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

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 la...

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Veröffentlicht in:Proceedings of the International Astronomical Union 2010-12, Vol.6 (S277), p.250-254
Hauptverfasser: Martel, Hugo, Richard, Simon, Brook, Chris B., Kawata, Daisuke, Gibson, Brad K., Sánchez-Blázquez, Patricia
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container_end_page 254
container_issue S277
container_start_page 250
container_title Proceedings of the International Astronomical Union
container_volume 6
creator Martel, Hugo
Richard, Simon
Brook, Chris B.
Kawata, Daisuke
Gibson, Brad K.
Sánchez-Blázquez, Patricia
description 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.
doi_str_mv 10.1017/S1743921311022885
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source Cambridge University Press Journals Complete
subjects Accretion disks
Chemicals
Contributed Papers
Gases
Numerical analysis
Simulation
title Chemical Signature of Gas-rich disc-disc Mergers at high Redshift
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