Results from and upgrades to the triple-etalon Fabry-Perot interferometer for OI 630-nm dayglow observations at Cerro Tololo

Details Results from and upgrades to the triple-etalon Fabry-Perot interferometer for OI 630-nm dayglow observations at Cerro Tololo Results from and upgrades to the triple-etalon Fabry-Perot interferometer for OI 630-nm dayglow observations at Cerro Tololo

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsa41a0290n&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SA41A-0290

Physics

0310 Airglow And Aurora, 0355 Thermosphere: Composition And Chemistry, 3360 Remote Sensing

Scientific paper

The Scientific Solutions triple-etalon air-gap Fabry-Perot Interferometer (FPI) has been installed at Cerro Tololo Interamerican Observatory (CTIO) in Chile to measure dayglow emissions from neutral oxygen at 630 nm, as a way of tracking thermospheric neutral winds. The instrument is designed to be operated remotely, using internet controls. It has yet to make the difficult dayglow Doppler measurements via remote operation, but analysis and equipment updates in 2007 have brought it much closer to that goal. A diffusion plate, to obtain diffuse integrated sunlight for data analysis, was delivered to Chile in Summer 2007. New instrument and data analysis in association with the University of Illinois has revealed more information about the remote operation parameters of the instrument. In addition, a new FPI calibration source was sent to Chile in Fall 2007. Previously, the instrument had used only a Helium-Neon laser (632.8 nm) for calibration, but a Cerium hollow cathode lamp, with an emission line at about 630.4 nm, will be added to the system. This will allow the system to be wavelength-calibrated and set much closer to the line of interest, making it significantly easier to detect the 630-nm emission. Both calibration sources will be active at the same time, and remotely switchable. The next step in data collection is to seek the 630-nm emission from nightglow, where the emission is very much easier to detect because of the lack of background light. This will show how the system responds to simple 630- nm emission, and make detecting that emission in dayglow (where it is surrounded by Solar Fraunhofer lines and copious background light) much easier. Instrument updates and current data analysis results will be presented in this talk.

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