AAO Newsletter July 1996 - Page 3


than do the other 4m-class telescopes (even after allowing for the half share factor). The oft-cited leanness of the AAO operation is at least in part simply due to under-nourishment. We are also concerned that the current plans to 'privatise' the Royal Observatories could lead to a decline in support for the Plate Library in Edinburgh, the fast measuring machines and related facilities upon which the effectiveness of the Schmidt Telescope operation, and hence 2dF, depends. The decision of the Australian Government not to join ESO earlier this year means that the AAT will remain Australia's primary optical telescope for rather longer than expected, and as such it must be kept fully equipped with state-of-the-art instruments if Australian astronomy is to maintain its internationally competitive position.

So the future of the AAO is rosy from the point of view of demand for the telescopes and the number of exciting new instruments that are being proposed, but only marginally healthy in budget terms. A relatively small injection of cash would make a big difference and enable the expertise and enthusiasm of the staff to be fully utilised for the benefit of astronomy. I am pleased to be able to hand over the Observatory in a good state, confident that it will continue to thrive under Brian Boyle's leadership, and grateful to have had the opportunity to work with such a good team and to contribute to so many exciting enterprises over the last decade.

Russell Cannon


2dF Commissioning

Significant progress has been made, on both positioner and spectrograph fronts, since my last newsletter article.

While the May commissioning was heavily compromised by poor weather, we were able to make significant progress with 2dF positioning and auto-guiding. In particular, simultaneous auto-guiding on all 4 guide fibres was achieved using stars beyond our expected practical, good seeing limit of V ~ 15. Furthermore we were able to demonstrate that the auto-guide signal was imperceptibly perturbed by movement of the fibre positioner gantry thus validating the design goal which requires us to observe while re-configuring.

The June on-telescope commissioning saw an incomplete but nevertheless impressive system, with about 250 fibres mounted, 190 of which fed our No. 1 spectrograph. While the positioner itself was routinely displaying fibre positioning accuracy's in the order of 0.3" rms we had not, at this stage, the ability to study radial trends in the data. More work clearly needed to be done to fully characterise the positioner's astrometric performance, however the signs were that the system was working close to the specified accuracy. Configuration speed, however, was still relatively slow and we await the new amplifiers (probably not until October) before attempting a significant increase in gantry speed.

After much effort, spectrograph focus was achieved approximately uniformly over the full surface of the chip to a ~ 2.3 pixel (FWHM) level, quite good enough for science observations but with still some way to go before getting to the sub 2-pixel, expected performance. Of some significance, however, was the fact that system throughput (telescope; fibres; spectrograph) approximated to expected performance levels. Only crude estimates were made and we await a careful photometric campaign before giving definitive numbers, however there is little doubt now that the 2dF will come

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