Morphological analysis of HI features - III. Metric space technique revisited

Details Morphological analysis of HI features - III. Metric space technique revisited Morphological analysis of HI features - III. Metric space technique revisited

Publishing date

Jun 2010

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mnras.405..638r&link_type=abstract

Journals

Monthly Notices of the Royal Astronomical Society, Volume 405, Issue 1, pp. 638-656.

Science

Astronomy and Astrophysics

Field

Astronomy

Additional info 2

1

Additional info 3

Methods: Analytical, Methods: Data Analysis, Techniques: Image Processing, Ism: Clouds, Ism: Structure

Type

Scientific paper

Abstract

This is the third paper on the morphological analysis of HI features. As in the first paper, we use the mathematical formalism of the metric space technique, developed by F. C. Adams and J. Wiseman, to quantify the complexity of 21-cm interstellar maps. This method compares the one-dimensional `output functions' of the maps, which characterize specific morphological and kinematical aspects of the maps. The HI feature catalogue, from our first paper, is increased from 28 to 51 features of known origin, such as star formation regions, the environment of Wolf-Rayet (WR) stars and supernova remnants. The maps come from the Canadian Galactic Plane Survey (CGPS), and have a resolution of 1 cos δ arcmin. Also, significant improvements are applied to the metric space technique. We present a new data reduction technique, new and improved `output functions' and a better characterization of the noise propagation and uncertainties in functions. We again look for correlations between the complexity of the HI features and other intrinsic aspects such as age, excitation parameter u, wind velocity, |z| and distance. Many interesting correlations are measured, for example: (i) more complex HI is associated with intense flux emission from star formation regions; (ii) the higher the wind velocity of the WR star, the more complex the HI topology; (iii) the higher the HI feature above the Galactic plane, the less complex its topology.

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