A. Walker, W.J. Zealey, PASA, 15 (1), 79
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| Next Section: Further work Title/Abstract Page: Searching For Supernova Remnants Previous Section: Introduction | Contents Page: Volume 15, Number 1 |
The Survey
The first stage of this search will be to obtain plates containing all known supernova remnants in the area of the survey. In Table 1, we show some statistics of the 215 known Galactic supernova remnants as of August 1996 (Green 1996). This shows that of the greater number visible in the southern sky, a smaller proportion have been optically detected than in the northern sky. The presence of the Galactic centre below the equator has resulted in more objects being detected through radio surveys at larger distances across the galaxy. This, combined with the increased amount of obscuring material present, has resulted in fewer southern remnants being seen optically.
Digitized images of these objects' fields will be obtained, and enhanced with image processing software to bring out the faintest possible detail. Where H
emission is observed, comparisons will be made with survey images available in other bands, and previously published observations.
Due to supernova remnants being concentrated along the Galactic plane and towards the Galactic centre, plates from only a small fraction of the survey will be required to complete this work. A time requirement of a year seems likely. A longer term project for the duration of the survey and beyond, will be to examine in detail all of the survey plates, searching for the faint filamentary and shell structures typical of supernova remnants.
What can we expect to find? Primarily the objects found will include HII regions, planetary nebulae and Wolf-Rayet shells, all of which can be similar in appearance. It is likely, however, that a significant number of supernova remnants will be discovered. High resolution radio surveys have detected many new remnants close to the Galactic plane (e.g., Whiteoak & Green 1996). These may miss some objects due to faintness, confusion, or a lack of clear structure. Further from the plane the density of supernova remnants decreases, but less obscuration increases their chance of being optically detected.
| Next Section: Further work Title/Abstract Page: Searching For Supernova Remnants Previous Section: Introduction | Contents Page: Volume 15, Number 1 |
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