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Title:
The Submillimeter Wave Astronomy Satellite (SWAS): Results from the First Six Months of Operations
Authors:
Melnick, G. J.; Stauffer, J. R.; Ashby, M. L. N.; Bergin, E.; Kleiner, S.; Patten, B.; Plume, R.; Tolls, V.; Wang, Z.; Zhang, Y.; Erickson, N.; Howe, J.; Snell, R.; Goldsmith, P.; Harwit, M.; Koch, D. G.; Neufeld, D. A.; Schieder, R.; Winnewisser, G.; Chin, G.
Affiliation:
AA(Harvard-Smithsonian CfA), AB(Harvard-Smithsonian CfA), AC(Harvard-Smithsonian CfA), AD(Harvard-Smithsonian CfA), AE(Harvard-Smithsonian CfA), AF(Harvard-Smithsonian CfA), AG(Harvard-Smithsonian CfA), AH(Harvard-Smithsonian CfA), AI(Harvard-Smithsonian CfA), AJ(Harvard-Smithsonian CfA), AK(U. Massachusetts), AL(U. Massachusetts), AM(U. Massachusetts), AN(Cornell U.), AO(Cornell U.), AP(NASA Ames), AQ(Johns Hopkins U.), AR(U. Cologne), AS(U. Cologne), AT(NASA GSFC)
Publication:
American Astronomical Society, 194th AAS Meeting, #47.08; Bulletin of the American Astronomical Society, Vol. 31, p.889
Publication Date:
05/1999
Origin:
AAS
Bibliographic Code:
1999AAS...194.4708M

Abstract

The Submillimeter Wave Astronomy Satellite (SWAS), a NASA Small Explorer class mission dedicated to the study of star formation and interstellar chemistry, has recently completed its first six months of operations. During this time SWAS has observed a number of galactic regions, including OMC-1, M17, and Sgr B2, at five frequencies corresponding to either the ground-state or a low-lying transition of H_2O 1_{1,0}-1_{0,1} (557 GHz), (13) CO J = 5-4 (551 GHz), H_2(18) O 1_{1,0}-1_{0,1} (548 GHz), O_2 (J,N) = (3,3)-(2,2) (487 GHz), and [CI] (3) P_1-(3) P_0 (492 GHz). SWAS employs two independent Schottky barrier diode mixers cooled to 170 K coupled to a 52 x 68 cm off-axis Cassegrain antenna. The SWAS beamsizes are measured to be 3.2' x 4.5' at 551 GHz and 3.6' x 5.0' at 492 GHz with very good (> 20 dB) sidelobe supression. The backend is a 1.4 GHz bandwidth acousto-optical spectrometer which yields a velocity resolution of 1 km s(-1) . We report on our progress to date including the detection of water toward most regions observed along with large-scale maps of CI and (13) CO toward OMC-1, M17, and Sgr B2.
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