Kinematics of the Diffuse Ionized Gas Halos of NGC 891 and NGC 5775

Details Kinematics of the Diffuse Ionized Gas Halos of NGC 891 and NGC 5775 Kinematics of the Diffuse Ionized Gas Halos of NGC 891 and NGC 5775

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...20716405h&link_type=abstract

American Astronomical Society Meeting 207, #164.05; Bulletin of the American Astronomical Society, Vol. 37, p.1423

Astronomy and Astrophysics

Astronomy

Scientific paper

As part of an ongoing effort to characterize the nature of the disk-halo interaction in spiral galaxies, we present an investigation into the kinematics of the diffuse ionized gas (DIG) halos of two edge-on spirals, NGC 891 and NGC 5775. Observations of optical emission lines were obtained at high spectral resolution with the SparsePak fiber array at WIYN, and the TAURUS-II Fabry-Perot interferometer at the AAT, respectively. Detailed three-dimensional models of the galaxies were created and compared with the data, revealing the presence of a vertical gradient in rotational velocity in each case. The sense of the gradient corresponds to decreasing rotation speed with increasing height above the disk; the magnitude is approximately 15 km s-1 kpc-1 in NGC 891, and 8 km s-1 kpc-1 in NGC 5775. Qualitatively, this behavior is predicted by models of the disk-halo interaction which consider gas being lifted out of the disk, but quantitative agreement has not yet been achieved. We describe the results of our observations, present a comparison with a purely ballistic model of disk-halo flow, and discuss prospects for a better understanding of this critical process in the evolution of galaxies.
This material is based on work partially supported by the National Science Foundation under Grant No. AST 99-86113.

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