Hostname: page-component-84b7d79bbc-g5fl4 Total loading time: 0 Render date: 2024-07-27T12:31:18.670Z Has data issue: false hasContentIssue false
  • English
  • Français

The ASTRO-F (IRIS) Mission

Published online by Cambridge University Press:  13 May 2016

Hiroshi Shibai
Hiroshi Shibai*
Affiliation:
Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

ASTRO-F (IRIS) is the first Japanese satellite dedicated to infrared astronomy. The primary purpose of this project is to investigate the birth and evolution of galaxies in the early universe through deep, wide-field surveys at wavelengths ranging from 2 to 200 microns. The spatial resolution and the point source sensitivity are nearly the same as those of the aperture diffraction limit and the natural background and/or confusion limit, respectively. In the far-infrared wavelength band, ASTRO-F will conduct an all-sky survey like the IRAS survey with several tens of times higher sensitivity and several times better spatial resolution. In the near- and mid-infrared, wide area sky-surveys will be conducted over pre-selected portions of the sky. In addition to these photometric surveys, low-resolution spectroscopic capabilities are available for all wavelength bands. The ASTRO-F mission will produce a fundamental database for the next generation of advanced observatories, for example FIRST, and NGST, and will complement the SIRTF mission by virtue of its wide sky coverage. The launch by an M-V rocket is scheduled for February or March of 2004.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 204: The Extragalactic Infrared Background and its Cosmological Implication , 2001 , pp. 455 - 466
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Becklin, E. E. 1998, SPIE, 3356, 492 Google Scholar
COBE DIRBE Explanatory Supplement. 1994, available at nssdca.gsfc.nasa.gov.Google Scholar
Fanson, J. L., et al. 1998, SPIE, 3356, 478 Google Scholar
Kawada, M. 1998, SPIE, 3354, 905 Google Scholar
Kessler, M. 1996, A&A, 315, L27 Google Scholar
Matsuhara, H. 1998, SPIE, 3354, 915 Google Scholar
Murakami, H., et al. 1996, PASJ, 48, L41 CrossRefGoogle Scholar
Murakami, H. 1998, SPIE, 3356, 471 Google Scholar
Nakagawa, T., et al. 1998, SPIE, 3356, 462 Google Scholar
Neugebauer, G., et al. 1984, ApJ, 278, L1 Google Scholar
Onaka, T., et al. 1998, SPIE, 3354, 900 Google Scholar
Pilbratt, G. L. 1998, SPIE, 3356, 452 Google Scholar
Seery, B. D., & Smith, E. P. 1998, SPIE, 3356, 2 Google Scholar
Shibai, H. 2000, Adv. Sp. Res., 25, 2273 Google Scholar
Takeuchi, T. 1999, PASP, 51, 81 Google Scholar