||old solar population. single old
burst or decreasing exponential SFR
||subsolar (log(Z/Zsun)=-0.4 10 Gyr old burst, slightly younger than spectrum 1|
||large velocity dispersion, not
sure the convolution has been done
properly in the mock data. Looks like its constant FWHM in angstrom,
not log(angstrom) Hence model lines are 1) too shallow in the
too deep in the red. Because of this its hard to get a really low
chi^2. The residuals are similar in amplitude to what we would have
with a S/N=300.
Since I cant get really low in chi^2 my interpretation is rather limited. My guess is a rather extended SFH , with a tentative second burst around 3 Gyr ago, just for the fun. The pop seems to be around solar metallicity.
||Real spectrum: needed to mask 3720.,3740.],[4855.,4870.],[5000.,5020.],[6290.,6320.],[6540.,6600.],[6710.,6750.]||Rather extended SFH. I dont really believe in the peaks of the best solution. I would need to regularize that better. Since the young young burst weighs only 1% in light, I dont really believe in it.|
||sorry, didn't do that one...|
||composite relatively old stuff: exponentially decreasing solar pop, about 10Gyr Luminosity-weighted age, with a supersolar burst around 3 Gyr|
||Same problem as spetrum no 3, unphysical convolution. All I can see is an old solar pop. Possibly exponentially decreasing SFR|