00-027

Cover Page/Proposal Summary

ROSS-99    NRA 99-OSS-01

Date Due: 5/3/99

NASA PROCEDURE FOR HANDLING PROPOSALS

This proposal shall be used and disclosed for evaluation purposes only, and a copy of this Government notice shall be applied to any reproduction or abstract thereof. Any authorized restrictive notices that the submitter places on this proposal shall also be strictly complied with. Disclosure of this proposal for any reason outside the Government evaluation purposes shall be made only to the extent authorized by the Government.

Proposal Type: New Proposal

Proposal Category: Laboratory

Major Equipment Proposal? No

Do you intend to submit an Education/Public Outreach (E/PO) proposal? No

Proposal Title:
Laboratory Spectroscopy of Carbon Dioxide in Support of Planetary Atmospheres Research

Abbreviated Proposal Title:
Lab Intensity Measurements of CO2 Bands

Principal Investigator:
Lawrence P. Giver
Atmospheric Physics Branch, Earth Science Div. N245-4
NASA Ames Research Center
Bldg. 245
Room 140
Moffett Field, CA 94035-1000
Phone: (650) 604-5231   Fax: (650) 604-3625   E-mail: giver@hertz2.arc.nasa.gov

SignatureDate
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Co-Investigators and Collaborators:
Type    Name    Affiliation    E-mail
Sci Co-I   Dr. Charles Chackerian Jr.   NASA-Ames Research Ctr.   cchackerian@mail.arc.nasa.gov
Sci Co-I   Dr. Richard S. Freedman   Space Physics Research Institute   freedman@hertz2.arc.nasa.gov
Sci Collab   Dr. Rohidas J. Kshirsagar   Bhabha Atomic Research Centre, Mumbai, India   rohidas@hertz2.arc.nasa.gov
Sci Collab   Dr. Linda R. Brown   Jet Propulsion Lab; Calif. Institute of Tech.   linda@regina.jpl.nasa.gov


Proposal Summary:

Near-infrared thermal emissions from the hot surface and lower atmosphere occur in Venus' nightside spectrum in the gaps between CO2 absorption bands. The CO2 bands in and near these emission windows are intrinsically very weak, but are nevertheless prominent features in Venus' spectrum because of the tremendous CO2 abundance in its atmosphere. Typically, analyses of these features in Venus' spectrum have to rely on unmeasured HITRAN and HITEMP intensity values; these intensities have been calculated by "direct numerical diagonalization" techniques based in part on measured intensities of the stronger CO2 bands. Using path lengths up to 1700 meters in our 25-meter base-path White cell, we have measured intensities of a number of these weak CO2 bands. We have recently finished first-time intensity measurements of the 5584 and 5687 wavenumber bands, and have preliminary intensity values for the 5858 and 5959 wavenumber bands. The 5687 and 5858 wavenumber bands form the low and high wavenumber boundaries of the 1.74 micron emission window in Venus' nightside spectrum. We propose to measure additional CO2 bands that will serve as inputs for improved DND computations of very weak band intensities in HITEMP, as well as being directly relevant for Venus' spectral analysis. Some bands in the 8000 to 12000 wavenumber region were measured about 30 years ago; we expect to make significant improvements for these bands using the higher signal/noise and higher resolution available now with our Bomem FTS instrument. We will also measure intensities of some weaker bands for the first time. Our lists of line intensity measurements and other results will be placed on the Planetary Data System node.