H-alpha Distance Constraints for High-Velocity Clouds in the Galactic Halo

Bland-Hawthorn, J.; Maloney, P. R.

H-alpha Distance Constraints for High-Velocity Clouds in the Galactic Halo

Authors

Description

We present some developments in determining H-alpha distances to high-velocity clouds (HVCs) in the Galactic halo. Until recently, it was difficult to assess the nature and origin of HVCs because so little was known about them. But now several HVCs have reliable distance bounds derived from the stellar absorption technique, and more than a dozen have abundance measurements. In addition, twenty or more HVCs have been detected in H-alpha (and a few in optical forbidden lines). Over the past five years, we have been developing a model of the halo radiation field which includes contributions from the stellar disk, the stellar bulge, the hot corona, and the Magellanic Clouds. In certain instances, the H-alpha flux from an opaque HI cloud can be used to derive a crude distance constraint to the cloud. For a UV escape fraction of f_esc ~ 6% perpendicular to the disk (f_esc ~ 1-2% when averaged over solid angle), the HVCs appear to be broadly consistent with the spiral arm model. We caution that a larger database with full sky coverage is required before the usefulness of H-alpha distances can be fully assessed. We present a number of detailed predictions from our distance frame to encourage independent assessments from future observations. If the model is valid, we find that most HVCs detected to date are scattered throughout the halo up to distances of 50 kpc from the Sun. Most of this material is likely to be debris from recent galaxy interactions, or even debris dislodged from the outer Galaxy disk. We propose some future tests of the H-alpha distance model and briefly discuss recent H-alpha detections along the Magellanic Bridge and Magellanic Stream.
17 pages, 15 figures; to appear in "Extragalactic Gas at Low Redshift", ASP Conf. Series, eds. J. Mulchaey & J. Stocke. The pulsar community may be interested in the extended version of the Taylor-Cordes pulsar dispersion model on which the spiral arm radiation field model is based