In May, 1994, the Lexington conference on photoionization modeling was
held in order to better understand the differences between the various
codes available for solving photoionization problems. The conference
was attended by approximately 8 modelers actively involved in the
solution of problems involving H II regions, nova envelopes, planetary
nebulae, and AGN clouds. As part of the workshop the participants were
asked to run several standard problems and compare the results. These
were chosen from what were thought to be representative models of H II
regions, planetary nebulae, and AGN clouds. The results will
appear in a book on the proceedings of the Space Telescope Institute
Conference on Emission Lines. In this appendix we reproduce
the comparison with the results of XSTAR 1.17 with the other models
given in the conference proceedings, along with the input files needed
to reproduce these results. Note that version 1.17 has added an
input command 'benchmark ', where
is an integer from 1 to 8,
representing the test case in the Lexington paper. This command produces
a table, similar to the 'print line_fluxes' command, but also including the
mean value and dispersion of each line flux from the ensemble of model results
in the Lexington paper (with the results of the current run substituted for
the XSTAR results given there; columns 5 and 6), the flux from the current
XSTAR run (in the appropriate units asadopted by the Lexington conference;
column 7), and the number of 'sigmas' the XSTAR result differs from the mean
(column 4). The last line gives the summed
for all lines from the
10 codes represented in the Lexington paper. The first two entries are always
zero; the XSTAR
is in the 4th non-zero column (column 6).