Richard A. Chamberlin (1), Bob Martin(2), Chris Martin (3) , and Tony
Stark(3).
Primary purpose in 2001: To measure the magnitude of the 1.5 THz atmospheric transmission window under various atmospheric conditions.
Technology: Our FTS is a polarizing Michelson interferometer of the Martin-Puplett type. For more information see:
booktitle = "Infrared and Millimeter Waves, Vol. 6: Systems and Components"
,
title="Polarizing Martin-Puplett Interferometric Spectrometers for
the Near and Submillimeter Spectra",
Publisher = "Academic Press",
Editor="K. E. Button",
Author = "D. H. Martin",
Year= "1982",
Pages= "66-148"
South Pole FTS in the CSO Hilo Base facility laboratory (April 2000).
FTS: close up view (April 2000).
FTS: assembled system in Hilo lab (September 2000).
FTS installed in the SUNY building at the summit of Mauna Kea for testing.
(c. Oct 2000)
Part of the FTS is the external "tipping" mirror assembly pictured here
on the outside of the SUNY building on the summit
of Mauna Kea. The tipping mirror allows the FTS to sample the
sky signal from zenith to horizon and also allows the measurement
of an ambient blackbody load at nadir.
FTS installed in AST/RO annex at the South Pole (Jan, 2001).
FTS data acquisition system installed in AST/RO annex at the South Pole (Jan, 2001).
FTS external tipping mirror installed at the South Pole (Jan, 2001).
Orthognal veiw from the 3-D Autocad model from which all the working
drawings were generated. The translation stage, optical enclosures,
roof reflectors, and polarizing wire grids were adapted from an earlier
instrument developed by Bob Martin for the University of Arizona Steward
Observatory.
South Pole FTS schematic diagram (Jan 2001).
Click here to see some preliminary results from the South Pole