J. English , A.R. Taylor , J.A. Irwin , S.M. Dougherty , S. Basu , C. Beichman , J. Brown , Y. Cao , C. Carignan , D. Crabtree , P. Dewdney , N. Duric , M. Fich , E. Gagnon , J. Galt , S. Germain , N. Ghazzali , S. J. Gibson , S. Godbout , A. Gray , D.A. Green , C. Heiles , M. Heyer , L. Higgs , S. Jean , D. Johnstone , G. Joncas , T. Landecker , W. Langer , D. Leahy , P. Martin , H. Matthews , W. McCutcheon , G. Moriarity-Scheiven , S. Pineault , C. Purton , R. Roger , D. Routledge , N. St-Louis , K. Tapping , S. Terebey , F. Vaneldik , D. Watson , T. Willis , H. Wendker , X. Zhang, PASA, 15 (1), 56
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Progress to Date
The progress of the consortium as a whole is described in Table 1. The DRAO portion of the survey has begun to produce useful mosaics and to distribute them to the consortium. Since we are awaiting the zero spacings our results are preliminary. However, detailed plans are in place for the scientific analysis of the CGPS/RCPG data and we have made significant progress to date. We outline a few examples below.
The pilot project observations of the Perseus Arm by Normandeau, Taylor, and Dewdney (1996) have been particularly fruitful. These data revealed a cavity in H I associated with the H II region W4. An OB association (OCl 352) exists at the apex of the cavity and dense molecular clouds in the cavity appear to be photo-evaporating. The vertically extended structure of these clouds contribute to the notion that this cavity is currently, or will evolve into, a ``chimney'' which will facilitate the exchange of energy between the disk and the halo.
Algorithms for distinguishing between filamentary H I features and dissociating regions are being explored by a team, headed by Joncas and Ghazzali, at Universit'e Laval. The resulting techniques will allow both the detection and classification of these features.
Fich and Johnstone are creating as reliable a determination of the velocity-distance relationship as possible. Their software for mapping observed spatial and velocity coordinates to distances will incorporate spiral streaming motions, known distances to objects with known velocities, uncertainty due to random motions of clouds, and other considerations. It will also output error estimates.
The Australia Telescope National Facility Karma package has been adopted as the preferred visualization software. Both English and Gibson have produced preliminary visualizations. Figure 1 shows a typical H I filamentary feature at 4 velocity steps in a version of a CGPS/RCPG data cube that has been block averaged (over 2 pixels in each direction) and median mask filtered. More images are available at
Figure 1: Filamentary Feature: These panels have been made using a preliminary mosaic of H I data from the DRAO survey. A subsection of the spectral line datacube has been block averaged over 2 pixels and median filtered to reduce both noise and the negative bowl artefacts due to the lack of zero spacings.
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