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Chemical Signature of Gas-rich disc-disc Mergers at high Redshift

  • Hugo Martel (a1) (a2), Simon Richard (a1) (a2), Chris B. Brook (a3), Daisuke Kawata (a4), Brad K. Gibson (a3) and Patricia Sánchez-Blázquez (a5) (a6) (a7)...

Abstract

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 [α/Fe] ratios at all metallicities. Stars formed later end up in a thin, rotationally supported disc which has lower [α/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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References

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Brook, C., Richard, S., Kawata, D., Martel, H., & Gibson, B. K. 2007, ApJ, 658, 60
Kawata, D. & Gibson, B. K. 2003a, MNRAS, 340, 908
Kawata, D. & Gibson, B. K. 2003b, MNRAS, 346, 135
Naab, T. & Burkert, A. 2003, ApJ, 597, 893
Richard, S., Brook, C. B., Martel, H., Kawata, D., Gibson, B. K., & Sánchez-Blásquez, P. 2010, MNRAS, 402, 1489
Toomre, A., 1977, in Evolution of Galaxies and Stellar Populations, eds. Tinsley, B. M. & Larson, R. B., (New Haven: Yale University Observatory), p. 401
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