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Early Results from the Infrared Astronomical Satellite

Neugebauer, G. and Beichman, C. A. and Soifer, B. T. and Aumann, H. H. and Chester, T. J. and Gautier, T. N. and Gillett, F. C. and Hauser, M. G. and Houck, J. R. and Lonsdale, C. J. and Low, F. J. and Young, E. T. (1984) Early Results from the Infrared Astronomical Satellite. Science, 224 (4644). pp. 14-21. ISSN 0036-8075. https://resolver.caltech.edu/CaltechAUTHORS:20150209-072745081

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Abstract

For 10 months the Infrared Astronomical Satellite (IRAS) provided astronomers with what might be termed their first view of the infrared sky on a clear, dark night. Without IRAS, atmospheric absorption and the thermal emission from both the atmosphere and Earthbound telescopes make the task of the infrared astronomer comparable to what an optical astronomer would face if required to work only on cloudy afternoons. IRAS observations are serving astronomers in the same manner as the photographic plates of the Palomar Observatory Sky Survey; just as the optical survey has been used by all astronomers for over three decades, as a source of quantitative information about the sky and as a "roadmap" for future observations, the results of IRAS will be studied for years to come. IRAS has demonstrated the power of infrared astronomy from space. Already, from a brief look at a miniscule fraction of the data available, we have learned much about the solar system, about nearby stars, about the Galaxy as a whole and about distant extragalactic systems. Comets are much dustier than previously thought. Solid particles, presumably the remnants of the star-formation process, orbit around Vega and other stars and may provide the raw material for planetary systems. Emission from cool interstellar material has been traced throughout the Galaxy all the way to the galactic poles. Both the clumpiness and breadth of the distribution of this material were previously unsuspected. The far-infrared sky away from the galactic plane has been found to be dominated by spiral galaxies, some of which emit more than 50 percent and as much as 98 percent of their energy in the infrared—an exciting and surprising revelation. The IRAS mission is clearly the pathfinder for future missions that, to a large extent, will be devoted to the discoveries revealed by IRAS.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1126/science.224.4644.14DOIArticle
http://www.sciencemag.org/content/224/4644/14.abstractPublisherArticle
http://www.jstor.org/stable/1692863 JSTORArticle
Additional Information:© 1984 American Association for the Advancement of Science. It is a particular pleasure to thank our colleagues on the joint IRAS science team-H. Habing, B. Baud, D. A. Beintema, N. Boggess, P. E. Clegg, T. de Jong, J. Emerson, S. Harris, R. Jennings, P. Marsden, G. Miley, F. Olnon, S. Pottasch, E. Raimond, M. Rowan-Robinson, R. Walker, and P. Wesselius- for allowing us to review and describe their work. We also thank all of our colleagues on both sides of the Atlantic- scientist, engineers. and managers- who have helped make IRAS a success. Throughout the planning, development, fabrication, operations, and data analysis this has been an international project with a tremendous effort by all concerned. A project of the size and complexity of IRAS could not have been accomplished without the wholehearted cooperation of all the people and agencies involved.
Issue or Number:4644
Record Number:CaltechAUTHORS:20150209-072745081
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150209-072745081
Official Citation:Early Results from the Infrared Astronomical Satellite G. Neugebauer, C. A. Beichman, B. T. Soifer, H. H. Aumann, T. J. Chester, T. N. Gautier, F. C. Gillett, M. G. Hauser, J. R. Houck, C. J. Lonsdale, F. J. Low, and E. T. Young Science 6 April 1984: 224 (4644), 14-21. [DOI:10.1126/science.224.4644.14]
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:54510
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:09 Feb 2015 21:45
Last Modified:03 Oct 2019 07:58

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