What Starburst99 Can Do For You

There are three options for the Starburst99 user:

• The first, and most convenient option is to access a large set of figures and tables showing the calculated models from the 1999 publication. As we did in Leitherer & Heckman (1995), we computed a model set for standard IMFs, metallicities and star-formation histories and plotted a variety of parameters in a uniform way. The full description of the figures is in Leitherer et al. (1999). Most users may find the information in these figures sufficient for a first orientation but we recommend to recalculate the desired quantities, as Starburst99 has changed over the years. We have also included the energy distributions that were used for the calculation of spectrophotomtric quantities, such as colors. This will allow users to compute colors in different filter systems if desired.
  
  
• If the figure and table set does not cover the required parameter space, the Starburst99 user has the option to run her/his own models. A typical example would be a case with a non-standard IMF. The input parameters can be entered via a web interface, and the computations are done remotely at Space Telescope Science Institute. Once the job is complete, the users are notified by e-mail and can retrieve the output files by ftp. While most of the output has the same structure as the figures and tables described before, some has not, and a bit of fiddling with the data may be necessary. In any case, we always recommend recomputing a starburst models using the most recent version of Starburst99.
  
  
• Finally, if all else fails, the Starburst99 user has the option to download the code and all auxiliary files. We distribute the source code freely to the community, and the users are free to modify the code to suit their needs. However, the user accepts sole responsibility for the results produced by the code. Although every effort has been made to identify and eliminate errors, we accept no responsibility for erroneous model predictions. The code and the models should be referenced as Leitherer et al. (1999) and Vazquez & Leitherer (2005).