Our survey for KUGs (Kiso Ultraviolet-excess Galaxies) is based on the multi-colour method applied to photographic plates taken with the Kiso Schmidt telescope. In total, 8,968 KUGs were detected on 170 plates covering some 5,100 square degrees. They are listed in 17 separate catalogues, where morphological type and UV-excess degree are given for each object together with position, size, and magnitude. After the appropriate editing of multiple entries of the same object detected on different plates, we produced a merged catalogue where 8,162 KUGs were arranged in order of right ascension. The accuracy of the position of KUGs was examined using the data of 806 KUGs whose positions were measured on different plates.

The Brorfelde Schmidt telescope has been modified to use a 1024 × 1024 12 micron pixels CCD camera. The field is 27 × 27 arcmin. When required, the spatial sampling is improved by co-adding multiple exposures with small offsets. The telescope is operated in service mode, with one observer carrying out several different observing programmes in parallel. The telescope is particularly well suited for long term monitoring programmes, most notably photometric monitoring of gravitationally lensed QSOs and searches for extragalactic supernovae.

I much regret not being able to attend this interesting meeting. However, I have two comments concerning useful Schmidt work on galaxies that I would like to pass on to you for further consideration.

Both relate to objective-prism surveys for emission-line galaxies. The first is a suggestion that the work of Wasilewski (1983) should be continued. (Additional studies of his objects have been made by Bothun et al. (1989), Osterbrock & Shaw (1988) and Osterbrock et al. (1992)). This utilized the Burrell Schmidt with a 4° prism that gave a dispersion of some 400 Å/mm in the neighborhood of N1, N2 and Hβ. With this relatively high dispersion one can clearly separate these three lines, giving useful information on their relative strengths and widths that cannot be obtained from lower-dispersion material. It might be worthwhile to employ even somewhat higher dispersions than Wasilewski used, though this would no doubt affect the limiting magnitude somewhat. My second suggestion is that one should carry out objective-prism survey work in longer-wavelength spectral regions than are currently being used. The purpose is the detection of additional extragalactic objects in the z = 3–5 range; this search should utilize the lowest available dispersion.

Schmidt telescopes have, for some three decades, provided one of the most important sources of data for studies of the quasar population at all wavelengths. In the 1980s the combination of Schmidt telescope plate material and automated scanning machines such as COSMOS and APM allowed a new generation of projects to be undertaken, the results from which are largely responsible for our present understanding of the evolution of the optically–selected quasar population. The digitisation of photographic plates coupled with the computer–based selection of candidate quasars has meant that quantitative calculation of survey selection functions can be accomplished. The first results from surveys with such selection functions are beginning to appear, and progress is being made in constraining the form of the evolution of the quasar luminosity function at high–redshifts, a regime where there has been much disagreement over the nature of evolution. The (still) unique wide–field capability of Schmidt telescopes, coupled with the application of analysis techniques developed using the automated scanning machines, will ensure that Schmidt telescopes continue to make an important contribution to quasar–astronomy over the next ten years.

Cosmological models for structure formation are severely constrained by several of the recent observational results. We now have observations which probe the power spectrum of fluctuations from about 0.5 h−1 Mpc to 3000 h−1 Mpc. These probes and the constraints they imply on models for structure formation are reviewed.

Digital stacking of Schmidt Plates greatly increases the depth of the data allowing detection of galaxies at ∼ 1. We can probe the angular correlations of galaxy and cluster positions over scales of ∼ 500h−1 Mpc. Radial distance information can be obtained by identifying radio galaxies in the field and using their “standard candle” properties. A search for cosmic string effects, beginning with the stacked dataset, has now been extended to ∼ 100 equatorial J-plates.

We report on the present status of an ongoing study of variability and proper motion of quasars based on Tautenburg Schmidt plates of the field around M3. The main aspects are: (i) a thorough investigation of variability of a sample of known quasars based on a large number of B plates with a long time baseline and the comparison of variability in U, B, and V; (ii) the variability - proper motion diagram for the objects with B ≲ 20.5 mag in this field and the loci of known quasars in this diagram. The primary aim of this work is to check the suitability of Tautenburg Schmidt plates for a combined variability - proper motion quasar survey.

We have developed an algorithm to search the COSMOS/UKST Southern Sky Object Catalogue for compact groups of galaxies, with the aim of finding regions of high mass-to-light ratio. With this catalogue, and quantitative criteria, we select groups objectively and therefore hope to improve upon earlier visual searches. We use a density enhancement measure to define a compact group.

We have made a preliminary search of 15 Schmidt fields (total area ∼ 390 deg2), finding 58 compact groups, ie. a mean density of 0.15 compact groups deg−2. In this paper we present finding charts and images of some of the compact groups found.

We demonstrate that the multi-object fibre-spectroscopy system ‘FLAIR’ on the UKST can be used to observe efficiently and effectively the brighter (B < 18.5) high-grade quasar candidates identified from UKST low-dispersion objective-prism plates. The quasar candidates were selected objectively by the application of AQD (automatic quasar detection) to prism plates that have been digitised using the COSMOS measuring machine. Thirteen high-grade quasar candidates with B ≤ 18.5 from a prism plate of ESO/SERC survey field 296 were observed with a 35-fibre version of FLAIR. From a total observing time of only 3 hours at a resolution of 8.4 Å/pixel six candidates were confirmed as quasars and four were identified as stars. The planned upgrade to a thinned, back-illuminated CCD in 1994 should yield a 3-fold increase in sensitivity and further enhance the capabilities of FLAIR for performing useful spectroscopic observations of quasars of moderate faintness over large areas of sky.

A new sample of active galaxies was obtained with the ESO Schmidt telescope. We derived quantitative redshifts for 97 emission line galaxies and semi-quantitative photometric and spectro-photometric properties for 62 of them. The results are directly extracted from the Schmidt plates after digitization by the MAMA machine of Observatoire de Paris (C.A.I, INSU Paris).

We have obtained BVRI CCD frames of the inner Abell radius of 14 Abell clusters as part of a survey that will eventually include 45 clusters with 0.03 < z < 0.08. We report on how the colours and surface brightness profiles can be used to identify galaxy Hubble type despite having rather large (2.1 arcsec) pixels and small images.

In this paper some of the major results from the COSMOS and APM digitised galaxy surveys are presented. The main motivation behind these catalogues was to study large-scale structure in the universe. We begin by outlining the importance of such studies to cosmology and discussing the early results from the visually compiled galaxy catalogues. The impact of the digitised catalogues is demonstrated by focussing on three key areas of research; the galaxy-galaxy two-point angular correlation function, the cluster-cluster spatial correlation function, and galaxy number counts.

We are using the UK Schmidt telescope (UKST) to carry out a new objective prism survey, covering 2000-3000 square degrees of high galactic latitude sky in the equatorial region. The survey is targeted at discovering both bright (R < 18) quasars in general and bright high redshift (2 < z < 4) quasars in particular, which will be valuable for high resolution spectroscopic follow-up studies. We are using a mixture of ultra-violet excess (XJVX) and a new template matching technique to identify all the bright quasars. Details of the project are discussed and some preliminary results of the survey are presented.

We intend to perform a deep multicolour survey for quasar candidates using the CCD equipment recently installed at the Schmidt telescope of Observatoire de la Côte d’Azur (OCA). As a first step, we will study small areas of 0.3 square degrees but we are especially interested in the forthcoming full coverage of the Schmidt field with a CCD mosaic. In order to prepare the selection of quasar candidates, we have computed their predicted colours on the basis of a composite quasar spectrum.

There are two obvious ways to make a quick survey work. A: A telescope with a wide field and a large size detector. B: Many telescopes with a rather narrow field and a small size detector. In Japan, there are now 47 telescopes with diameters of 50-100 cm dedicated to public use. If we develop a simple-to-handle detector system, non-professional observers at each public observatory would have the possibility of joining a collaborative survey network. We started a test observation which is expected to extend to a survey network.

A historical account of co-operation in astronomy for Japan, IAU activities in Asia, and recent regional co-operation are briefly reviewed.

In the Asia Pacific environment some astronomical centres already exist. It must be understood that while quite a few are already deeply involved in frontline astronomical research; others are still struggling to make their existence appreciated in their home countries, or, are trying to be recognized within the astronomical community. Whatever their status now, the basic underlying principle for the establishment of astronomy centres is the same and is motivated by the same ideals. These are to pursue scientific truths about the sun, planets, stars and galaxies.

It is often the case that inherent national problems (economic or political) can inadvertently push the astronomy institutions behind. Furthermore, there exists among the political elite in a country different, not to say lack of, visions and perceptions about science in general and astronomy in particular. In such a situation the scientists and astronomers in that country find themselves in a twofront battle-line. Firstly, they must try to overcome the shortages of manpower and funds for hardware, so that their institutions can grow. Secondly, they must elevate their national programmes so that they can be accepted by international research standards.

At the conclusion of the meeting, Karel van der Hucht and Martin McCarthy S J shared the task of giving a comprehensive summary of all the papers presented. I thank them for making their extensive notes available to me. There were also a number of lively discussions on specific topics during the course of the week. Here I will attempt to set out the main conclusions that can be drawn from the papers and discussions, and to see the way forward for Schmidt telescope astronomy. Much of the following is based on the results of a questionnaire which was circulated by the Scientific Organising Committee towards the end of the meeting, with 28 responses received.