MASSIV: Mass Assembly Survey with SINFONI in VVDS. III. Evidence for positive metallicity gradients in z~1.2 star-forming galaxies

Details MASSIV: Mass Assembly Survey with SINFONI in VVDS. III. Evidence for positive metallicity gradients in z~1.2 star-forming galaxies MASSIV: Mass Assembly Survey with SINFONI in VVDS. III. Evidence for positive metallicity gradients in z~1.2 star-forming galaxies

2011-11-16

arxiv.org/abs/1111.3697v1

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

13 pages, 9 figures. Accepted for publication in A&A

Scientific paper

A key open issue for galaxy evolution and formation models is the understanding of the different mechanisms of galaxy assembly at various cosmic epochs. The aim of this study is to derive the global and spatially-resolved metal content in high-redshift galaxies. Using VLT/SINFONI IFU spectroscopy of a first sample of 50 galaxies at z~1.2 in the MASSIV survey, we are able to measure the Ha and [NII]6584 emission lines. Using the N2 ratio as a proxy for oxygen abundance in the interstellar medium, we measure the metallicity of the sample galaxies. We develop a tool to extract spectra in annular regions of these galaxies, leading to a spatially-resolved estimate of the oxygen abundance in each galaxy. We derive a metallicity gradient for 26 galaxies in our sample and discover a significant fraction of galaxies with a "positive" gradient. Using a simple chemical evolution model, we derive infall rates of pristine gas onto the disks. Seven galaxies display a positive gradient at a high confidence level. Four out of these are interacting and one is a chain galaxy. We suggest that interactions might be responsible for shallowing and even inverting the abundance gradient. We also identify two interesting correlations in our sample: a) galaxies with higher gas velocity dispersion have shallower/positive gradients; and b) metal-poor galaxies tend to show a positive gradient whereas metal-rich ones tend to show a negative one. This last observation can be explained by the infall of metal-poor gas into the center of the disks. We address the question of the origin of this infall under the influence of gas flows triggered by interactions and/or cold gas accretion.

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