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Examples of the Scientific Motivation
Since the Milky Way is composed of complex and interdependent elements, the scientific motivations are not only numerous but also inter-related. The consortium has set up science teams to focus on specific elements. However, these teams will analyse the data in parallel, meet annually, and communicate regularly. Although the motivations highlighted below can be organized into simple categories, these bins are actually intertwined and we expect that a global but detailed picture will emerge.
In the sections below, we highlight a few of the numerous scientific motivations.
Large Scale Characteristics of the Milky Way
The high spatial resolution will aid in determining the topological structure of the ISM. We can improve estimates of volume filling factors and the resolution of features in the vertical direction away from the mid-plane. Multi-wavelength comparisons will help illuminate the physics. We can contrast polarization effects with the distribution of cosmic rays. The high resolution and our ability to separate the emission into thermal and non-thermal components could allow us to investigate the origin of the far-infrared/radio continuum correlation.
Stars and Compact Objects
Multi-waveband comparisons will allow us to catalogue and statistically classify objects such as Há II regions, Wolf-Rayet stars, pulsars and will also identify candidates, such as variable or highly polarized sources, for further study. Supernova Remnants in particular will allow us to test many apparent correlations (e.g. that between the ISM density and synchrotron emission intensity).
Exchanges of Energy
We will be able to systematically study, on a parsec scale, the interaction of stars with the ISM. Of particular interest are shells and superbubbles around OB associations. Godbout and Joncas describe, in another contribution to this meeting, a supplemental project which uses Fabry-Perot H observations to study diffuse nebulae associated with older Há II regions. They hope to determine whether the region's energy input could produce turbulence on the scales necessary to affect the shape of Há I features. Studies of vertical Há I features emanating from the disk should indicate how the gas in the Galaxy's halo is replenished and the halo's energy input is maintained.
Next Section: Progress to Date Title/Abstract Page: The Canadian Galactic Plane Previous Section: Contributions to the project | Contents Page: Volume 15, Number 1 |
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