1997/11/10 by U. Fritze - v. Alvensleben, Alvensleben, U. Fritze - v., U. Lindner +3
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9711089
5 pages Latex, 2 POSTSCRIPT figures, using psfig and crckapb.sty To appear in the proceedings of IAU Symposium 187 `Cosmic Chemical Evolution', August 26-30, 1997, Kyoto, Japan
arxiv created 1997/11/10 · openalex publication_date 1997/11/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We use our unified chemical and spectrophotometric evolutionary synthesis code to describe galaxies of various Hubble types. With stellar evolutionary tracks and element yields for 5 different metallicities we follow the spectrophotometric evolution of composite stellar populations and the chemical evolution of ISM abundances in a chemically consistent way, i.e., accounting for the increasing initial metallicities of successive generations of stars. Evolutionary galaxy models are required to give agreement with template nearby galaxies of various Hubble types in terms of SEDs, stellar absorption indices or HII region abundances, respectively. Within the framework of a given cosmological model the redshift evolution of ISM abundances and abundance ratios is compared to damped Lyman α abundances. This provides information about the early star formation and nucleosynthesis history of the absorber galaxies and, at the same time, our models predict their spectral energy distributions. Optically identified DLA absorbers, with their spectral and chemical properties, provide, of course, the strongest constraints for the model parameters.