pip install ezgal

Or see the github repository

Important: Citing this work

If you use the results of this web form in a paper please remember that you are making use of two data products: EzGal, as well as the model set that you have chosen. These magnitude evolution calcualations are only possible because someone else has gone through effort of generating stellar evolution models. So, I certainly appreciate an acknowledgement or citation for EzGal if you make use of it, but it is most important that you cite the paper which describes the model sets you are using. Here are the appropriate references:

Model Reference
PÉGASE.2Fioc and Rocca-Volmerange 1997 (A&A, 326, 950)
Bruzual and Charlot 2003:Bruzual and Charlot 2003 (MNRAS, 344, 1000)
Charlot and Bruzual 2007:Currently unpublished. Please reference as an updated BC03 model.
Maraston 2005:Maraston et al. 2005 (MNRAS, 362, 799)
BaSTI:Percival et al. 2009 (ApJ, 690, 472)
Conroy 2009:Conroy, Gunn, and White 2009 (ApJ, 699, 486C) and Conroy and Gunn 2010 (ApJ, 712, 833C (Please cite both)

Model file downloads

To make the EzGal web interface as convenient as possible I converted a large number of models into the EzGal model format. These models are avaialable for download on this page, that way if you want to run EzGal yourself you have ready-to-use model files. All of these files can be read directly by EzGal. The model file naming convention is described below. To view a complete list of all available model files for download click here. Here are some wget commands you can use to download particular model sets:

**NOTE** Maraston used a different normalization model when generating CSPs (mentioned briefly in the EzGal paper). This results in dramatically different magnitude predictions (for her CSP models) when this normalization difference is not accounted for. This is not a problem for results generated with the web interface, as it uses CSP models which have all been generated using EzGal in the same way. However, the models distributed here were not generated by EzGal but are simply the original models distributed by the authors and converted into the EzGal model format. EzGal cannot account for this difference and as such the relevant model files have been removed. In the next few months (i.e. by the end of 2012) I should have time to update the webstie and only include CSP files generated with EzGal.

Command Fetches
wget -r models
wget -r BaSTI models
wget -r BC03 models
wget -r CB07 models
wget -r M05 models
wget -r C09 models
wget -r PEGASE2 models
wget -r SSP models
wget -r models with exponentially decaying SFHs

Naming Convention

All filenames contain information on the model set, SFH, IMF, and metallicity. The naming convention is:


Here is the list of the model set abbreviations (as they appear in the filenames) and their corresponding references:
Abbreviation Reference
bc03Bruzual and Charlot 2003 (MNRAS, 344, 1000)
cb07Currently unpublished. Please reference as an updated BC03 model.
m05Maraston et al. 2005 (MNRAS, 362, 799)
bastiPercival et al. 2009 (ApJ, 690, 472)
c09Conroy, Gunn, and White 2009 (ApJ, 699, 486C) and Conroy and Gunn 2010 (ApJ, 712, 833C (Please cite both)

SFH can be one of the following. With the exception of the SSP each SFH has an additional paramter, which is listed right after the SFH type.
Abbreviation SFH Additional Parameter
sspA simple stellar population (delta-burst) 
expExponentially decaying burst of star formationE-folding time for exponential decay (Gyrs)
burstA short burst of constant star formationLength of burst (Gyrs)
constConstant star formation from z=zf to z=0V-band optical depth of dust extinction

Next is the metallicity. Different model sets use different values for solar metallicity. These values are:
Model Set Solar Metallicity

Finally is the IMF. These are simply abbreviated as:
Abbreviation IMF
krouKroupa (2001)
chabChabrier (2003)
salpSalpeter (1955)

Some examples:

Specifies n burst of length 0.1 Gyrs, solar metallicity, a Chabrier IMF, and the CB07 model set.

Specifies an exponentially decaying burst of star formation with a timescale of 0.5 Gyrs, solar metallicity, a Kroupa IMF, and the models from Conroy, Gunn, and White (2009).