Issue |
A&A
Volume 483, Number 2, May IV 2008
|
|
---|---|---|
Page(s) | 461 - 469 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20078922 | |
Published online | 04 March 2008 |
Gaussian decomposition of H I surveys
IV. Galactic intermediate- and high-velocity clouds
Tartu Observatory, 61602 Tõravere, Tartumaa, Estonia e-mail: urmas@aai.ee
Received:
25
October
2007
Accepted:
22
January
2008
Context. Traditionally intermediate- (IVC) and high-velocity hydrogen clouds (HVC) were defined to be concentrations of H I gas, with line-of-sight velocities that are inconsistent with data on the differential rotation of the Galaxy.
Aims. We attempt to demonstrate that IVCs and HVCs can be identified from density enhancements in parameter distributions of Galactic H I 21 cm radio lines.
Methods. To investigate the properties of the 21 cm radio lines, the profiles of “The Leiden/Argentine/Bonn (LAB) Survey of Galactic H I” are decomposed into Gaussian components using a fully automatic algorithm. We focus on some regions with an increased number of Gaussians in phase space, defined by the component central velocity (VC) and the full width at the level of half maximum (FWHM). To separate the Gaussians responsible for the phase-space density enhancements, we model the width distributions of Gaussian components at equally-populated velocity intervals, using lognormal distributions.
Results. We study the Gaussians, which parameters fall into the regions of
the phase-space density enhancements at and
, where the indexes indicate
the half widths at the level of half maximum (HWHM) of the
enhancements. The sky distribution of the Gaussians,
corresponding to the first two concentrations, very well
represents the sky distribution of HVCs, as obtained on the basis
of the traditional definition of these objects. The Gaussians of
the last concentration correspond to IVCs. Based on this
identification, the division line between IVCs and HVCs can be
drawn at about
= 74 km s-1, and
IVCs can be identified down to velocities of about
= 24 km s-1. Traces of both IVCs
and HVCs can also be seen in the sky distribution of Gaussians
with FWHM ≈ 7.3 km s-1. In HVCs,
these cold cores have small angular dimensions and low observed
brightness temperatures Tb. In IVCs, the cores are
both larger and brighter.
Conclusions. When neglecting the general decrease in the amount of gas at
higher , the IVCs and HVCs are observed as
distinctive maxima in the
distribution of the Gaussians, representing the structure of the
21 cm radio lines of the Galactic H I. This definition is
less dependant than the traditional one, on the differential
rotation model of the Galaxy. The consideration of line-width
information may enable IVCs and HVCs to be better distinguished
from each other, and from the ordinary Galactic H I.
Key words: ISM: atoms / ISM: clouds / radio lines: ISM
© ESO, 2008
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.