<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2 Final//EN"> <!--Converted with LaTeX2HTML 98.1p1 release (March 2nd, 1998) originally by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds * revised and updated by: Marcus Hennecke, Ross Moore, Herb Swan * with significant contributions from: Jens Lippmann, Marek Rouchal, Martin Wilck and others --> <HTML> <HEAD> <TITLE>Introduction</TITLE> <META NAME="description" CONTENT="Introduction"> <META NAME="keywords" CONTENT="vol2"> <META NAME="resource-type" CONTENT="document"> <META NAME="distribution" CONTENT="global"> <META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso-8859-1"> <LINK REL="STYLESHEET" HREF="vol2.css"> <LINK REL="next" HREF="node179.html"> <LINK REL="previous" HREF="node176.html"> <LINK REL="up" HREF="node176.html"> <LINK REL="next" HREF="node178.html"> </HEAD> <BODY > <!--Navigation Panel--> <A NAME="tex2html3645" HREF="node178.html"> <IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="icons.gif/next_motif.gif"></A> <A NAME="tex2html3642" HREF="node176.html"> <IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="icons.gif/up_motif.gif"></A> <A NAME="tex2html3636" HREF="node176.html"> <IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="icons.gif/previous_motif.gif"></A> <A NAME="tex2html3644" HREF="node1.html"> <IMG WIDTH="65" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="contents" SRC="icons.gif/contents_motif.gif"></A> <BR> <B> Next:</B> <A NAME="tex2html3646" HREF="node178.html">Principle of the Program</A> <B> Up:</B> <A NAME="tex2html3643" HREF="node176.html">Inter-stellar/galactic Absorption Line Modelling</A> <B> Previous:</B> <A NAME="tex2html3637" HREF="node176.html">Inter-stellar/galactic Absorption Line Modelling</A> <BR> <BR> <!--End of Navigation Panel--> <H1><A NAME="SECTION001310000000000000000"> Introduction</A> </H1> The program described here is a general code for modelling <EM>interstellar or intergalactic absorption</EM> features on an initial polynomial continuum which may also contain emission lines. For each absorption line the input parameters are : atomic transition, column density, thermal width and position (velocity shift). <P> The output spectrum is computed at a given instrumental resolution and can therefore be used for a direct comparison with observations (provided that the lines are resolved). In this case the step is completely interactive with no possibility for a ``least square approach''. <P> <BR><HR> <!--Table of Child-Links--> <A NAME="CHILD_LINKS"> </A> <UL> <LI><A NAME="tex2html3647" HREF="node178.html">Principle of the Program</A> </UL> <!--End of Table of Child-Links--> <BR><HR> <ADDRESS> <I>Petra Nass</I> <BR><I>1999-06-15</I> </ADDRESS> </BODY> </HTML>
