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The High Velocity Gas toward Messier 5: Tracing Feedback Flows in the Inner Galaxy

Authors
  • Zech, William F.
  • Lehner, Nicolas
  • Howk, J. Christopher
  • Dixon, W. Van Dyke
  • Brown, Thomas M.
Type
Preprint
Publication Date
Feb 03, 2008
Submission Date
Feb 03, 2008
Identifiers
DOI: 10.1086/587135
Source
arXiv
License
Yellow
External links

Abstract

We present Far Ultraviolet Spectroscopic Explorer (FUSE) and Space Telescope Imaging Spectrograph (STIS E140M) observations of the post-asymptotic giant branch star ZNG 1 in the globular cluster Messier 5 (l=3.9, b=+47.7; d=7.5 kpc, z=+5.3 kpc). High velocity absorption is seen in C IV, Si IV, O VI, and lower ionization species at LSR velocities of -140 and -110 km/s. We conclude that this gas is not circumstellar on the basis of photoionization models and path length arguments. Thus, the high velocity gas along the ZNG 1 sight line is the first evidence that highly-ionized HVCs can be found near the Galactic disk. We measure the metallicity of these HVCs to be [O/H]=+0.22\pm0.10, the highest of any known HVC. Given the clouds' metallicity and distance constraints, we conclude that these HVCs have a Galactic origin. This sight line probes gas toward the inner Galaxy, and we discuss the possibility that these HVCs may be related to a Galactic nuclear wind or Galactic fountain circulation in the inner regions of the Milky Way.

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