J Anglo- Australian Telescope 1982/83

Anglo- Australian Telescope 1982/83

Report of the Anglo-Australian Telescope Board 1 July 1982 to 30 June 1983

Australian Government Publishing Service Canberra 1983 Correspondence to the Board may be addressed to: The Secretary Anglo-Australian Telescope Board Correspondence to the Observatory may be addressed to: The Director Anglo-Australian Observatory P.O. Box 296 Epping,N.S.W.2121 Australia Telephone: (02) 868 1666 Telex: AA23999 (AAOSYD)

Frcwt Cover: The Cartwkwl Galaxy. This very unusual galaxy is surrounded by a ring rotating at 250 km/s and expanding at 90 km/s. It is thought to have been formed by a collision with one of the neighbouring small galaxies. Photo by W. D. Pence.

Printed by C. J. THOMPSON, Commonwealth Government Printer, Canberra J

The Right Honourable Sir Keith Joseph, M.P. Secretary of State for Education and Science, Government of the United Kingdom of Great Britain and Northern Ireland.

The Honourable Barry O. Jones, M.P. Minister for Science and Technology, Government of the Commonwealth of Australia.

In accordance with Article 8 of the Agreement between the Australian Government and the Government of the United Kingdom to provide for the establishment and operation of an optical telescope at Siding Spring Mountain in the State of New South Wales, I present herewith a report by the Anglo-Australian Telescope Board for the year from 1 July 1982 to 30 June 1983. The report summarises the operations of the Board for the period under review and includes financial statements and statements of estimated expenditure in accordance with the provisions of the Agreement.

Chairman Anglo-Australian Telescope Board November 1983 ANGLO-AUSTRALIAN TELESCOPE BOARD Board Membership for the period 1 July 1982 to 30 June 1983

For the United Kingdom: Sir Harrie Massey, F.R.S. (Chairman) Professor Emeritus, University College London Dr H.H.Atkinson Director, Astronomy, Space and Radio and Nuclear Physics, Science and Engineering Research Council Professor M. S. Longair, F.R.S.E. (from 1 July 1982) Director, Royal Observatory, Edinburgh For Australia: Professor J. H. Carver (Deputy Chairman) Director, Research School of Physical Sciences, Australian National University DrR.H.Frater.F.T.S. Chief, CSIRO Division of Radiophysics Dr W. J. McG. Tegart, F.T.S. Secretary, Department of Science and Technology Director, Anglo-Australian Observatory: Dr D. C. Morton Executive Officer, Anglo-Australian Observatory: MrD.W.Cunliffe Secretary to the Board: Mr J.M. Franklin Secretary designate to the Board 1983-84: Miss K. M. Proust ANGLO-AUSTRALIAN TELESCOPE BOARD ORGANISATION

UNITED KINGDOM GOVERNMENT AUSTRALIAN GOVERNMENT Science and Engineering Department of Science Research Council and Technology

THE BOARD 3 Members 3 Members appointed by the appointed by United Kingdom Australia

AATB Secretariat (Canberra)

ANGLO-AUSTRALIAN OBSERVATORY

AAO Laboratory Telescope (Epping, NSW) (Siding Spring Director Mountain, NSW)

Astronomers Research-Support Administrative Groups Staff Electronic Optical/Mechanical Photographic Programming Telescope Operations

RESPONSIBILITIES OF THE BOARD The Anglo-Australian Telescope Board operates under an Agreement between the Governments of the United Kingdom and Australia. The Board is an independent bi-national authority which consists of members appointed from each country and draws its funds in equal shares from each Government. In accordance with its responsibilities under the Agreement, the Board operates and maintains facilities which enable United Kingdom and Australian astronomers to undertake astronomical observations for the advancement of scientific knowledge. The Board's facilities consist of the Anglo-Australian Telescope (AAT) at Siding Spring Mountain, near Coonabarabran, N.S.W., and the associated Laboratory at Epping, N.S.W. Collectively, these facilities are known as the Anglo-Australian Observatory (AAO). A brief history of the AAT project appears in Appendix D, page 42.

NATIONAL AGENCIES DESIGNATED UNDER THE AGREEMENT Under the terms of Article 1 (2) of the Anglo-Australian Telescope Agreement, each Govern- ment acts through an agency designated for that purpose. The designated agencies are the Science and Engineering Research Council of the United Kingdom and the Australian Department of Science and Technology. The agencies are jointly responsible for implementing the Agreement. Contents

1. INTRODUCTION TheYcarPast 1 Scientific Highlights 2 Co-operation with Other Institutions 2 Changes in Board Membership 3 Meetings of the Board 3 Symposia and Publications 3 Advisory Committee on Instrumentation 3 Freedom of Information Act 4 2. OPERATIONS OF THE OBSERVATORY Observatory Staff 5 Building and Accommodation Programme 5 Allocation of Observing Time 5 Visiting Scientists 6 Photography 6 Public Relations 6 3. RESEARCH Overview 7 Gas Motions in Barred Galaxies 9 A Collapsing Supercluster 10 An Infrared Nucleus in Ml04 11 Asymmetric Supernova Explosion 11 Infrared Views of Jupiter 12 NGC 4696—A Centre of Activity 14 Do Supernovae Liberate Dust? 14 4. INSTRUMENTATION Introduction 16 Available Equipment 16 Computing Facilities 17 Development of Instrumentation 19 Image Photon Counting System (IPCS) 19 Spcctropolarimetcr 19 Hatfield Infrared-Optical Polarimeter 19 Faint Object Red Spectrograph (FORS) 19 Optical Fibres 20 5. FINANCIAL STATEMENTS A. Audited Accounts 1982-83 21 Report of the Auditor-General 21 Statement of Fixed Assets 21 Statement of Receipts and Payments 22 B. Disposal of Assets in 1982-83 23 C. Expenditure Forecast 1983-84 to 1987-88 23

Vll APPENDIXES A. Research Papers 25 Published Scientific Papers based on AAT data (1 July 1982 to 30 June 1983) 25 Papers delivered at AAO Research Symposia 30 B. Telescope Allocation 33 PATT Allocations 33 ATAC Allocations 34 Summary of Observing Programmes 35 C. Staff of the Anglo-Australian Observatory 41 D. History of the AAT Project 42

via 1 Introduction

The Year Past In this eighth year of full scientific operation the Anglo-Australian Telescope continues to hold its place as one of the foremost scientific instruments of its kind world-wide. The introduction of new devices for making astronomical observations, particularly long-baseline radio telescopes and satellites designed to detect radiation which cannot be satisfactorily observed at ground level, increases the demand for complementary observations at optical wavelengths using the most far-seeing and accurate telescopes. The list of scientists of many nationalities who, against considerable competition, have won observing time on the AAT and the ever-growing list of scientific achievements based on these observations are the proper testimony to the value of the Telescope. The excellence of the original design and engineering of the Telescope and its lo- cation in the Southern Hemisphere laid firm foundations on which to build a reputation. It has been through two other elements—the technical developments which have maximised the quality of the observational data obtained from the Telescope and the high standard of service to visiting observers—that the Observatory has become a major international focus for observational astronomy. The Board acknowledges with great appreciation that this reputation is due to the efforts of the observers, the Direc- tor of the Observatory and his staff, and the members of associated institutions in the United Kingdom and Australia who contribute to the development of instrumentation for the Telescope. The Board has again given close attention during the year to the efficient manage- ment of the funds provided by the two contributing Governments. The economy measures which have been imposed generally on public authorities in both countries have not yet made a noticeable impact on the Board's operations. Some protection from cuts in funding may have been derived from the agreed programme of instrumentation and building development established by the 1979 report on future funding of the AAT, referred to in the last two annual reports. The end of this five-year programme is now approaching, and the Board is examining the essential and desirable needs of observers with respect to new detector and spectroscopic instrumentation and augmented computing resources. It is to be hoped that the level of funding for the Board will remain adequate to maintain the Observatory's standard of facilities and services. On 1 April 1983, the Board concluded an occupancy agreement with CSIRO for the continued use and enjoyment of the Epping site for as long as the Anglo-Australian Telescope Agreement remains in force. Early in the 1983-84 year, the Board's Secretariat will be re-located from Canberra to Sydney, where it will be accommodated at the Anglo-Australian Observatory's Lab- oratory at Epping. The Board's Secretary will continue to have responsibility for various functions, relating particularly to the Board's bi-national and statutory status, independently of the Director of the Observatory. The Board's new secretary will be Miss Katrina Proust, B.A., LL.B. The Sec- retariat's new address, the same as that for the Observatory, is shown on p.ii. These changes will take effect from 4 July 1983. Since 197S, an officer of the Australian designated agency, which is currently the Department of Science and Technology, has been made available to serve full-time as

1 the Board's Secretary, on a cost recovery basis. This arrangement, coinciding with the first operational years of the Observatory, has been very beneficial to the Board, as a major task in this period has been to establish and implement administrative procedures suitable to Australian governmental practices within the framework of which the Board largely operates. The employment of suitable personnel and the provision of access to the Department's resources for the Secretariat have also assisted the Board. The Board is very appreciative of this support from the Australian Government. It recognizes that the current limitations on departmental resources necessitates ter- mination of the arrangement.

Scientific Highlights Some of the scientific highlights from research programmes conducted during the year are described briefly below. Additional details for some items are reported in the section on research. • The infrared imaging mode of AAT has detected cloud structure on the dark side of Venus, discovered new sources in the Orion Nebula and located hydrogen in molecular form around many nebulae. • This mode also has permitted the study of the centre of our Galaxy in greater detail than ever before. Infrared observations that penetrate the intervening dust have shown the central object, IRS 16, to consist of separate components. The outermost two components are congregations of young, hot stars and gas, whilst the middle component appears to be a very tight cluster of cooler stars that prob- ably coincides with our Galaxy's nucleus. The central concentration of these cooler stars suggests, but does not prove, that a dense, dark object such as a black hole is present within. • An observation of the giant elliptical galaxy NGC 4696 has revealed the presence of filamentary gas in its core, adding further evidence that some galaxies are today accreting gas from their surroundings. • A very populous supercluster of galaxies has been found to be collapsing because of its own gravity, supporting the idea that the growth of such clusters is still occurring in the Universe.

Co-operation with Other Institutions The AAT shares the Siding Spring Mountain site with astronomical facilities operated by two other bodies; these are the Siding Spring Observatory of the Australian National University (ANU) and the UK Science and Engineering Research Council's Schmidt Telescope Unit (UKSTU) of the Royal Observatory, Edinburgh. Under Article 4 of the Anglo-Australian Telescope Agreement, the Board and the University co-operate in the use of supporting facilities provided by the ANU on the Mountain. In addition to basic services and fire protection, the ANU provides housing for some AAO staff resi- dent on the Mountain and operates a Lodge which accommodates users of the AAT. The Board is happy to record its gratitude to the University for the continuing co- operation it has received. The AAO Laboratory is located in the grounds of the CSIRO Division of Radiophysics at Epping, New South Wales. The Board has made arrangements with CSIRO for continued occupancy of the Epping site for as long as the Anglo-Australian Telescope Agreement remains in force. The Board is grateful to the CSIRO for its co- operation in these arrangements and for the space which has been made available for the Laboratory's workshop, pending further expansion of the permanent AAO building. There is no doubt that the scientific and technical interchange between AAO staff, the optical astronomers of the ANU and UKSTU, and the radio astronomers of the CSIRO has made a significant contribution towards the success of the AAT. The Board records its thanks to the staff of these institutions.

Changes in Board Membership Professor F. Graham Smith, Director of the Nuffield Radio Astronomy Laboratories at Jodrell Bank in Cheshire, retired from the Board on 30 June 1982 after a three-year term. The Board appreciates the diligent attention Professor Smith gave the affairs of the AAT, and in particular is grateful for his valuable contribution to the continuing review of dome seeing at the Telescope. Professor Smith was succeeded on the Board by Professor M.S. Longair, Astron- omer Royal for Scotland and Director of the Royal Observatory, Edinburgh, who was appointed for a three-year term from 1 July 1982.

Meetings of the Board The Board held two meetings during the year. In September 1982 it met at the Royal Greenwich Observatory, Herstmonceux Castle, Sussex and in March 1983 it met at the AAO, Epping and Siding Spring and at the ANU Research School of Physical Sciences, Canberra.

Symposia and Publications The Board sponsors a one-day research symposium in conjunction with each of its meetings. The thirieenth symposium was held at the University of Sussex in September 1982, and the fourteenth at the CSIRO Division of Radiophysics at Epping in March 1983. The papers presented are listed in Appendix A, page 30. The symposia have continued to attract lively interest from astronomers and Board members alike. As well as their scientific function, the symposia provide a useful opportunity for the users of the AAT to meet Board members and give their views on how the Telescope and its operation might be improved. The Board has asked all users to supply the AAO Library with copies of any publications using data obtained with the AAT. Based on these records, the Board lists publications of which it is aware in an appendix to each Annual Report (see Appendix A, page 25).

Advisory Committee on Instrumentation The Advisory Committee on Instrumentation for the AAT (ACIAAT) held meetings with interested astronomers at several locations in the United Kingdom and Australia during February and March 1983 to discuss plans for the future. At present this committee consists of Dr K.C. Freeman (Chairman), Dr D.C. Morton and Professor W.L. Wilcock. The AAT Board considered the Committee's report in March 1983 and adopted the following decisions: (a) A replacement should be found for the 25cm camera on the RGO spectrograph. The present camera has poor UV transmission and significant vignetting when used with the grating blaze-to-collimator, a mode that is popular for its high demagnification ratio. (b) An echelle spectrograph should be acquired for high dispersion observations. This would fill a serious gap in the scientific capabilities of the AAT. (c) A Taurus Fabry-Perot imaging interferometer should be available for AAT observations at regular intervals. This type of instrument has proved its useful- ness on the AAT during a three-year loan from the UK. (d) There should be a thorough review of the plans for computer control of instruments, on-line data analysis, links between computers, and remote observing. A workshop is planned for September in Britain leading to a report for consideration by the AAT Board.

Freedom of Information Act On 1 December 1983, the Freedom of Information Act, an enactment of the Australian parliament in respect of Australian administrative law, came into operation. Under Part III of the Act, statutory bodies such as the Anglo-Australian Telescope Board, are required to establish procedures to deal with requests for information pursu- ant to the Act. These requirements have been met by the Board, although no requests were received during the period to 30 June 1983. 2 Operations of the Observatory

Observatory Staff Dr D. A. Allen became the first appointee to the newly created permanent Staff As- tronomer position on 1 April 1983. Dr J. Lucey from the University of Sussex took up the SERC research fellowship which fell vacant on 1 October when Dr J. Bailey transferred to the Board's scientific staff. Owing to unexpected departures, the time required for advertising and selection, and delays in arrivals, the Observatory was one below its full complement of six staff astronomers for the entire year under review. Mr R. M. Smith, Experimental Officer, a member of the electronics group, resigned on 26 January to take up an appointment with the Cerro Tololo Inter-American Ob- servatory in Chile. Mr J. R. Rock, Supervising Draftsman, resigned on 31 March to enter private enterprise and Mr A. E. T. Schinckel, Technical Assistant, left on 29 April to take up an appointment at the Australian National Radio Observatory at Parkes. At 30 June 1983, the total number of full-time staff was 48, including 2 fixed-term appointees assisting with the programming of new instrumentation, plus the two SERC Research Fellows. There were 4 unfilled vacancies. A list of staff is provided at Appen- dix C, page 41. Building and Accommodation Programme The upper level of the Laboratory building at Epping was completed during 1982-83 and the new space, comprising the library, offices, and a conference room was occupied on 1 November 1982. At the Telescope the lunch room on the upper level of the workshop was extended to provide more space for the staff.

Allocation of Observing Time Under Article 5 of the Anglo-Australian Telescope Agreement, observing time on the Telescope and use of associated facilities and services is shared equally by Australia and the United Kingdom. It is the Board's responsibility to make arrangements consistent with this principle for the use of the Telescope and its associated facilities. The Board has chosen to exercise its responsibility for the allocation of time through arrangements made with the two designated agencies. Under guidelines laid down by the Board, each agency operates through a national committee—the Australian Time Assignment Committee (ATAC) or the UK Panel for the Allocation of Telescope Time (PATT)—which allocates time on the basis of the merit of proposals submitted by astronomers from each country and by the scientific staff of the Anglo-Australian Observatory. Arrangements also exist for the Director of the AAO and the Chairmen of the committees to co-ordinate research programmes; the Director is responsible for the detailed scheduling of the programmes. In 1982-83 there were 3648 night-time hours potentially available for observing, commissioning or telescope maintenance. The use of this time and comparisons with past years are shown below. Sometimes during instrument commissioning the equipment is tested by obtaining useful astronomical data, in which case the time is included in observing. The addition of daylight observing at infrared and microwave wavelengths brings the totals above 100 per cent. Details of scheduled night-time use by the home institutions of the astronomers are tabulated in Appendix B, page 33. This year representatives of two further countries- Canada and Finland—were awarded time on the Telescope, bringing the total to four- teen countries, besides Australia and the U.K. Percentage of total night-time hours

1979-80 1980-81 1981-82 1982-83

Night observing 60.0 60.6 58.1 60.8 Loss due to weather 35.0 34.5 36.6 35.4 Loss due lo AAT equipment failures 2.0 2.3 2.7 1.7 Loss due to visitors' equipment failures and set-up difficulties 1.5 0.4 0.9 1.0 Aluminising, instrument commissioning, and seeing tests 1.5 2.2 1.7 1.1 Daylight observing 2.5 2.9 1.5 2.0

Visiting Scientists During 1982-83 a greater emphasis was given to encouraging visits from scientists from other institutions to interact with the staff of the Observatory. Dr D. Axon from Uni- versity College London spent eight weeks at the Observatory in late 1982 and early 1983 and Professor Franz Kahn from the Department of Astronomy, University of Manchester, visited for two weeks in May.

Photography The programme of prime-focus service photography was continued in 1982-83, with eleven nights allocated during the year.

Public Relations Considerable interest has been shown in the infrared images described in the 1981-82 Annual Report (page 22-23 and Fig. 2) and in similar images acquired during the year. There have been requests for some of these as illustrative material for books and articles, and they have consequently been incorporated into the Observatory's stock of publicity material. The combination into a colour picture of three infrared images made at different wavelengths has produced some particularly pleasing results. The first set of such pictures was reproduced in a dedicated centre-spread article in the February 17 issue of New Scientist, while the planetary pictures were featured in a lead article in the February issue of Sky and Telescope. During 1982-83 about 34 400 tourists passed through the ANU Visitors' Centre at Siding Spring Observatory and saw the Telescope. 3 Research

Overview During the last decade, while progress in many areas of science has continued to be marked by a process of increasing specialisation, there has been within astronomy a convergence of separate sub-fields which has proved exceedingly productive. Thus, astronomical observers world-wide are becoming more versatile and are not confining themselves to single specialities such as optical, radio, or X-ray astronomy. The AAT has been one of the catalysts in this process, which has been greatly facilitated by interaction with radio-astronomy, traditionally strong in Australia, and X-ray and far ultraviolet astronomy which are areas of strength in the United Kingdom. In addition, the AAT itself is used for observations at infrared and millimetre wavelengths. This collaboration across different fields has been matched by co-operation among the different institutions at Siding Spring Mountain and Epping (see page 2) and, more recently, with astronomers from the United States and the United Kingdom responsible for conducting X-ray and ultraviolet observations from satellites. In all these complementary endeavours, the AAT's main role, and its greatest contribution, has been in the detection and examination of very faint objects. Briefly, some of the major areas under study are as follows:

Galaxies Galaxies are massive systems of stars, gas and dust, the largest galaxies having a mass greater than a million million times that of our own Sun. Most galaxies themselves are found in clusters, some having, only a few members while others have a thousand or more. Since galaxies occur throughout the whole visible Universe and are one of its principal components, we can hope to deduce the structure and evolution of the Universe from their study. The reliability of these deductions depends, however, on how well the galaxies themselves are understood. How do galaxies form? How do they interact? How does the luminosity and colour of a galaxy evolve as the Universe ages? Why are some galaxies powerful X-ray and radio emitters while others are not? And finally, why are some galaxies ejecting large quantities of gas from their nuclei? The current work on the AAT is helping to resolve some of these problems in conjunction with the UK Schmidt Telescope, CSIRO's Parkes Radio Telescope and various X-ray satellites.

Quasi-stellar Objects (QSOs) The study of quasi-stellar objects (quasars or QSOs) and related phenomena occupies a major part of the research programmes of both staff and visiting astronomers. The class of quasars contains the most luminous objects known in the Universe. They have been discovered by radio or optical surveys and, more recently, X-ray techniques have also become important in their detection. Some twenty years after the first discovery of a quasar, it is clear that many important questions still remain to be answered. We still do not understand what quasars are. The redshift of an object's spectral lines is generally accepted as an indication of its distance, but if this is so, many quasars must be a hundred times more luminous than the brightest galaxies. Some quasars also show irregular variations in their luminosity from one day to the next. An exotic system, such as a black hole with a mass of 100 000 000 suns which consumes a mass equivalent to our Sun each day, is one way to explain such high luminosity and its fluctuation. The effort to understand quasars includes the study of other extragalactic objects which share some of their properties. These objects are described as active galaxies because of X-ray or radio emission, variable light from the nucleus (BL Lacertae Objects) or bright nuclei having spectra with strong emission lines (Seyfert galaxies).

Stars Our nearest star, the Sun, lies a mere eight light-minutes away, but it is only one example among stars which vary widely in mass, other physical properties and internal structure. The A AT offers the potential for studying many of the 100 000 million stars in our Galaxy, and a good many in other galaxies besides, although the many competing demands for its time means that the Telescope must be used selectively to investigate particular members of each type. Data collected are used to determine the physical properties of stars and their internal structure and evolution, and to seek a better understanding of the nucleosynthesis of the elements. Amongst the varieties of stars studied are extremely dense white dwarf stars, some of which possess intense magnetic fields; symbiotic stars which simultaneously combine temperature regimes below 3000 K and above 100 000 K; hot stellar cores which have ejected material and now illuminate planetary nebulae; and stars which radiate disproportionately at X-ray or infrared wavelengths. Often the only examples are extremely faint and consequently must be studied through a large telescope.

Supernova Remnants (SNRs) Supernova remnants (SNRs) are the relics of stars which have ended their lives in violent explosions, throwing most of their matter off into space at velocities up to 10000 kilometres per second. SNRs in our own Galaxy are most easily found by a characteristic radio emission known as synchrotron radiation, which arises when charged particles (in this case electrons) move in a magnetic field at speeds approaching that of light. However, due to the absorption of light by interstellar dust within the galactic plane, only about 20 per cent of the SNRs have been identified optically. The situation is different in our nearest neighbour galaxies, the Large and Small Magellanic Clouds. Since the interstellar absorption is not large towards these galaxies, the success rate for optical detection is close to 100 per cent for both the radio SNRs and several new ones revealed by recent X-ray observations. The optical emission from the ionised gas inside the SNR shells indicates temperatures from 10 000 to 10 million degrees K, the hottest ones corresponding to the X-ray emitters. The remnants themselves are some of the most beautiful objects in the sky. Much work is currently being done to study how the ejected material interacts with the ambient interstellar matter, producing radiation throughout the spectrum from X-rays to radio frequencies.

Interstellar Material Between the stars of our Galaxy lies a turbulent domain of gas and dust. Some portions are tortured by the violent explosions of supernovae, while in other parts the gradual collapse of denser knots proceeds unhindered until stars form their material. Some regions are extremely tenuous; others contain such quantities of gas and dust as to dim the light of more distant stars a millionfold or more. AAT observations are made of the interstellar medium in its many guises. It is believed that much of the interstellar gas originates in stellar explosions—the supernovae. The chemical abundances in the remnants of supernovae provide evidence for nucleosynthesis, the process which creates heavy elements in stars. In the nearest galaxies, the Magellanic Clouds, the abundances of the chemical elements reveal the history of supernova explosions and stellar evolution. Dust clouds hide some of these processes from conventional optical telescopes, but infrared observations can now pierce the murkiest clouds to reveal hitherto unseen stars and demonstrate the presence of icy coatings on the dust grains themselves. Often one or more stars in a cloud of interstellar gas are hot enough to :onise the hydrogen. Then it glows bright red from the emission of the H a line when the hydrogen recombines. Lines of helium, nitrogen, oxygen, neon, sulphur and argon also can be present. In nebulae like Orion the hot stars have condensed from the surrounding interstellar gas in the last few million years. At the other end of stellar evolution, a planetary nebula is formed when a star which has consumed most of the nuclear fuel ejects a shell of gas and ionises it.

Gas Motions in Barred Galaxies About one half of ail spiral galaxies have an elongated central concentration of stars described as a bar. A typical barred spiral is shown in Figure 1. Any interstellar clouds of gas which orbit around the bar will move in rather distorted patterns as they pass in and out of the bar and are consequently accelerated by the combined gravitational pull of all the stars. Over the past few years astronomers in the USA and the Netherlands

Figure 1: The Barred Spiral NGC1365 In normal spiral galaxies the arms start from the nucleus and wind out in the characteristic pattern. However, in about one half of all spirals the arms originate from the ends of a bar, as shown in this plate of NGC 1365. The faint trail of a meteor or artificial satellite has crossed the upper left corner of the photograph. have developed a complex hydrodynamical theory to explain the motion of the gas in barred galaxies. By simulating the galaxy using a computer model, the velocity that the gas should have at each position in the galaxy can be predicted. One of the main predictions of this theory is that as the gas passes through the bar it will collide with other gas already there and lose velocity suddenly. According to this theory, the collision produces a huge shock wave which compresses the gas and creates the long thin dust lanes often seen along the leading edge of the bar in these galaxies. A crucial observational test of the theory is to measure the velocity of the 6as as it passes through the dust lane to see if it slows down by the predicted amount. Last year astronomers from the AAO and the Royal Observatory, Edinburgh used the Telescope to observe the barred spiral NGC 6221 and found that, indeed, the gas in that galaxy has a sudden change of velocity as it passes through f-s dust lane in good agreement with the predictions. Several other barred spirals observed with the AAT are now being studied to see if the same effect can be seen.

A Collapsing Superclr.ster Most galaxies are located in small groups, but there exist some very populous systems called clusters of galaxies which contain many hundreds of members. These clusters and groups are themselves often grouped together in larger systems called superclusters. It is suggested that the observed clustering of galaxies is produced by a step-by-step process of growth. First, galaxies collect together in groups and then some of these groups amalgamate to form the clusters. Has this process of cluster growth come to an end, or is it occurring today in the Universe?

Figure 2: A Rick Outer of Galaxies This superb photograph of the central region of a very populous cluster of galaxies in the constellation of Reticulum is from a deep exposure at the A AT. The cluster has a recession velocity of 18 000 km/s, which suggests its distance is about 600 million light-years.

10 Astronomers from the University of Sussex, the Royal Greenwich Observatory and the Royal Observatory, Edinburgh have recently surveyed a rich supercluster in the constellations of Horologium and Reticulum. This prominent supercluster consists of two very populous clusters of galaxies and a few smaller groups. The Reticulum cluster is shown in Figure 2. The two rich clusters have a separation of about 25 million light-years. By measuring the radial velocities of member galaxies in the supercluster components, the mass of the supercluster has been determined. The derived value strongly suggests that the supercluster has sufficient mass to cause it currently to be collapsing under the effect of its own gravity. It is estimated that the two rich clusters are approaching each other at about 300 km/sec and irc 5000 million years they will merge to form one enormous cluster of galaxies. Clearly the growth of clustering is occurring today in the Universe.

An Infrared Nucleus in M104 A number of spiral galaxies are known to have infrared nuclei. That is, they are significantly brighter in the infrared than would be expected from the amount of starlight seen at visible wavelengths. These nuclei have usually been detected by observations at a wavelength of lOjtm (micrometres) where the contribution of starlight is very small. However, at shorter wavelengths, for v/hich infrared detectors are much more sensitive, the contrast between such a nucleus and the starlight from the galaxy is much reduced. An infrared nucleus has been found in the spiral galaxy M104 (The Sombrero Hat galaxy) using the AAO infrared photometer in its imaging mode. Images of the central regions of the galaxy were made at wavelengths of 1.2fim and 2.2pm. The 1.2/tm image was subtracted from the 2.2/im image in such a way as to remove the expected starlight contributions. This left a point-like object at the centre of the galaxy which is significantly redder than starlight. The nature of the nucleus in Ml04 cannot be determined without further observations. Many such infrared nuclei are thought to be due to 'starbursts', episodes of recent star formation which give rise to many hot young stars. These stars heat surrounding dust causing it to emit the infrared radiation. Alternatively, the nucleus may be a low luminosity quasar-like object which is either intrinsically red or is reddened by obscuring dust clouds.

Asymmetric Supernova Explosion Astronomers at Mount Stromlo Observatory have investigated the dynamical properties of an unusual new supernova remnant discovered in the Small Magellanic Cloud. The remnant, shown in Figure 3, is the result of the catastrophic explosion, about 1000 years ago, of a star with a mass about 25 times that of the Sun. During the explosion, huge quantities of oxygen synthesised within the massive star were expelled outwards forming a network of visible filaments. These expanding filaments reveal both the composition of the material within the star and the nature of the supernova explosion. Measurements of Doppler shifts in the oxygen emission lines show that the filaments are expanding in a highly asymmetric manner with velocities between 2500 km/sec towards us and 4000 km/sec away from us. This asymmetry is believed to result from rotation of the exploding star. A further interesting observation concerns a faint emission halo which partially surrounds the remnant. Spectroscopic measurements show this region to be highly excited, most likely as a result of an intense ultra-violet burst of emission accompanying the supernova event. It is the first clear detection of such an effect.

11 Figure 3: An Oxygen-rich Supernova Remnant in the Small Magellanic Cloud This picture was obtained in the light of doubly ionised oxygen using the image photon counting system on the A AT. The remnant is in the centre of the picture and a bright region of ionised hydrogen is at the tower right. A faint halo of emission partially surrounds the supernova remnant, which has been found to be expanding at high velocity in a very asymmetric paltern.

Infrared views of Jupiter If, like pit vipers, we could sense infrared wavelengths, the sky would appear grossly different. Figure 4 shows how the view of the planet Jupiter changes as we progress beyond the visible range to various infrared wavelengths. 1. At a wavelength of 1.6Mm Jupiter still resembles the visible view. Bright and dark belts of cloud traverse the planets, and turbulent areas can be seen near the centre. Around the edge of the planet, especially near the poles, the increased path length through Jupiter's atmosphere reduces the amount of sunlight reflected. 2. At 2.2jtm the appearance is radically different. Much of Jupiter's atmosphere contains gaseous methane and ammonia. At this wavelength, methane absorbs rather well so that portions of the atmosphere rich in methane appear dark. By contrast note the bright poles, where methane is rare. One pole is brighter than the other because it is tilted slightly towards us. 3. At 4.8AHH we see a different view again. Rather than shining by reflecting sunlight, Jupiter is now radiating its own energy, released as the planet gradually shrinks. The

12 Figure 4: Infrared Images of Jupiter From top to bottom these pictures show Jupiter at wavelengths of 1.6pm, 2.2pm and 4.8pm, obtained from scans with the infrared photometer on the AAT. At 1.6pm the image has the bright and dark belts of clouds familiar from optical photographs; at 2.2pm methane in Jupiter's atmosphere strongly absorbs the incident solar radiation, causing the very dark belts; and at 4.8pm the planet's internal thermal radiation escapes through some of the more transparent cloud layers.

13 heat escapes only through certain of the cloud layers. Dark areas on this picture are opaque high-level clouds whilst bright areas are gaps in this upper cloud layer giving views of the warm interior. By observations such as these the chemistry and structure of the planet's atmosphere can be studied. These are just three of the many infrared images which have now been acquired using the infrared photometer (IRPS) with the precise scanning of the A AT.

NGC 4696—A Centre of Activity Clusters of galaxies are observed to be extended sources of X-ray emission which is caused by tenuous hot gas within the cluster. Theory suggests that denser cooled gas can be pushed down onto the central cluster galaxy by the pressure of the surrounding gas. Density inhomogene>.ies in this flow of gas can lead to the formation of visible blobs of material in the galaxy. Optical line emission is expected from the blobs of material giving the galaxy a filamentary appearance when imaged at the wavelength of this line emission. The giant central elliptical galaxy NGC 4696 in the Centaurus cluster is an X-ray source, and if this galaxy has a cooling flow it should show a filamentary structure. A team of astronomers from the University of Cambridge, Imperial College London and the AAO have recently obtained images of NGC 4696 at a wavelength of the emission features. These images show an extensive filamentary structure which extends up to 18 000 light-years from the galaxy nucleus and, in conjunction with X-ray observations, strongly implies that about 60 solar masses of material per year are falling on this galaxy. Another exciting discovery about this galaxy was made from adding four contrast- enhanced photographic plates of the cluster core. The result, presented in Figure 5 shows a large faint linear feature or jet which is aligned accurately with the nucleus of NGC 4696. This feature starts about 300 000 light-years from the galaxy and has a length of 250 000 light-years. It may be a jet of material being ejected from the galaxy, although further observations will be required to test this hypothesis.

Do Supernovae Liberate Dust? In the late stages of their lives some stars explode violently—as supernovae. The explosion is so energetic that simple elements may be processed to yield such exotica as lead and gold. The products of this cosmic alchemy disperse into space in gaseous form. But do solid grains of dust also form in the ejected gas? If so, supernovae will be important in seeding their parent galaxies with metallic grains which could form the nuclei of meteoric particles, and eventually new planets. Dust can be detected most readily by its infrared radiation when heated to a few hundred degrees above absolute zero. Some supernovae have been known to exhibit dust radiation about three months after their explosion, and this has been interpreted as evidence that dust grains are indeed formed in the outflowing gas. But there is an alternative: a dust cloud might already have enveloped the star before its eruption. In this case, the dust would be heated because of the great increase of radiation from within. A pulse of light would radiate outwards from the supernova at the speed of light, and this is the speed that would be inferred from the rate at which the dust cooled. By contrast, if the dust formed in a shell of ejected gas, it would cool at a rate commen- surate with the supernova's ejection speed, which is typically a few per cent of the speed of light. Since we can measure the rate of cooling of the dust, the two theories can, in principle, be tested. Results of this test have been inconclusive for the few supernovae observed to date. In 1982, however, a supernova erupted in the galaxy NGC 1332. Conditions conspired

14 in^mni

. . •*.. .• •. • • ••

'••', ".-.•'•. '%: '•?; ••.•'.•' ..*«. ."'•' •"':"-.. "."•*••• ":•• ' •• '

•.•••• *

Figare 5: Detection of a Ftfet Jer-Like Fealyre Associited with NGC 4696 The giant elliptical galaxy, NGC 4696, is the brightest member of the nearby Centaurus cluster. The lower picture shows a normal contrast image of the cluster core, with NGC 4696 the largest galaxy in the upper right corner. In the upper view is a high contrast version, derived in the AAO Laboratory from 3 plates taken on the CT10 4m. telescope by Malcolm G. Smith. This specially enhanced photograph shows the extremely faint jet-like feature extending towards the lower left corner. to be ideal for such a study to be made, and observations were secured by a team from AAO, Imperial College London, the University of Keele arid the Royal Observatory, Edinburgh. Analysis of the data showed unequivocally that the inferred speed of the dust was that of light. For the supernova in NGC 1332 at least, the dust grains were not formed from the rich chemical meliSe of the ejected gas.

15 4 Instrumentation

Introduction During the past three decades, with the aid of radio and space observations to complement the optical data, there has been a revolution in astronomy which has transformed a once conservative and archaic science into what is now recognised as the most exciting and rapidly advancing branch of physics. Over the same period the optical telescope, which developed slowly for a hundred years after the days of Herschel, has undergone a rapid transformation. Part of this is due to the development of computerised automation and part to the introduction of new, extremely sensitive, detection devices that for many purposes have replaced the photographic plate. Today, a telescope is only as good as the instrumentation that is used to gather, analyse and present the light received from the heavens, and to organise, digest and manipulate the data so gathered. The achievements of the A AT have been based primarily on detection systems and other instrumentation in the forefront of technology. Since its inception it has thus been able to maintain a position in the front line of discovery.

Available Equipment The instruments now available at the AAT are summarised in t'.ie following table. Some

Focus Equipment Detector Prime Autoguider with locally set probe. direct f/3.3 Prime focus camera—aspheric Full range of sizes and types of sensitised plate, doublet and triplet correctors, photographic plates. sub-beam prism. Carnegie image tube with S20 photocathode. RGOCCD camera. RCA thinned CCD. Cassegrain Acquisition and guidance unit including instrument rotator, autoguider with remotely set probe and S20 integrating TV for viewing fieid and slit. direct f/8 Ritchey-Chretien camera. Photographic plates, but only one plateholder 355 x 355 mm. Carnegie image tube with S20 photocathode. f/8orf/15 RGOCCD camera. RCA thinned CCD. f/8orf/15 Image photon counting system EMI 4-stage intensifier with quartz window (IPCS). photometers and S20 photocathode. f/8orf/15 Twin, chopping and auxiliary photometers. SI, S20 and GaAs photomultiplier tubes. f/15 Infrared photometer-spectrometer (IRPS). InSb photovoltaic detector. f/36 Chopping secondary and matching infrared photometer spectrometer. spectrographs f/15 Boiler and Chivens spectrograph. Image dissector scanner with extended S20 photocathode and quartz window. f/8 RGO spectrograph 25 and 82 cm Image photon counting system with quartz cameras—optional fibre optic coup- window and S20 photocathode. ler and optional spectropolarimeter RGO CCD camera. mode. Photographic plates (82 cm camera only). Coude f/36 Rotating mount for small auxiliary equipment

16 of the recent additions are described in more detail below. Further information can be found in the AAT Observer's Guide and the Quarterly Journal of the Royal Astronomical Society, v. 19, p. 234 (1978). An indication of the demand for, and actual usage of, each instrumental combination is given by the following table.

Summary of nights applied for and allocated*, per instrument 1982 September-1983 August

Nights Nights % nights applied for allocated allocated RGO spectrograph + IPCS 392 128 38.9 1R Photometer-Spectrometer 146 53 16.1 Prime focus with CCD camera 75 24 7,3 Taurus with IPCS 51 20 6.1 RGO spectrograph with fibre coupler and IPCS 43 18 5.5 RGO spectrograph with CCD camera 43 17 5.2 Hatfield polarimeter with IRPS 32 15 4.6 Spectropolarimeter, RGO spectrograph, IPCS 27 11 3.3 B & C spectrograph with IDS 19 5 1.5 Prime focus with Carnegie image tube 3 3 0.9 Prime focus direct photography 7 0.6 IPCS in direct mode 2 2 0.6 Twin-channel photometer 8 2 0.6 Outside users' equipment not listed above 86 29 8.8

Totals 934 329 100.0

* Allocations by PATT and AT AC only. The table does not include use of the AAT in the Director's discretionary time. In particular, eight nights' use of prime focus for the service photography programme is excluded.

Computing Facilities The AAT was the first large telescope of its type constructed to use a computer for all routine operations. The telescope is controlled by a Perkin-Elmer Model 70 computer. Two of its functions are to point the telescope precisely at celestial objects and to track them accurately across the sky. The computer compensates for the rotation of the Earth, its motion around the sun, atmospheric refraction and a variety of mechanical misalignments and flexures in.the telescope's structure. Th° accurate setting capability of the AAT—achieved by the combination of this computer correction with mechanical excellence—is recognised as a world standard. In routine use, the absolute pointing is good to three or four arcseconds, while a two arcsecond result can be achieved following a full pointing calibration on fifty accurately known stars. The relative pointing ac- curacy is similarly outstanding and permits precision acquisition to about 0.1 arcsecond relative to a star within a few degrees. Two more Model 70 computers, the instrumentation computers, are dedicated to the acquisition and on-line reduction of data. The duplication provides operational backup as well as greater flexibility in the testing of equipment and off-line data reduction without disturbing the observer. The interface between the computers and the instruments is based on the internationally accepted modular system known as CAMAC. At the Epping Laboratory another two Model 70 computers are configured to be similar to the instrumentation computers, and are used for the testing of new instruments, development of software and control of the Perkin-Elmer PDS microdensitometer. The AAO is grateful for a further Model 70 computer that has recently been obtained from St. Andrews University, Scotland, where there was no further use for it. This computer is being used in hardware development and testing, and is welcome as an additional spare unit for hardware support of the other systems in the longer term.

17 In recent years, as part of the instrumentation development programme, two larger computer systems based on the Digital Equipment VAX-11/780 have been installed, one each at the Telescope and the Epping Laboratory. The much greater capacity of these computers will be necessary for the acquisition of data from new detectors, and it will make efficient on-line and off-line data reduction and analysis possible. Similar VAX computers are widely used for astronomical purposes in Australia, the United Kingdom, and elsewhere. The Telescope VAX was initially limited in both disc storage and memory capacity, but this system has now been upgraded to be similar to the Lab- oratory system. Each VAX computer now has two 516 megabyte (Mb) disc drives, two 256 Mb disc drives, and two dual density magnetic tape drives. The Telescope system currently has 3.5 Mb main memory while that at the Laboratory has 4.5 Mb. There are now two Sigma ARGS 7000 series image display systems at both the Telescope and the Laboratory. The Observatory staff are currently engaged on preparing the VAX systems for on- line use with astronomical instrumentation. A VAX controller for CAMAC is being installed so that there will be a direct VAX interface for instruments as well as a direct control link between the VAX and the Telescope control computer, in the same way as for the Perkin-Elmer instrumentation computers. It is necessary to extend the VAX's input/output bus up to the Telescope control room; this will be the communication path between the VAX and the CAMAC system, and it also will be part of a high speed interface to each of the Perkin-Elmer computers for taking data from them into the VAX for additional processing. At the Telescope, a 75 Kw three-phase no-break power supply has been installed to provide AC power for the VAX computer to minimise down-time arising from power supply fluctuations and blackouts. This no-break supply should have adequate capacity to support future computers and instrumentation. The original, single-phase AAT no- break supply, which is now almost fully loaded, will be kept in operation. Consideration is being given to a system of communications links between the VAX computers of the AAO and those of other organisations, especially Mount Stromlo Ob- servatory, the CSIRO Division of Radiophysics, and the UK Starlink network. For remote communications at present each VAX computer has dial-up connections to the public telephone network. These are of major assistance to software support between Epping and Siding Spring, and they also provide a limited on line connection to Starlink computers in the UK. the latter via the Overseas Telecommunications Commission's MIDAS service. A daily exchange of "mail' messages between the AAO and Starlink establishments has begun, as an alternative to telex. At both the Telescope and the Laboratory, serial links (960 bytes per second) have been installed between the VAX and each Model 70. These carry astronomical data to the VAX, and are also being used to support all new program development for the Perkin-Elmer computers. A further potential application of these links is communication with the Model 70 computer which drives the Telescope, via the VAX, for the purpose of remote observing. Demonstrations of driving the Telescope remotely have already been made from the Epping VAX and from the Rutherford Appleton Labora- tory's VAX in the UK. While the Perkin-Elmer computers will need to be maintained for as long as they are supporting existing instrumentation and the Telescope drive, it is proposed that future new instruments should in general be interfaced directly to the VAX. The CCD and infrared detector systems currently under development are expected to be the first AAO instruments that will be entirely VAX orientated.

18 Development of Instrumentation

Image Photon Counting System (IPCS) A new EMI intensificr was installed in October 1982 to replace one that had lost sensitivity due to excessive exposure to light. The new tube's granularity, or fixed pattern noise, is the lowest yet seen and it is free of the floppy electrode which gave large image shifts when previous tubes were moved through a horizontal position. Other problems of small jitter and drifts in the image positions also have been much reduced. The dark current with the present cooling system is a little high for some high dispersion applications, unfortunately, but the improvements in granularity and stability are important for all observers.

Spectropolarimeter A polarimeter module has been built by the Royal Observatory, Edinburgh for use with the RGO spectrograph and IPCS. This system was successfully commissioned on the Telescope at the end of August 1982. The module makes use of a Pockels cell modu- lator, which is an electrically-switched quarter wave retarder. It is mounted in the acquisition and guiding unit on one of the guide probe arms and is switched in synchronization with the IPCS. Together with a calcite analyser mounted behind the spectrograph slit, the Pockels cell provides a measurement of the circular polarization of the source. Two achromatic quarter wave plates can be inserted into the beam for linear polarization measurements.

Hatfield Infrared-Optical Polarimeter A simultaneous infrared-optical polarimeter built at the Hatfield Polytechnic Institute has been used regularly on the Telescope over the last year. The polarimeter makes use of the AAO infrared photometer-spectrometer (IRPS) as its infrared detector. It is used at the Casscgrain focus of the AAT with the f/36 chopping secondary. The polarimeter has achieved very high sensitivity in the near-infrared J and H bands, making possible a number of projects which were not previously feasible. For example, the instrument was used for the first studies of infrared circular polarization in AM Herculis type binaries. Software for the instrument has been implemented on the AAO Interdata computers. This includes the facility for determining the polarization of an image by stepping the Telescope over a grid of points while making the measurements. This feature was used to make a polarization map of the infrared cluster in the Orion nebula. Other projects carried out with the instrument include studies of the wavelength dependence of polarization in Seyfert galaxies and BL Lac objects, and measurements of the infrared polarization of sources in the Galactic Centre.

Faint Object Red Spectrograph (FORS) To improve the AAT's capabilities in studying the very faintest objects, a new spectrograph, the FORS, has been constructed at the Observatory. It is designed with maximum efficiency in mind, and will form a simple addendum to the existing RGO spectrograph, thereby enhancing the versatility of this instrument. As detector, the FORS will utilise a charge-coupled device (CCD) for which the control electronics have also been designed and built at AAO. At the longer visible wavelengths the CCD will have about four times the sensitivity of the photoelectron counting system (IPCS). The FORS will become available to observers early in 1983-84. Uses of this instrument will include the study of galaxies and quasars at very great distances and hence at a very early stage in the evolution of the Universe.

19 Optical Fibres The AAO is among the first observatories to use optical fibres regularly as light guides for astronomical observations. These fibres are the large-core, step-index, fused silica variety which are normally used in short distance communication systems. An application which shows much promise is the use of fibres for multiple object spectroscopy. In some observing programmes the objects of interest lie clustered together and their images all fall within the field of view of the Telescope at one time. However, the standard astronomical instrument, the slit spectrograph, can be aligned with only one or possibly two of these objects at once. By positioning an optical fibre behind the focal plane image of each object of interest, the light can be collected for a large number of objects simultaneously. Light from each object can then be transferred down a fibre which can be lined up along the entrance slit of the spectrograph. The light is then dispersed in the normal manner and the spectrum from each fibre individually recorded. It is therefore possible to observe the spectra of many objects at once and thus save a considerable amount of valuable observing time. The prototype bundle of 25 fibres was first used on the AAT during December, 1981 and on several other occasions during 1982 by outside observers. With this experience an improved version with SO fibres and better throughput was built. This has been used with much success recently during a run of three nights when an average of two hours exposure was obtained for each of 400 objects. Even with a transmission efficiency of only SO per cent, the fibre system saved approximately 380 hours of telescope time over single-object spectroscopy. Development of these fibre systems is continuing, to further improve their efficiency and simplify their use. Other potential applications of fibres are being investigated. These include the use of coherent fibre bundles to transfer images to the Telescope's TV system for acquisition and alignment purposes; long lengths of fibre to couple the various foci to instruments in stable, stationary locations off the Telescope; and a bundle of fibres close-packed at the input end feeding a spectrograph to obtain the spectra of a grid of points across an extended object such as a nebula.

20 5 Financial Statements

A. Audited Accounts 1982-83 As provided for in the Anglo-Australian Telescope Agreement, the accounts, records and financial transactions of the Board are audited by the Australian Auditor-General. The form of the Board's financial statements is agreed between the Board and the authorities in each country. The Board submits detailed estimates of receipts and expenditure annually for approval by each Government, for a financial accounting period running from 1 July to 30 June. All estimates are expressed in Australian dollars.

REPORT OF THE AUDITOR-GENERAL In accordance with sub-section 19 (1) of the Anglo-Australian Telescope Agreement Act 1970, the accompanying financial statements of the Anglo-Australian Telescope Board for the year ended 30 June 1983 have been submitted for my report:— Operation Account—Statement of Receipts and Payments Statement of Fixed Assets at Original Cash Outlay I now report in terms of sub-section 19 (1) of the Act that the statements are in agreement with the accounts and records and in my opinion:— (a) the statements are based on proper accounts and records; and (b) the receipt and expenditure of moneys, and the acquisition and disposal of assets, by the Board during the year have been in accordance with the Act and the Agreement.

K. F. BRIGDEN A uditor-General 23 November 1983 Aaglo-Australian Telescope Board Stateauit of Fixed Assets it Original Cash Outlay as at 30 Jaae 1983

30 June 1982 30 June 1983

$'000 S'000 Buildings' and services 6 8312 74032 Telescope and ancillary equipment 6999 7179 Telescope instrumentation 1955 2 269 Plant, equipment, vehicles, furniture and fittings 1970 2 123 Development of the Siding Spring site, including contributions to The Australian National University3 and to local authorities 909 981 Library 102 109

18766 20 064 1 The Board's buildings at Siding Spring and Epping are on land owned by The Australian National University and the Com- monwealth Scientific and Industrial Research Organisation respectively. A permissive occupancy agreement was concluded between the Board and the Commonwealth Scientific and Industrial Research Organisation on I April 1983. Negotiations with The Australian National University in respect of a similar agreement over Siding Spring site are proceeding. ' Includes J9000 being the sort of land in Coonabarabmn owned by the Board and occupied by two sun" cottages. 1 Some site works have been undertaken by The Australian National Univeuity on the basis of the Board meeting the capital cost and interest over a twenty-year period. The amounts to be met over this period arc $759 932 for the capital expenditure and $674 708 interest. Repayments commenced in 1970-71. J.H. CARVER DC. MORTON Deputy Chairman of the Board Accounting Officer of the Board

21 Anglo-Australia* Telescope Board Operation Account Statement of Receipts and Payments for the Year Ended 30 June 1983

Receipts

Previous Year Current Year S $ Cash on hand 1 July 1982 9971 London imprest 9 971 400 Petty cash 400 — Cash at bank 1

Contributions by Contracting Parties 1 738 000 Australia 1884 000 1738 000 United Kingdom 1924 000'

9 723 Receipts from disposal of assets 11982 773 Recovery of employees' superannuation contributions paid in 325 advance by the Board in the previous financial year 439 Recovery of expenses incurred on behalf of users in former years 705 11074 Sales of photographs and other material to the public 10926 9407 Other revenue 210682

3 517 787 3 8633.78

Payments

1 302 793 Salaries and salary related expenditure 1 475 994 33 487 Expenses of the Board 34 767

106 380 Staff travel and subsistence 111707 13979 Recruitment of staff 16 279 103 726 Office and other expenses 102611 116833 Stores and materials 96957 115032 Repairs, maintenance and motor vehicle operating expenses 210406 138913 ANU service charge 192 837 Audit fees 12 300 108 173 Other service charges 128 120 12167 Furniture and fittings 17073

363 622 Instrumentation 357 618 556 454 Plant and equipment 346145 409 336 Buildings 573 063 18 527 Purchase of motor vehicles 19 985 36 259 Library 45 414 71732 Site works and development contribution to ANU4 71732

Cash on hand 30 June 1983 9971 London imprest 9 971 400 Petty cash 400 1 Cash at bank 39 9991

3 5177S7 3 863 378

1 lnchidHMaiwwiHorS40000rorcxpenditure(inyearending30.6.84. 1 IRCMM K 392 for natal of •oard homing by staff and S10 610 for refund of staff superannuation contributions plus

•an amount of S2 271 Motived by cheques and banked on 28 June 1983 and cleared on 6 July 1983. 1 Tht balance of liability to The AwtraKan National University for site works and development is $502 124. This amount inchinn both capital and intttut liability.

J. H. CARVER D. C. MORTON Deputy Chairman of the Soari Accounting Officer of the Board

22 B. Disposal of Assets in 1982-83 The financial rules adopted by the Board provide that a statement is presented which indicates any assets written off or disposed of and any losses written off in 1982-83. Assets Disposed Of or Written Off ii 1982-83

Date of Original Sale Method of Assets purchase cost proceeds disposal

% $ Polisher/scrubber, Bramil 150/300 22.05.73 161 Written Off Polishing Machine "Hishine" 16" 1970 130 Written Off Book, Library, quantity 9 — 98 Written Off Liquid Nitrogen Container LR.25 9.04.77 205 Written Off Canon Printing Calculator 15.07.74 186 Auction Canon Calculator 23.10.70 615 22 Auction Canon Calculator 26.05.71 304 Auction Motor Vehicle, Ford Cortina Reg. No. KJS 537 23.10.79 5 137 3 050 Auction Bull Bar for the above 10.12.79 226 Auction Ford Cortina Reg. No. KPH 769 13.03.80 6 308 3400 Auction Toyota Corona SE Reg. No. LDS 940 19.03.81 5 901 5 510 Tender

C. Expenditure Forecast 1983-84 to 1987-88 As well as providing detailed annual estimates to both Governments, the Board is required under Article 16 of the Agreement to submit outline estimates of expenditure to cover a five-year period. AAO Forecast of Expenditure1 Subject to the Approval of the two Contracting Parties SA'000 at estimated January 1984 prices

Item 1983-84 1984-85 1985-86 1986-87 1987-88

1. Salaries and salary related expenditure 1 593 1 570 1 570 1 570 1 570 2. Expenses of the Board 38 38 38 38 38 3. Staff travel and subsistence 115 115 115 115 115 4. Recruitment of staff 22 22 22 22 22 5. Office and other expenses 118 118 118 118 118 6. Stores and materials 116 116 116 116 116 7. Repairs, maintenance and motor vehicle operating expenses 183 183 183 183 183 8. Service charges 373 373 373 373 373 9. Instrumentation, plant and equipment, furniture and fittings 745 680 623 623 623 10. Buildings 265 55 50 50 50 II. Purchase of motor vehicles 22 22 22 22 22 12. Library 45 45 45 45 45 13. Site works and development contribution to ANU 72 72 72 72 72

3 707 3409 3 347 3 347 3 347 1 Approved by the Board in March 1983.

23 Appendixes

Appendix A

Research Papers Published Scientific Papers based on AAT data (1 July 1982 to 30 June 1983)* ADAMS, D. J.1, ADAMSON, A. J.1, GILES, A. B.11983. A 2.2-^m map of NGC 5128. Mon. Not.R.astr.Soc.V202,241. AITKEN, D. K.2, ALLEN, M. C.3, ROCHE, P. F." 1982. Spatial and spectral studies of the galactic centre near 10/um. A. I. P. Conf. Proc. No. 83: "The Galactic Centre", C. I. T., 1982., edited by G. R. Riegler and R. D. Blandford. N. Y., A. I. P., 1982, p67. AITKEN, D. K..2, ROCHE, P. F.41982.8-13fun spectrophotometry of compact planetary nebulae and emission line objects. Mon. Not. R. astr. Soc. V200,217. AITKEN, D. K.2/«, ROCHE, P. F.4, ALLEN, D. A.21982. The infrared spectrum of 7 Velorum. Mon. Not. R. astr. Soc. V200,69P. ALLEN, D. A.21982. Infrared studies of symbiotic stars. IAU Colloquium No 70 "The nature of symbiotic stars", edited by M. Friedjung and R. Viotti. Dordrecht, Reidel, p27. ALLEN, D. A.2, BAINES, D. W. T.\ BLADES, J. C.s WHITTET, D. C. B.61982. A survey of 3firn emission features in stellar spectra. Mon. Not. R. astr. Soc. V199,1017. ALLEN, D. A.2, BARTON, J. R.2, GILLINGHAM, P. R.2, CARSWELL, R. F.11982. The Lya/Ha ratio in high-redshift quasars. Mon. Not. R. astr. Soc. V200,271. ALLEN, D. A.2, CHEREPASHCHUK, A. M.81982. The ellipsoidal light curve of VV Puppis. Mon. Not. R. astr. Soc. V201,521. ALLEN, D. A.2, WARD, M. J.7, HYLAND, A. R.' 1982. The near-infrared continua of BL Lacertae objects. Mon. Not. R. astr. Soc. V199, p969. ALLEN, D. A.2, WRIGHT, A. E.10, ABLES, J. G.101982. The identification of CTA21. Jnl. Astrophysics and Astronomy V3,189. ALLEN, D. A.21983. Infrared views of the giant planets. Sky & Telescope. V65, P110. ALLEN, D. A.2, CRAGG, T. A.21983. The AAO JHKL photometric standards. Mon. Not. R. astr. Soc. V203,777. ALLEN, R. J.26, ATHERTON, P. D.",OOSTERLOO, T. A.26, TAYLOR, K.'2/= 1983. Recent Taurus results on Ha velocities in M83. IAU Symposium No. 100 "Internal kinematics and dynamics of galaxies" Besancon, France, 1982, p. 147. Edited by E. Athanassoula. Dordrecht, Reidel. ATHERTON, P. D.", TAYLOR, K.2, PIKE, C. D.12, HARMER, C. F. W.12, PARKER, N. M.'2, HOOK, R. N.131982. TAURUS: a wide-field imaging Fabry-Perot spectrometer for astronomy. Mon. Not. R. astr. Soc. V201,661. ATHERTON, P. D.", TAYLOR, K2/" 1983. TAURUS: a wide-field imaging Fabry-Perot spectrometre for astronomy. IAU Symposium No. 100 "Internal kinematics and dynamics of galaxies" Besancon, France, 1982 p. 31. Edited by E. Athanassoula Dordrecht, Reidel. AXON, D. J.4, ALLEN, D. A.2, BAILEY, J.14/', HOUGH, J. H.14, WARD, M. J.1, JAMESON, R. F.11982. The variable infrared source near HH100. Mon. Not. R. astr. Soc. V200,239. AXON, D. J.4, BAILEY, J.2, HOUGH, J. H.141982. The discovery of a very red nucleus in the radio elliptical IC 5063 (PKS 2048 57). Nature V299,234. BAILEY, J.'V'.HOUGH, J. H.'4, AXON, D. J.4, GATLEY, I.15, LEE, T. J.24, SZKODY, P.24, STOKES, G.M, BERRIMAN G." 1982. A multiwavelength study of the AM Herculis type binary 2A 0311-227. Mon. Not. R. astr. Soc. V199,801,1982. BAILEY,}."/', HOUGH, J. H.14, AXON, D. J.41983. The wavelength dependence of polarization in BL Lac objects. Mon. Non. R. astr. Soc. V203,339.

• The Board aims at recording in these annual lists all publications utilising AAT observations and all papers published by AAO staff. Papers inadvertently omitted from previous years are included where these have since come to notice.

25 BAILEY, J.14/', HOUGH, J. H.14, GATLEY, I.15, AXON, D. J.41983. Simultaneous IR and optical light curves of 2A 0311 -227. Nature V301, p223. BARLOW, M. J.4, HUMMER, D. G.M/» 1982. The WO Wolf-Rayet stars. IAU Symposium No. 99 "Wolf-Rayet Stars: observations, physics, evolution" edited by C.W.H. de Loore and A. J. Willis p. 287. Dordrecht. Reidel. BARRAL, J. F.", CANTO, J.", MEABURN, J.17, WALSH, J. R." 1982. The physical conditions within the poly-polar nebula NGC 6302-111. Mon. Not. R. astr. Soc. V199,817. BARRELL.S. L.' 1982. Beat Cepheid studies HI. Photometric search for additional beat Cepheids. Mon. Not. R. astr. Soc. V200,139. BESSELL, M. S.9, NORRIS, J.91982. Nitrogen overabundances in population II dwarfs. Astrophys. J.V263.L29. BESSELL, M. S.9, WOOD, P. R.91983. Shell ejection from the variable carbon star HV 2379. Mon. Not. R. astr. Soc. V2D2,3 IP. BESSELL, M. S.9, WOOD, P. R.9, LLOYD-EVANS, T." 1981. The masses and origins of carbon stars. Proc. astr. Soc. Austr. V4,201. BESSELL, M. S.9, WOOD, P. R.9, LLOYD-EVANS, T.1B 1983. carbon stars in clusters in the Galaxy and the Magellanic Clouds. Mon. Not. R. astr. Soc. V202,59. BLACKMAN, C. P."/2° 1982. Surface photometry and mass distributions of the interacting spiral galaxies NGC 5426 and 5427. Mon. Not R. astr. Soc. V200,407. BLADES, J. C.51982. Optical observations of halo gas. Observatory V102, No. 1050, pi 72. BLADES, J. C.2'5, HUNSTEAD, R. W.3, MURDOCH, H. S.3, PETTINI, M.121982. Optical absorption lin's in the high redshift BL Lac object 0215+015. Mon. Not. R. astr. Soc. V200, 1091 BOOTH, L.21, CHARLES, P. A.211982. The X-ray transient 3A 1431 -409: a highly active RS CVn system? Mon. Not. R. astr. Soc. V201,25P. BRAND, P. W. J. L.19, HA WARDEN, T. G.IS, LONGMORE, A. J.15, WILLIAMS, P. M.IS, CALDWELL, J. A. R." 1983. Cometary globule I. Mon Not. R. astr. Soc. V203,215. CARTER, D.2'9, MALIN, D. F.2,1983. A narrow line radio galaxy behind the Fornax cluster. Mon. Not. R. astr. Soc. V203,49P. CHARLES, P. A.21, PHILLIPS, M. M.21982. Einstein observations of the confused 2A 2315-428. Mon. Not. R. astr. Soc. V200,263. CHARLES, P. A.21, BOOTH, L.21, DENSHAM, R. H.21, BATH, G. T.21, THORSTENSEN, J. R.22, HOWARTH, I. D.\ WILLIS, A. J.4, SKINNER, G. K.2J, OLSZEWSKI, E.241983. Extreme variability in the Be-type, periodic recurrent X-ray transient AO538-66: a highly eccentric interacting binary. Mon. Not. R. astr. Soc. V202,657. CLOWES, R. G.33,1983. The variation with wavelength of the response of Kodak emulsion 11 la-J. AAS Photo-Bulletin, No. 32, p. 14. DANZIGER, I. J.25, BAADE, D.2$, ATHERTON, P. D.",TAYLOR, K.2, BOKSENBERG, A.12 1983. A dynamical and chemical study of NGC 6302.1AU Symposium No. 83 "Planetary Nebulae" London, 1982; edited by D. R. Flower, Dordrecht, Reidel. DANZIGER I. J.2S, GOSS, W. M.« 1983. Optical spectroscopy of 28 southern radio galaxies. Mon. Not. R. astr. Soc. V202; 703. DAVIES, R. L.', MORTON, D. C.21982. A mass estimate for the companion to the 'Cartwheel' galaxy. Mon. Not. R. astr. Soc. V201,69P. DAVIES, R. L."27, EFSTATHIOU, G.', FALL, S. M."28, ILLINGWORTH,G.2', SCHECHTER, P. L.2' 1983. The kinematic properties of faint elliptical galaxies. Astrophys. J.V266,41. DAVOUST, E.29, PENCE, W.21982. Detailed bibliography on the surface photometry of galaxies. Astron. Astrophys. Suppl. V49,631. DENSHAM, R. H.21, CHARLES, P. A.211982. Optical photometry and spectroscopy of the X-ray pulsar 1E1145.1-6141. Mon. Not. R. astr. Soc. V201,171. DIAZ, A. I.'2, PAGEL, B. E. J.12, EDMUNDS, M. G.M, PHILLIPS, M. M.311982. On the nature of the stellar population in the nucleus of the Sd galaxy NGC 7793. Mon. Not. R. astr. Soc. V201.49P. DOPITA, M. A.9, BINETTE, L.9, SCHWARTZ, R. D.321982. The two-photon continuum in Herbig-Haro objects. Astrophys. J. V261,183. DOPITA, M. A.9, SCHWARTZ, R. D.32, EVANS, I." 1982. Herbig-Haro objects 46 and 47: evidence for bipolar ejection from a young star. Astrophys. J. V263, L73.

26 ELLIS, R.33,1 983. Evolution of faint galaxies. International School of Cosmology and Gravitation, Erice, 1981. "The origin and evolution of galaxies" edited by B. J. T. Jones and J. E. Jones, p. 225. Dordrecht, Reidel, 1983. ELLIS, R. S.33, ALLEN, D. A.2,1983. Infrared colours of a complete sample of faint galaxies. Mon. Not. R. astr. Soc. V203,685. EFSTATHIOU, G.7, ELLIS R. S.33, CARTER, D.21982. Further observations of the elliptical galaxy NGC 5813. Mon. Not. R. astr. Soc. V201,975. FABIAN, A. C, ATHERTON, P. D.", TAYLOR, K.2, NULSEN, P. E. J.71982. Optical filament around NGC 4696 in the Centaurus cluster. Mon. Not. R. astr. Soc. V201,17P. FOSBURY, R. A. E.', BOKSENBERG, A.4", SNIJDERS, M. A. J.4, DANZIGER, I. J.2S, DISNEY, M. J.30,GOSS, W. M.» PENSTON, M. V.34'7, WAMSTEKER, W.25'34, WELLINGTON, K. J.10, WILSON, A. S.351982. Very extended ionised gas in radio galaxies-I. A radio, optical and ultraviolet study of PKS 2158-380. Mon. Not. R. astr. Soc. V201.991. FRENCH, R. G.^37, ELLIOT, J. L.*'3t, ALLEN, D. A.2 J 982. Inclination of the Uranian rings.. Nature V298,827. FRENCH, R. G.38, ELLIOT, J. L.3', DUNHAM, E. W.», ALLEN, D. A.2, ELIAS, J. H.3' FROGEL, J. A.31, L1LLER, W.™, 1983. The thermal structure and energy balance of the Uranian upper atmosphere. Icarus V53,399 GATLE Y, I.15, HYLAND, A. R.9, JONES, T. J.' 1982. Star formation in the Magellanic Clouds. II Discovery of a protostar in the Small Magellanic Cloud. Mon. Not. R. astr. Soc. V200,521. GENZEL, R.3', WATSON, D.3', TOWNES, C.3', DINERSTEIN, H.«, LESTER, D.«, WERNER, M.40, STOREY, J.21982. Detection of far-infrared [OI] and [OIII] from the Galaxy M82. Bulletin of the American Astr. Soc. V14, P611. GENZEL, R.3', WATSON, D.3', TOWNES, C.3', DINERSTEIN, H.« LESTER, D.« WERNER, W.40, STOREY, J. W. V.21982. OI and OIII in SGR A: Neutral and ionized gas at the galactic centre. A.I.P. Conference Proceedings No. 83 "The Galactic Center" C.I.T., 1982; edited by G. R. Riegler and R. D. Blandford. N.Y., A.I.P., 1982, p. 72. GILMOZZI, R.12, MURDIN, P.12, CLARK, D. H.5, MALIN, D.21983. Velocity and spectrum of the supernova remnant 30 Dor B. Mon. Not. R. astr. Soc. V202,927. GRAY, P. M.2, PHILLIPS, M. M.31, TURTLE, A. J.3, ELLIS, R.331982. Fibre optic development at the AAO. Proc. Astr. Soc. Austr. V4,477. GRIFFITHS, R. E.63, MURRAY, S. S.63, GIACCONI, R.63, BECHTOLD, J.63, MURDIN, P. G.'2, SMITH, M.15, MACGILLIVRAY, H. T.15, WARD, M.7, DANZIGER, J.25, LUB, J.25, PETERSON, B. A.', WR]GHT, A. E.10, BATTY, M. J.10, JAUNCEY, D. L.10, MALIN, D. F.21983. The optical identification content of the Einstein Observatory deep x-ray survey of a region in Pavo. Astrophys. J. V269,375. HANES, D. A.21982. A re-examination of the Sandage-Tammann extragalactic distance scale. Mon. Not. R. astr. Soc. V201,145. HANES, D. A.21982. Safe with Cepheids? Nature V300,478. HANES, D. A.2, GRIEVE, G. R.411982. UBV sequences for South Polar cap galaxies. Mon. Not. R. astr. Soc. V198,193. HANES, D. A.21983. The distance of the Virgo cluster. General Assembly IAU, Patras, Greece, 1982. IAU Highlights of Astronomy Vol. 6,227. Dordrecht. Reidel, 1983. HARRIS, D. E.42, ROBERTSON, J. G.43«, DEWDNEW, P. E.42, COSTAIN, C. H «1982. Radio and X-ray galaxies in Abell 566. Astron. Astrophys. VI11,299. HASSALL, B. J. M.7, PRINGLE, J. E.7, SCHWARZENBERG-CZERNY, A.7, WADE, R. A.', WHELAN, J. A. J.', HILL, P. W.» 1983. Ultraviolet and optical observations of the dwarf novae VW and WX Hydri during outburst. Mon. Not. R. astr. Soc. V203.865. HUNSTEAD, R. W.', DURDIN, J. M.3, LITTLE, A. G.\ REYNOLDS, J. E.3, KESTEVEN, M. J. L.31982.1733-565: A compact radio galaxy at low galactic latitude. Proc. Astr. Soc. Austr. V4,p447. HYLAND, A. R.', ALLEN, D. A.21982. An infrared study of quasars. Mon. Not. R. astr. Soc. V199.943. HYLAND, A. R.', JONES, T. J.', MITCHELL, R. M.441982. A study of the Chamaeleon dark cloud complex survey, structure and embedded sources. Mon. Not. R. astr. Soc. V201,1095.

27 JAUNCEY, D. L.10, BATTY, M. J.10,GULKIS, S.«, SAVAGE, A.'s 1982.2. 3-GHz accurate positions and optical identifications for selected Parkes radio sources. Astronomical Jnl. V87, 763. JONES, T. J.', HYLAND, A. R.9, CASWELL J. L.10, GATLEY, I.'51982. A search for the infrared counterpart of type II OH masers II: Statistical Analysis. Astrophys, J. V253,208. JORDEN, P. R.12, THORNE, D. J.12, VAN BREDA, I. G.121982. Royal Greenwich Observatory (RGO) charge-coupled device (CCD) camera. SPIE Proc. V331 "Instrumentation in Astronomy IV", p. 87. Edited by D. L. Crawford. KEENAN, F. P.46, DUFTON, P. L.46, MCKEITH, C. D.461982. Atmospheric parameters and chemical compositions of eighteen halo OB stars. Mon. Not. R. astr. Soc. V200,673. KEENAN, F. P.46, DUFTON, P. L.46, MCKEITH, C. D.46, BLADES, J. C.51983. Interstellar Call and Nal line profiles toward halo OB stars. Mon. Not. R. astr. Soc. V203,963. KING, D. J.33/20SCARROTT, S. M.", TAYLOR, K. N. R.471983. Optical polarization in the Serpens Nebula. Mon. Not. R. astr. Soc. V202,1087. KLIS, M. van der48, PARADIJS, J. van48, CHARLES, P. A.21, THORSTENSEN, J. R.22, TUOHY, I.', ELSO, J.' 1983. Photometric and spectroscopic observations of an optical candidate for the X-ray source H0544-665. Mon. Not. R. astr. Soc. V203,279. LUCEY, J. R.13, DICKENS, R. J.12, DA WE, J. A.'s, MITCHELL, R. J.121983. The Horologium-Reticulum supercluster of galaxies. Mon. Not. R. astr. Soc. V203,545. MALIN, D. F.21982. Photographic image intensificatoin and reduction—a unified optical approach. Journal of Photographic Science V30,87. MALIN, D. F.21982. Photography in astronomy. Physics Bulletin V33,207. MALIN, D. F.2, PETERSON, B. A.91982. Photometric calibration of astronomical photographic plates: II The Anglo-Australian Telescope prime focus spot sensitometer. Publ. astr. soc. Pacific V94,595. MASON, K. O.3"4, MIDDLEDITCH, J.64, CORDOVA, F. A.64, JENSEN, K. A.64, REICHERT, G.3', MURDIN, P. G.12, CLARK, D.s, BOWYER, S.39,1983. Optical indentification of the x-ray source E 1405-451: a 101.5 minute binary system with extremely rapid quasi-periodic variability. Astrophys. J. V264,575. MASON, K. O.39, MURDIN, P. G.12, TUOHY, I. R.9, SEITZER, P.9, BRANDUARDI-RAYMONT, G.4,1982. Phase resolved optical spectroscopy of the compact X-ray binary 2A 1822-371. Mon. Not. R. astr. Soc. V200,793. MATHEWSON, D. S.9, FORD, V. L.9, DOPITA, A. M.9, TUOHY, I. R.', LONG, K. S.49, HELFAND, D. J.s01983. Supernova remnants in the Magellanic Clouds. Astrophys, J. Suppl.VS 1,902. MEABURN, J.17, HEBDEN, J. C", MORGAN, B. L.", VINE, H." 1982. Speckle observations of RI36A. Mon. Not. R.astr. Soc. V200, IP. MEABURN, J.17, TERRETT, D. L.171982. The structure and dynamics of the nucleus of the hot spot galaxy NGC 2997. Mon. Not. R. astr. Soc. V200,1. MEABURN, J.17, WHITE, N. J.171982. A Herbig-Haro object in the core of M16(NGC 6611) Mon. Not. R. astr. Soc. V199,121. MEABURN, J.'7, WHITE, N. J.171982. The structure and dynamics of a 3.5pc diameter filamentary shell on the edge of the NGC 6344 interstellar complex. Mon. Not. R. astr. Soc. V200.771. MORGAN, D. H.15, NANDY, K.151982. Infrared interstellar extinction in the LMC. Mon. Not. R. astr. Soc. V199,979. MORTON, D. C.21983. Infall and outflow of S+3Ions in 15 Monocerotis, Tau Canis Majoris and lotia Orionis. Astrophys. J. V268,217. MURDOCH, H. S.3, HUNSTEAD, R. W.3, ARP, H. C.51, CONDON, J. J."'», BLADES, J. C.2, BURBliDGE, E. M." 1983.1107 + 036: An unusual QSO galaxy pair. Astrophys. J. V265, P610. NORRIS, J.9, FREEMAN, K. C.91983. The chemical inhomogeneity of M22. Astrophys. J. V2M.130. NULSEN, P. E. J.7,STEWART, G. C.7, FABIAN, A. C.7, MUSHOTSKY, R. F.s\ HOLT, S. S.55, KU, W. H-M.50, MALIN, D. F.21982. A detailed X-ray study of the cooling intraclustergas in A496. Mon. Not. R. astr. Soc. V199,1089. PENSTON, M. V.'2, LAGO, M. T. V. T* 1983. Optical and ultraviolet line profiles and ultraviolet line intensities in the T Tauri star LHa 332-21. Mon. Not. R. astr. Soc. V202, p77.

28 PETERSON, B. A.9, SAVAGE, A.15, JAUNCEY, D. L.'°, WRIGHT, A. E.'° 1982. PKS 2000-330: A quasi-stellar radio source with a redshift of 3.78. Astrophys, J. V260, L27. PHILLIPS, M. M.2/", TURTLE, A. J.2/3, EDMUNDS, A. J.30, PAGEL, B. E. J.121983. Remarkable kinematics of the ionized gas in the nucleus cf NGC 1365. Mon. Not. R. astra. Soc. V203,759. PICKLES, A. J.', VISVANATHAN, N.« 1982. Recent optical observations of the X-ray source HO J 39-68: an AM Herculis type binary system. Proc. Astr. Soc. Aust. V4,425. PI HLLIPS, M. M.2/31, MALIN, D. F.21982. NGC 4388: A Seyfert 2 galaxy in the Virgo cluster. Mon. Not. R. astr. Soc. V199,905. PHILLIPS, M. M.2/31, CHARLES, P. A.21 BALDWIN, J. A.311983. Nearby galaxies with Seyfert-like nuclei. Astrophys. J. V266,485. REAY, N. K.", ATHERTON, P. D.", TAYLOR, K.21983. Kinematic structure of planetary nebulae—I. The highly evolved nebulae Abell 30. Mon. Not. R. astr. Soc. V203,1079. REAY, N. K.", TAYLOR, K.2 ATHERTON, P. D." 1983. Kinematic structure of planetary nebulae—II. The Eskimo NGC 2392. Mon. Not. R. astr. Soc. V203,1087. REID, N.", GILMORE, G.IS 1982. New light on faint stars-II A photometric study of the low luminosity main sequence. Mon. Not. R. astr. Soc. V201, p73. SEWARD, F. D.63, HARNDEN, Jr., F. R.63, MURDIN, P.12, CLARK, D. H.51983. MSH 15-52: A supernova remnant containing two compact x-ray sources. Astrophys. J. V267,698. SHARPLES, R. M.", CARTER, D.2, HAWARDEN, T. G.'s, LONGMORE, A. J.151983. Kinematics of elliptical-like galaxies with dust lanes. Mon. Not. R. astr. Soc. V202,37. SHAVER, P. A.25, BOKSENBERG, A.12, ROBERTSON, J. G.21982. Spectroscopy of theQSO pair Q0018+O03/QO029 +003. Astrophys. J. V261, L7. SHAVER, P. A.25, ROBERTSON, J. G.21983. Common absorption systems in the spectra of the QSO pair QO3O7-195 A, B. Astrophys. J. V268, L57. SHAVER, P. A.25, ROBERTSON, J. G.21983. A new test of the cosmological interpretation of QSO redshifts. Nature V303,155. SHERRINGTON, N. R.1, JAMESON, R. F.1, BAILEY, J.u, GILES, A. B." 1982. Infrared light curves of the dwarf nova OY Carinae. Mon. Not. R. astr. Soc. V200,861. SHUKRE, C.""°, MANCHESTER, R. N.10, ALLEN, D. A.21983. SS 433 modelled as an aligned magnetic neutron star. Nature V303,501. SMITH, R. M.9, BICKNELL, G. V.', HYLAND, A.R.9, JONES, T. J.' 1983. Infrared observations of the jet in M87. Astrophys. J. V266,69. SMITH, G. H.', NORRJS, J.91983. The cyanogen distribution of the red giants in M5. Astrophys. J.V264,215. STOREY, J. W. V.21982. Mapping and imaging of the galactic centre in the near infrared. A.I.P. Conference Proceedings No. 83 "The Galactic Centre" C.I.T., 1982; edited by G. R. Riegler and R. D. Blandford. N.Y., A.I.P., 1982, p. 85. STOREY, J. W. V.21982. The potential for far infrared astronomy in Australia. Publ. astr. Soc. Austr.V4,474. STOREY, J. W. V.2, BAILEY, J.21982. Infrared images of Southern HII regions. Publ. astr. Soc. Austr.V4,429. STOREY, J. W. V.2, STRAEDE, J. O.2, JORDEN, R. R.12, THORNE, D. J.12, WALL, J. V.12 1982. A CCD image of the galactic centre. Nature V296,333. STOREY, J. W. V.21983. Detection of molecular hydrogen in G333.6-0.2 Mon. Not. R. astr. Soc.V202,105. SZKODY, P.", BAILEY, J. A.14, HOUGH, J. H." 1983. Optical and IR light curves of VV Puppis. Mon. Not. R. astr. Soc. V203,749. TAYLOR, K.2/12, ATHERTON, P. D." 1983. Taurus observations of the emission-line velocity field of the Centaurus A (NGC 5128) IAU Symposium No. 100 "Internal kinematics and dynamics of galaxies" Besancon, France, 1982, p. 311. Edited by E. Athanassoula. Dordrecht Reidel. TOWNES, C. H.39, GENZEL, R.39, WATSON, D. M.3', STOREY, J. W. V.21983. Detection of interstellar NH3 in the far-infrared: warm and very dense gas in Orion—KL. Astrophys. J. V269.L11 TUOHY, I. R.', CLARK, D. H.5, BURTON, W. M.s 1982. The peculiar X-ray morphology of the supernova remnant G292.0+1.8: evidence for an asymmetric supernova explosion. Astrophys. J. V260, L65.

29 TUOHY, I. R.', DOP1TA, M. A.9, MATHEWSON, D. S.9, LONG, K. S.», HELFAND, D. J.50 1982. Optical identification of Balmer-dominated supernova remnants in the Large Magellanic Cloud. Astrophys. J. V261,473. TUOHY, I. R.', DOP1TA, M. A." 1983. Ring ejection of Type II Supernova: IE 0102.2-7219 in the Small Magellanic Cloud. Astrophys. J. V268, LI 1 WALSH,J. R." 1983. NGC 2346: a bipolar nebula produced by mass-loss from a binary system. Mon. Not. R. astr. Soc. V202,303. WARD, M.\ ALLEN, D. A.2, WILSON, A. S.3S, SMITH, M. G.'s, WRIGHT, A. E.101982. The near infrared properties of Seyfert and related active galaxies. Mon. Not. R. astr. Soc. V199, 953. WATSON, D. M.3', GENZEL, R. L.39, TOWNES, C. H.39, STOREY, J. W. V.' 1982. Spectroscopy of Orion-KL: new far-infrared observations of CO and OH emission lines and the far-infrared detection of NH3. Bulletin of the American Astr. Soc. V14,p. 610. WATTS, D. J.", GREENH1LL, J. G.57, HILL, P. W.2, THOMAS, R. M.581982.2AO526-328, an optical and X-ray study of a cataclysmic variable. Mon. Not. R. astr. Soc. V200,1039. WERNER, M. W.«, DINERSTE1N, H. L.« HOLLENBACH, D. J.«, LESTER, D. F.« GENZEL, R.3', WATSON, D. M.39, STOREY, J. W. V.21982. The distribution of OI63 nm emission from the Orion nebula region. Bull. American Astr. Soc. V14, p. 610. W1CKRAMASINGHE, D. T.1S, STOBIE, R. S.15, BESSELL, M. S.' 1982. Simultaneous spectroscopy and photometry of the non-synchronous rotator H2252-O35. Mon. Not. R. astr. Soc.V200,605. WICK.RAMASINGHE, D. T.15, REID, N.'51983. The DB white dwarfs—I. The He 14388+4471 +4516 blend. Mon. Not. R. astra. Soc. V203,865. WILKES, B. J.7, CARSWELL, R. F.' 1982. The Lyman-alpha emission-lijie profiles in high-redshift QSOs. Mon. Not. R. astr. Soc. V201,645. WILKES, B. J.7, WRIGHT, A. E.J/1°, JAUNCE Y, D. L.10, PETERSON, B. A.91983. An atlas of QSO spectra. Proc. astr. Soc. Austr. V5,2. WOOD, P. R.9, BESSELL, M. S.' 1983. Long-period variables in the galactic bulge: evidence for a young super-metal-rich population. Astrophys. J. V265, p. 748. WELSH, Barry. Y.41983. Optical observations of the interstellar absorption lines toward the M8 nebula. Astrophys. & Space Science V90,437.

Appendix A Part 2

Papers Delivered at AAO Symposia

Thirteenth AAO Research Symposium, University of Sussex, September 1982

BATH, G. T.21 and MANTLE, V. J.21 Interpretation of the Cambridge VW Hydri observations. WATSON, F. G.15, CLUBE, S. V. M.ls and GRAY, P. M.1S R R Lyrae velocities. GONDH ALEKAR, P. M.5, MORGAN, D. H.ls and ELLIS, R. S.33 Infrared colours of dwarf blue emission line galaxies. WALSH, J. R.17 The structure of the R Monocerotis, NGC 2261 and HH39 Nebula Complex. HANES, D. A.2 The chemical composition of globular clusters in galaxies. DAVIES, J. K.6, WHITTET, D C. B.6, KILKENNY, D.", BAINES, D. W. T.4, BODE, M. F.59 and EVANS, A.39 Optical and infrared simultaneous monitoring of pre-main-sequence stars. BODE, M. F.S9, EVANS, A.59, KILKENNY, D.18, WHITTET, D. C. B.'and DAVIES, J. K.6 Infrared observations of Nova Aquilae, 1982. SHERRINGTON.M. R.1 Infrared observations of VZ Sculptor. HILDITCH, R. M.20 and KING, D. J.20 Solar-type interacting binary systems. WHITTET, D. C. B.', DAVIES, J. K.\ BAINES, D. W. T.4, BODE, M. F.59 and EVANS, A.59 3-micron spectrometry of Herbig Be/Ae stars. SAVAGE, A." Radio and optical selection effects in searches for high redshift quasars.

30 GASKELL, C. M.7 Narrow emission lines in high redshift quasars and the origin of'infalling' absorption line systems. ROBERTSON, J. G.2 and SHAVER, P. A.2 Absorption lines in close pairs of quasars. COUCH, W. J.33 ELLIS, R. S.33, GODWIN, J.21, CARTER, D.' and NEWELL, E. B.' CCD 1 observations of distant galaxy clusters. INGLIS, I.33, CARTER, D.3\ EFSTATHIOU, G.» and ELLIS, R. S.33 Nuclear velocity dispersions of giant elliptical galaxies. BUTCHINS, S. A.21 Observational evidence for recent evolution of galaxies. ADAMS, D. J.1 and ADAMSON, A. J.1 J H K mapping of M83 and Centaurus A. MEABURN, J.17, MORGAN, B. L.", PEDLAR, A.62 and SPENCER, R.62 Nucleus of NGC 1068. EDMUNDS, M. G.30, PHILLIPS, M. M.2, TURTLE, A. J.3and PAGEL, B. E. J.'2 Velocity field of NGC 1365. BOOTH, L.21 and DENSHAM, R. H.21 Photometry and spectroscopy of the recurrent X-ray transient AO 538-66. ELLIS, R. S." and ALLEN, D. A.2 Multi-object spectroscopy at the Anglo-Australian Telescope. METCALFE,N.21 Multi-colour photometry of the SC 1329-311 cluster of galaxies off UKSTU plates. ATHERTON, P. D." Taurus. DAVIES, R. L.7 The kinematics of low luminosity elliptical galaxies. WARD, M.7 CCD spectroscopy. ALLEN, D. A.2, BODE, M. F.w, EVANS, A.59, GRAHAM, J." LONGMORE, A. M.15, MIEKLE, P.", PEARCE, G.5', SELBY, M." and WILLIAMS, P." Dusty extragalactic supernovae. BRANSGROVE, S.wand BECKMAN, J.60 Velocity field of the barred spiral NGC 1566.

Fourteenth AAO Research Symposium, CSIRO Division of Radiophysics, Epping, March 1983.

HUNSTEAD, R. W.3, MURDOCH, H. S.3, PETTINI, M.12 and BLADES, J. C.5" Techniques for analysing the detailed velocity structure in QSO/BL Lac absorption lines. ROBERTSON, J. G.2, and SHAVER, P. A.25 Absorption systems in the spectra of the QSO pair Q0307-195A/B. MURDOCH, H. S.3, HUNSTEAD, R. W.3, CONDON, J. J.»and PHILLIPS, M. M.2-31 Tidal interaction between a QSO and nearby galaxy. PETERSON, B. A.9 QSO absorption lines. WRIGHT, A. E.10, ALLEN, D. A.2 and ABLES, J. G.10 Infrared data on a representative sample of compact radio sources. CARTER, D.9, VISVANATHAN, N.' and PICKLES, A.' Far-red spectroscopy of various galaxies. KILLEEN, N.' Two-dimensional IR observations of the M87 jet. ELLIS, R. S.33, COUCH, W. J.33, GODWIN, J.2', CARTER, D.' and NEWELL, E. B.' CCD observations of distant clusters of galaxies. VISVANATHAN, N.9 A global value of the Hubble constant. MORTON, D. C.2 and DAVIES, R. L.7-27 The Cartwheel Galaxy and its companions. ROCHE, P. F.4- **, AITKEN, D. K.4-44 and PHILLIPS, M. M.2-3I The nature of 10 j«m emission from galaxy nuclei. SMITH, R. M.' The study of the elliptical/spiral pair of galaxies NGC 5090/5091. TUOH Y, I.9 and DOPITA, M.' The velocity structure of the young oxygen-rich supernova remnant in the Small Magellanic Cloud. H YLAND, A. R.9 The cool stellar population in the Bar of the Large Megellanic Cloud. GRAY, P. M.2 Fibre optics at the AAO. BOTHWELL, G. W.2 Future plans for AAO computers. FREEMAN, K. C.9 Report on instrumentation meetings. RUELAS, A.9 Photometric studies of the stellar population in Baade's window. R ATNATUNGA, K. A.9 Discovery of two carbon stars in the outer regions of our galactic halo.

31 WOOD, P. R.» Shell ejection from the variable carbon star HV2379 ALLEN, D. A.2 Infrared views through the AAT. BAILEY, J.2, ALLEN, D. A.2, AXON, D. J.4 and HOUGH, J. H.14 Imaging polarimetry of the Orion Nebula at 2.2 microns. TAYLOR, K. N. R.47 and STOREY, J. W. V.47 The Corona Austrina T-Association.

Institutional list 1. University of Leicester. Astronomy Department. 38. Massachusetts Institute of Technology. Department of 2. Anglo-Australian Observatory. Physics. USA. 3. University of Sydney. School of Physics. 39. University of California. Berkeley. USA. 4. University College London. Department of Physics 40. NASA Ames Research Center. USA. and Astronomy. 41. University of Toronto and David Duntap Observatory. 5. Rutherford Appleton Laboratory. Canada. 6. Preston Polytechnic. Division of Physics and 42. Herzberg Institute of Astrophysics. Canada. Astronomy. 43. Netherlands Foundation for Radio Astronomy. 7. Institute of Astronomy. Cambridge. Dwingeloo. The Netherlands. 8. Slernberg Slate Astronomical Institute, Moscow. 44. University of Melbourne. RAAF Academy. School of USSR. Physics. 9. Australian National University. Mount Stromlo & 45. California Institute of Technology. Jet Propulsion Siding Spring Observatory. Laboratory. USA. 10. CSIRO Division of Radiophysics. 46. The Queen's University of Belfast. Department of Pure 11. Imperial College London. Astronomy Group, Blacken and Applied Physics. Laboratory 47. University of NSW. School of Physics. 12. Royal Greenwich Observatory. 48. University of Amsterdam. Astronomical Institute. The 13. University of Sussex. Astronomy Centre. Netherlands. 14. Halfield Polytechnic Institute. School of Natural 49. John Hopkins University. Baltimore. USA. Sciences. 50. Columbia University. Columbia Astrophysics 15. Royal Observatory Edinburgh. Laboratory. USA. 16. Universidad Nacional, Autonoma de Mexico. Institute 51. Mount Wilson and Las Campanas Observatories. de Astronomia. Mexico Carnegie Institute of Washington. USA. 17. University of Manchester. Department of Astronomy. 52. National Radio Astronomy Observatory. USA. 18. South African Astronomical Observatory. South 53. Virginia Polytechnic Institute. Department of Physics. Africa USA. 19. University of Edinburgh Department of Astronomy. 54. Center for Astrophysics and Space Sciences. University 20. University Observatory. St. Andrews. of California. San Diego. USA. 21. University of Oxford. Department of Astrophysics. 55. NASA Goddard Space Flight Center. USA. 22. Dartmouth College, Hanover. Department of Physics 56. l/niversidade do Porto. GrupodeMatcmatica and Astronomy. USA. Aplicada. Portugal. 23. University of Birmingham. Department of Space 57. University of Tasmania. Physics Department. Research. 58. Defence Research Centre. Salisbury, Adelaide. South 24. University of Washington. Department of Astronomy. Australia. USA. 59. University of Keele. 25. European Southern Observatory. Europe 60. Queen Mary College, London. 26. Kapteyn Astronomical Institute. Groningen. The 61. Space Telescope Science Institute, John Hopkins Netherlands University. USA 27. Kill Peak National Observatory. USA. 62. Nuffield Radio Astronomy Laboratories, Jodrell Bank. 28. Institute for Advanced Study, Princeton, New Jersey. 63. Karvard-Smithsonian Centre for Astrophysics. USA. 64. University of California, Los Alamos National 29. ObservatoiredeBesancon. France. Laboratory, USA. 30. University College of Wales, Cardiff. Department or 65. Pennsylvania State University. Department of Applied Mathematics and Astronomy. Astronomy. USA. 31. Cerro Tololo Inter-American Observatory. USA/Chile 66. Battelle Observatory. Richland, Washington. USA. 32. University of Missouri. Department of Physics. USA. 67. California Institute of Technology. Division of Physics, 33. University of Durham. Department of Physics. Mathematics and Astronomy. USA. 34. European Space Agency, Villafranca Satellite Tracking 68. University of Colorado. Joint Institute for Laboratory Station. Astronomy Division ESTEC. Astrophysics. USA. 35. University of Maryland. Astronomy Program. USA. 69. United States. National Bureau of Standards. 36. Massachusetts Institute of Technology. Department of 70. Instituto Isaac Newton. Ministerio de Educacion de Earth and Planetary Sciences. USA. Chile. 37. Wellesley College. Department of Astronomy. 71. Raman Research Institute. Bangalore, India. Massachusetts. USA.

32 Appendix B

Telescope Allocation Allocation of night time by institution Scheduled night-time use by astronomers is entered as nights allocated per quarter, per applicant, summed by home institution. For the purposes of compiling the data, time allocated for collaborative programmes has been divided equally among the collaborators.

Semesters

PATT Allocations 1982 Sept.- 1983 (to UK institutions except where indicated) 1983 Feb. Mar.-Aug. AAO - Australian Scientific Staff 2.6 - UK Scientific Staff 5.5 5.4 - Director 3.0 - SERC Fellows 3.0 2.5 - Technical Staff 0.7 3.1 Arizona State University (USA) 1.0 CerroTololo Inter-American Observatory (USA/Chile) 2.1 0.5 Institute of Astronomy, University of Cambridge 10.9 11.1 Hatfield Polytechnic Institute 1.7 2.0 Imperial College of Science and Technology, London 4.5 1.5 Kapteyn Astronomical Institute, University of Groningen (Netherlands) — 1.4 Mount Stromlo & Siding Spring Observatories, Australian National University (Aust.) 2.0 — Preston Polytechnic _ 1.2 Queen's University, Belfast 2.0 Royal Greenwich Observatory 9.1 11.7 Royal Observatory, Edinburgh 5.2 8.5 Rutherford Appleton Laboratory 3.3 3.9 University College London 4.6 6.9 University College of Wales, Cardiff 1.7 0.5 University of Birmingham 0.8 — University of Durham 3.7 4.4 University of Edinburgh 3.8 — University of Hawaii (USA) — 3.0 University of Keele 0.7 1.2 University of Leicester 2.3 5.0 University of Manchester 1.8 3.2 University of Montreal (Canada) 1.0 — University of Oxford 2.2 0.4 University of Sussex 4.1 0.5 University of Sydney (Aust) 1.9 —

Total 80 83

33 Quarters AT AC Allocations (to Australian institutions except where indicated) 82/4 83/1 83/2 83/3

AAO - Australian Scientific Staff 2.0 1.0 2.8 1.7 - UK Scientific Staff 0.2 1.9 0.5 2.7 - Director 2.3 1.2 0.5 0.5 - SERC Fellows 1.0 1.0 - Technical Staff 0.5 0.5 — 0.5 Australian National University, Dept. of Mathematics 0.3 0.7 CerroTololo Inter-American Observatory (USA/Chile) 0.4 0.4 0.7 CSIRO Division of Radiophysics 1.5 1.0 3.7 1.2 European Southern Observatory (Europe) 1.0 1.5 1.0 Helsinki Observatory (Finland) — — 0.2 0.5 Imperial College of Science and Technology, London (UK) _ 0.3 _ _ Massachusetts Institute of Technology (USA) — — 2.0 0.5 Mount Stromlo & Siding Spring Observatories, Australian National University 23.4 19.9 21.4 16.6 Princeton University Observatory (USA) 0.7 1.3 0.5 0.5 Royal Greenwich Observatory (UK) 0.7 0.8 0.5 Royal Observatory, Edinburgh (UK) 2.0 1.0 1.8 1.4 Rutherford Appleton Laboratory (UK) 0.2 — 0.5 — Space Telescope Science Institute, John Hopkins University (USA) 0.5 _ _ 0.5 University College London (UK) 0.6 0.7 University of Chicago (USA) 0.5 0.5 University of Durham (UK) 0.5 0.3 1.0 University of Melbourne 1.3 2.0 University of Minnesota (USA) _ 1.0 _ University of Montreal (Canada) 1.6 University of New South Wales 1.0 2.7 1.2 3.5 University of Oxford (UK) — 1.0 University of Queensland 2.0 University of Sydney 2.0 1.5 1.0 1.0 University of Tasmania _ 1.5 University of Texas (USA) 0.7 1.2 University of Wollongong — 0.8 — —

Total 40 39 43 41

Director's Discretionary Time—

Instrument Commissioning, Seeing Tests, Aluminising, Service Photography, etc. 10 13 8 8

34 Summary of Observing Programmes 1982 Quarter IV 1983 Quarters I, II & HI A list of the abbreviations used for institutions follows this table.

Number of Nights Observers and Institutions Allocated Title of Observing Programme

Adams, D. J., Adamson, R. S. and Warwick, R. S. 2 Infrared (J-K) colour gradients in spiral (Leicester) galaxies Aitken, D. K., Roche, P. F. (Melbourne) and 3 Spectropolarimetry of astronomical objects Bailey, J.(AAO) between 8 and 13 microns Allen, D. A. (AAO) and Hyland, A. R. (MSSSO) 2 Infrared imaging of the Orion nebula Allen, D. A. (AAO) 1 Luminosities of symbiotic stars Allen, D. A. (AAO), Ellis, R. (Durham) and 1 Evolution in distant field galaxies Peterson, B. A. (MSSSO) Allen, D. A. (AAO) 1 Infrared [Fe II] lines Allen, R. J., Atherton, P. D. and Oosterloo, T. A. I The kinematics of ionized gas in M83 (Groningen) Argue, A. N. (IOA), Morgan, B. L. and Vine, H. I Selection of objects to tie Hipparcos (ICST) astrometric measurements to extragalactic reference frame Atherton, P. D. (ICST), Ward, M. J. (IOA) and 3 Multi-object spectroscopy in deep X-ray Taylor, K. (AAO) survey fields Axon, D. J. (UCL), Allen, D. A. Bailey, J. (AAO) 3 Is there a bipolar outflow from the and Hough, J. H. (Hatfield) Becklin-Neugebauer object? Axon, D.J. (UCL) 1 i High velocity molecular flows: do they penetrate into HII regions? Axon, D. J. (UCL), Ward, M. J. (IOA), Hough, J. 8 High resolution spectropolarimetry of the H. (Hatfield), Bailey, J. (AAO), McLean, I. and emission lines in Seyfert galaxies Heathcote, S. (ROE) Bailey, J. (AAO), Hyland, A. R. (MSSSO) and 4 Simultaneous infrared and optical Axon,D.J. (UCL) polarirnetry of BL Lac objects Bailey, J. (AAO), McLean, I., Heathcote, S. R. 3 Spectropolarimetry of AM Herculis type (ROE), Axon, D. J. (UCL) and Hough, J. binaries (Hatfield) Barlow, M. J., Clegg, R. E. S. and Seaton, M. J. 2 Determination of the carbon abundances and (UCL) the ionisation structures of southern planetary nebulae Bessell. M. S. and Norris, J. E. (MSSSO) I 47 Tucanae and the abundance scale of globular clusters Bessell, M. S. (MSSSO), Wickramasinghe, D. T. 1 High speed photometry of DA and DB white (ANU) and Wood, P. R. (MSSSO) dwarfs Bessell, M. S., Freeman, K. C. and Wood, P. R. 4 Kinematics of long period variable stars in (MSSSO) the Large Magellanic Cloud Bessell, M. S. and Norris, J. E. (MSSSO) 2 Element abundances in population II dwarf stars Bessell, M. S., Wood, P. R. (MSSSO) andCarty, 1 i Time-dependent angular diameters of Mira T. C. (AAO) variables Binette, L., Dopita, M. A., Jenkins, C. R., Sadler, 4 Southern emission-line E and SO galaxies E. (MSSSO) and Phillips, M. M. (CTIO) Blades, J. C. (RAL), Pettini, M. (RGO), 5 High resolution spectroscopy of the BL Lac Murdoch, H. S. and Hunstead, R. W. (Sydney) object0215 + 015

35 Burton, P., Van Nagy—Felsobuki, E., Smith, L. 1 Search for H3 + emission from dark clouds (Wollongong) and Storey, J. W. V. (UNSW) Buta, R., Kalnajs, A. (MSSSO), Taylor, K. 1 Kinematics of ringed spiral galaxies (AAO) and Atherton, P. D. (RGO) Carswell, R. F., Webb, J. K. (IOA) and Baldwin, 4 The intergalactic medium at high redshifts J.A. (CTIO) Carter, D. (MSSSO) and Gray, P M. (AAO) 1 Dynamics of the rich cluster of galaxies 0004. 8-3450 Carter, D. (MSSSO) and Gray, P. M. (AAO) 1 Fibre optic investigation of the dynamics of rich clusters of galaxies Carter, D., Bicknell, G. V., Smith, R. M., Saddler, 2 CCD and infrared surface photometry of E. M., Killeen, N. E. (MSSSO), Jenkins,C. R. active and normal galaxies (RGO) and Reid, N. (ROE) Carter, D., Visvanathan, N. and Pickles, A. J. 4 Dwarf star indicators in galaxies (MSSSO) Charles, P. A., Booth, L., Densham, R. H. 3 Simultaneous optical, ultraviolet and X-ray (Oxford) and Skinner, G. K. (Birmingham) observations of the periodic recurrent X-ray transient A0538-66 Chen, J. S. (ESO) and Morton, D. C. (AAO) 1 Study of unidentified absorption lines longward of Lyman alpha emission in the QSOPKS 0528-250 Clark, D. H. (RAL), Murdin, P. G., Wood, R. 4 The study of southern supernova remnants (RGO) and Allen, D. A. (AAO) Clark, D. H., Wallace, P., Kent, B. (RAL) and 2 Development of a scanning long-slit mode for Fosbury,R.A.E.(RGO) the RGOspectograph/IPCS Clube, S. V. M., Watson, F. G. (ROE) and Gray, 4 Sp;ctroscopy of variable stars in the Galactic P. M. (AAO) nuclear bulge Cooke,J. A., Beard, S.M., Emerson, D. 3 Velocity calibration of spectra from UK (Edinburgh) and Kelly, B. D. (ROE) Schmidt objective prism plates Couch, W. J. and Sharpies, R. M. (Durham) 3 Infrared observations of Butcher-Oemler clusters of galaxies Dopita, M. A., Evans, I. (MSSSO), Gondhalekar, 1 Hyperactive star formation in blue emission P. M. (RAL) and Morgan, D. H. (UKSTU) line galaxies Dopita, M. A. (MSSSO), Binette, L. (Texas) and 2 The nature of emission line filaments in Phillips, M. M. (CTIO) Centaurus A Dufton, P. L., Byrne, F. N., Kingston, A. E. and 2 Nitrogen deficient early-type stars and Lennon, D. J. (Belfast) clusters Elliot, J., Baron, R. (MIT) and Allen, D. A. I Occultation of a bright star by Neptune (AAO) Ellis, R. S. (Durham), Allen, D. A. and Gray, P. 2 M. (AAO) Evolutionary studies of faint galaxies Ellis, R. S., Couch, W. J. (Durham), Atherton, P. 2 Multi-object spectroscopy and the nature of (Groningen), Taylor, K. and Gray, P. M. (AAO) galaxies in temote clusters Ellis, R. S., Sharpies, R. M. (Durham) and Gray, 4 The dynamical structure of rich clusters of P. M. (AAO) galaxies Elso, J. T., Kawara, K., Hyland, A. R. (MSSSO), 2 Taylor, K. N. R. and Han, (UNSW) Infrared photometry of dark clouds Evans, I. N., Dopita, M. A. and Ford, V. L. 4 (MSSSO) The ionising spectrum of Seyfert galaxies Evans, A. (Keele), Allen, D. A. (AAO), Bode, M., 2 Infrared emission of southern hemisphere Pearce, G. (Keele), Meikle, P., Selby, M., supernovae Graham, J. (ICST), Williams, P. and Longmore, A. (UKIRT) Fabian, A. C. and Nulsen, P. E. J. (IOA) 3 A detailed study of cooled intracluster gas

36 Fosbuiy, R. A. E. (RGO) and Bland, J. (Sussex) 4 Stellar properties of extended emission line radio galaxies Fosbury, R. A. E (RGO), Wilkinson, A. 2 Two dimensional velocity field and velocity (Manchester) and Wallace, P. T. (RAL) dispersion mapping of radio elliptical galaxies Gascoigne, S. C. B. and Bessell, M. S. (MSSSO) 2 Photometry of star clusters in the Magellanic Clouds Gatley, I. (UKIRT), Hyland, A. R. and Jones, T. 3 A search for protostars in the Magellanic J. (MSSSO) Clouds Gilmore, G. (ROE) and Reid, N. (Edinburgh) 3 The metallicity gradient of the Galactic halo Gilmore, G. (ROE) and Reid, N. (RGO) 3 Infrared photometry of very red stars. Glaspey.J. (Montreal), Freeman, K.C. 2 Abundance anomalies in globular cluster (MSSSO), Demers, S., Michaud, G. and Moffat, horizontal branch stars T. (Montreal) Greenhill, J. G., Giles, A. B., Watts, D. J. 2 Spectrophotometry of X-ray cataclysmic (Tasmania) and Bailey, J. (AAO) variables V1223 Sgr and V20S1 Oph Hanes, D. A. (AAO), Shara, M. (Arizona) and 3 Search for cataclysmic variable stars in Moffat, A. J. (Montreal) globular clusters Hanes, D. A., Taylor, K. (AAO), Atherton, P. 3 Globular clusters as probes of M87 (IICL) and Smith, M. G. (ROE) Hanes, D. A. (AAO) 4 The nature of blue stragglers in globular clusters and open clusters Harvey, P. (Texas), Hyland, A. R. (MSSSO) and 2 Near infrared observations of star formation Wilking, B. (Texas) regions Hunstead, R. W., Murdoch, H. S. (Sydney), 2 High-resolution spectroscopy of the QSO Pettini, M. (RGO) and Blades, J. C. (Space 2000-330 (redshift=3.78) Telescope) Hyland, A. R. (MSSSO) and Bailey, J. (AAO) 2 Infrared polarimetry of sources obscured by a dense Bok globule Hyland, A. R. (MSSSO), Jones, T. J. (Minnesota) 6 The 2 micron field of the Magellanic Clouds and Gatley, I. (UKIRT) Impey, C. D. (Hawaii) 3 The velocity field in clusters with twin radio galaxies Jauncey, D. L., Wright, A. E., Batty, M. J. 4 High redshift radio quasars (CSIRO), Savage, A. (ROE) and Paterson, B. A. (MSSSO) Jenkins, C. R. and Killeen, N. E. (MSSSO) 2 Velocity fields in active elliptical galaxies Jenkins, C. R., Carter, D. and Sadler, E. M. 1 Multicolour CCD surface photometry of (MSSSO) active and normal galaxies Jenkins, E. B. (Princeton), Morton, D. C. (AAO), 4 Deuterium in intergalactic space York, D. G. (Chicago) and Rodgers, A. W. (MSSSO) Jones, D. H. P., Schwarzenberg-Czerny, A., 3 Detection of secondaries in cataclysmic Echevarria, J., Collier, A., (RGO), Pringle, J., variables in the near infrared Berriman, G., Wade, R., Verbunt, K. D. and Horne.K.D. (IOA) Kibblewhite, E. J. (IOA), Cawson, M. G., Phillips, 4 CCD studies of surface photometry of S., Disney, M. J. (Cardiff), Whittle, D. M., Ward, galaxies extended emission line sources in M. J. Morris, S., Carswell, R. F. and Webb, J. K. active galaxies, and search for galaxies near (IOA) QSO lines-of-sight Kileen, N. E. and Bicknell, G. V. (MSSSO) I Spectroscopy of radio galaxies Lucey, J. R. (AAO) and Dickens, R. J. (RGO) 5 The environmental dependence of the colour-magnitude relation for galaxies Lynden-Bell, D. (IOA) and Cannon, R. D. (ROE) 3 The Fornax-Leo-Sculptor stream and the Galaxy's mass at 100-200 kpc

37 Malijauskas, S. and Carter, D. (MSSSO) I Velocity fields in dustlane ellipticals Manchester, R. N. (CSIRO), Peterson, B. A. 2 Search for optical pulses from pulsars PSR (MSSSO), Wallace, P. T. (RAL) and Murdin, P. 1509-58 and new fast pulsar PSR 1937+21 G. (RGO) Mathcwson, D. S., Tuohy, I. R., Dopita, M. A. and 2 Emission line imaging of supernova remnants Ford, V.L. (MSSSO) in the Magellanic Clouds using the CCD McHardy, I. M. and Cooke, B. A. (Leicester) 3 A search for extremely distant clusters of galaxies surrounding radio sources with steep low-frequency spectra Meaburn, J., Ohtani, H. (Manchester), Morgan, 7 Speckle interferometry observations of active B., Hebden, J., Vine, H. (1CST), Pedlar, A., galactic nuclei Spencer, R. and Davis, R. (Manchester) Morton, D.C.(AAO) 2 Interstellar absorption lines in blue stars towards the South Galactic pole Morton, D. C. (AAO), York, D. G. (Chicago) and 3 QSOs as probes of extended halos of nearby Jenkin, E. B. (Princeton) galaxies Morton, D.C. (AAO) 2 Spectroscopy of faint stars and galaxies in survey field at 22h-19 Morton, D. C. (AAO) and Blades, J. C. (RAL) 2 Interstellar absorption lines in the halo of the Galaxy Newell, E. B. (MSSSO) and Couch, W. J. 1 Redshift of the distant cluster of galaxies CI (Durham) 0024+1654 O'Mara, B. J., Ross, J. E. and Aller, L. H. 2 The near-ultraviolet spectra of planetary (Queensland) nebulae in the Large Magellanic Cloud Pagel, B. E. J. (RGO), Edmunds, M. G. (Cardiff), 2 Oxygen and nitrogen abundances in Phillips, M. M. (CTIO) and Diaz, A. 1. (Sussex) emission-line nuclei of spiral galaxies Peach, J. V. (Oxford), Ellis, R. S. (Durham), i Velocity dispersions in clusters of galaxies Godwin, J. G., Metcalfe, N. and Spenser, S. D. (Oxford) Pence, W. D. (AAO) and Turtle, A. J. (Sydney) 4 Kinematics of gas in bright galactic nuclei Spectroscopic survey of nuclei of barred Pence, W. D. (AAO) 3 spiral galaxies Gas dynamics in the barred spiral galaxy Pence, W.D. (AAO) i NGC7496 Kinematics of density waves in spiral galaxies Pence, W. D. and Taylor, K. (AAO) 2 Studies of the interstellar gas—the Penston, M. V., Pettini, M. (RGO), Blades, J. C. 4 Magellanic Stream (RAL) and Ward, M. J. (IOA) Peterson, B. A. (MSSSO), Savage, A. (UKSTU), 1 High redshift QSOs Jauncey, D. L. and Wright, A. E. (CSIRO) Peterson, B. A. (MSSSO), Savage, A. (UKSTU), 2 QSO absorption lines as probes of the Jauncey, D. L. and Wright, A. E. (CSIRO) intergalactic medium Peterson, B. A. (MSSSO) 3 Luminosity evolution of galaxies Peterson, B. A. (MSSSO) and Ellis, R. (Durham) 2 Correlation analysis of weak QSO absorption lines Phillips, A. P. (UCL), Gondhalekar, P. M. (RAL) 2 Expanding shells of interstellar gas around and Pettini, M. (RGO) southern OB associations Ratnatunga, K. and Freeman, K. C. (MSSSO) 6 Giant stars in the outer regions of the Galactic halo Robertson, J. G. (AAO) and Shaver, P. A. (ESO) 4 Absorption lines in close pairs of QSOs Robertson, J. G. (AAO) and Shaver, P. A. (ESO) 2 Search for calcium and sodium absorption in the QSO 1228+077 due to a nearby galaxy Robertson, J. G. and Hanes, D. A. (AAO) 2 Spectrophotometric standard stars for the AAT

38 Robinson, G., Mitchell, R. (Melbourne) and 2 Morphology of the infrared line and Hyland.A.R.(MSSSO) continuum from Eta Carina Roche, P. F., Ailken, D. K., Whitmore, B. (UCL) 3 8—13 micron spectrophotometry of the and Phillips, M.M.(CTIO) nuclear region of NGC136S Rodgers, A. W. and Harding, P. (MSSSO) 1 Stellar populations in the Galactic bulge Rowley, G. and Freeman, K. C. (MSSSO) 3 Kinematics of the bulges of disc galaxies Sharp,N.A. (MSSSO) 2 Companion galaxies with apparently anomalous redshifts Sharpies, R. M. (Duram) and Hawarden, T. G. 2 Kinematical studies of early-type galaxies (ROE) with dust lanes Sherrington, M. R. (Leicester), Bailey, J. (AAO), 3 Infrared light curves of cataclysmic variables Jameson, R. F. and King, A. R. (Leicester) Slee, O. B. (CSIRO) and Reynolds, J. (Sydney) 1 Redshifts of optical identifications in X-ray emitting clusters of galaxies Smith, R. M, and Carter, D. (MSSSO) 1 Dynamics of the radio galaxy NGC 1316 Smith, L. J. and Pettini, M. (RCO) 2 The velocity structure of wind-blown nebulae surrounding WR stars Sparks, W. B. (Sussex) and Wall, J. V. (RGO) 2 Optical emission in the jets and lobes of radio galaxies Storey, J. W. V. ( UNSW) t Infrared study of molecular hydrogen in planetary nebulae Taylor, K. N. R. (UNSW) and Visvanathan, N. 1 Polarimetry of bipolar nebulae (MSSSO) Taylor, K. N. R. (UNSW) 2i Infrared studies of bipolar nebulae Taylor, K. N. R. and Storey, J. W. V. (UNSW) 3 Infrared sources in Corona Austrina Taylor, K. (AAO), Turtle, A. J. (Sydney), 2 The kinematics of the high excitation gas in Edmunds, M. G. (Cardiff), Pagel, B. E. J. (RGO) NGC 1365 and Atherton, P. D. (ICST) Taylor, K. (AAO), Sparks, W. B., Hook, R. N. 3 Two-dimensional flux and abundance studies (Sussex), Axon, D. J. (UCL) and Atherton, P. D. of external galaxies (ICST) Tuohy, I. R., Mathewson, D. S. and Dopita, M. A. 2 The velocity structure of young supernova (MSSSO) remnants in the Large Magellanic Cloud Tuohy, I. N. (MSSSO), Bradt, H. V. and 3 Optical identification of HEAD-1 X-ray Remillard, R. (MIT) sources Tuohy, I. R. (MSSSO), and Charles, P. A. 2 Search for binary behaviour in faint Galactic (Oxford) X-ray sources Tuohy, I. R., Wickramasinghe, D. and 1 Determination of the geometry and Visvanathan, N. (MSSSO) magnetism of two new AM Her variables Turtle, A. J. and Mills, B. Y. (Sydney) I Supernova remnants in the Large Magellanic Cloud Van der Kruit, P. C. and Freeman, K. C. (MSSSO) 2 Kinematics of stellar discs in spiral galaxies Visvanathan, N. and Hyland, A. R. (MSSSO) 3 The colour-magnitude relation of galaxies in the Fornax cluster Visvanathan, N. (MSSSO) 2 Photometry of the intermediate age population in E and SO galaxies Visvanathan, N. (MSSSO) 3 Determination of a global value for the Hubble constant Visvanathan, N. (MSSSO) 2 Two colour photometry of the intermediate age population in E and SO galaxies Wade, R. A., Pringle, J, Hassall, B., Brunt, C. 3 Emission line profiles of cataclysmic variable (IOA), Schwarzen berg-Czerny, A., Echevarria, J. stars, and radial velocity study of dwarf (Sussex) and Jones, D. (RGO) 39 Ward, M. and Morris, S. (IOA) 4 Medium resolution spectrophotometry of active galaxies Waid, M. (IOA), Axon, D. J. (UCL), Hough, 3 The optical and infrared polarisation of J. H. (Hatfield) and Bailey, J. (AAO) Seyfert and related galactic nuclei Whiteoak, J. B., Gardner, F. F. (CSIRO), 1 The velocity structure of HII regions in the Taylor, K. (AAO) and Atherton, P. D. (ICST) Large Magellanic Cloud Whiteoak, J. B. and Gardner, F. F. (CSIRO) 2 The velocity structure in the gas clouds near Eta Carina Whittet, D. C. B. (Preston), Blades, J. C. (RAL), 3 3 micron spectrometry of dust in southern Bode, M. R, Evans, A. (Keele) and Butchart, I. dark clouds (Preston) Wickramasinghe, D. T. (ANU), Bessell, M. S. 2 Spectroscopy of white dwarfs in front of the (MSSSO) and Reid, N. (ROE) Coalsack dark cloud Zealey, W. J., Williams, P. M. (ROE), Taylor, 4 Mapping of Herbig-Haro complexes in the K. N. R., Storey, J. W. V. (UNSW) and Sandell, S( 1) line of molecular hydrogen G. (Helsinki)

Institution abbreviations used above AAO Anglo-Australian Observatory ANU Departmentof Mathematics, Australian National University Arizona Arizona Stale University (USA) Belfast Queen's University Belfast (UK) Birmingham University of Birmingham (UK) Cardiff Univeristy College of Wales, Cardiff (UK) Chicago University of Chicago (USA) CSIRO Division of Radiophysics, Commonwealth Scientific and Industrial Research Organization CTIO Cerro Tololo Inter-American Observatory (Chile) Durham University of Durham (UK) Edinburgh University of Edinburgh (UK) ESA European Space Agency (Europe) ESO European Southern Observatory (Europe) Groningen Kapteyn Astronomical Institute, University of Groningen (Netherlands) Hatfield Hatfield Polytechnic Institute (UK) Hawaii University of Hawaii (USA) Helsinki Helsinki Observatory (Finland) ICST Imperial College of Science and Technology, London (UK) IOA Institute of Astronomy, University of Cambridge (UK) Jodrell Bank Nuffield Radio Astronomy Laboratories, University of Manchester (UK) Keele University of Keele (UK) Leicester University of Leicester (UK) Manchester University of Manchester (UK) Melbourne University of Melbourne Minnesota Universityof Minnesota (USA) MIT Massachusetts Institute of Technology (USA) Montreal University of Montreal (Canada) MSSSO Mount Stromlo and Siding Spring Observatory Oxford University of Oxford (UK) Preston Preston Polytechnic (UK) Princeton Princeton University Observatory (USA) Queensland University of Queensland RAL Rutherford Appleton Laboratory (UK) RGO Royal Greenwich Observatory (UK) ROE Royal Observatory Edinburgh (UK) Space Telescope Space Telescope Science Institute, Johns Hopkins University (USA) Sussex University of Sussex (UK) Sydney University of Sydney Tasmania llnivereityofTasmania Texas University of Texas (USA) UCL University College London (UK) UKIRT UK Infrared Telescope Unit, Royal Observatory Edinburgh UKSTU UK Schmidt Telescope Unit, Royal Observatory Edinburgh UNSW University of New South Wales Wollongong University of Wollongong

40 Appendix C

Staff Anglo-Australian Observatory.

D.C. Morton, PhD Director D.W.Cunliffe Executive Officer P.R.Gillingham.BE* AAO Officer-in-charge, Siding Spring D.A.Allen, PhD1 Staff Astronomer J. A. Bailey, D Phil Research Scientist J. R. Barton, BE Experimental Officer G.W.Bothwell,BE Experimental Officer M. G. Callaway Technical Officer T.F.Carty.PhD Experimental Officer K.J. Cooper* Technical Officer, TSO T.A.Cragg* Senior Technical Officer, Chief TSO H.Davies,BE Experimental Officer R.G.Dean* Senior Technical Officer L.C. Denning B.E.M.* Principal Technical Officer D. S. Denny* Senior Laboratory Craftsman C. J. Emmott* Clerical Assistant F. F. Freeman* Technical Officer, TSO J. A. Freshwater Word Processor Typist E.J.Galvin* Assistant J.L.Gollan* Stores Supervisor K.W.Gorham Administrative Officer P.M. Gray, BE Experimental Officer G.G.Hall Technical Officer D.A.Hanes.PhD Research Scientist J. Hardy Technical Officer K.Harwood.PhD Experimental Officer J. Huxley Clerical Assistant D. W. Jenkins Technical Officer P. W. Knight* Senior Laboratory Craftsman S.Lee* Technical Officer, TSO P. L. Lindner* Senior Laboratory Craftsman J.Lucey.PhDf SERC Fellow P. McCartney* Technical Assistant C. J. McCowage* Technical Officer G. M. Mager Technical Assistant D.F.Malin Experimental Officer D.J.Mayfield Senior Technical Officer D. M. Paton Clerical Assistant W. D. Pence, PhDf SERC Fellow D. N. Phipps* Supervising Engineer A. C. Porteners Draftsman V.D.Pos Senior Laboratory Craftsman J. G. Robertson, PhD Research Scientist G.E.Schafer* Senior Laboratory Craftsman, TSO R.M.Shobbrook Library Officer P. Simon Purchasing Officer A.Stacey Steno-Secretary J. O. Straede, MSc Experimental Officer J.E. Sullivan* Senior Technical Officer K. Taylor, PhD Senior Research Scientist

• Stationed at SidingSpring as at 30.6.83 t Funded by the Science and Engineering Research Council 1. from 1.4.83

TSO-Tclescope Systems Operator

41 Appendix D

History of the AAT Project

After representations to the Australian and British Governments, made in the mid-1960s by the Australian Academy of Science and the Royal Society of London, it was decided in April 1967 to build a large optical telescope, similar in design to the 4-metre telescope of the Kitt Peak National Observatory in the United States. As a result of discussions held between the two Governments and the Australian National University, it was decided that the telescope would be built at the site of the University's observatory at Siding Spring Mountain near Coonabarabran in New South Wales. A Joint Policy Committee consisting of six members, with three chosen by each Government, served as an executive body from September 1967 until February 1971. The Committee was succeeded by the present Anglo-Australian Telescope Board which operates under the authority of an inter-governmental Agreement which came into effect at that time. Under the Agreement concluded by the two Governments, the costs of the construction, operation and maintenance of the telescope were to be shared equally, whilst observing time was to be available in equal shares to astronomers in the UK and Australia. A Project Office to supervise the construction of the telescope was set up in January 1968 by the Joint Policy Committe. Some two to three years were required for the preparation of detailed design specifications and the letting of major contracts, which were awarded on an international basis, with important contributions coming from Japan, Switzerland and the United States, as well as from the United Kingdom and Australia. Figuring of the mirrors was carried out by the British firm, Sir Howard Grubb Parsons and Co. Ltd. The telescope mounting and the drive and control systems were manufactured by Mitsubishi Electric Corporation of Japan. The telescope building and dome, constructed by the Australian companies Leighton Constructions Ltd and Evans-Deakin Industries Ltd, were completed by the end of 1972, while the structural components of the telescope itself were assembled during 1973. The final cost of construction was $A15 932 250. Following a complex process of adjustment and the installation of instrumentation, the telescope was inaugurated in October 1974 by His Royal Highness, The Prince Charles. The primary mirror, which has a usable surface of diameter 3.89m, was aluminised late in 1974 and scientific work commenced early in 1975. Regularly scheduled observations began in June 1975. In October 1974 the Board established temporary quarters in the grounds of the CSIRO Division of Radiophysics at Epping, an outer suburb of Sydney, to provide technical and administrative support for the Telescope. Subsequently, the Board decided to maintain this establishment, known since March 1976 as the Laboratory of the Anglo-Australian Observatory (AAO), as a complementary facility to the Telescope at Siding Spring Mountain. The AAO Laboratory provides facilities for administrative and scientific staff, staff concerned with instrumental development, and visiting astronomers from Australia and overseas.