Global properties of the HI high velocity sky

Free access article

Issue		A&A Volume 455, Number 2, August IV 2006


Page(s)		481 - 498
Section		Galactic structure, stellar clusters, and populations
DOI		http://dx.doi.org/10.1051/0004-6361:20054750

A&A 455, 481-498 (2006)
DOI: 10.1051/0004-6361:20054750

A statistical investigation based on the LAB survey

P. M. W. Kalberla¹ and U. Haud²

¹ Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
e-mail: pkalberla@astro.uni-bonn.de
² Tartu Observatory, 61602 Toravere, Estonia
e-mail: urmas@aai.ee

(Received 22 December 2005 / Accepted 10 April 2006 )

Abstract
Context.Since 1973, it has been known that some H I high velocity clouds (HVCs) have a core-envelope structure. Recent observations of compact HVCs confirm this, but more general investigations have been missing so far.
Aims.We study the properties of all major HVC complexes from a sample compiled in 1991 by Wakker & van Woerden (WvW).
Methods.We use the Leiden/Argentine/Bonn all sky 21-cm line survey and decompose the profiles into Gaussian components.
Results.We find the WvW line widths and column densities to be underestimated by ~40%. In 1991, these line widths could not be measured directly, but had to be estimated with the help of higher resolution data. We find a well-defined multi-component structure for most of the HVC complexes. The cold HVC phase has lines with typical velocity dispersions of $\sigma = 3$ km s^-1 and exists only within more extended broad line regions, typically with $\sigma = 12$ km s^-1. The motions of the cores relative to the envelopes are characterized by Mach numbers $M = (v_{{\rm core}}-v_{{\rm envelope}})/\sigma_{{\rm envelope}} \sim 1.5$ . The center velocities of the cores within a HVC complex have typical dispersions of 20 km s^-1. The well-defined two-component structure of some prominent HVC complexes in the outskirts of the Milky Way is remakable: Complex H lies approximately in the Galactic plane, and the most plausible distance estimate of $R \sim 33$ kpc places it at the edge of the disk. The Magellanic Stream and the Leading Arm (complex EP) reach higher latitudes and are probably more distant, $R \sim 50$ kpc. There might be some indications for an interaction between HVCs and disk gas at intermediate velocities. This is possible for complex H, M, C, WB, WD, WE, WC, R, G, GCP, and OA, but not for complex A, MS, ACVHV, EN, WA, and P.
Conclusions.The line widths, determined by us, imply that estimates of HVC masses, as far as those derived from the WvW database are concerned, need to be scaled up by a factor 1.4. Correspondingly, guesses for the external pressure of a confining coronal gas need to be revised upward by a factor of 2. The HVC multi-phase structure implies in general that currently the halo pressure is significantly underestimated. In consequence, the HVC multi-phase structure may indicate that most of the complexes are circumgalactic. HVCs have turbulent energy densities which are an order of magnitude larger than that of comparable clumps in the Galactic disk.

Key words: Galaxy: halo -- ISM: clouds -- radio lines: ISM

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