Internal kinematics of isolated modelled disc galaxies

Free access article

Issue		A&A Volume 446, Number 3, February II 2006


Page(s)		847 - 854
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:20053993

A&A 446, 847-854 (2006)
DOI: 10.1051/0004-6361:20053993

Internal kinematics of isolated modelled disc galaxies

W. Kapferer¹, T. Kronberger^{1, 2}, S. Schindler¹, A. Böhm² and B. L. Ziegler²

¹ Institut für Astrophysik, Leopold-Franzens-Universität Innsbruck, Technikerstr. 25, 6020 Innsbruck, Austria
e-mail: wolfgang.e.kapferer@uibk.ac.at
² Institut für Astrophysik, Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany

(Received 5 August 2005 / Accepted 12 September 2005)

Abstract
We present a systematic investigation of rotation curves (RCs) of fully hydrodynamically simulated galaxies, including cooling, star formation with associated feedback, and galactic winds. Applying two commonly used fitting formulae to characterize the RCs, we investigated systematic effects on the shape of RCs by both the observational constraints and internal properties of the galaxies. We mainly focused on effects that occur in measurements of intermediate and high redshift galaxies. We found that RC parameters are affected by the observational setup, like slit misalignment or the spatial resolution and that they also depend on the evolution of a galaxy. Therefore, a direct comparison of quantities derived from measured RCs with predictions of semi-analytic models is difficult. The virial velocity $V_{\rm {c}}$ , which is usually calculated and used by semi-analytic models, can differ significantly from fit parameters like $V_{\rm {max}}$ or $V_{\rm {opt}}$ inferred from RCs. We found that $V_{\rm {c}}$ is usually lower than typical characteristic velocities derived from RCs. $V_{\rm {max}}$ alone is in general not a robust estimator of the virial mass.

Key words: galaxies: kinematics and dynamics -- galaxies: spiral -- galaxies: structure

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