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Specifically, we plan to:
Compare different chemical evolution models developed by members of our team,
focusing first on their predictions of availability of raw material
(O, C, N, Si, etc.) as a function of time;
Incorporate dust grain formation/destruction mechanisms into those models currently
without them, and compare the chemical depletion onto grains predicted
by the models;
Endeavor to incorporate in a self-consistent way molecule formation processes in
the chemical evolution models to predict molecular abundances;
Use the Photon-Dominated-Region and Large-Velocity-Gradient models
available to our group to estimate molecular emission line ratios
for a given set of physical conditions, considering the
intrinsic abundances predicted by the chemical evolution models.
We will also include constraints from dust continuum measurements and spectral
energy distribution (SED) fitting;
Continue and expand our observational program
of low-metallicity dwarf galaxies with ground-based
sub-millimeter/mm facilities including IRAM, APEX, and JCMT,
in conjunction with Spitzer observations already in hand;
Be ready for Herschel line and continuum observations
which we will be able to plan for and interpret, thanks
to the preparatory work we propose here.
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