\documentstyle[paasms4,pptwocol,psfig]{preprint}
\input pub.sty
\def \um             {\ifmmode \mu \hbox{m}\else $\mu $m\fi }
\def \HOH            {\ifmmode H_2O\else H$_2$O\fi}
        
\begin{document}

\title{CARBON MONOXIDE IN JUPITER AFTER\\
~\\
 COMET SHOEMAKER-LEVY 9}
\author{Keith S.~Noll,\thanks{Visiting Astronomers at the NASA Infrared 
Telescope Facility, which is operated by the University of Hawaii under 
contract with the National Aeronautics and Space Administration.}
Diane Gilmore\/\samethanks{1}\\
\\
Space Telescope Science Institute, 3700 San Martin Drive, 
Baltimore, MD 21218\\
\\
phone:410-338-1828, fax:410-338-4767, email: noll@stsci.edu\\
\and
Roger F.~Knacke,\samethanks{1} Maria Womack\\
\\
The Pennsylvania State University, Erie, PA 16563\\
\and
Caitlin A.~Griffith\/\samethanks{1}\\
\\
Northern Arizona University, Flagstaff, AZ 86011\\
\and
Glenn Orton\/\samethanks{1}\\
\\
Jet Propulsion Laboratory, Pasadena, CA 91109}

\pub{Icarus}
\recacc{1 February 1996}{11 October 1996}

\maketitle

\abstract{
Observations of the carbon monoxide fundamental vibration-rotation
band near 4.7~\um\ before and after the impacts of the fragments of
comet Shoemaker-Levy~9 showed no detectable changes in the R5 and R7
lines, with one possible exception.  
Observation of the G-impact site 21~hours after impact do not
show CO emission, indicating that the heated portions of the
stratosphere had cooled by that time.  The large abundances of CO
detected at the millibar pressure level by mm-wave observations did
not extend deeper in Jupiter's atmosphere. Predicted upwelling of
shocked, O-rich material from below also did not occur. Combined
with evidence for upwelling of N- and S-rich gas, our observations 
indicate that the comet fragments may not have penetrated to the 
\HOH\ cloud. We find that CO concentrations in Jupiter's
stratosphere may be higher than previously suspected suggesting that 
some of the CO detected after the impacts may already have
been present in Jupiter's stratosphere. }