Seeing measurements at UKIRT:

Consequently, until recently quantitative image quality information at UKIRT has really been obtained only on engineering nights by occasional special efforts, and we have had only a hazy idea of the image quality distribution over many nights. This is clearly unsatisfactory, especially as we enter the phase of the telescope development programme where we are trying to learn to exploit the Dome Ventilation System and the soon-to-be-completed mirror cooling system. Anecdotal information simply will not let us learn how these systems are best used.
 

The observers are asked to take appropriate images, and to process them in a defined manner to determine the FWHM, on all nights on which IRCAM (imaging) data is taken, using whatever magnifier the observer happens to be using. The observation involves securing a set of three to five images of stars of suitable K-band brightness, just after focussing the telescope, roughly midway through each of the first and second halves of the night.
 

To determine the undersampling corrections we have used engineering time on a number of nights to secure consecutive sets of images using no magnifier (X1), the X2 magnifier and on just one glorious night so far (see below) the X5 magnifier, in each case just after focus checks. The comparison of image FWHMs derived using 0."28/pixel and 0."14/pixel showed dramatic effects of undersampling, which becomes perceptible at about 3.7 pixels/FWHM and reaches a factor >2 at 2 pixels/FWHM for both pixel scales. The X1/X2 measurement sets, taken on different nights and in differing seeing, nevertheless fall on a well-defined curve, indicating that a single correction function can be used to convert FWHM results from variously sampled images into "true" results. The construction of the function assumed that undersampling of large images at 0."28/pixel has similar effects to a similar degree of undersampling of smaller images at 0."14/pixel. This assumption appears to have been justified: see below.
 

We currently have 139 image quality measurements taken between 13 February 1998 and 29 September 1998. For the corrected data set the median FWHM is 0."433. For comparison with data from other sites, more commonly measured in the optical, we note that this is nominally equivalent to 0."57 at the optical V band (0.55 µm, scaling as lambda ^-0.2).

As the data set increases we plan to investigate dependences of seeing on such variables as wind direction (likely to be linked with boundary layer effects), dome and mirror air temperatures, wind velocity and Dome Ventilation System settings. The programme of seeing monitoring will be continued with the UKIRT Fast Track Imager (UFTI) after its delivery. Its 0."09 pixels will remove most (but evidently not quite all! - see below) of the need for undersampling corrections.
 

Since the majority of these (apparently) very good images come from the X1 sample we have been anxious to validate the correction function. The bump near the diffraction limit, of images with corrected FWHM less than 0."15, derives from much larger measured values of <0."51 with X1 and <0."28 with X2, so direct confirmation was clearly essential before we would be justified in believing that we really do sometimes see images this close to the diffraction limit at K.

We were therefore extremely pleased that recent data taken with the X5 magnifier (PFOV = 0."056) as well as X2 and X1 has validated the correction function to better than 10%, not far from the small-FWHM end where we were most concerned.
 

The image above is the best of three consecutive 20-s K-band exposures which produced images with near-diffraction-limited cores (the FWHM of the others were 0."183 and 0."180) secured by Antonio Chrysostomou and Thor Wold on the night of 8 September 1998 UT. We believe they are the best images ever obtained from the ground without the use of higher-order adaptive optics (at any rate, they are the best we have heard of!). We note too, with surprise, that Thor, the TSS, did not consider the night to be one of exceptionally good seeing! The correction function then in use, applied to the X2 images taken just before these, gave FWHM = 0."17 and the corresponding X1 images yielded 0."16: both slightly - but pretty insignificantly - optimistic relative to the 0."178 of the (slightly undersampled!) X5 data. We have adjusted the correction function to match the X5 measures and the data set (displayed in the histogram above) has been re-analysed.
 

The 30th of September 1998 was the first engineering night of the new UKIRT Fast Track Imager (UFTI). We will therefore probably not be collecting much more seeing data with IRCAM, and future measurements will benefit from the smaller pixel scale offered by UFTI.

The table below shows a month-by-month analysis of the corrected image quality data collected using IRCAM since the campaign began in February 1998.
 

The number of measurements in a given month is mainly determined by the availability of IRCAM on the telescope.

IRCAM has certainly left us with excited expectations of the results from UFTI. September was a spectacular month, with 20% of the images measured being nominally diffraction limited. Furthermore, the results suggest that this has been achieved at some time in nearly every other month! It now remains to be seen if UFTI confirms this expectation. Watch this space...