\documentstyle{preprint}

\def\etal{{\it et al.\thinspace}}
\def\eg{{\it e.g.\thinspace}}

\begin{document}

\title{M87 IN THE NEAR-INFRARED:\\
~\\
THE JET AND THE COUNTER--JET REGION\thanks{
Based on observations collected at the United Kingdom InfraRed Telescope, 
Mauna Kea and at the European Southern Observatory, La~Silla.}}

\author{M.\ Stiavelli\/\thanks{On assignment from the Space Science Department 
of ESA.}\morethanks{Scuola Normale Superiore, Piazza dei Cavalieri, I56126, 
Pisa, Italy.}\\
\\
Space Telescope Institute\\
\\
3700 San Martin Drive\\
\\
Baltimore, MD 21218\\
\and
R.~F.\ Peletier\/\thanks{Istituto del Astrof{\'\i}sica de Canarias, Via Lactea, 
s/n, 38200 La Laguna, Tenerife, Spain.}\\
\\
Kapteyn Astronomical Institute\\
\\
Postbus 800, 9700~AV~~Groningen, the Netherlands\\
\and
C.~M.\ Carollo\\
\\
Sterrewacht Leiden\\
\\
Postbus 9513, 2300~RA~~Leiden, the Netherlands}

\pub{MNRAS}
\recacc{8 August 1995}{1 October 1996}

\maketitle

\begin{abstract}
We have investigated the structure at near-infrared wavelengths ($J$
and $K$ bands) of the jet in M87, and of the expected counter-jet
region.  We discuss the morphology of the IR emission not associated
with optical sources and find that the near-IR structures of the jet and
of the hot--spot are morphologically intermediate between the radio
and the optical, with both the hotspot and the jet more extended
than in the optical.  We attempt to measure the flux from the
counterjet region and obtain an upper limit to its flux.
Finally, we apply to our data models of
synchrotron emission and discuss the implications of these fits.
\end{abstract}
\end{document}