MAPPIT 2: Second Generation High-Resolution Imaging at the AAT

J.G. Robertson, PASA, 14 (2), in press.

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Scientific Programme

The principal targets for which MAPPIT 2 will be suitable are similar to those that have been observed by existing speckle and NRM facilites, namely diameters and surface features of red giant and Mira stars, and study of binary and multiple star systems. But MAPPIT 2 is expected to be able to make successful observations of fainter objects, to have higher dynamic range, and to observe at wavelengths presently unusable due to sensitivity limitations (eg observation of red giants in the blue, where diameter measurements are particularly useful because of reduced absorption blanketing, and the angular resolution from a given telescope is greatest). The ability to image more complex objects would be appropriate for well-resolved stars and perhaps the brightest asteroids.

MAPPIT 2 would be ideal for the `large-scale' checkout of fields observed by the SUSI long baseline interferometer (Davis 1994). SUSI is insensitive to companions with separations greater than about 70 mas, whereas MAPPIT 2 would readily find companions at separations between 70 mas and the seeing disc size, down to a magnitude limit similar to that of SUSI.

MAPPIT 2 would also be suitable for imaging of bright novae (and supernovae), especially in the early phases with high brightness and small angular diameter.


Next Section: Conclusion
Title/Abstract Page: MAPPIT 2: Second Generation
Previous Section: Sensitivity Limits
Contents Page: Volume 14, Number 2

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