Physics
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003assl..281..311d&link_type=abstract
The IGM/Galaxy Connection: The Distribution of Baryons at z=0, ASSL Conference Proceedings Vol. 281. Edited by Jessica L. Rosenb
Physics
Scientific paper
The environmental influences on spiral galaxy rotation curves are investigated. Our large, homogeneously collected sample of 510 cluster spiral galaxy rotation curves is used to test whether the shape of a galaxy's rotation curve strongly depends on its location within the cluster, and thus presumably on the strength of the local intracluster medium and on the frequency and strength of tidal interactions with the cluster and cluster galaxies. The data do not corroborate such a scenario, consistent with the fact that Tully-Fisher residuals are independent of galaxy location within the cluster; while the average late-type spiral galaxy shows more rise in the outer parts of its rotation curve than does the typical early-type spiral galaxy, there is no apparent trend for either subset with cluster environment. Rotation curve asymmetry and the radial distribution of HII region tracers within galactic disks are also investigated as a function of cluster environment. Mild trends with projected cluster-centric distance are observed: (i) the (normalized) radial extent of optical line emission averaged over all spiral galaxy types shows a 4 +/- 2% increase per Mpc of galaxy-cluster core separation, and (ii) rotation curve asymmetry falls by a factor of two between the inner and outer cluster for early-type spirals (a negligible decrease is found for late-type spirals). Such trends are consistent with spiral disk perturbations or even the stripping of the diffuse, outermost gaseous regions within the disks as galaxies pass through the dense cluster cores.
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