backward of the orbital direction. Due to the height [Sakanoi et al., 2011] of VISI mapped at the emission layers. difference between ground/clouds and airglow emission layers, the spatial relationship between the structure of ground and cloud reflections and airglow pattern seen in the forward field-view data Table 2. Specifications of VISI should be displaced to that seen in the backward field-view data. Rectangular-shaped (90 x 0.09 degrees) In this way, we subtract the background contaminations from Field-of-view field-of-views pointing 45 degrees forward and measured data. Each field-of-view has a wide viewing angle (90 45 degrees backward (see Figure 3) degrees) perpendicular to the orbital plane whose mapped widths Objective lens F/0.96, and f= 5.5 mm are ~600 km at an altitude of 95 km and ~300 km, respectively. Spectroscopic Wavelength coverage 630 762 nm with VISI will perform line-scanning for forward and backward properties resolution of ~1.0 nm/pixel (R~800) field-of-views, that is, continuous measurement of airglow e2V 47-20 back-illuminated AIMO, 1024 x 1024 CCD sensor emissions in nighttime. Successive exposure operation at an pixels, 1 pixel size=13.3 x 13.3 um interval of a few to several sec (described later) contributes to Below -25 deg. C with a Peltier electrical cooling CCD cooling obtain seamless scanning images for the airglow emissions in the connected to a radiator toward the earth nightside hemisphere. Size 450 (X) x 240 (Y) x 210 (Z) * Weight and power 14.5 kg, 7.9 W 3. Instrumental Design * X, Y, Z directions are in the ISS coordinate system. VISI optics is designed to have sufficient sensitivity in order to achieve two line-scannings of faint airglow emissions in the A bend mirror is adopted to stabilize the instrument for 2 IEEJ Trans. , Vol., No., [http://eol.jsc.nasa.gov] Airglow Aurora EUVI-FOV VISI-FOV Extreme Ultraviolet Imager (EUVI) Resonant scattering: 83.4 nm (O+), 30.4 nm (He+) Observation in the day side and the night side Limb observation in backward FOV 15 deg. Weight: 19.3 kg, Size: 170 mm X 370 mm X 480 mm Initial test of EUVI: Lid close on August 11, 2012 EUVI He+ (September 26, 2012 07:26UT) Visible and near-infrared spectrographic imager (VISI) Airglow: O (630 nm), OH (8-3 band around 730 nm), O2 (762 nm) Observation in the night side Nadir direction observation with FOVs pointing 45 degrees forward and 45 degrees backward Weight: 14.5 kg, Size: 170 mm X 370 mm X 480 mm Several observational mode CCD ISS moving direction Backward FOV Forward FOV Observational mode of VISI Calibration mode Calibration mode Images are read out without binning. Full frame data are recorded. Exposure time: 2 - 4 seconds Spectral mode Data at three ROIs (ROI = Region of interest) determined in the forward FOV and three ROIs in the backward FOV are recorded. Exposure time: 1 - 6 seconds Binning: 8, 16, 32 pixels in spatial direction Peak mode The peak and background on each spectrum in the ROIs are determined and recorded. Left: Spectral mode Exposure time and binning are same as Right: Peak mode spectral mode. Averaged intensity of calibration data spectrum Averaged for 56 calibration mode data 400 taken from August to Forward FOV [6] December, 2012. Backward FOV 300 [1] 557.7nm(O) [2] 589.6nm(Na) [9] [3] 630.0nm(O) 200 [1] [4] 636.4nm(O) [2] Intensity [R/nm] [3] [5] [7] [5] 732.0nm(O+) 100 [4] [8] [6] 761.9nm(O2) 0 [7] 777.4nm(O) 500 600 700 800 900 [8] 844.6nm(O) Wavelength [nm] [9] 864.5nm (O2) Averaged intensity of OH band emissions Average of 56 calibration mode data taken from 70 Forward FOV August to December, [6] Backward FOV 2012. 60 [2][3] [5] [1] 7-1 (560-570nm) [1] [4] 50 [2] 8-2 (590-600nm) [7] 40 [8] [3] 5-0, 9-3 (620-640nm) 30 [4] 6-1 (650-670nm) Intensity [R/nm] 20 [5] 7-2 (690-705nm) 10 [6] 8-3, 4-0, 9-4, 5-1 (720-810 nm) 0 500 600 700 800 900 [7] 6-2 (840-860nm) Wavelength [nm] [8] 7-3 (880-900nm) 762-nm Peak mode observation Observation around 2012/9/25 02:15 UT 762-nm (95 km altitude) Background 630-nm Peak mode observation Observation around 2012/9/25 02:15 UT 630-nm (250 km altitude) Background Calibration and flattening of observational data White pixels are already 1000 subtracted from the observational data. Two strong lines are seen in the 800 762-nm forward FOV peak image. These are also seen in background images. Counts 600 The strength of this effect is not uniform in the same observation. Strength is Coordinate [pixel] affected by the intensity of the 400 light passed the optical system. 0 10 20 30 40 50 60 Summary ISS-IMAP mission started the observation of the upper atmosphere in August. Nominal observations by VISI and EUVI has been carried out. VISI observes the airglow in the nadir direction with two field of views. Target is the airglow originated from the atomic oxygen (630-nm wavelength), OH molecules (0-0 band) and oxygen molecules (762- nm wavelength). It is able to observe 557.7-nm emission from the atomic oxygen, Na emission and other OH band emissions in calibration mode observation.
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