Rotation curves for spiral galaxies in clusters and in the field

Details Rotation curves for spiral galaxies in clusters and in the field Rotation curves for spiral galaxies in clusters and in the field

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.156..175w&link_type=abstract

(Instituto de Astrofisica de Canarias and Comision Interministerial de Ciencia y Tecnologia, Summer School on Evolutionary Pheno

Astronomy and Astrophysics

Astrophysics

1

Galactic Clusters, Galactic Rotation, Spiral Galaxies, Emission Spectra, H Alpha Line, Luminosity, Mass Distribution, Mass To Light Ratios

Scientific paper

This paper compares the H-alpha emission-line rotation curves and the H I rotation curves of spiral galaxies in clusters with their counterparts in the field, using the following three criteria: the inner and outer velocity gradients, the mass-to-light ratio (M/L) gradients, and the Burstein's mass-type methodology. Results show a good correlation between the outer gradient of the rotation curve and the galaxy's distance from the center of the cluster; namely, the inner galaxies tend to have falling rotation curves, while the outer galaxies and field galaxies tend to have flat or rising rotation curves. In addition, a correlation was found between the M/L gradient across a galaxy and the galaxy's position in the cluster, with the outer galaxies having steeper M/L gradients. Contrary to earlier reports, the mass types for field spirals were found to be a function of both Hubble-type and luminosity. These correlations indicate that the inner cluster environment can strip away some fraction of the mass in the outer halo of a spiral galaxy.

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