Using Mappings


Photoionization Models

  • The first thing a user should do before running a Mappings model is to check whether any of the pre-run photoionization grids are suitable. The pre-run photoionization grids have been calculated for a wide range in ionization parameter and metallicity. The grids were calculated with ionizing radiation fields from the stellar population synthesis models Starburst99 and Pegase 2.0 for both instantaneous and continuous star-formation. Self-consistent dust models were included. A full description of the grids is in Dopita et al. 2000, ApJ, 542, 224 (instantaneous models) and Kewley et al. 2001, ApJ, 556, 121 (continuous models).

  • If the pre-run grids do not cover the required parameter space, or a photoionization model for a blackbody or power-law ionizing radiation field is required, then the user has the option to run his/her own models via the Mappings or Starburst99 webpages:

    1. Users wishing to use a stellar population synthesis spectrum as the ionizing radiation field should use the Starburst99-Mappings web portal available from the STScI website. This web portal accepts inputs for both the Starburst99 stellar population synthesis code and the Mappings III photoionization code. Once the input parameters have been submitted, Starburst99 will run at STScI and produce a spectrum ready for input into Mappings. The spectrum and input parameters are then transferred to CfA where Mappings runs each hour. The resulting Mappings output files are transferred back to STScI. The users are notified by e-mail and can retrieve the output files by ftp from STScI.

    2. Users wishing to calculate a photoionization model for a blackbody or power-law ionizing radiation field have the option to enter the input parameters via the Mappings website at CfA. Mappings runs once an hour. The users are notified by email once their model(s) are complete and the resulting output files can be retrieved from the CfA Mappings website.

  • If the user prefers to use Mappings on his/her own machine (useful when calculating a large number of models), then the user can download the Mappings source code from this website. Users are free to modify the code to suit their needs. However, the user accepts sole responsibility for the results produced by the code.


Shock Models

  • The pre-run shock grids will be made available to the astronomical community once the associated paper has been accepted for publication. Users wishing to use shock models are encouraged to use the pre-run shock grid which is available from this website. Shock models were calculated for a wide range of shock velocities and for four metallicities. Both the shock and precursor line and continuum emission have been calculated.

  • If the parameter range available in the pre-run shock grid is not suitable, users may either download the Mappings source code or contact Ralph Sutherland. Because shock models are difficult to run, users are recommended to run shock models in collaboration with Ralph Sutherland and/or Mike Dopita to avoid errors.


Note: Although every effort has been made to identify and eliminate errors, we accept no responsibility for erroneous model predictions.



Lisa Kewley



[Back]