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We study and compare different examples of stellar evolutionary synthesisinput parameters used to produce photoionisation model grids using the MAPPINGSV modelling code. The aim of this study is to (a) explore the systematiceffects of various stellar evolutionary synthesis model parameters on theinterpretation of emission lines in optical strong-line diagnostic diagrams,(b) characterise the combination of parameters able to reproduce the spread oflocal galaxies located in the star-forming region in the Sloan Digital SkySurvey, and (c) investigate the emission from extremely metal-poor galaxiesusing photoionisation models. We explore and compare the stellar input ionisingspectrum (stellar population synthesis code [Starburst99, SLUG, BPASS], stellarevolutionary tracks, stellar atmospheres, star-formation history, sampling ofthe initial mass function) as well as parameters intrinsic to the H II region(metallicity, ionisation parameter, pressure, H II region boundedness). We alsoperform a comparison of the photoionisation codes MAPPINGS and CLOUDY. On thevariations in the ionising spectrum model parameters, we find that thedifferences in strong emission-line ratios between varying models for a giveninput model parameter are small, on average ~0.1 dex. An average difference of~0.1 dex in emission-line ratio is also found between models produced withMAPPINGS and CLOUDY. Large differences between the emission-line ratios arefound when comparing intrinsic H II region parameters. We find thatlow-metallicity galaxies are better explained by a density-bounded H II regionand higher pressures better encompass the spread of galaxies at high redshift.

Comparison of Theoretical Starburst Photoionisation Models for Optical Diagnostics