- 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:
- Users wishing to use a stellar
population synthesis spectrum as the ionizing radiation field should use
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.
- 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.
- 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
- 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.