While it has long been recognized that the primary outgassing product
which drives most of the observable phenomena of comets is HO,
direct observation of H
O to date has been possible in only one comet
because of interference by terrestrial water vapor. The primary
photodisassociation product, OH, can be detected at both UV and radio
wavelengths. Only the radio lines can be observed with velocity
resolution finer than the outflow velocity. The only cometary images
which are resolved both spatially and in velocity have been obtained
with the VLA. However, the scalelength of OH is fairly large so that
in the D configuration typically only 1/2 to 1/3 of the total flux is
detected. Because the emission is variable from day to day,
the missing spacings must be filled in simultaneously with the
VLA observations. The use of the E configuration to increase the
surface brightness sensitivity and a total power system to measure the
spectra with individual antennas would allow images which contain all
of the OH flux. This would unambiguously resolve long-standing
uncertainties about the degree of symmetry in outgassing of comets.
So far, only the 1667 MHz transition of OH has been imaged because it
is not possible to image multiple transitions with adequate frequency
resolution and sensitivity. All four 18cm OH lines need to be imaged
simultaneously in both sense of polarization to obtain full data about
the cometary emission. Because the velocity range to be studied is not
large, 8 sets of 64 1.5kHz channels would be adequate. Interference
excision would be needed, especially at 1612 MHz and 1720 MHz.