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The program described here is a general code for modelling interstellar
or intergalactic absorption 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).
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''.