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astro-ph/0907.2014


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\title{An analysis of infrared  emission spectra  from the regions near the Galactic Center}
\author[M. Contini ]{ Marcella Contini$^{ }$
\\
$^{ }$School of Physics and Astronomy, Tel Aviv University, Tel Aviv
69978, Israel \\
}




\begin{document}

\date{Accepted: Received ; in original form 2008 month day}

\pagerange{\pageref{firstpage}--\pageref{lastpage}} \pubyear{2009}

\maketitle

\label{firstpage}


\begin{abstract}
We present consistent modelling of  line and continuum IR  spectra in the region  close to the
Galactic center. The models account for the coupled effect of shocks and
photoionization from an external source.
The results show that the  shock velocities range between $\sim$ 65 and 80 \kms,
the pre-shock densities between   1\cm3 in the ISM to  200\cm3 in the filamentary structures.
The pre-shock magnetic field increases from 5. 10$^{-6}$ gauss  in  the surrounding  ISM
to  $\sim$ 8 10$^{-5}$ gauss in the Arched Filaments.
The stellar temperatures are $\sim$ 38000 K in the Quintuplet cluster and $\sim$ 27000 K in the Arches Cluster.
The ionization parameter is relatively low ($<$ 0.01 ) with  the highest values near the clusters, reaching
 a maximum  $>$0.01 near the Arches Cluster.
Depletion from the gaseous phase of Si is  found throughout the  whole observed region, indicating the presence of
silicate dust. Grains including iron,  are concentrated throughout  the Arched Filaments.
The  modelling of the continuum SED in the IR range,  indicates that a component
of dust  at temperatures of $\sim$ 100-200 K  is present in the central region of the Galaxy.
Radio emission appears to be  thermal bremsstrahlung in the E2-W1 filaments  crossing strip,
however a synchrotron component is not excluded. More data are  necessary to resolve this questions.

\end{abstract}

\end{document}