Figures

Fig. 1. The main image of NGC 2685 was made by combining photographically amplified derivatives from three UKST IIIa-J plates and shows a series of low surface brightness loops extending from the galaxy. Inset is a normal contrast photograph of NGC 2865 made to the same scale. The inset print is 5 arc min on a side.

Fig. 2. This image shows the enormous extent of the faint outer envelope of NGC 5266 compared with the superimposed positive, which is to the same scale. Note the large, faint, structureless SE extension. The scale bar is 5 arc min.

Fig. 3. The interacting system NGC 5018/22 is clearly linked by a low surface brightness `bridge' of luminous material. The arrow indicates the optical detection of a companion dwarf galaxy detected in HI by Kim et al. (1988). Scale bar is 10 arc min.

Fig. 4. The extent of the faint outer envelope of NGC 253 is evident when compared to the normal contrast positive image, inset to the same scale. The scale bar is 30 arc min.

Fig. 5. Even well-known galaxies can spring surprises. This deep image of M83 reveals an enormous loop around the NW quadrant of the galaxy. The inset image is the same scale as the main picture. The scale bar is 30 arc min.

Fig. 6. M104 looks like an E2 galaxy at low surface brightness. The outer `elliptical' component is featureless except for a faint loop to the SSW and a corresponding faint feature without structure to the NNE. Scale bar is 30 arc min.

Fig. 7. NGC 2855 seems to be a perfectly ordinary SA(r) galaxy that has not previously attracted attention. However, its very extensive low surface brightness disk or ring suggest that the dynamics of this galaxy are unusual.

© Copyright Astronomical Society of Australia 1997