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Solar Submillimeter and Millimeter Spectroscopy between 7 and 30 cm–1 from the James Clerk Maxwell Telescope

Published online by Cambridge University Press:  03 August 2017

D. A. Naylor ,
G. J. Tompkins ,
T. A. Clark ,
G. R. Davis  and
W. D. Duncan
D. A. Naylor
Affiliation:
Department of Physics, University of Lethbridge, Lethbridge, Alberta T1K 3M4, Canada
G. J. Tompkins
Affiliation:
Department of Physics, University of Lethbridge, Lethbridge, Alberta T1K 3M4, Canada
T. A. Clark
Affiliation:
Physics Department, University of Calgary, Calgary, Alberta T2N 1N4, Canada
G. R. Davis
Affiliation:
University of Saskatchewan, Saskatoon, Saskatchewan S7N 0W0, Canada
W. D. Duncan
Affiliation:
Joint Astronomy Centre, University Park, Hilo, HI 96720, U.S.A.

Abstract

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A two-beam Martin-Puplett polarizing interferometer has been used in the rapid-scan mode on the 15 meter JCMT in conjunction with the facility detector, UKT14, to survey the solar sub-millimeter and millimeter spectrum in the four wavebands at 7-11, 11-15, 21-24 and 27-30 cm–1 to a spectral resolution of 0.01 cm–1 and at spatial resolutions of 19″, 16″, 7″ and 6″, respectively. Overall atmospheric transmission through these windows has been evaluated by comparison with synthetic spectra generated with FASCOD/HITRAN. A search has been made for contributions to these spectra from high-n transitions of H and heavier elements by several methods, including the comparison of solar with lunar and limb with disk center spectra.

Keywords

infrared: starsinstrumentation: interferometricSun: radio radiation
Type
Part 4: Infrared Atomic Physics and Line Formation
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 371 - 376
Copyright
Copyright © Kluwer 1994 

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