The infrared astronomical mission AKARI

Publications- Astronomical Society of Japan (Impact Factor: 2.07). 08/2007; 59(sp2). DOI: 10.1093/pasj/59.sp2.S369
Source: arXiv


AKARI, the first Japanese satellite dedicated to infrared astronomy, was launched on 2006 February 21, and started observations in May of the same year. AKARI has a 68.5 cm cooled telescope, together with two focal-plane instruments, which survey the sky in six wavelength bands from the mid- to far-infrared. The instruments also have the capability for imaging and spectroscopy in the wavelength range 2 - 180 micron in the pointed observation mode, occasionally inserted into the continuous survey operation. The in-orbit cryogen lifetime is expected to be one and a half years. The All-Sky Survey will cover more than 90 percent of the whole sky with higher spatial resolution and wider wavelength coverage than that of the previous IRAS all-sky survey. Point source catalogues of the All-Sky Survey will be released to the astronomical community. The pointed observations will be used for deep surveys of selected sky areas and systematic observations of important astronomical targets. These will become an additional future heritage of this mission. Comment: 13 pages, 4 figures, and 3 tables. Accepted for publication in the AKARI special issue of the Publications of the Astronomical Society of Japan

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Available from: Pedro García-Lario, Oct 29, 2012
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    • "The Infrared Camera (IRC: Onaka et al. 2007) on board the AKARI satellite (Murakami et al. 2007) is composed of three channels (NIR, MIR-S, MIR-L) and has a capability of low-resolution (R=λ/∆λ~20-120) spectroscopy (Ohyama et al. 2007) in addition to the deep imaging pointed observation in the near-to mid-infrared. It provides both the slit-less spectroscopic data in its imaging field-of-view (FOV) (approximately 10'×10') and the slit spectroscopic data in the small slit areas which are settled just next to the FOV. "
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    ABSTRACT: Infrared Camera (IRC) onboard AKARI satellite has carried out more than 4000 pointed observations during the phases 1 and 2, a significant amount of which were performed in the spectroscopic mode. In this paper, we investigate the properties of the spectroscopic data taken with MIR-S channel and propose a new data reduction procedure for slit-less spectroscopy of sources embedded in complicated diffuse background structures. The relative strengths of the 0th to 1st order light as well as the efficiency profiles of the 2nd order light are examined for various objects taken with MIR-S dispersers. The boundary shapes of the aperture mask are determined by using the spectroscopic data of uniform zodiacal emission. Based on these results, if the appropriate template spectra of zodiacal light emission and the diffuse background emission are prepared and the geometries of the diffuse structures are obtained by the imaging data, we can reproduce the slit-less spectroscopic patterns made by a uniform zodiacal emission and the diffuse background emission by a convolution of those template profiles. This technique enables us to obtain the spectra of infrared sources in highly complicated diffuse background and/or foreground structures, such as in the Galactic plane and in nearby galaxies.
    Full-text · Article · Aug 2008 · Proceedings of SPIE - The International Society for Optical Engineering
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    • "The space infrared telescope for cosmology and astrophysics (SPICA) mission [1] [2], as illustrated in Fig. 1, has been proposed to the Japan aerospace exploration agency (JAXA) as the second Japanese infrared (IR) space telescope to be launched in the mid- 2010s, following the successful AKARI (previously called the AS- TRO-F) mission launched in 2006 [3]. The SPICA spacecraft, launched with an H-IIA launch vehicle, is to be transferred into a halo orbit around the Sun–Earth L2 (second Lagrangian point), where effective radiant cooling is feasible owing to solar rays and radiant heat fluxes from the Earth constantly coming from the same direction. "
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    ABSTRACT: The next Japanese infrared space telescope SPICA features a large 3.5-m-diameter primary mirror and an optical bench cooled to 4.5 K with advanced mechanical cryocoolers and effective radiant cooling instead of using a massive and short-lived cryogen system. To obtain a sufficient thermal design margin for the cryogenic system, cryocoolers for 20 K, 4 K, and 1 K have been modified for higher reliability and higher cooling power. The latest results show that all mechanical cryocoolers achieve sufficient cooling capacity for the cooling requirement of the telescope and detectors on the optical bench at the beginning of life. Consequently, the feasibility of the SPICA cryogenic system concept was validated, while attempts to achieve higher reliability, higher cooling capacity and less vibration have continued for stable operations at the end of life.
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