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G. H. Heald, R. J. Rand (University of New Mexico), R. A. Benjamin (University of Wisconsin), J. A. Collins (University of Colorado), J. Bland-Hawthorn (Anglo-Australian Observatory)
Models of disk-halo interactions in edge-on spiral galaxies provide detailed predictions for line-of-sight velocities as a function of galactocentric radius (R) and height above the midplane (z). Observationally, an excellent tracer of the disk-halo interface is the diffuse ionized gas (DIG) component. To date, measurements of DIG velocities have come from long-slit spectroscopy. Both models and data show a decrease in rotational velocity with z, but the observations do not provide information about how this dropoff changes with R. To better test models as a function of location (R and z) within galaxies, we have performed imaging Fabry-Perot observations of NGC 5775. These data allow us to examine the entire velocity field. The data, and comparison with our ballistic model, are presented. We also present recent spectroscopic observations of NGC 4302, a preliminary two-dimensional velocity field, and further comparisons with the ballistic model.
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Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.