Interpreting the galaxy group CG J1720-67.8 through evolutionary synthesis models

Abstract

This paper is part of a series devoted to a detailed analysis of the properties of the compact group CG J1720-67.8 and its member galaxies with the aim of sheding light on its evolutionary history. Here we interpret our previously published observational results through comparison with chemically consistent spectrophotometric evolutionary synthesis models in order to gain further clues to the evolutionary history of the galaxies in this group. In order to reduce the number of free parameters, we considered the simplest case of a single burst of star formation turned on after 11 - 12 Gyr of undisturbed galaxy evolution. However, we also briefly explore the effect of multiple, interaction-induced bursts of star formation. We find that the two spiral galaxies are consistent with interaction induced strong starbursts switched on \~ 40 to 180 Myr ago and still active. For the early-type galaxy a <~ 0.9 - 1.3 Gyr old star formation event (depending on the considered model) appears consistent with observed properties. The comparison with models cannot rule out the possibility that this galaxy is already the result of a merger. Alternatively, a star formation episode in this galaxy might have been triggered by a gas inflow as a consequence of the interaction with the companion galaxies. Estimates of galaxy masses are derived from the comparison with the models. Finally our results are discussed in comparison with other well studied poor galaxy systems.

19 pages, 15 figures out of which one in jpeg format. Accepted for publication in A&A on 22/09/2005

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Cited by in corpus (6)

• GALEV evolutionary synthesis models - I. Code, input physics and web-interface
• X-ray Selected Intermediate-Redshift Groups of Galaxies
• The Evolution of Galaxies in X-ray Luminous Groups
• The K luminosity-metallicity relation for dwarf galaxies and the tidal dwarf galaxies in the tails of HCG 31
• The impact of binary star yields on the spectra of galaxies
• Past and Future of CG J1720-67.8: Constraints from Observations and Models