a) Code is currently being written to introduce the computation of
He II lines into SPECTRUM. This will also be accompanied by the
inclusion of continuous opacities important for hot (O-type)
stars. Eventually, the goal is for SPECTRUM to compute good
synthetic spectra for O-type stars. This will involve introducing
partition functions for higher stages of ionization, especially for C,
N and O, and NLTE computations for Hydrogen, He I and He II and
possibly other species.
b) Code is slowly being introduced into SPECTRUM which will enable
it to compute reasonable spectra for cooler and cooler stars.
Code has already been written to introduce H2O into SPECTRUM, and this
code is currently being evaluated and tested.
c) A very long term goal is to add code to SPECTRUM which will
enable the user to model a multi-level atom for the non-LTE computation
of specific lines and multiplets.