Chemical signature of gas-rich disc-disc mergers at high redshift

Details Chemical signature of gas-rich disc-disc mergers at high redshift Chemical signature of gas-rich disc-disc mergers at high redshift

2011-01-17

arxiv.org/abs/1101.3295v1

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

5 pages, 5 figures, IAU symposium No. 277 : Tracing the Ancestry of Galaxies

Scientific paper

We performed numerical simulations of mergers between gas-rich disc galaxies, which result in the formation of late-type galaxies. Stars formed during the merger end up in a thick disc that is partially supported by velocity dispersion and has high [alpha/Fe] ratios at all metallicities. Stars formed later end up in a thin, rotationally supported disc which has lower [alpha/Fe] ratios. While the structural and kinematical properties of the merger remnants depend strongly upon the orbital parameters of the mergers, we find a clear chemical signature of gas-rich mergers.

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