As I do chemical evolution models for spiral galaxies, I am computing
the SED's of these kind of galaxies using directly the star formation
history and the age-metallicity relation provided by the results of our
code as the SSP's for calculating the SED. (The inverse technique that
the usual one, I think!)
n fact in a very simple way I have done a figure (sp2_scott.eps) with
the spectrum2 and our model for the most massive spiral and the highest
star formation efficiency in order to check how well (or bad!) goes and
I think it is not so bad... I have not taken into account any
dispersion velocity nor other calculations, except the normalization,
only drawing what I have over the data. Although, like this is a
model for a spiral galaxy, I have taken the results for three radial
regions located at 4, 8 and 12 kpc of the center and I have done an
averaged spectrum...
I send you the file spgal_n4dis28_r8kpc for the spectra corresponding
to a galaxy like MWG, Sbc, with a rotation velocity of 200 km/s . The
file has 2 columns. The first one is lambda (in AA), the second one the
spectrum the radial region of R=8 kpc which would correspond to the
solar vicinity, for which we know the star formation history and the
age-metallicity relation with quiet precise measurements....I have the
spectra for more radial regions, since R=2 kpc up R=24 kpc so if you
prefer another...
The file n4dis28genR8kpc gives for each time step (in Gyr), column 1,
the mass of stars created in each time (19^9Msun) in column 2), the
total abundance Z (column 3) and some elemental abundances in the
following ones. The last one is [Mg/Fe]. With this file, the SFH
and Z(t) are well defined.
Added 27 October 2006:
We have found an error in the chemical evolution model we have taken to
do the figure I send you in september (which correspond to sp2 of
test3) . We have repeated this figure, and we have added two other
panels to show [Fe/H] (different of the total Z) and [Mg/Fe].
Figure
Spectrum
(old)
Model
output (old)