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Kinematic Evolution of Field and Cluster Spiral Galaxies

Published online by Cambridge University Press:  10 April 2015

Bodo L. Ziegler  and
Asmus Böhm
Bodo L. Ziegler
Affiliation:
University of Vienna, Department of Astrophysics, Türkenschanzstr. 17, 1180 Vienna, Austria email: bodo.ziegler@univie.ac.at
Asmus Böhm
Affiliation:
Institute for Astro- and Particle Physics, Technikerstrasse 25/8, 6020 Innsbruck, Austria email: asmus.boehm@uibk.ac.at
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Abstract

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We investigate the evolution of the Tully–Fisher relation out to z = 1 with 137 emission-line galaxies in the field that display a regular rotation curve. They follow a linear trend with lookback time being on average brighter by 1.1 Bmag and 60% smaller at z = 1. For a subsample of 48 objects with very regular gas kinematics and stellar structure we derive a TF scatter of 1.15mag, which is two times larger than local samples exhibit. This is probably due to modest variations in their star formation history and chemical enrichment.

In another study of 96 members of Abell 901/902 at z = 0.17 and 86 field galaxies with similar redshifts we find a difference in the TFR of 0.42mag in the B-band but no significant difference in stellar mass. Comparing specifically red spirals with blue ones in the cluster, the former are fainter on average by 0.35 Bmag and have 15% lower stellar masses. This is probably due to star formation quenching caused by ram-pressure in the cluster environment. Evidence for this scenario comes from strong distortions of the gas disk of red spirals that have at the same time a very regular stellar disk structure.

Keywords

galaxies: spiral - galaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S311: Galaxy Masses as Constraints of Formation Models , July 2014 , pp. 146 - 149
Copyright
Copyright © International Astronomical Union 2015 

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