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We investigate the environmental dependence of the mass-metallicty (MZ)relation and it's connection to galaxy stellar structures and morphologies. Inour studies, we analyze galaxies in massive clusters at z~0.4 from the CLASH(HST) and CLASH-VLT surveys and measure their gas metallicities, star-formationrates, stellar structures and morphologies. We establish the MZ relation for 90cluster and 40 field galaxies finding a shift of ~-0.3 dex in comparison to thelocal trends seen in SDSS for the majority of galaxies with logM<10.5. We donot find significant differences of the distribution of 4 distinctmorphological types that we introduce by our classification scheme (smooth,disc-like, peculiar, compact). Some variations between cluster and fieldgalaxies in the MZ relation are visible at the high mass end. However, obvioustrends for cluster specific interactions (enhancements or quenching of SFRs)are missing. In particular, galaxies with peculiar stellar structures that holdsigns for galaxy interactions, are distributed in a similar way as disc-likegalaxies - in SFRs, masses and O/H abundances. We further show that our samplefalls around an extrapolation of the star-forming main sequence (the SFR-M*relation) at this redshift, indicating that emission-line selected samples donot have preferentially high star-formation rates (SFRs). However, we find thathalf of the high mass cluster members (M*>10^10Msun) lie below the mainsequence which corresponds to the higher mass objects that reach solarabundances in the MZ diagram.

CLASH-VLT: Is there a dependence in metallicity evolution on galaxy structures?