Worthey Model Interpolation Engine - Padova94-based
This form allows one to create arbitrary mixtures of
single-burst populations based upon an alternate stellar evolutionary
isochrone library (Bertelli et al. 1994, A&AS, 97, 851). The
models are still those of Worthey
1994, ApJS, 95, 107.
Keep ages between 0.0039 and 19.9 Gyr, and [Fe/H]
between -1.7 and +0.4. Lick/IDS spectral indices will be output only
if no age is younger than 0.4 Gyr = 400 Myr.
The relative (mass) weights you give will be normalized so
that the total initial population mass comes out to a million solar masses.
In the box, enter (Age in Gyr, [Fe/H], relative weight) trios separated by
E.g., typing 12.0 0.0 97 (return)
0.5 0.1 3 (return)
will show you what an
old, solar metallicity population looks like when "polluted" by
3% (by mass) of a younger population 500 Myr old but 0.1 dex more metal-rich.
Disclaimer: Some aspects of these models are clearly wrong, like
RGB/AGB tip temperatures and horizontal branch behavior, so the user is
advised that the results obtained from this page are "substandard"
compared to models actually published in the literature. This page is
meant to be helpful but not authoritative.
Show colors, magnitudes, spectral indices, SBF magnitudes
Send a file
with all of that plus an SED.
Default models: Salpeter (2.35) IMF.
Note: although there are choices for IMF exponent, the Padova
isochrones do not include stars below 0.6 solar masses, so for old
populations the very stars that cause spectral changes as the IMF
changes are missing. For young populations the 0.6 Mo cutoff becomes