Статья

The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images

Masaru MatsuokaKazuyoshi KawasakiShiro UenoHiroshi TomidaMitsuhiro Kohama1ISS Science Project Office, ISAS, JAXA, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505 [email protected]Motoko SuzukiYasuki AdachiMasaki IshikawaTatehiro Mihara2Cosmic Radiation Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama 351–198Mutsumi Sugizaki2Cosmic Radiation Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama 351–198Naoki Isobe2Cosmic Radiation Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama 351–198Yujin Nakagawa2Cosmic Radiation Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama 351–198Hiroshi Tsunemi3Department of Earth and Space Science, Osaka University , 1-1 Machikaneyama, Toyonaka, Osaka 560-0043Emi Miyata3Department of Earth and Space Science, Osaka University , 1-1 Machikaneyama, Toyonaka, Osaka 560-0043Nobuyuki Kawai4Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551Jun Kataoka4Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551Mikio Morii4Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551Atsumasa Yoshida5Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 229-8558Hitoshi Negoro6Department of Physics, Nihon University, 1-8-14, Kanda-Surugadai, Chiyoda-ku, Tokyo 101-8308Motoki Nakajima6Department of Physics, Nihon University, 1-8-14, Kanda-Surugadai, Chiyoda-ku, Tokyo 101-8308Yoshihiro Ueda7Department of Astronomy, Kyoto University, Oiwake-cho, Sakyo-ku, Kyoto 606-8502Hirotaka Chujo2Cosmic Radiation Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama 351–198Kazutaka Yamaoka5Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 229-8558Osamu Yamazaki5Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 229-8558Satoshi Nakahira5Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 229-8558Tetsuya You5Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 229-8558Ryoji Ishiwata6Department of Physics, Nihon University, 1-8-14, Kanda-Surugadai, Chiyoda-ku, Tokyo 101-8308Sho Miyoshi6Department of Physics, Nihon University, 1-8-14, Kanda-Surugadai, Chiyoda-ku, Tokyo 101-8308Satoshi Eguchi7Department of Astronomy, Kyoto University, Oiwake-cho, Sakyo-ku, Kyoto 606-8502Kazuo Hiroi7Department of Astronomy, Kyoto University, Oiwake-cho, Sakyo-ku, Kyoto 606-8502Haruyoshi KatayamaKen Ebisawa9Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510

2009en

ABI

Аннотация

Abstract The Monitor of All-sky X-ray Image (MAXI) mission is the first astronomical payload to be installed on the Japanese Experiment Module — Exposed Facility (JEM-EF or Kibo-EF) on the International Space Station. It has two types of X-ray slit cameras with wide FOVs and two kinds of X-ray detectors consisting of gas proportional counters covering the energy range of 2 to 30 keV and X-ray CCDs covering the energy range of 0.5 to 12 keV. MAXI will be more powerful than any previous X-ray All Sky Monitor payloads, being able to monitor hundreds of Active Galactic Nuclei. A realistic simulation under optimal observation conditions suggests that MAXI will provide all-sky images of X-ray sources of $\sim $20 mCrab ($\sim $7 $\times$ 10$^{-10} $erg cm$^{-2} $s$^{-1}$ in the energy band of 2–30 keV) from observations during one ISS orbit (90 min), $\sim $4.5 mCrab for one day, and $\sim $2 mCrab for one week. The final detectability of MAXI could be $\sim $0.2 mCrab for two years, which is comparable to the source confusion limit of the MAXI field of view (FOV). The MAXI objectives are: (1) to alert the community to X-ray novae and transient X-ray sources, (2) to monitor long-term variabilities of X-ray sources, (3) to stimulate multi-wavelength observations of variable objects, (4) to create unbiased X-ray source cataloges, and (5) to observe diffuse cosmic X-ray emissions, especially with better energy resolution for soft X-rays down to 0.5 keV.

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Идентификаторы

DOI: 10.1093/pasj/61.5.999

Цитирования и источники

Цитирований: 2Использованных источников: 0

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