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Metals and Molecules in Halo Clouds

Published online by Cambridge University Press:  03 August 2017

Klaas S. de Boer ,
Uwe Herbstmeier  and
Ulrich Mebold
Klaas S. de Boer
Affiliation:
Astronomical Institutes of the University of Bonn Auf dem Hügel 71 D-5300 Bonn, F.R. Germany
Uwe Herbstmeier
Affiliation:
Astronomical Institutes of the University of Bonn Auf dem Hügel 71 D-5300 Bonn, F.R. Germany
Ulrich Mebold
Affiliation:
Astronomical Institutes of the University of Bonn Auf dem Hügel 71 D-5300 Bonn, F.R. Germany

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The abundance of the elements in clouds of halo gas, as determined from observations, is an important parameter for the test of the validity of models explaining the existence of, e.g., the high latitutude high-velocity clouds (HVCs) of the Milky Way. Individual HVCs have been detected in absorption only on very few lines of sight so that the distance of the HVCs, another important parameter for the models, stays ill determined as well. We will follow here the more or less established convention by calling HVCs those with /v/ >100 km s−1 and IVCs (intermediate-velocity clouds) those with 50 </v/ <100 km s−1. We will define halo as the space with /z/> 1 kpc, although for /b/> 45 also /z/> 0.5 kpc is used.

Type
I. The Disk-Halo Interface in Our Galaxy
Information
Symposium - International Astronomical Union , Volume 144: The Interstellar Disk-Halo Connection in Galaxies , 1991 , pp. 161 - 164
Copyright
Copyright © Kluwer 1991 

References

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