The ATMOS (atmospheric trace molecule spectroscopy) instrument, a high speed
Fourier transform spectrometer operating in the middle IR (2.2–16
μm), recorded more than 1500 solar spectra at
~0.0105-cm−1 resolution during its first mission onboard
the shuttle Challenger in the spring of 1985. These spectra were acquired during
high sun conditions for studies of the solar atmosphere and during low sun
conditions for studies of the earth’s upper atmosphere. This paper
describes the steps by which the telemetry data were converted into spectra
suitable for analysis, the analysis software and methods developed for the
atmospheric and solar studies, and the ATMOS data analysis facility.
Fredrick W. Irion, Michael R. Gunson, Geoff C. Toon, Albert Y. Chang, Annmarie Eldering, Emmanuel Mahieu, Gloria L. Manney, Hope A. Michelsen, Elizabeth J. Moyer, Michael J. Newchurch, Gregory B. Osterman, Curtis P. Rinsland, Ross J. Salawitch, Bhaswar Sen, Yuk L. Yung, and Rodolphe Zander Appl. Opt. 41(33) 6968-6979 (2002)
You do not have subscription access to this journal. Cited by links are available to subscribers only. You may subscribe either as an Optica member, or as an authorized user of your institution.
You do not have subscription access to this journal. Figure files are available to subscribers only. You may subscribe either as an Optica member, or as an authorized user of your institution.
You do not have subscription access to this journal. Article tables are available to subscribers only. You may subscribe either as an Optica member, or as an authorized user of your institution.
You do not have subscription access to this journal. Equations are available to subscribers only. You may subscribe either as an Optica member, or as an authorized user of your institution.
An optical filter isolating a narrower wavelength region is used to
record each occultation. The spectral coverages of the four filters most
frequently used during Spacelab 3 are 600–1200,
1100–2000, 1580–3400, and 3100–4700
cm−1.
Table II
Molecular Parameters Adopted for the Calculation of the Temperature
Dependences of Line Intensities and Linewldths
Molecule No.
Molecule Name
α
β
Frequencies
(cm−1) of the Normal Vibrations and their
degrees of degeneracy (in parentheses)
Average of Values for the a and s levels.
Torsional mode excluded in the vibrational partition function
calculations. Its contribution to the internal partition function has
been incorporated into the value of β.
Normal modes are for trans-HONO.
Vibrational assignments have not been reported.
Arbitrary values of 100 cm−1 have been assumed for the
unassigned modes.
Differing assignments for the fundamentals have been reported. The
identifications of Ref. 60 have
been assumed for the ν4,
ν5,
ν6, and
ν8 modes; the others are from
Ref. 61.The frequencies are
mostly from Ref. 62.
Tables (2)
Table I
Characteristics of the ATMOS Fourier Transform Spectrometer
An optical filter isolating a narrower wavelength region is used to
record each occultation. The spectral coverages of the four filters most
frequently used during Spacelab 3 are 600–1200,
1100–2000, 1580–3400, and 3100–4700
cm−1.
Table II
Molecular Parameters Adopted for the Calculation of the Temperature
Dependences of Line Intensities and Linewldths
Molecule No.
Molecule Name
α
β
Frequencies
(cm−1) of the Normal Vibrations and their
degrees of degeneracy (in parentheses)
Average of Values for the a and s levels.
Torsional mode excluded in the vibrational partition function
calculations. Its contribution to the internal partition function has
been incorporated into the value of β.
Normal modes are for trans-HONO.
Vibrational assignments have not been reported.
Arbitrary values of 100 cm−1 have been assumed for the
unassigned modes.
Differing assignments for the fundamentals have been reported. The
identifications of Ref. 60 have
been assumed for the ν4,
ν5,
ν6, and
ν8 modes; the others are from
Ref. 61.The frequencies are
mostly from Ref. 62.