The infrared astronomical mission AKARI

The infrared astronomical mission AKARI
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DOI:
10.1093/pasj/59.sp2.s369
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发表时间:
2007-08
影响因子:
2.3
通讯作者:
H. Murakami;H. Baba;P. Barthel;D. Clements;M. Cohen;Y. Doi;K. Enya;E. Figuerêdo;N. Fujishiro;N. Fujishiro;H. Fujiwara;M. Fujiwara;P. Garcı́a-Lario;T. Goto;S. Hasegawa;Y. Hibi;T. Hirao;N. Hiromoto;S. Hong;K. Imai;M. Ishigaki;M. Ishiguro;D. Ishihara;Y. Ita;W. Jeong;K. S. Jeong;H. Kaneda;H. Kataza;M. Kawada;Toshihide Kawai;A. Kawamura;M. Kessler;D. Kester;T. Kii;Dong Chan Kim;Woojung Kim;Hisato Kobayashi;Hisato Kobayashi;B. Koo;S. Kwon;Hyung-Mok Lee;R. Lorente;S. Makiuti;H. Matsuhara;T. Matsumoto;H. Matsuo;S. Matsuura;T. Müller;N. Murakami;H. Nagata;T. Nakagawa;T. Naoi;M. Narita;M. Noda;S. Oh;A. Ohnishi;Y. Ohyama;Y. Okada;H. Okuda;S. Oliver;T. Onaka;T. Ootsubo;S. Oyabu;S. Pak;Yong-Sun Park;C. Pearson;C. Pearson;M. Rowan‐Robinson;T. Saito;T. Saito;I. Sakon;A. Salama;S. Sato;R. Savage;S. Serjeant;H. Shibai;M. Shirahata;Jungjoo Sohn;Toyoaki Suzuki;Toyoaki Suzuki;T. Takagi;H. Takahashi;T. Tanabé;T. Takeuchi;S. Takita;S. Takita;M. Thomson;K. Uemizu;M. Ueno;F. Usui;E. Verdugo;T. Wada;Lingyu Wang;T. Watabe;H. Watarai;G. White;G. White;I. Yamamura;C. Yamauchi;A. Yasuda;A. Yasuda
H. Murakami;H. Baba;P. Barthel;D. Clements;M. Cohen;Y. Doi;K. Enya;E. Figuerêdo;N. Fujishiro;N. Fujishiro;H. Fujiwara;M. Fujiwara;P. Garcı́a-Lario;T. Goto;S. Hasegawa;Y. Hibi;T. Hirao;N. Hiromoto;S. Hong;K. Imai;M. Ishigaki;M. Ishiguro;D. Ishihara;Y. Ita;W. Jeong;K. S. Jeong;H. Kaneda;H. Kataza;M. Kawada;Toshihide Kawai;A. Kawamura;M. Kessler;D. Kester;T. Kii;Dong Chan Kim;Woojung Kim;Hisato Kobayashi;Hisato Kobayashi;B. Koo;S. Kwon;Hyung-Mok Lee;R. Lorente;S. Makiuti;H. Matsuhara;T. Matsumoto;H. Matsuo;S. Matsuura;T. Müller;N. Murakami;H. Nagata;T. Nakagawa;T. Naoi;M. Narita;M. Noda;S. Oh;A. Ohnishi;Y. Ohyama;Y. Okada;H. Okuda;S. Oliver;T. Onaka;T. Ootsubo;S. Oyabu;S. Pak;Yong-Sun Park;C. Pearson;C. Pearson;M. Rowan‐Robinson;T. Saito;T. Saito;I. Sakon;A. Salama;S. Sato;R. Savage;S. Serjeant;H. Shibai;M. Shirahata;Jungjoo Sohn;Toyoaki Suzuki;Toyoaki Suzuki;T. Takagi;H. Takahashi;T. Tanabé;T. Takeuchi;S. Takita;S. Takita;M. Thomson;K. Uemizu;M. Ueno;F. Usui;E. Verdugo;T. Wada;Lingyu Wang;T. Watabe;H. Watarai;G. White;G. White;I. Yamamura;C. Yamauchi;A. Yasuda;A. Yasuda
中科院分区:
物理与天体物理4区
文献类型:
--
作者:
H. Murakami;H. Baba;P. Barthel;D. Clements;M. Cohen;Y. Doi;K. Enya;E. Figuerêdo;N. Fujishiro;N. Fujishiro;H. Fujiwara;M. Fujiwara;P. Garcı́a-Lario;T. Goto;S. Hasegawa;Y. Hibi;T. Hirao;N. Hiromoto;S. Hong;K. Imai;M. Ishigaki;M. Ishiguro;D. Ishihara;Y. Ita;W. Jeong;K. S. Jeong;H. Kaneda;H. Kataza;M. Kawada;Toshihide Kawai;A. Kawamura;M. Kessler;D. Kester;T. Kii;Dong Chan Kim;Woojung Kim;Hisato Kobayashi;Hisato Kobayashi;B. Koo;S. Kwon;Hyung-Mok Lee;R. Lorente;S. Makiuti;H. Matsuhara;T. Matsumoto;H. Matsuo;S. Matsuura;T. Müller;N. Murakami;H. Nagata;T. Nakagawa;T. Naoi;M. Narita;M. Noda;S. Oh;A. Ohnishi;Y. Ohyama;Y. Okada;H. Okuda;S. Oliver;T. Onaka;T. Ootsubo;S. Oyabu;S. Pak;Yong-Sun Park;C. Pearson;C. Pearson;M. Rowan‐Robinson;T. Saito;T. Saito;I. Sakon;A. Salama;S. Sato;R. Savage;S. Serjeant;H. Shibai;M. Shirahata;Jungjoo Sohn;Toyoaki Suzuki;Toyoaki Suzuki;T. Takagi;H. Takahashi;T. Tanabé;T. Takeuchi;S. Takita;S. Takita;M. Thomson;K. Uemizu;M. Ueno;F. Usui;E. Verdugo;T. Wada;Lingyu Wang;T. Watabe;H. Watarai;G. White;G. White;I. Yamamura;C. Yamauchi;A. Yasuda;A. Yasuda

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AKARI是日本第一颗专门用于红外天文学的卫星,于2006年2月21日发射,并于同年5月开始观测。AKARI有一个68.5厘米的冷却望远镜,以及两个焦平面仪器,它们在从中红外到远红外的六个波长波段上观测天空。这些仪器还具有在2-180 μ m波长范围内以定点观测模式进行成像和光谱分析的能力,偶尔插入连续勘测操作。在轨冷冻剂寿命预计为一年半。此次巡天将覆盖整个天空的90%以上,比以往的IRAS巡天具有更高的空间分辨率和更宽的波长覆盖范围。全天巡天的点源目录将向天文学界公布。定点观测将用于选定天空区域的深度观测和重要天文目标的系统观测。这些将成为这一使命今后的额外遗产。
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 mid- to far-infrared. The instruments also have a capability for imaging and spectroscopy in the wavelength range 2-180 mu m in the pointed observation mode, occasionally inserted into a 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% of the whole sky with a higher spatial resolution and a 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. 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.