Kinematics of Ionized Gas in Edge-on HALOGAS Galaxies

Astronomy and Astrophysics – Astronomy

Scientific paper

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Scientific paper

Extra-planar gas generally shows a decrease in rotational velocity with increasing height above the disk. It can originate from disk-halo cycling driven by star formation in the disk or from infalling gas clouds. Studies at optical and radio wavelengths suggest that a combination of the two is the most likely scenario. Our goal is to measure velocity gradients of the ionized gas in a large number of halos, which can then be used as a constraint for models of the origin of halo gas. Because we are observing in optical, our measurements are likely not affected by warps which generally occur further out in radial distance. Our targets are drawn from a well-defined sample and are also a subset of the HALOGAS survey, which is investigating cold gas accretion in spiral galaxies with deep WSRT observations. We restrict our targets to edge-on galaxies, and our data provide an optical complement to HALOGAS data. We perform our observations using a multi-slit spectroscopic setup on the ARC 3.5m telescope. Arranging the slits parallel to the minor axis allows us to measure velocities of H-alpha emitting gas as a function of height above the plane in 11 radial distance bins in a single exposure. Our field of view is 3.75' x 4', and our total exposure time for a typical field is 6-8 hours. We present our ionized halo gas velocities for three nearby, edge-on galaxies and show a comparison with HI data.

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