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3D Spectroscopic Surveys: Exploring Galaxy Evolution Mechanisms

Published online by Cambridge University Press:  05 December 2011

Benoît Epinat
Benoît Epinat*
Affiliation:
Université de Toulouse; UPS-OMP; IRAP; Toulouse, France CNRS; IRAP; 14, avenue Édouard Belin, F-31400 Toulouse, France email: benoit.epinat@ast.obs-mip.fr
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Abstract

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I review the major surveys of high redshift galaxies observed using integral field spectroscopy techniques in the visible and in the infrared. The comparison of various samples has to be done with care since they have different properties linked to their parent samples, their selection criteria and the methods used to study them. I present the various kinematic types of galaxies that are identified within these samples (rotators, mergers, etc.) and summarize the discussions on the mass assembly processes at various redshifts deduced from these classifications: at intermediate redshift (z ~ 0.6) merger may be the main mass assembly process whereas the role of cold gas accretion along cosmic web filaments may increase with redshift. The baryonic Tully-Fisher relation is also discussed. This relation seems to be already in place 3 Gyr after the Big-Bang and is then evolving until the present day. This evolution is interpreted as an increase of the stellar mass content of dark matter haloes of a given mass. The discovery of positive abundance gradients in MASSIV and LSD/AMAZE samples is highlighted. At z ~ 3 this discovery might be linked to cold gas accretion along cosmic filaments toward the centre whereas at lower redshift (z ~ 1.3), this may be mainly due to accretion of gas from outer reservoirs toward the centre via tidal tails due to interactions.

Keywords

galaxies: evolutiongalaxies: high-redshiftgalaxies: kinematics and dynamicsgalaxies: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S277: Tracing the Ancestry of Galaxies (on the land of our ancestors) , December 2010 , pp. 128 - 133
Copyright
Copyright © International Astronomical Union 2011

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