Phase Correction for mm-arrays

Details Phase Correction for mm-arrays Phase Correction for mm-arrays

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999alma.confe..60s&link_type=abstract

Science with the Atacama Large Millimeter Array (ALMA), Associated Universities, Inc., held October 6-8, 1999 at Carnegie Instit

Astronomy and Astrophysics

Astronomy

Emission, Tropospheric, Water Vapor, Phase Correction, Fluctuations, Radiometer, Bima, 183 Ghz

Scientific paper

Monitoring the line emission from tropospheric water vapor can be used for phase correction of mm and sub-mm signals, since phase fluctuations at these wavelengths are predominantly caused by fluctuations in the distribution of water vapor. We have built a prototype cooled broad band 16-channel radiometer which allows us to measure the shape of the optically thin 22 GHz water vapor line. In the optically thin limit, line intensity and shape information allows the measurement of the total water vapor column and a coarse separation of the altitude distribution of the fluctuating water vapor component. This altitude information can be used to reduce the uncertainties in the conversion between the measured sky fluctuations and the actual phase fluctuations of astronomical signals. The use of a multi channel measurement will allow robust phase corrections over a wide range of weather conditions, including the presence of liquid water clouds. The system that we are building is targeted for implementation on the BIMA array with a goal of path length correction to 35 mu m rms. The system is the low frequency analogy to the 183 GHz system planned for the ALMA array. It will provide valuable experience in high accuracy phase correction.

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