Vasiliki Petropoulou, Jose Manuel Vilchez, Jorge Iglesias-Paramo
In this paper we study the chemical history of low-mass star-forming (SF)
galaxies in the local Universe clusters Coma, A1367, A779, and A634. The aim of
this work is to search for the imprint of the environment on the chemical
evolution of these galaxies. Galaxy chemical evolution is linked to the star
formation history (SFH), as well as to the gas interchange with the
environment, and low-mass galaxies are well known to be vulnerable systems to
environmental processes affecting both these parameters. For our study we have
used spectra from the SDSS-III DR8. We have examined the mass-metallicity
relation of cluster galaxies finding well defined sequences. The slope of these
sequences, for galaxies in low-mass clusters and galaxies at large
cluster-centric distances, follows the predictions of recent hydrodynamic
models. A flattening of this slope has been observed for galaxies located in
the core of the two more massive clusters of the sample, principally in Coma,
suggesting that the imprint of the cluster environment on the chemical
evolution of SF galaxies should be sensitive to both the galaxy mass and the
host cluster mass. The HI gas content of Coma and A1367 galaxies indicate that
low-mass SF galaxies, located at the core of these clusters, have been severely
affected by ram-pressure stripping. The observed mass-dependent enhancement of
the metal content of low-mass galaxies in dense environments seems plausible,
according to hydrodynamic simulations. This enhanced metal enrichment could be
produced by the combination of effects such as wind reaccretion, due to
pressure cofinement by the intra-cluster medium (ICM), and the truncation of
gas infall, as a result of the ram-pressure stripping. Thus, the properties of
the ICM should play an important role in the chemical evolution of low-mass
galaxies in clusters.
View original:
http://arxiv.org/abs/1202.4164
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