\documentstyle[paasms,pptwocol,psfig]{preprint}
\newcommand{\FeII}{\mbox{[\ion{Fe}{2}]}}
\newcommand{\FeJ}{[\mbox{\ion{Fe}{2}]~1.257\,$\mu$m}}
\input pub.sty

\begin{document}

\title{FORBIDDEN Fe$^+$ EMISSION FROM ACTIVE GALAXIES}

\author{Chris Simpson\\
\\
Space Telescope Science Institute\\
\\
3700 San Martin Drive, Baltimore, MD 21218\\
\and
Duncan A.\ Forbes\/\thanks{School of Physics and Space Research, University of
Birmingham, Edgbaston, Birmingham B15 2TT}\\
\\
Lick Observatory\\
\\
University of California, Santa Cruz, CA 95064\\
\and
Amanda C.\ Baker\\
\\
Institute of Astronomy\\
\\
Madingley Road, Cambridge CB3 0HA\\
\and
Martin J.\ Ward\/\thanks{Present address: X-ray Astronomy Group, Department of
Physics and Astronomy, University of Leicester, Leicester LE1 7RH}\\
\\
Astrophysics, Oxford University\\
\\
Keble Road, Oxford OX1 3RH}

\pub{M.N.R.A.S.}
\recacc{May 1966}{July 1966}

\maketitle

\abstract{
We present intermediate resolution ($\sim 400$\,km\,s$^{-1}$)
near-infrared spectra for eight Seyfert and three starburst galaxies,
covering the \FeJ\ and Pa$\beta$ lines. We combine these data with
those in the literature to investigate the origin of the forbidden
Fe$^+$ emission in active galaxies, which is still under debate. In a
study of 26 active galaxies, Forbes \& Ward provided evidence that
\FeII\ emission in starburst galaxies is shock-excited by supernova
remnants.  Interestingly, the Seyfert galaxies in their sample also
appeared to have shock-excited \FeII\ emission, although the radio
jets were believed to be responsible. Analysis of our sample of 46
objects provides some support for the finding of Forbes \& Ward that
\FeII\ is more tightly correlated with radio power than the hydrogen
recombination emission. However, we argue that the observed line
ratios are inconsistent with the substantial grain destruction that is
an inevitable consequence of shocks. Together with the fact that the
dispersion in the \FeII--radio correlation is still fairly large, we
deduce that photoionization of material with normal ISM abundances
must be the dominant excitation mechanism, although we suggest that a
significant contribution ($\sim 20$\%) of the \FeII\ emission may be
shock-excited.}