Top End

Andy Adamson

Head of UKIRT Operations/Director of Science

If one had to characterize the last few months, one might begin with the fact that the main functions of UKIRT - high-resolution imaging and moderate and high-resolution spectroscopy in the near-infrared - have been superbly catered for by the two workhorse instruments - UFTI and CGS4. However, this would seriously understate the degree to which UKIRT has been developing during this period.

IRCAM/TUFTI was successfully commissioned - wonderfully efficient use of the taxpayer's investment, reusing the IRCAM2 cryostat with some optics now internal, cold and taking the place of the external reflections which characterized the previous IRCAM optical bench. IRCAM/TUFTI now sits on the west port of ISU2, with its cold snout extending in toward the telescope axis.

ORAC, the new integrated software system by which you will control UKIRT in future, was installed for the first time in October 1999, in coincidence with the first trial of the new Telescope Control System. After such an intense effort by both ATC and JAC staff, to see these systems come together was nothing short of an emotional experience. Using this system to control UKIRT both in on-the-fly mode and in the more programmed (exec-like) mode for which the system is designed, is simple, intuitive and very efficient by comparison with the current system. Due to the obvious success of the system, we have decided to attempt a "Big Bang" release, for all instruments, in May 2000.

UFTI, just coming out of shared-risks at the time of the previous newsletter, is now well established, reliable and well-calibrated, and is regularly producing 0.5 arcsecond imaging. It is frustrating to report that to take fullest advantage of the short periods of truly excellent (0.3 arcsecond and better) seeing would require a commitment to flexible scheduling which we are currently unable to make. However some of the groundwork has been laid (see the report by John Davies in these pages) and the benefits are not hard to see.

Hopes of an early delivery of MICHELLE foundered on a set of problems mainly centred on the grating exchange mechanism. This large mechanism is fundamental to the flexibility of Michelle in terms of spectral coverage and resolution. The resulting delays have been frustrating for ourselves and for the ATC, but at the time of writing good progress is being made.

Visiting instruments have figured little in UKIRT's roster over the past year. February marked a major change in that situation, with TRISPEC coming to the telescope for a run of four nights. Successful in many respects, this run revealed that some work remains to be done before TRISPEC will realise its full potential. We will be working with the Nagoya group to push this forward, and hope to be able to offer the instrument for a long run in the autumn of 2000.

One year ago, I made brief mention of the WFCAM project which was at that point in its early stages of development at the ATC. Following a successful Conceptual Design Review in November, the camera has now been granted formal approval by PPARC Council. In 2003, UKIRT will embark on the most ambitious infrared surveys ever undertaken. Our most important task is to ensure that UKIRT retains its ability to support the users of its other instrumentation into this new era.