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The Wide-Field Infrared Explorer (Wire) Mission

Published online by Cambridge University Press:  25 May 2016

D.L. Shupe ,
P.B. Hacking ,
T. Herter ,
T.N. Gautier ,
P. Graf ,
C.J. Lonsdale ,
G.J. Stacey ,
S.H. Moseley ,
B.T. Soifer  and
M.W. Werner
...Show all authors
D.L. Shupe
Affiliation:
Infrared Processing and Analysis Center, Pasadena, CA
P.B. Hacking
Affiliation:
Jamieson Science & Engineering, Bethesda, MD
T. Herter
Affiliation:
Cornell University, Department of Astronomy, Ithaca, NY
T.N. Gautier
Affiliation:
Jet Propulsion Laboratory, Pasadena, CA
P. Graf
Affiliation:
Ball Technologies, Boulder, CO
C.J. Lonsdale
Affiliation:
Infrared Processing and Analysis Center, Pasadena, CA
G.J. Stacey
Affiliation:
Cornell University, Department of Astronomy, Ithaca, NY
S.H. Moseley
Affiliation:
Goddard Space Flight Center, Greenbelt, MD
B.T. Soifer
Affiliation:
California Institute of Technology, Pasadena, CA
M.W. Werner
Affiliation:
Jet Propulsion Laboratory, Pasadena, CA
J.R. Houck
Affiliation:
Cornell University, Department of Astronomy, Ithaca, NY

Extract

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The Wide-Field Infrared Explorer (WIRE) (Schember et al. 1996 and references within) is a small spaceborne telescope specifically designed to study the evolution of starburst galaxies. This powerful astronomical instrument will be capable of detecting typical starburst galaxies at z ∼ 0.5, ultraluminous infrared galaxies beyond a z ∼ 2, and luminous protogalaxies beyond z ∼ 5. The WIRE survey, to be conducted during a four month period in 1998, will cover over 100 deg2 of high Galactic latitude sky at 25 μm and 12 μm.

Type
Part 2. Survey Projects
Information
Symposium - International Astronomical Union , Volume 179: New Horizons from Multi-Wavelength Sky Surveys , 1998 , pp. 118 - 120
Copyright
Copyright © Kluwer 1998 

References

Schember, H., Kemp, J., Ames, H., Hacking, P., Herter, T., Everett, D., Sparr, L., and Fafaul, B., 1996, Infrared Technology and Applications XXII, SPIE Proceedings 2744, in press.Google Scholar
Soifer, B.T., & Neugebauer, G., 1991 Astron. J. 101, 354.Google Scholar