Статья

THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE): MISSION DESCRIPTION AND INITIAL ON-ORBIT PERFORMANCE

E. L. WrightUCLA Astronomy, P.O. Box 951547, Los Angeles, CA 90095-1547, USA; [email protected]Peter EisenhardtJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAAmy MainzerJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAMichael E. ResslerJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAR. M. CutriInfrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USAT. H. JarrettInfrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USAJ. Davy KirkpatrickInfrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USADeborah PadgettInfrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USAR. S. McMillanUniversity of Arizona, 1629 East University Boulevard, Tucson, AZ 85721, USAMichael F. SkrutskieDepartment of Astronomy, University of Virginia, Charlottesville, VA 22903, USAS. A. StanfordInstitute of Geophysics and Planetary Physics, LLNL, Livermore, CA 94551, USAMartin CohenMonterey Institute for Research in Astronomy, 200 8th Street, Marina, CA 93933, USARussell G. WalkerMonterey Institute for Research in Astronomy, 200 8th Street, Marina, CA 93933, USAJohn C. MatherNASA Goddard Space Flight Center, Greenbelt, MD 20771, USADavid LeisawitzNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAT. N. GautierJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAIan S. McLeanUCLA Astronomy, P.O. Box 951547, Los Angeles, CA 90095-1547, USA; [email protected]Dominic J. BenfordNASA Goddard Space Flight Center, Greenbelt, MD 20771, USACarol J. LonsdaleNational Radio Astronomy Observatory, Charlottesville, VA 22903, USAA. W. BlainCalifornia Institute of Technology, Pasadena, CA 91125, USAB. J. MéndezSpace Sciences Laboratory, University of California, Berkeley, CA 94720, USAWilliam R. IraceJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAValérie DuvalJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAFengchuan LiuJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAD. RoyerJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAI. HeinrichsenJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAJoan HowardMark ShannonM. KendallAmy L. WalshM. F. LarsenSpace Dynamics Laboratory, 1695 North Research Park Way, North Logan, UT 84341, USAJoel CardonSpace Dynamics Laboratory, 1695 North Research Park Way, North Logan, UT 84341, USAScott SchickPractical Technology Solutions, Inc., P.O. Box 6336, North Logan, UT 8434, USAMark SchwalmL-3 Communications SSG-Tinsley, Wilmington, MA 01887, USAMohamed AbidJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USABeth FabinskyJet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USAL. G. NaesLockheed Martin Advanced Technology Center, Palo Alto, CA 94304, USAChao‐Wei TsaiInfrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA

2010en

ABI

Аннотация

The all sky surveys done by the Palomar Observatory Schmidt, the European Southern Observatory Schmidt, and\nthe United Kingdom Schmidt, the InfraRed Astronomical Satellite, and the Two Micron All Sky Survey have\nproven to be extremely useful tools for astronomy with value that lasts for decades. The Wide-field Infrared\nSurvey Explorer (WISE) is mapping the whole sky following its launch on 2009 December 14. WISE began\nsurveying the sky on 2010 January 14 and completed its first full coverage of the sky on July 17. The survey\nwill continue to cover the sky a second time until the cryogen is exhausted (anticipated in 2010 November).\nWISE is achieving 5σ point source sensitivities better than 0.08, 0.11, 1, and 6 mJy in unconfused regions on\nthe ecliptic in bands centered at wavelengths of 3.4, 4.6, 12, and 22μm. Sensitivity improves toward the ecliptic\npoles due to denser coverage and lower zodiacal background. The angular resolution is 6".1, 6".4, 6".5, and 12".0 at 3.4, 4.6, 12, and 22μm, and the astrometric precision for high signal-to-noise sources is better than 0".15.\n

Идентификаторы

DOI: 10.1088/0004-6256/140/6/1868

Цитирования и источники

Цитирований: 13Использованных источников: 0

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