GALEV SSP models for star clusters in tidal fields

Models described in:
GALEV SSP models for star clusters in tidal fields
P. Anders, H.J.G.L.M. Lamers & H. Baumgardt - A&A 502, 817 (2009)
View ADS entry

On this page we present the SSP models for clusters evolving in a tidal field (and therefore changing stellar mass function). The time evolutions of cluster masses and magnitudes for a large number of filter systems are provided for 5 metallicities ([Fe/H] = -1.7, -0.7, -0.4, 0.0, +0.4) and cluster dissolution timescales ranging from 100 Myr to 200 Gyr.

This page is going to be updated regularly. New grids for other isochrones are on their way and will be published here soon!

We apologize that the production of the new grids for other isochrones is currently delayed due to technical issues. Stay tuned!

The file naming conventions and formats are described in the following README-files: README.ps  README.txt

For further questions and/or requests drop me an email: p.anders /at\ uu.nl or visit my webpage at Utrecht university, Netherlands

Tarballs

containing files with mass and magnitude evolutions for all available dissolution timescales.
(If you require the integrated spectra, please contact me via email):

• SSP models for z=0.0004 == [Fe/H]=-1.7
• SSP models for z=0.004 == [Fe/H]=-0.7
• SSP models for z=0.008 == [Fe/H]=-0.4
• SSP models for z=0.02 == [Fe/H]=0.0
• SSP models for z=0.05 == [Fe/H]=+0.4

Individual files can be found here:

• SSP models for z=0.0004 == [Fe/H]=-1.7
• SSP models for z=0.004 == [Fe/H]=-0.7
• SSP models for z=0.008 == [Fe/H]=-0.4
• SSP models for z=0.02 == [Fe/H]=0.0
• SSP models for z=0.05 == [Fe/H]=+0.4

Test cases - Use on own risk

• Some test cases (for different isochrones, IFMRs and changing-MF parametrisations) to estimate uncertainties
• Tarball of all test cases