Australia Telescope National Facility Australia Telescope National Facility Annual Report 2002

Annual Report 2002 © Australia Telescope National CSIRO Australia Telescope National Facility Annual Report 2002 Facility ISSN 1038-9554 PO Box 76 Epping NSW 1710 This is the report of the Steering Australia Committee of the CSIRO Tel: +61 2 9372 4100 Australia Telescope National Facility for Fax: +61 2 9372 4310 the calendar year 2002.

Parkes Observatory PO Box 276 Editor: Dr Jessica Chapman, Parkes NSW 2870 Australia Telescope National Facility Design and typesetting: Vicki Drazenovic, Australia Australia Telescope National Facility Tel: +61 2 6861 1700 Fax: +61 2 6861 1730 Printed and bound by Pirion Printers Pty

Paul Wild Observatory Narrabri Cover image: Warm atomic hydrogen gas is a Locked Bag 194 major constituent of our Galaxy, but it is peppered Narrabri NSW 2390 with holes. This image, made with the Australia Australia Telescope Compact Array and the Parkes radio telescope, shows a structure called Tel: +61 2 6790 4000 GSH 277+00+36 that has a void in the atomic Fax: +61 2 6790 4090 hydrogen more than 2,000 light years across. It lies 21,000 light years from the Sun on the edge of the [email protected] Sagittarius-Carina spiral arm in the outer Milky Way. www.atnf.csiro.au The void was probably formed by winds and supernova explosions from about 300 massive stars over the course of several million years. It eventually grew so large that it broke out of the disk of the Galaxy, forming a “chimney”. GSH 277+00+36 is one of only a handful of chimneys known in the Milky Way and the only one known to have exploded out of both sides of the Galactic plane. It extends more than 3,000 light years out of the disk of the Galaxy.

Image credit: N. McClure-Griffiths (ATNF); J. Dickey (University of Minnesota, USA); A. Green (University of Sydney); B. Gaensler (Harvard University, USA) Contents

Chairman’s report 2

The ATNF in brief 3

Performance indicators 9

Astronomy reports 17

Observatory reports 39

Current activities 49

Technology developments 57

Appendices 65 Chairman’s report

Over the past year, it is been a delight and a privilege to chair the Australia Telescope National Facility (ATNF) Steering Committee. As is evident from the pages of this annual report, the ATNF has had an excellent year. The strengths of the organisation derive from the excellence of its staff, coupled with its clear vision to play a world- leading role in radio astronomy.

In this regard, the ATNF’s continuing pro-active role in the international Square Kilometre Array (SKA) project has been particularly impressive. The ATNF has not only been involved in the development of a number of key Photo: Kristen Clarke design technologies, but has also carried out important work in relation to the potential siting of the SKA in Chairman’s report Australia. The ATNF has also continued to contribute at a high level to the science goals of the SKA program. Perhaps one of the most important opportunities to emerge from the ATNF’s SKA work during 2002 was the approach made by a US-Dutch consortium to investigate siting LOFAR, a next-generation low-frequency radio Professor Brian Boyle, Director of the Anglo-Australian Observatory and Chairman telescope, in Australia. of the ATNF Steering Committee.

The ATNF’s strong international profile is underpinned by the continued outstanding performance of its own facilities: the Compact Array at Narrabri and the Mopra and Parkes radio telescopes. During 2002, it was particularly encouraging to see some of the first scientific results emerging from the prototype 12- and 3-mm systems on the Compact Array. The Parkes multibeam receiver system also continues to produce world-leading research, including important new discovery of pulsars associated with supernovae remnants and the results from the surveys for neutral hydrogen emission from galaxies.

These scientific successes would not be possible without the technological innovation that has seen the ATNF maintain its telescopes at the forefront of the world’s radio astronomy facilities. The successful completion of the monolithic microwave integrated circuits program this year again demonstrates that the ATNF remains at the cutting edge of technology. In this regard, the ATNF has benefited greatly from its strategy of further enhancing links with other CSIRO divisions and industrial partnerships.

The link between astronomy and technology is a fundamental one. Some of the big questions for astronomy to answer over the coming decade will require the development of new technologies, particularly those in signal processing, information technology and communications, with applications far beyond the astronomical community. The ATNF has positioned itself well to take full advantage of these new opportunities, maintaining Australia not just at the forefront of an inspiring area of scientific endeavour, but also as a world leader in cutting-edge technology for society.

page 2 F F Status asaNational Status asaNational Status withinCSIRO Status withinCSIRO Size andfunding Size andfunding Mission Mission overseas institutions. Australia The Telescope is Australian and at astronomy for astronomers inradio facilities provides world-class observing As aNationalFacility, theAustralia Telescope ATNFThe became aNationalFacilityApril 1990. in F Status asaNational Astronomy Sector. CSIRO’s Committeefor Advisory Radio to advisetheATNF Director, alsoactsasthe Committee, by theMinisterforScience appointed January AustraliaThe 1989. Telescope Steering Radiophysics, division in itbecameaseparate theCSIRO Division of CSIRO. of part Formerly Australia’s national research institution, largest ATNFThe asaNational Facility ismanaged by Status withinCSIRO fromCSIRO.direct appropriation A$12.9M was which of was A$17.3M, budget 2001 –2002theorganisation’s totalexpenditure ATNFThe employs approximately 135staff. In Size andfunding ♦ ♦ ♦ Mission eightindividual radiotelescopes. set of astronomy,Australiathe by Telescope, operating a modern of themajorfields astronomy, oneof ATNFThe Australia’s supports research inradio The ATNF inbrief F F Status asaNational Status asaNational Status withinCSIRO Status withinCSIRO Size andfunding Size andfunding Mission Mission acility acility acility acility acility ofrhrteavneeto knowledge. To theadvancement of further astronomy observatory. maintain itspositionasaworld-class radio to location andtechnologicaladvantages To exploitthetelescope’s uniquesouthern researchers. use byAustralian andinternational Telescope asanationalresearch facility for To anddevelop operate Australia the page 3 A A The A The A telescopes telescopes Users ofA Users ofA the ATNF. hasstronglinkswith organisation The Australian outthrough radio astronomy iscarried Australia.institution in Approximately 90%of astronomical ATNF single The isthelargest 24 othercountries. 14 institutionsinAustralia and126institutionsin proposals allocatedtimeincludedscientistsfrom users comefromoutsidetheATNF. In2002the thetelescopes’ Committee. Approximately 90%of Assignment Committeeappointedby theSteering by aTime theirproposedresearch programs of themerits awarded toresearchers onthebasisof ATNF’s timeonthe Observing telescopesis A The A telescopes Users ofA Technology Council. originally establishedAustralian by the Scienceand Facility asaNational operated underguidelines A A The A The A telescopes telescopes Users ofA Users ofA Professor RonEkers,Director ofthe ATNF ustralian conte ustralian conte ustralian conte ustralian conte ustralian conte TNF inthe TNF inthe TNF inthe TNF inthe TNF inthe TNF TNF TNF TNF TNF xt xt xt xt xt

Photo: Kristen Clarke

The ATNF in brief Photo: Kristen Clarke Kristen Photo: John Brooks, Assistant Director of the ATNF of the Director Assistant John Brooks, Compact Array, located at the Paul Wild located at the Paul Array, Compact Observatory of near the town Narrabri. of Five ofthese antennas sit on a 3-km stretch rail track to different running they can be moved east–west; to build up detailed images points along the track of of to the west A sixth antenna lies 3 km the sky. ofEach the main group. these antennas has a reflecting 22 metres surface in diameter. “collected” After the radio signals from space are transformed they are the antennas’ surfaces by into brought together at a central electrical signals, location, and then processed. The end result is usually a picture or a spectrum of the object being to a photograph,but studied—a picture equivalent instead of waves made from radio light. A further as the Mopra antenna, 22-m known in the is located near Mopra Rock, telescope, Mountains near Coonabarabran, Warrambungle Wales. South New The other key component of the Australia 64-m radio telescope, is the Parkes Telescope oflocated near the town Thistelescope has Parkes. been successfully operated since 1961 and is famous scientific as a national symbol for Australian upgrades Recent to accommodate a achievement. maintained its 13-beam focal-plane array have position as a state-of-the-artworld-class instrument. page 4 ’s ’s ’s ’s ’s TNF TNF TNF TNF TNF vatories vatories vatories TNF in the global TNF in the global xt xt vatories vatories TNF in the global xt TNF in the global TNF in the global xt xt A A A A A obser obser The The The A The A conte conte The Australia Telescope consists ofconsists Telescope The Australia radio-eight located at three sites in New antennas, receiving South Wales. Six of Telescope up the Australia them make obser The Of the fields of ultra- modern astronomy—X-ray, makes infraredviolet, optical, and radio—Australia to one of the most significant contributions This is through radio astronomy. astronomy world a result of early lead in the field, Australia’s and southern advances, technological continuous is the Telescope Australia location. hemisphere The kind in the only major radio telescope of its and thus can viewsouthern part hemisphere, of the sky is out of which reach of northern one of It provides hemisphere telescopes. the most facilities in the world. radio astronomy powerful and internationalAustralian observers use This is in the telescope without access charges. with a generalaccordance practice of the world- telescope in which wide astronomical community, users from different countries gain reciprocal access to facilities on the basis of scientific scientists to use merit.This Australian allows telescopes in other countries and international as particlefacilities such accelerators and access provides Such space-based instruments. of scientists with a diversity Australian instruments of network and leads to a rich international collaborations. The A its primary user base, the university community. The community. its primary the university user base, interests of telescope users are represented the by Users Committee. Telescope Australia headquarters Sydney are co-located The ATNF’s with those of Observatory, Anglo-Australian the that provides an independent Facility bi-National This close optical and infrared facilities. world-class terms, promotes and in world association is unique, the two collaboration between valuable organisations. conte obser obser The The The A The A conte conte

The ATNF in brief technology development technology development Engineering and Engineering and technology inAustralia. technology cutting-edge forthedevelopment of platform technology. ATNFinformation The provides a systems, processingand processing, control data receiver technology, signaldetectionand electronics, areaswhich include of in arange technological developments thelatest on exploiting crucially radioastronomy depends advanceThe of technology development Engineering and (VSOP). Program Observatory China, Hawaii andIndia, andtheVLBISpace which Japan, telescopesinAustralia, links radio the Asia-Pacific Telescope of regularly usedaspart Australia and Western Australia. LBA The isalso andradioantennasinTasmania,Canberra, South near Tidbinbilla, trackingsatellite antennasat telescopes which theNASA includes radio Australian networklarger of a sky. LBA The of isusedaspart small areasof which of isusedtoobtainhighresolutionimages (VLBI) longbaselineinterferometry known asvery (LBA)as theLongBaselineArray foratechnique eight ATNFThe telescopescanbeusedtogether technology development technology development Engineering and Engineering and Figure 1 Telecommunications & Telecommunications & Telecommunications & Telecommunications & Telecommunications & Industrial Physics Industrial Physics Industrial Physics Industrial Physics Industrial Physics Theorganisational structure ofthe ATNF. CSIRO CSIRO CSIRO CSIRO CSIRO Minister forScience Minister forScience Minister forScience Minister forScience Minister forScience CSIRO Executive CSIRO Executive CSIRO Executive CSIRO Executive CSIRO Executive Telescope National Telescope National Telescope National Telescope National Telescope National page 5 Australia Australia Australia Australia Australia Facility Facility Facility Facility Facility

AnnualAnnualAnnual ReportReportReport Committee Committee A A Committee Appendix C. committee membersfortheyear2002arelistedin time. The proposals andallocate observing Time AssignmentCommittee(TAC)the toreview feedback andadvicefromtheusercommunity, and Telescope UsersCommittee(ATUC) toprovide SteeringCommitteeappointstheAustraliaThe Facility and,indirectly, time. forallocatingobserving also responsibleforpromotingtheuseof theAustralia Telescope. Itis the development of theATNF’s scientificactivities and directions of met atleastonceayear, todefinethebroad Committee was heldinMay 1989.Sincethenithas ATNF the Steering inauguralmeetingof The CSIRO todevelop theATNF’s strategy. long-term by Committeehelps theMinisterforScience. The committeeappointedCommittee, anindependent byATNF theATNF policyisdetermined Steering A Committee Committee A A TNF Steering TNF Steering TNF Steering TNF Steering TNF Steering

Policy Advice

Allocation Allocation Allocation Allocation Allocation

User Feedback User User Feedback User User Feedback User User Feedback User User Feedback User Time Time Time Time Time Assignment Assignment Assignment Assignment Assignment Committee Committee Committee Committee Committee Committee Committee Committee Committee Committee Steering Steering Steering Steering Steering Time Time Time Time Time Committee Committee Committee Committee Committee User User User User User

The ATNF in brief To position the ATNF to participate in To major international radio astronomy next decade the over projects developing to The upgrade MNRF the ATNF will allow eight to maintain a leading position for the next that, Beyond radio will be astronomy ten years. major internationaldominated by two the Atacama Largedevelopments: Millimetre Array(ALMA) and the SKA. These instruments questions pursue key astronomers to will allow of evolution about the early For Universe. the to maintain its position in radio Australia a signficiant role in to have it needs astronomy, least one ofat The SKA is a these projects. the “next-generation”billion-dollar project, radio telescope with a collecting area of one Its constructionsquare kilometre. is expected to start positioned is well around 2012. Australia of role in the development a key to play the offers an ideal SKA. In some respects Australia of location for the SKA as it has a number regions of population are low density which free fromThe radio interference. relatively technology required for the SKA development wide industrial applications and the will have significant industrial construction will involve contracts. 2001, the Government announced August In the allocation of A$155M under the MNRF- During the last five years the Narrabri years and last five During the been extensively have Mopra telescopes upgraded, Major National Research under the (MNRF) program,Facilities 1997, to funded in The shorter at (millimetre) wavelengths. work devices for upgradedtelescopes use innovative the detection of millimetre-wave extremely weak been jointly These have signals from space. and CSIRO the ATNF designed by and Industrial Physics Telecommunications the CSIRO (CTIP), a project funded by Special Project. The MNRF Executive of upgrade network the also extends Australian has both VLBI, telescopes used for which astronomical and geodeticThe applications. MNRF upgrades will be fully completed in 2004. ♦ ♦ ♦ ♦ ♦ page 6 . elescope elescope elescope elescope elescope Develop and extend the performance and extend the Develop of the to maintain its Australia Telescope in the medium termcompetitiveness (3 – 8 years) To continue to operate to the continue Australia To as to maintain a a way in such Telescope leading international position access to its facilities to will provide TheATNF the needs ofsatisfy and overseas Australian At least 70% ofusers. and time on the Parkes Narrabri telescopes will be used for astronomy. observingTime lost during scheduled periods 5%. to below will be kept ustralia T ustralia T ustralia ustralia T ustralia ustralia T ustralia T ustralia Strategic objectives Strategic objectives Time Assignment Time Assignment Committee Committee Users Committee Users Committee A A ♦ ♦ ♦ ♦ ♦ ♦ The ATNF is one ofThe ATNF leading radio the world’s The strategic organisations. astronomy objectives are: for the ATNF The ATNF receives more applications for receives The ATNF observing time than it can accommodate: and Narrabri the Parkes for time on both proposals of a factor by the time available telescopes exceed The and proposals are assessed, two. approximately meets The TAC the TAC. by time allocated to them, one three times a year and reviews approximately meeting. hundred telescope applications at each Strategic objectives Time Assignment Committee ATUC represents of the interests ATUC the Australia Thecommittee provides users. Telescope’s discussing Director, feedback to the ATNF with, and suggestingproblems ATNF changesto, scientificdiscusses and ranks by operations; it also ATUC projects. development future merit various forummeetings are also a for informing users AT of the current of status and planned development ATUC and recent scientific results. facilities, ATNF at the web discussions can be found on www.atnf.csiro.au/management/atuc Users Committee A ♦ ♦ ♦ ♦ Strategic objectives Strategic objectives Time Assignment Time Assignment Committee Committee Users Committee Users Committee A A

The ATNF in brief ♦ ♦ ♦ ♦ ♦ maintain good community relationships.maintain good high school students andtheirteachers; andto by at providing targetted educationalresources scientists of thenextgeneration to encourage inAustralia;astronomy andrelated technology of toraisethenationalprofile has several goals: has anactive which publicoutreachprogram and theParkes Observatories andNarrabri of The ATNF operates Visitors Centresat thesites program To conduct aneffective outreach under thisaward was received in2002. single allocationofA$23.5M.Initialfunding optical Geminitelescopes, received thelargest SKA development, andimproved access to the ATNF-led thesethe for proposal Australia. Of in to15successfulprograms 2001 program Professor DeputyDirector Ray Norris, oftheATNF page 7 changes in2002 changes in2002 A A a role in the management of the ATNF the forthe of inthemanagement a role fellowship Ekers is that Professor willceasetohave this theconditionsof inAustralia.offered Oneof and richest publicly-funded research positionsever Federation themostprestigious Fellowship, oneof announced thatProfessor Ekers was awarded a In July 2002theAustralian Research Council Brooks continuingAssistant Director. as theATNF withJohn of Acting Director as the 2002,Professor tookover Ray Norris remainder of the muchof andfor During hisabsence, Berkeley astronomy department. California take upaMillerProfessorship attheUniversity of absencefromJulyApril 2002to 2001until leave of ATNFThe Director, Professor Ron Ekers, was on changes in2002 A changes in2002 changes in2002 A A TNF management TNF management TNF management TNF management TNF management

© CSIRO

The ATNF in brief SKA SKA SKA SKA SKA P J Hall W E Wilson Engineering Engineering Engineering Engineering Engineering M J Kesteven B M Thomas Special Projects Special Projects Special Projects Special Projects Special Projects Development Group Development Group Development Group Development Group Development Group J W Brooks Assistant Director Assistant Director Assistant Director Assistant Director Assistant Director Manager Manager Manager Manager Manager P J Howson Commercial Commercial Commercial Commercial Commercial B M Thomas B F Parsons Administration Administration Administration Administration Administration B Wilcockson RPL Eng. Services RPL Eng. Services RPL Eng. Services RPL Eng. Services RPL Eng. Services RPL Eng. Services RPL Eng. Services RPL Eng. Services RPL Eng. Services RPL Eng. Services (Research Support) (Research Support) (Research Support) (Research Support) (Research Support) (Research Support) (Research Support) (Research Support) (Research Support) (Research Support) Narrabri, Marsfield. to Dr Bob Sault also moved as the Narrabri Officer-in-Chargetook over on 1 2002 bringing to the observatoryJanuary a broad range of expertise in engineering, and astronomy computing. Director Director Director Director Director R D Ekers page 8 Mopra Mopra Mopra Mopra Mopra Narrabri Narrabri Narrabri Narrabri Narrabri R J Sault Support Support Support Support Support Manager Manager Manager Manager Manager Business Business Business Business Business Observatory Observatory Observatory Observatory Observatory Development Development Development Development Development J M Chapman Kieran Greene National Facility National Facility National Facility National Facility National Facility R P Norris Deputy Director Deputy Director Deputy Director Deputy Director Deputy Director LBA LBA LBA LBA LBA The management structure of the ATNF in July 2002. ATNF of the The management structure Parkes Parkes Parkes Parkes Parkes Computing Computing Computing Computing Computing Observatory Observatory Observatory Observatory Observatory A K Tzioumis J E Reynolds D McConnell Astrophysics Astrophysics N E B Killeen Astrophysics Astrophysics Astrophysics Special Projects Special Projects Special Projects Special Projects Special Projects L Staveley-Smith five-year termfive-year of 2003. from March fellowship the and CSIRO announcement, this ATNF Following processes were put into motion to find and appoint a new Director. appointed Ball was 2002 Dr Lewis In May as Deputy Officer-in-Charge of the Parkes Observatory Manager for Resources and Human Dr In December 2001, as a whole. the ATNF his term McConnell completed David Officer- as in-Charge of the Narrabri Observatory and returned up a management to Marsfield to take position as Head of Mr Ron Special Projects. Beresford, the Deputy Officer-in-Charge at Figure 2

The ATNF in brief 2 ResponseoftheA 2 ResponseoftheA ATNF. developments.priorities forfuture Typically, ATUC recommendationsarefollowed upby the 90%of Director. ATUC operations, raisedby considersmatters theuser community andsets andcurrent recommendations tothe decision-making process. Aftereach meetingthecommitteepresentsalistof ATNFThe UsersCommittee(ATUC) meets twiceayear, theusercommunity torepresent intheATNF 2 ResponseoftheA for aNationalFacility. bygenerally CSIRO tobeappropriate but adapted indicators, basedonthoseused performance throughkey ATNFThe assessesitsperformance indicators Performance oniedrn ceue bevtos24 5.2% 82.0% 2.4% downtime for theParkesThe telescopeincludestimelostforwindstows (3.8%). 79.1% Downtime duringscheduled observations Time allocatedforscheduled observations timefortheyear2002: following valuesThe show theuseof 2 ResponseoftheA 2 ResponseoftheA 1 1 below 5%. equipment failureshouldbe from observations thetimelostduringscheduled isthat second target thefacilities.) A maintenance andupgrading remaining30%isneededfor observations. (The available shouldbeallocatedforastronomical thetime ATNF that atleast70%of setsatarget For theParkes Observatories, the andNarrabri 1 1 1 Users Committee Users Committee Users Committee Users Committee Users Committee obser obser successfully completed successfully completed Scheduled and Scheduled and obser successfully completed Scheduled and obser obser successfully completed successfully completed Scheduled and Scheduled and ving time ving time ving time ving time ving time TNF torecommendationsbythe TNF torecommendationsbythe TNF torecommendationsbythe TNF torecommendationsbythe TNF torecommendationsbythe arbiParkes Narrabri page 9 Head, ATNF NationalFacilitySupportGroup Dr JessicaChapman

Photo: Kristen Clarke

Performance indicators developed for the Parkes developed overseas are Hobart, in use at the Tidbinbilla, page 10 non-ATNF Australiannon-ATNF including routines visualisation and fundamental measures, developed at ATNF is used by more 30 astronomical than is used by at ATNF developed are an essential component of the FARADAY (Focal-plane Arrays (Focal-plane are component of an essential the FARADAY jointly written at the ATNF and BIMA, is in routine use at radio and BIMA, is in routine ATNF jointly written at the ATNF are building a multibeam receiver for the Arecibo L-band Feed Array (ALFA). forFeed the Arecibo L-band building a multibeam receiver are 1989 1991 1993 1995 1997 1999 2001 2003 uments and processes developed by CSIRO processes developed uments and by CSIRO processes developed uments and 0 uments and processes developed by CSIRO processes developed uments and uments and processes developed by CSIRO processes developed uments and by CSIRO processes developed uments and

60 50 40 30 20 10 Compact Array time allocation, 1990 – 2002. time allocation, 1990 Array Compact % of time available time of % instr instr ATNF engineersATNF Indium phosphide MMIC chips Indium phosphide MMIC chips the European Union. by project, funded Design, ThisAccess and Yield) is a for Radio Astronomy: that aims to Italy and Australia programPoland, The the UK, co-operative Netherlands, between prototypesproduce of intergrated focal plane arrays to study large and arrays for future implementation. surveys high sensitivity to be extremely system, operating near 1.4 GHz, will allow This seven-feed Areciboconducted using the 305-m telescope in Puerto Rico. Multibeam observing techniques and data management systems Components of AIPS++ software Miriad data reductionMiriad data software world. institutions around the astronomy correlator digital ATNF and control hardware software Hartebeesthoek,Ceduna, Bank and SEST Observatories. Jodrell Bank. Observatory Jodrell by been adopted have institutions including the Herzberg Institute for Astrophysics several are being used by written at ATNF, (JIVE). Institute for VLBI in Europe Bank and the Joint Jodrell (Canada), Karma visualisation software institutions. instr instr instr 3 Adoption by users and organisations of practices, organisations users and by 3 Adoption of practices, organisations users and by 3 Adoption ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ This of indicator lists a selection in now are which at the ATNF and software developments hardware are: Some examples use at other organisations. ♦ 3 Adoption by users and organisations of practices, organisations users and by 3 Adoption ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ ♦ Figure 3 3 Adoption by users and organisations of practices, organisations users and by 3 Adoption of practices, organisations users and by 3 Adoption

Performance indicators 4 TimeallocationonA 4 TimeallocationonA 02 iue6sostettlnme finstitutions, 1999–2002. authorsandcountriesfortheyears 2002. Figure6shows thetotalnumber of in authorsfromeach country 126 overseas institutionsin24countries. 5shows Figure thenumber of these, 42authors were fromtheATNF, 83were from13otherAustralian institutions and297were from authors. 416different Of ATNFIn 2002theproposalsallocatedtimeon includedatotalof facilities theteamleader. the totalallocatedtime, by affiliation of andParkes teamsontheCompactArray of radiotelescopeasapercentage time allocatedtoobserving isgiven programs inAppendixD. theobserving Figures3and4show the Baseline Array. of Asummary Array, 48were forthe Parkes telescope, sixwere fortheMopratelescopeand13were fortheLong these, 138were fortheCompact year althoughsomeproposalsare submittedtwo orthreetimes).Of 205 proposalsATNF allocated were timeon facilities(each proposaliscountedonceonlypercalendar In2002atotalof scientific merit. timeontheATNF facilitiesisdoneonthebasisof allocationof The Figure 5 4 TimeallocationonA 4 TimeallocationonA 4 TimeallocationonA Figure 4 Australian and overseas participation, 2002. Australian andoverseasparticipation, Parkes timeallocation,1990 – 2002.

Number of authors % of time available 100 120 10 20 30 40 50 60 70 20 40 60 80 0 9919 9319 9719 012003 2001 1999 1997 1995 1993 1991 1989 0

Australia USA UK Italy Netherlands ATNF Canada TNF facilities TNF facilities TNF facilities Germany TNF facilities TNF facilities

page 11 India

France non-ATNF Australian Chile Russia Argentina China Sweden Japan Mexico Brazil South Africa Austria Overseas Belgium Spain New Zealand Finland Indonesia Korea

Performance indicators 2002 conference 2001 TNF staff TNF staff TNF staff TNF staff TNF staff 2000 refereed page 12 1999 vised by A vised by A vised by A vised by A vised by A Authors Institutions Countries 1997 1998 1999 2000 2001 2002 0 80 60 40 20

200 180 160 140 120 100

0

50 publications of Number

450 400 350 300 250 200 150 100 Number journals and conference published in refereed Australia Telescope, data obtained with the Papers from Australian and overseas participation in 1999 – 2002. eaching, measured by the number of postgraduate eaching, measured by the number of postgraduate eaching, measured by eaching, measured by the number of postgraduate eaching, measured by eaching, measured by the number of postgraduate eaching, measured by the number of postgraduate eaching, measured by Number of publications Number of publications T T students super students super Number of publications T students super Number of publications Number of publications T T students super students super Figure 7 proceedings. Figure 6 6 6 5 5 Figure 7 shows the number of the number Figure 7 shows in refereed publications that include journals and conference proceedings, The publication counts include papers dealing with Telescope. obtained with the Australia data reports, telegrams, historical papers, abstracts, not include IAU operations or data reduction but do Appendix G lists the 103 papers authors. articles ATNF for popular magazines, or other papers by journalspublished in refereed proceedings in 2002. published in conference 76 papers and the In December 2002 ATNF staffIn December 2002 ATNF co-supervising Their were affiliations and project titles 26 PhD students. are listed in Appendix H. 6 5 6 6 5 5

Performance indicators The Visitors Centre PaulWild attheNarrabri attractsapproximately Observatory 10,000visitorseachyear. 7 Publicrelationsactivities 7 Publicrelationsactivities fvisitorscontinued throughout2002. of number facilities inMarch increased 2001.The thenew VisitorsCentrebuildingandupgraded opening of thefilm in2001,following therelease of greatly Centre increased visitors totheParkesVisitors numberThe of in2002. VisitorsCentre 10,000 peoplevisitedtheNarrabri andParkes totheNarrabri Centres. visitors Visitors Approximately Figure 9shows thenumberof with 15.1millionhitsrecordedfor2002. web hitsincreasesfromyeartoyear, search by engines. external number andhitsgenerated of The staff web hitstothecentralATNF useby website. includesinternal This Figure 8alsoshows thenumber of (television, radio, arelikelyreports allyears tohave newspapers) for beenundercounted. numbers shownThe inFigure 8have beenverified wherepossible. However, media thenumbers for university andcommunity groups. given whileapproximately 45talkswere toschool, interviews and45radio interviews television gave atleast30 least100pressitems. inat (AppendixF)andfeatured media releases ATNF staff Figure 8shows publicrelations activitiesfortheyears1999–2002.DuringyearATNF issuedsix 7 Publicrelationsactivities 7 Publicrelationsactivities 7 Publicrelationsactivities page 13 The Dish

in October2000andthe

© CSIRO

Performance indicators Public talks Web hits (x100,000) Narrabri Parkes page 14 TV interviews Newspaper articles 1999 2000 2001 2002 1997 1998 1999 2000 2001 2002 0 Media releases Radio interviews 0 80 60 40 20

80 60 40 20

160 140 120 100 160 140 120 100

Number (thousands) Number Centres. Number of visitors to the Parkes and Narrabri Visitors ATNF public relations activities. relations public ATNF Number Figure 9 Figure 8

Performance indicators 8 UserfeedbackatNar 8 UserfeedbackatNar Observatory. theParkes and84%for average over Observatory allitemsranked theNarrabri was85%for provided high.In2002the satisfactionwithfacilities isgenerally Figures 10and11show thelevel that of andParkes areasked tocompleteauserfeedbackquestionnaire. theNarrabri Observatories at Observers 8 UserfeedbackatNar Figure 11 8 UserfeedbackatNar 8 UserfeedbackatNar Figure 10 Observatory staff (after staff hours) Observatory Compact Array Users Guide Users Array Compact Technical support (after hours) support Technical Observatory staff (daytime) staff Observatory Freedom fromFreedom interference Off-line imaging facilities Off-line imaging Technical support (daytime) support Technical Freedom from interference hardware computer Online Parkes user feedback on a scale of 1 – 10whereParkes userfeedbackonascale of1 1=poorand10 excellent. Offline computer hardwareOffline computer Narrabri userfeedbackonascaleof1 – 10where 1=poorand10excellent. Other computing services computing Other Calibrator information Calibrator Duty astronomers Telescope hardware Telescope Unix computers Unix Documentation Pre-arrival support Pre-arrival Observer comfort Observer training Online software Online Documentation Administration Library PCs Library Lodge 012345678910 0246810 rabri andP rabri andP rabri andP rabri andP rabri andP page 15 arkes arkes arkes arkes arkes

Performance indicators Photo: John Sarkissian

The Parkes radio telescope observed during a solar eclipse on 4 December 2002

page 16 stars TWHyaandHD100546 stars TWHyaandHD100546 circumstellar disksaroundtheyoung circumstellar disksaroundtheyoung Millimetre obser Millimetre obser have thedustcontinuum andHCO observed sky. diskslocatedinthesouthern protoplanetary We of forhighresolution imaging new opportunity withreceivers theCompactArray forthe3-mmatmosphericwindow provides a of recentupgrade The thespectrum. of detail inthispart andthephysical degrees, and chemical conditionscanbeprobedin from afewtenstohundreds of temperaturesranging thesedisksbecausethediskmaterialbeyond afewstellarradiiisat of properties millimetre wavelengths at System. Observations for characterising areespeciallyimportant thephysical similartotheearlySolar Many young emissionfromcircumstellardustdiskswithproperties stars exhibit T. Wong (ATNF) D. Wilner, T. Bourke(CfA,USA);C.Wright (ADFA); J.Jörgensen, E.vanDishoeck(Leiden,TheNetherlands); stars TWHyaandHD100546 circumstellar disksaroundtheyoung Millimetre obser reports Astronomy component. thiscompactdisk evidencefor provide direct thefirst observations Array TheCompact system. thatacircumstellardiskcomponentmust bepresentinthe at1.2mmwhich observed suggests the flux HD100546usingonlyanextendedenvelope donotaccountfor thefar-infraredreproduce emission of distribution. Modelsthat energy from itsspectral well withexpectations TWHyaagrees from observed flux Figure 12shows the89GHzcontinuumThe emissiondetectedfromTWHyaandHD100546. thedustwithindisk. substantialprocessingof Hale-Bopp andindicative of incomet bands, silicate similartothoseobserved spectroscopy shows strongcrystalline remarkably AU),size, (8,000 about8arcseconds aswell Mid-infrared emissionfromdust. asstrongmillimetre substantial HD 100546isanearby HerbigBestarandshows adisk-like lightdistributionof scattered objects. i.e.,evolution growth, toward significantparticle planet-sized substantially evolved, withindicationsof wavelengths theTWHya diskis usingsingledishtelescopes. Modellingallavailable datasuggests molecularlinesat submillimetre astronomical units(AU). Itsdiskhasbeendetectedinanumber of approximately 200 at least3.5arcseconds, equivalent toalinearsizeof extends toaradiusof TW Hyaisisolatedfromanymolecularcloudbutretainsaface-ondiskvisibleinscatteredlightthat two about arcseconds. of three antennas, withanangularresolution usingtwowere compactantennaconfigurationsof observed comet-like dust.These silicates, shows indicative crystalline of spectrum Herbig Bestarwhose infrared disk targets, TWHya,theclosestknownyoung classical TTauri southern star, andHD100546,anearby stars TWHyaandHD100546 stars TWHyaandHD100546 circumstellar disksaroundtheyoung circumstellar disksaroundtheyoung Millimetre obser Millimetre obser vations of vations of vations of vations of vations of page 17 +

( J = 1–0)

line emission at 89GHz(3.4mm)fromtwoline emissionat

Astronomy reports = 1 – 0) J (

+ are depleted due to a + line for collisional excitation is excitation line for collisional = 1 – 0) J (

+ line. The models all have disk masses of The line. models all have 0.03 + page 18 spectrum of TW Hya, position. the continuum integrated over

= 1 – 0) J (

+ , the detection ofextended be present must emission indicates high densities -3 cm line emission from the line emission from Gaussian size with a fitted TW Hya disk is spatially resolved, 4 = 1 – 0) J (

Images obtained with the Compact Array showing radio continuum emission at 89 GHz from the showing radio continuum emission at 89 GHz from Array Images obtained with the Compact + Figure 12 young stars TW Hya and HD 100546. to large radii, independent of model for the disk. and chemical HCO No any detailed physical solar masses and disk radii of 200 AU. High depletion High solar masses and disk radii of has been observed disks of in other young 200 AU. varying size and indicates that substantial depletion occurs throughout the disk, as expected for planet formation through accretion. combination ofcombination in the warm photodissociation and freezing-out surface in the cold parts layers of the disk accretion based either on a radiatively-heated These models, disk shielded from stellar activity. disk structure,structure two-layer consistent with the Compact Array are for or a passive observations, ofboth the size scale and the absolute intensity the HCO emission was detected toward HD 100546, HD a surprising detected toward result.emission was Observations of more abundant the 110 – 115 GHz rangespecies CO in the needed. are modelling ofPrevious the TW Hya disk suggestsHCO CO and like that species Figure 13 shows the HCO the shows Figure 13 approximately 6 x 10 approximately of of Since the critical density 3.2 arcseconds. the HCO The velocity and line-width of and The velocity the narrow emission line are in agreement with single dish observations. The HCO

Astronomy reports kilometres persecond. Figure 13 Imaging HCNemissionaroundRScl Imaging HCNemissionaroundRScl has been observed inseveral othersources.has beenobserved HCNinthedetached shellismostlikely due toitsphotodissociationintoCN, as lack of emission. The theCO which thattheHCNenvelopeHCN spectra, indicate isexpandingmoreslowly thanthebulkof by higher-transition, single-dish iscorroborated ingeometry difference theCOdata. The from inferred attached envelope detachedshell recentmasslossratherthantheolder(andhencelarger) resultingfrom withinthecalibrationuncertainties. Thus,flux withan itappearsthattheHCNemissionisassociated isconsistentwiththeSEST flux totalCompact resolvesArray The thesource (Figure14). partially only aboutonearcsecond,sothateven ourhigh-resolutionimaging maximum (FWHM)of full widthathalf between June andOctober2002.We withaGaussian thattheHCNemissionisextremely compact, found threeantennas, 31–413m, withbaselinesranging from R Sclinseveral compactconfigurationsof Array’s theHCN ledustoobserve restrictedfrequencyrange were madeinaCOemissionlinewiththeSwedish-ESO SubmillimetreTelescope (SEST),theCompact RScl ashellaround of thathadindicatedthepresence Although theprevioussingle-dishobservations (compared, forinstance, tomolecularclouds). smallangularsize relatively 3-mmsystembecausethey of are thecurrent for simplestructures theshell).Notwithstanding theirscientificinterest,circumstellarshellsalsomake ideal“testsources” of thewind(relatedtosymmetry isotropy of of variation (related totheshellthickness)anddegree themass-loss theshell,butalsotimescaleof not onlytheexpansionvelocity of one candetermine molecularemissionintheshellathighangularresolution, heliumshellburning. Byobserving onset of massloss, perhaps duetothesudden increaseintherateof at somepointinthepasttherewas asudden athindetached shellindicatesthat losing massinaslow stellarwindisquitetypical,butthepresenceof anddust.For moleculargas adyingstartobe which is believed tobeencircledby adetached shellof 3-mmsystemwas theCompactArray thecarbon-richredgiantstarRSculptoris, for targets thefirst One of M. Lindqvist,H.Olofsson(Stockholm Observatory, Sweden) T. Wong (ATNF); F. L.Schoeier(LeidenObseratory, TheNetherlands&Stockholm Observatory, Sweden); Imaging HCNemissionaroundRScl Imaging HCNemissionaroundRScl Imaging HCNemissionaroundRScl HCO + spectrum ofTWHyashowingthedetectionanarrowspectrum emissionlinecentred atavelocityof3 Velocity (kilometrespersecond) page 19 (J = 1–0 ) lineat88.6GHz.We observed

Astronomy reports ) and envelope size, using the HCN size, ) and envelope 2 page 20 Channel maps of HCN (J =1 – 0) emission from R Scl. The beam size is 2.7 x 1.8 arcseconds. The velocity R Scl. The beam size is 2.7 x 1.8 arcseconds. Channel maps of HCN (J =1 – 0) emission from data (both single-dish and interferometer) as constraints. The best-fit envelope size is about 1,000 AU, about 1,000 size is The envelope best-fit and interferometer) (both single-dish data as constraints. modelling the Compact Arraywhereas data of alone yields a size (comparable to the size of only 300 AU in our high-resolution maps).the emission region Thus a single set of model parameters cannot high optical depth the of single-dish and interferometer fit both the simultaneously Possibly data. the to changes conditions of in the physical the emission very sensitive HCN lines makes envelope the inner that as clumping in the mass distribution) are(such not accounted for in our model. A detailed radiative transfer code, based on the Monte Carlo method, has been used to jointly model the been used to jointly method, has on the Monte Carlo based transfer code, radiative A detailed Array Compact data. The and single-dish HCN are the current inputs to the model main mass-loss rate have we year) and the stellar radiation(in solar masses per for these, With reasonable assumptions field. to H for (relative the HCN abundance values calculated the best-fit Figure 14 per second. have been binned to 2 kilometres of rest) to the local standard channels (given relative

Astronomy reports wings wings Planetar Planetar characteristic isknown. More unusual emissionpeaks. withfour isthe“DD”source withthis Onlyoneothersource aswell areexpectedtobestarswithbipolarshells. asslopinginneredges.with slopingouteredges These thestarthanonother. “Dw”starshave The OH1612-MHzspectra is much ononesideof stronger have oneemissionpeak which much isvery thantheother—thisshows stronger thatthemaseremission the shell.Inoursamplewe seeseveral variations ontheclassicdouble-peaked “De” spectra The profiles: an expandingsphericalshell,withthetwo onthefrontand rear of peaksbeingemittedfromsmall“caps” between thetwo andslopinginneredges outer edges peaks.steep ischaracteristic spectralprofile This of the85sources, (“D-type”)at1612MHz,with double-peaked 57exhibit aclassic spectrum profiles. Of thespectral We have ontheshapeof categories, classifiedthespectrausingsixdifferent depending 1612MHz. OHmaserspectra,forsourcesinoursample, atafrequency of Figure 15shows examplesof symmetrical ordistorted. onthewindspeeds,provide andonwhetherthewindsarelikely accurateinformation tobespherically lasers.molecules isproducedby maserspectraalso amasereffect—themicrowave The equivalent of conditionsinalayer onthephysical aroundthecentralstar. fromthese gas radiation formation The stellarwinds.outflowing Each moleculerequiresdifferentphysical andprovides conditionstoexist in- radioemissionfrom hydroxyl, waterobserving andsiliconmonoxide moleculesthatarelocatedinthe OHmasersourcesintheGalacticplane(Sevenster etal.). For thissample, we are previous studyof To 85post-AGB starsfrom a investigate this question, we have selectedawell-defined sampleof nebulae. seeninsomeplanetary andothercomplicatedstructures geometries causes thebutterfly-wing stellarevolution. Bystudying thepost-AGB what starswe maybeable todetermine post-AGB phaseof windsbeginsearly nebulae inthe non-sphericalplanetary stars anditseemslikely thatthe shapingof phase known astheAGB. nebulae arealsoseeninpost-AGB seen inplanetary different geometries The known (post-AGB) aspost-asymptoticgiantbranch starsandhave evolved beyond the secondgiant nebulae. stars are These toplanetary starsthatare theimmediateprecursors We are studyingasampleof may beimportant. thecentralstars may effects, causegravitational of orrotation insomedirectionsonly. thestellarwindstoflow stars constrain Alternatively, companionstarsorplanets fieldsfromthe isthatseveral explanation magnetic theoriesarebeingdebated. Onepossible different known, are notyet but geometries of causesforthisproliferation The structures. complex, filamentary wings, butterfly orshow ellipticalorbipolarshapes, insomecaseswith circular, othershave theshapes of nebulae canbespectacularlybeautifulandreveal forms.While someappear manydifferent Planetary nebulae. as planetary stars andtheswept-up shellsmay thenbeseenasglowing areknown ionisednebulae. Starsinthisstage mass inhot,low-density, the fastwinds. hot windssweep uptheremainingmaterialsurrounding The have gas beenblown away, fromouter layers losingmassinslow of densewindstolosing change stars the astar’sAfter mostof originalmassback intotheinterstellarmedium. of transfer morethanhalf theirmassthroughslow, densestellarwinds. fractionof isthat Such moststarsshedalarge stages winds interestinthe“giant” particular insizeandbecomehotter.expand whilethestellarcoresdecrease Of outer layersgreatly changes. The structural throughasequenceof hydrogen, theygo core-burning of low-to-middlemassstars. Whenstars, out like ourown Sun, run nebulaearetheremnantsof Planetary R. Deacon(UniversityofSydney);J.Chapman(ATNF); A. Green (UniversityofSydney) wings Planetar wings wings Planetar Planetar y nebulaeandbutter y nebulaeandbutter y nebulaeandbutter y nebulaeandbutter y nebulaeandbutter page 21 fly fly fly fly fly

Astronomy reports page 22 Some examples of OH 1612 MHz spectra of post-AGB stars, obtained from data taken with the Parkes data taken with Some examples of OH 1612 MHz spectra of post-AGB stars, obtained from In our sample we also find five “S-type” sources. These only show a single peak of “S-type” sources. find five also we In our sample emission, maser but the “I” or irregular Finally stars. and post-AGB with AGB in common characteristics have otherwise stars with such emission peaks and a larger range. multiple Post-AGB than usual velocity spectra have geometries. irregular envelope with exotic associated spectra are usually of with still-to-come measurements together our maser data, From the stellar magnetic fields and imagesdetailed radio of have to some stars evolve to clarify why we hope the outflowing winds, and others do not. asymmetric winds Figure 15 top right-hand corner with a radio telescope in September 2002. The catalog name of each star is given in the types type given below the name. The 85 stars in this study have been classified into six different category DD-types), single (S-type) or irregular double (D, De, Dw and are depending on whether the OH maser profiles (I-type).

Astronomy reports Image reference: (Stockholm University, Sweden);NASA(USA) Photo credit: B.Balick(UniversityofWashington, USA);V. Icke(LeidenUniversity, TheNetherlands);G. Mellema super-sonic velocitiesofmore than300kilometres persecond. Hubble SpaceTelescope, showsapairofhigh-speed“jets”gasmovingawayfrom thecentre ofthenebulaat Figure 16 M2-9 isastrikingexampleof“butterfly”orbipolarplanetarynebula.Thisimage,takenwiththe Image STScI-PRC1997-38 page 23

Astronomy reports ray captures a captures ray a captures ray ray captures a captures ray ray captures a captures ray a captures ray page 24 nova nova nova nova nova ” super ” super ” super ” super ” super On the evening of 10 December 2001, the Rev. Robert Evans was conducting his regular supernova conducting of was Evans Robert On the evening the Rev. 2001, 10 December of from his backyardpatrol Mountains west in the Blue when he came across in the an interloper Sydney, late-type spiral galaxy majority of In an era when the vast nearby NGC 7424. are discoveries supernova or as part of telescopes, robotic made by trained Evans’ programs, search supernova the high-redshift him to maintain a proud record of allowed and trusty photographic have telescope eye, 12-inch memory, of discovery the 241st supernova and his 39th discovery, 2001ig was Supernova discoveries. supernova 2001. Since its commissioning, the Compact has played a leading roleArray in the monitoring of several II Type from most notably SN 1987A and SN 1978K. Radio emission at wavelengths, radio supernovae years after the or even months, searched for) until weeks, is typically not detected (or even supernovae ofoutburst. On the evening made use of 15 December 2001, we Saturday six hours of unallocated time on the Compact Array to make images of SN 2001ig at frequencies of 8.6, 4.8, 2.5 and 1.4 GHz. Eve, Year’s On New detection at the highest frequencies. a positive surprise, to our Somewhat there was on three Compact Array system 12-mm receiver detected at 18.8 GHz using the prototype it was antennas. Figure 17 shows an image of the field at 4.8 GHz from Compact Array observations taken on 17 February 2002. SN 2001ig is the upper of as contours; bright sources shown the source to the the two the results from our Compact is an unrelated background Figure 18 shows Arraysouthwest source. The 4.8 GHz data are shown. only the 8.6 and radio “light curve”of monitoring program; clarity, for a into three phases—a rapid turn-on can be divided supernova with a steep spectral index, due in large part to a decrease in the line-of-sight absorption; a peak in the flux is first seen at the higher which density frequencies;SN 2001ig had begun to 2002, a more gradual By March phase. decline in an optically-thin fade at 5 and 8 GHz, but then abruptly before doubled in flux for three weeks, and remained that way it again from a briefly In late dramatic excursions August, resuming its decline. Such halted its decline. and generally ofsmooth decline are rare, thought to be associated with the interaction the blast ejecta with a dense and rather inhomegenous circumstellar medium. SN 2001ig is one of only a half of examples dozen or so known the in which IIb” supernova, a “Type suggesting ofmuch that lines seen in their early optical spectra soon fade away, their outer hydrogen could also account which for this, possible mechanisms Two shed before the star exploded. were layers for the bumps in the radio light curve, are thermal pulses due to carbon/helium flashes in the core of a progenitor occurring5 – 10 solar mass asymptotic giant branch star, on periodic time scales of around or a modulation of500 years, a red supergiant progenitor a wind due to eccentric orbital motion about binary clumping Efforts leading to a pinwheel-like in the circumstellar medium. companion, massive are to model the observed in the context underway behaviour ofnow while Compact Array these scenarios, monitoring of 2003. throughout SN 2001ig will continue S. Ryder (Anglo-Australian Observatory); (Anglo-Australian of Sydney); E. Sadler (University S. Ryder Subrahmanyan (ATNF); R. USA) Laboratory, Research (Naval K. Weiler “baby “baby The Compact Ar Compact The Ar Compact The “baby The Compact Ar Compact The “baby “baby The Compact Ar Compact The Ar Compact The

Astronomy reports frequencies of4.8 and8.6GHzoveraperiodofapproximately 400days. Figure 18 radio sources. Thelowerradiosource isanunrelated background source. ofthegalaxyNGC7424fromimage oftheoutskirts theDigitizedSkySurvey. SN2001igisupperleftofthetwo Figure 17 The radiolightcurveofSN2001ig, showingthechangeinintensityofradioemissionat Contours showingthe4.8-GHzradioemissionfrom theregion around SN2001ig,overlaidonan page 25

Astronomy reports A . X-ray ObservatoryX-ray some can, in arkes arkes arkes arkes arkes Chandra ), and a characteristic age of 2,900 years. -3 observation of in SNR G292.0+1.8, shown

to look for new detections of pulsarsyoung , Chandra page 26 source, with a fluxsource, density at 1,400 MHz of and a low 80 microJansky

as deeply as possible results encouraged new In a 10-hour integration using the efforts. at Parkes very weak Chandra Pulsar discoveries at P discoveries Pulsar at P discoveries Pulsar Figure 19. The X-ray data of TheFigure 19. X-ray is pulsar wind nebula within which arcminute a two this source reveal previously without a pulsar remnant had been searched While this supernova located a point source. detection, the radio luminosity. X-ray pulsations were with the help of detected subsequent to and X-ray radio luminosity. the radio discovery. central beam of detected PSR J1124–5916, with a pulse period of system,we the multibeam 135 a moderate dispersion measure (330 pc cm milliseconds, PSR J1124–5916 is a Pulsar discoveries at P discoveries Pulsar of USA); D. R. Lorimer (University University, USA); B. M. Gaensler (Harvard (Columbia University, Camilo F. (ATNF) UK); R. N. Manchester Manchester, 2002 yielded a remarkable vintage of a central telescope playing the Parkes with pulsar discoveries, young role. of pulsars are objects Young of interest for a variety The of physics reasons. core collapse in evolved and magnetic stars can be inferred from observations spin period, space velocity, the initial which provide offield distributions of while measurements stars, neutron and luminosities, their beaming properties, spectraare crucial for determining the Galactic population and birthrate of pulsars Young pulsars. and emit substantial amounts of exhibit period glitches, frequently X- and gamma can be rays—these observed to learn about the internal composition of and the pulse emission mechanisms. neutron stars, in compact non-thermal neutron stars are embedded In addition, young wind pulsar radio and/or X-ray wind, or otherwise interact with their pulsar medium confines the relativistic where the ambient nebulae The embedded pulsars are of remnants. unique probes host supernova and immediate their environment the local interstellar medium. pulsars young for is the Galactic plane and more specifically in supernova location to search A natural and supernova Galactic pulsars between associations establishing bona fide However, remnants. 1970 (those of by known were business: two remnants has been a painfully slow five the Crab and Vela), 2000, remnants and 1,400 pulsars are known. and only 1985, than 200 supernova although more 10 by by in this regard—a survey productive not been immensely of for associations have Searches 88 supernova pulsars! remnants in the 1990s netted zero associated pulsar survey multibeam of recently the Parkes More system using a 13-beam receiver the Galactic plane, at a frequency of a very large broadly covered comparable to that of with sensitivity 1,400 MHz, area the best previous surveys of This survey remnants. been extraordinarily has successful, supernova but a pulsar between to date has yielded only one new association 700 pulsars, approximately discovering a discussion of remnant (for and a supernova remnant in the supernova PSR J1119–6127, pulsar, this Report Annual 2000). G292.2–0.5 see the ATNF that the existence of pulsars that relies on the premise a method to detect young used have We a pulsar the presence of also indicate must wind nebula decided to We pulsar. an energetic young and reasonably search pulsar wind nebulae cases, unambiguously identify a pulsar wind nebula and its embedded pulsar even when pulsations are when pulsations unambiguously identify a pulsar wind nebula and its embedded pulsar even cases, not detected. the beautiful by example is provided One such complication with this approach is that it is not always clear whether a particular clear compact object is a always is that it is not complication with this approach images recent X-ray from the pulsar wind nebula. However, Pulsar discoveries at P discoveries Pulsar at P discoveries Pulsar

Astronomy reports of PSRJ1124–5916, obtainedfrom Parkesdata,isoverlaid. G292.0+1.8. Thepositionofthepulsarisindicatedbyarrow andthemeanpulseprofile Figure 19 tolearn. relatively pulsarobservers newlessonforradio interest,such asyoung pulsars, thisisa photonsfromastronomicalsourcesof obtaining ahandfulof have atall!WhileX-ray astronomers longbeenusedtospendingaday aday orso, if timesof integration using when withthebestpresent-day telescopesonly aredetectable radio with luminositiesthat themdoso Our studyhasshown manyyoung However, pulsarsbeamtowards that the Earth. of many young pulsars. luminosity distributionandbeamingfractionof relevant tothesesearches isunderway onthecombinationof andshouldyieldusefulconstraints thesensitivity andselectioneffects andX-raystudies at radio wavelengths, analysisof andacareful two years, andthesearches continue. newly discovered The objectsarebeinginvestigated infollow-up pulsars, associated withwindnebulae (insomecaseswithinsupernovae), have beendetectedinthepast Arecibo, Bank,Jodrell Green BankandParkes telescopes. young weak sixvery andenergetic Inall, Following thisdiscovery, pulsarwindnebulaewere aspossiblewiththe searched manymore asdeeply Chandra X-rayimageoftheoxygen-rich1,700yearoldcomposite SNR page 27

Image credit: NASA/Rutgers/J. Hughes et al.

Astronomy reports solar 12 -massive spiral -massive spiral -massive -massive spiral -massive -massive spiral -massive spiral -massive solar masses and a total dynamical mass of solar masses and a total dynamical mass 1.5x10 page 28 solar masses. Thedensity of solar masses. more massive galaxies much 9 10 y of a super y of a super y of y of a super y of y of a super y of a super y of galaxy galaxy Discover Discover than this characteristic value is poorly constrained, however, as these super-massive galaxies are very rare. as these super-massive constrained, is poorly however, value than this characteristic a super-massive discovered have we Through a large receiver, multibeam survey that utilised the Parkes spiral galaxy at a distance of suggest telescope Data from the Parkes 140 Megaparsecs. that the galaxy J0836–43 has an HI mass ofHIZOA 7x10 galaxy How massive can a spiral galaxy can Current become? massive predict that theoretical models How galaxies spiral the like form the merger from ofMilky Way 25% and between was smaller galaxies at times when the Universe 50% of its current age. This merger process is thought to create a population of spiral present-day M*. galaxies densities decline value, whose number a characteristic exponentially at masses higher than see page 32) support this theory and set M* to a neutral HIPASS, from Observational (e.g. evidence (HI) mass ofhydrogen 6x10 approximately J. Donley, B. Koribalski (ATNF); R. Kraan-Korteweg (University of Guanajuota, Mexico); A. Schroeder A. Kraan-Korteweg R. Mexico); (University of Guanajuota, (ATNF); B. Koribalski J. Donley, team ZOA and the (ATNF) UK); L. Staveley-Smith (University of Leicester, Discover masses. Thistimes that of HI mass is 20 masses. and the total mass is at least five Galaxy Milky our own Way spiral galaxies known, J0846–43 among the most massive mass! This places HIZOA times the Milky Way’s a handful ofwith only galaxies whose such Some masses are comparable. HI and/or total dynamical galaxies 1752, UGC 12591, and NGC 1961. include Malin I, ISOHDFS 27, UGC high-resolution observations with the Compact ArrayFollow-up confirmed J0836–43 is in that HIZOA fact a single system, with a disk radius of and an inclination-corrected kiloparsecs 66 rotational velocity of as a function of rotation curve, the rotational velocity 312 kilometres per second. The galaxy’s radius, largeis constant at radii. This suggests J0836–43 has a large dark normal that, like HIZOA spiral galaxies, a propertyby current also predicted disk radius, the beyond well halo extending hierarchical matter clustering models of galaxy formation.This that, galaxy if is so large and massive formed at the very ofbeginning us had time to complete 10 rotations! to giving In addition only have it would the Universe, insights into the HI properties of J0836–43, our observations at the HIZOA determined have we that these data, data. From radio continuum also provided ArrayCompact have formingJ0836–43 is probably stars at a rate of per year. about 26 solar masses in the near- (AAT) J0836–43 with the Anglo-Australian Telescope also observed have HIZOA We behind the plane of J0836–43 is located Because HIZOA in a infrared K and H bands. the Milky Way as the Zone ofregion known the optical B-band emission originating from the galaxy is Avoidance, by nearly 12 magnitudes ofobscured us from obtaining an optical image of dust extinction, preventing than that on the optical light. The less severe emission is much the effect on infrared Luckily, the galaxy. us to determine allowed observations therefore of both the inclination have AAT 65 degrees, the galaxy, of as the distribution as well its old stellar population. Both a galactic bulge and disk can be inferred from emission. Thethe infrared bulge of has a central surface brightness 15 magnitudes per square arcsecond and a scale length of The disk has a scale length of 2 kpc. out to a radius of 4 kpc and can be detected 20 through 1 magnitude of even kpc, K band. extinction in the infrared J0836–43 is one ofThe galaxy HIZOA Although a nearby galaxies spiral detected. ever the most massive The galaxies image, are there is no evidence that interacting. two the galaxy can be seen in the AAT and integrated field emission ofvelocity suggesting no disturbances, J0836–43 show it is a that HIZOA The detection ofnormal, galaxy. J0836–43 albeit very galaxy massive, such as HIZOA a super-massive fundamental questions that arise when formulatinghelps us to answer theories ofgalaxy evolution. galaxy galaxy Discover Discover

Astronomy reports seen asthebrightstripextending overvelocitiesfrom approximately 10,400to11,000 kilometres persecond. Figure 21 peak value,inincrements of10%. obtained from Compact Array data,overlaid.Thecontour levelsshowtheHIemissionfrom 10%to90% ofthe Figure 20 ways todetectsuch hiddengiants. withreceivers thebest blindsurveys Large-scale such astheParkes multibeam receiver provide oneof A “position–velocity”diagramforHIZOA J0836–43alongthemajoraxisofgalaxy. Thegalaxyis A K-bandimageofHIZOA J0836–43from theAnglo-AustralianTelescope withtheHIcontours, page 29

Astronomy reports vey vey vey vey vey The observing team present at Narrabri for the team present The observing left to right: Lister From September pilot survey. Kate Ron Ekers, Jennifer Donley, Staveley-Smith, Carole Smith, Mike Kesteven, Elaine Sadler, In the background, Wilson. Jackson, Warwick seen observing the antennas CA02 and CA03 are –70 meridian between declinations of –60 and degrees. time with the antennas which were not being used were time with the antennas which for fast scanning. radio imaging ofFollow-up detected the sources carriedin the survey was out in October 2002, more accurate positions and fluxgiving densities. Almost half within the 226 detected sources lay degrees offive and can be the Galactic plane, and supernovae identified with Galactic HII regions, planetary The nebulae. remainder are extragalactic made up ofsources, candidate quasars (60%), galaxiesradio (20%) and faint optical objects or blank fields (20%). The 18 GHz survey in 2003. will continue page 30 ray 18 GHz pilot sur ray 18 GHz pilot sur ray 18 ray 18 GHz pilot sur ray 18 ray 18 GHz pilot sur ray 18 GHz pilot sur ray 18 irst results from the Compact from results irst the Compact from results irst irst results from the Compact from results irst irst results from the Compact from results irst the Compact from results irst Ar Ar F F In Septemberfor 2002, as a pilot study an all-sky we radio imaging survey wavelengths, at millimetre observed square degrees 1,216 of the southern sky wideband (4 GHz a novel at 18 GHz using bandwidth) analogue correlator on one baseline of imaging surveys Several ofthe Compact Array. the already been carriedradio skyhave out at where the 0.3 and 5 GHz, between frequencies radio population powerful source is dominated by galaxies but at and fainter starburst galaxies, 5 GHz only small areas of above frequencies sky been studied in detail. This is mainly because have small fields of large radio telescopes typically have at high frequencies, arcminutes) view (one to two making it extremely to observe time consuming large areas of Measuring the high-frequency sky. properties of extragalactic radio sources is crucial for interpreting and high- the high-sensitivity resolution maps of the cosmic microwave background that being produced are now by WMAP and is also importantsatellite missions like for studies of galaxies and their cosmic active evolution. The survey is made possible by using the new in combination Compact Array 12-mm receivers with a 4 GHz bandwidth prototype correlator (the standard at ATNF recently developed Compact Array correlator of a bandwidth has 128 MHz).The increased bandwidth means that the for short is high even sensitivity continuum large areas of allowing integration times, sky to be On 13 – 17 observed in a fast-scanning mode. scanned the region ofSeptember 2002, we sky declinationsbetween of –60 and –70 degrees antennas ofusing two the array as a two-element We interferometer with the wide-band correlator. 15 square roughly degrees per hour to a covered detection limit of The Compact 60 milliJansky. used in a “split array” so that Array mode, was regular synthesis imaging could be carried out at the same Ar Ekers, Mike team; Roberto Ricci (SISSA, Italy); Ron of Sydney) for the 20-GHz survey Elaine Sadler (University (ATNF/University Walker Mark (ATNF); Wilson Ravi Subrahmanyan, Warwick Kesteven, Lister Staveley-Smith, Italy) Observatory, (ANU); Gianfranco De Zotti (Padova Jackson of Sydney); Carole F Ar Ar F F

Astronomy reports from thegalaxy’s nucleusterminateanddumptheirenergy. concentrated atthehotspots(roughly onemillionlightyearsfrom theparent galaxy)where relativistic jetsofplasma in thePilotSurvey, overlaid onanopticalimagefrom theDigitizedSkySurvey. Thehigh-frequency radio emissionis frequency (843MHz)radioemission from theSUMSSsurvey. Thebluecontoursshowthe18 GHzemissionimaged radio galaxyshownhere (anellipticalgalaxyatz=0.0963) are relatively nearby. Here thered contoursshowlow- Figure 23 due tosources associatedwiththeLarge MagellanicCloud. Galactic disksources suchasHIIregions. Thesmaller excessatlatitudesof–30to–40degrees is degree binsinGalacticlatitude.Thepeaknearlatitudezero corresponds tothepopulationof Figure 22 While manyofthesources are detectedin thePilotSurvey associatedwith distantquasars,some,likethe A histogramshowingthe detected source densityfrom infive- the18GHzPilotSurvey page 31

Astronomy reports page 32 An unbiased census of hydrogen in hydrogen of census unbiased An in hydrogen of census unbiased An Universe the local Universe the local In 1997 an international of team set out to survey astronomers the entire southern sky for neutral receiver. multibeam radio telescope equipped with the 21-cm the Parkes (HI) emission using hydrogen This instrument is a very survey efficient the first us to conduct tool, allowing large-scale blind neutral intermediate both in the and out to distances neighbourhood of survey, hydrogen Galaxy, the MilkyWay All Sky Survey),of (HI Parkes as HIPASS known The 170 Megaparsecs. data taking for this survey, effort has gone and since then much finished in 2002, into analysing the largewas we Here, dataset. on some ofconcentrate the progress the extragalactic that has been made for component of HIPASS. data consists of and The eight degrees HIPASS eight by cover sky, on the which each 530 cubes, thirds these cubes comprise almost two from –1,200 to 12,700 kilometres per second. Together velocities of 388 has been directed to the most attention So far, –90 to +25 degrees. from declination the sky, southern cubes south of Our first task after creating the data cubes is to identify declination 2 degrees. extragalacticthis was found that line signals in the noisy background. HI 21-cm emission It was the results of independent automaticmost efficiently finder done using two scripts, which were merged. man-made detections at clouds and by to be polluted Galactic high-velocity frequencies known from the list of removed interference were The remaining 130,000 potential detections were detections. subjected to a series of this process, After three different individuals. by for verification checks manual times larger almost a twenty than any sample 4,300 HI selected galaxies, left with approximately were we existing HI selected sample. the skyFigure 24 shows distribution ofThe = 0 indicates dashed line at b the plane sources. the HIPASS of hinders which All optical redshift surveys extinction close to this line, from severe suffer the Galaxy. ofthe identification a large region of extragalactic sources over an incomplete and hence leads to sky, ofpicture the large-scale structure ofaffected by is not that HIPASS The figure clearly shows galaxies. extinction and measures the galaxy in all regions of distribution equally efficiently This illustrates the sky. ofthe power the large-scale to study structure in the local Universe. HIPASS of analysis A more quantitative the large-scale structure as the two-point is possible with a tool known correlation This probability of function. measures the excess distance finding another galaxy at a given this function has been studied extensively optically selected galaxies, For any galaxyfrom in the sample. morphological and star formation type, to be dependentand has been shown on galaxy luminosity, form a two-dimensional Figure 25 shows ofactivity. the correlation function of The galaxies. HIPASS correspondvertical and horizontal axes to separations galaxies between orthogonal and parallel to the finally leads to line of some mathematics, Integrating and applying lines, along vertical sight, respectively. ofa measurement comparison, the 26. the real space correlation is shown in Figure For function, which of (AAT), Telescope the at Anglo-Australian correlation function from the 2dF galaxy redshift survey, selected galaxies optically This diagram is also shown. that our sample of shows HI-selected galaxies, representing a population of clustered than the optically- is less strongly galaxies, evolving more slowly These here. gas-rich effects galaxies play are at two in might only survive Possibly, selected sample. could triggerwhich regions without too many interactions with neighbouring galaxies, star formation and burn galaxies is that the HI-rich up the HI. Another explanation are formed density actually in lower regions. M. Zwaan, M. Meyer, R. Webster (University of Melbourne); L. Staveley-Smith, B. Koribalski (ATNF) and the B. Koribalski (ATNF) (University of Melbourne); L. Staveley-Smith, R. Webster M. Zwaan, M. Meyer, team HIPASS An unbiased census of hydrogen in hydrogen of census unbiased An Universe the local An unbiased census of hydrogen in hydrogen of census unbiased An in hydrogen of census unbiased An Universe the local Universe the local

Astronomy reports pole isinthecentre oftheimage. neutral hydrogen massofthesources. Thedashed linemarkedwithb=0istheGalacticplane.Thesouth celestial distances ofthesources, inthesense thatredder colourscorrespond tohigherdistances.Thesymbolsize indicates the Figure 24 galaxies. conversion tostarsinthedisksof indicatingthegradual from 10%itspresentage, neutralgas only isapproximately 0.038%. This fivedensity isonly timeslower thanatthetimewhenUniverse was theUniverse, mass theneutralgas thecriticaldensityof at thepresentepoch. Expressedasafraction of massdensity theneutralgas earlier, much andallows forapreciseevaluation poorerdeterminations, of with agreement new HImassfunctionisingood theHImassfunctiontodate.This of measurement containingthe1,000brightestdetections,Bright GalaxyCatalogue resulted inthemostaccurate HIPASS, the thefirstproductsof oneof differentmasses.An analysisof distributed over of galaxies HIPASS structure, fromstudyingthelarge-scale Apart measuringexactlyhow HIis isusefulfor The distributionofextragalacticHIPASS sources inthesouthernskey. Thecolourcodingcorresponds tothe page 33

Astronomy reports ) and σ page 34 The two-point correlation function for HIPASS galaxies, plotted as a function of transverse ( galaxies, plotted as a function HIPASS function for The two-point correlation The projected real space correlation function for HIPASS and 2dF galaxies. The HI-selected galaxies function for HIPASS space correlation real The projected ) pair separation. π Figure 26 the 2dF galaxy survey. than galaxies found in clustered less strongly are Figure 25 radial (

Astronomy reports The Souther The Souther spiral arm. theouter may beadistantextensionof This emission. of theHIdiskasathinridge of detect theedge interestingfeaturesinthisimage. Atlarge, positive velocities (<100kilometrespersecond)we number of the plane. dataallow These ustotracespiralfeatures outtoGalacticradius30kiloparsecs. area There HIin emission, shown inFigure28.We of thishigh-resolutionimage combinealmost10,000spectrafor HI Using datafromtheentireSGPSIregionwe have of createdanewlongitude–velocity diagram intheISM. structure thesmallscale tothecoolphaseandthesemay much of accountfor returns gas instabilities that onlyafewparsecs. these It is through onscalesof this shellwe have instabilitystructures detectedgas overparsecs indiameterandextends above akiloparsec andbelow theGalacticplane.Along thewalls of chimney shown onthecover, was discovered GSH277+00+36, intheSGPSI;itismorethan600 fromthediskintohalo. theGalacticplaneandexpelhotgas The supernovae, canbreak outof stellarwindsand objects,These ISM. by of which thecombinedeffects arebelieved tobeformed objectsinthe thelargest which aresomeof thisreport), and chimneys theoneoncover (including of HIshells, bubbles newandexciting SGPSisproducingmany The results. work The studiesof includes oneKelvin. kilometre persecondandasensitivity limitof one onearcminute, aspectralresolutionof HI intheentireGalacticplanewithanangularresolutionof the anatlasof thiscollaborationistoconstruct GalacticPlaneSurvey.International of ultimategoal The the toform hemisphere GalacticplanemadewithtelescopesinCanada,theUSA,andGermany thenorthern of hasbeencombinedwithtwoThe SGPS data surveys ionic medium. Way theMilky andthemagneto- of continuum fieldstructure thatwe areusingtostudythemagnetic We theISM. inthe alsohave information fullpolarisation hydrogen theneutral componentof of distribution dynamics, aretounderstandthestructure, andthermal thesurvey of goals general 27. The dataset thatissensitive toallangularscalesfromtwo arcminutes toseveral inFigure asillustrated degrees, fromtheParkes radiotelescope provides spacinginformation a andshort from theCompactArray high-resolutiondata thisregion. Additionally, the combinationof sensitivity over of previous surveys magnitude improvement inbothangularresolutionand SGPSconstitutesmorethananorderof The anticipated inmid-2004. along theGalacticmidplanetolongitude+20degrees. SGPSIIisinprogress, withcompletion The second phase, SGPSII,which covers regionaroundtheGalacticCentreandextends a100square-degree a spanningGalacticlongitudesfrom253to358degrees. In2002we began latitudes –1to+1degrees), ontheGalacticmidplane(Galactic centred 210squaredegrees the survey, SGPSI,covered anareaof Way. theMilky of firstpart intheplaneof The 335squaredegrees hydrogen lineinaregion of spectral the21-cmcontinuum emissionandatomic (SGPS),aimstoimage GalacticPlaneSurvey the Southern Way. Milky theISMinSouthern the ATNF hasbeeninvolved project, This of survey inalarge-scale limited.However, theISMisremarkably thepastfive for years theatomicphaseof of thermodynamics thedynamicsand studieswithradiotelescopes, of ourknowledge Despite some50years of theinterstellarmedium(ISM). Way Milky The studyingthephysics of for provides theclosest laboratory B. Gaensler(Harvard University, USA) N. McClure-Griffiths (ATNF); J.Dickey(UniversityofMinnesota,USA); A. Green (University ofSydney); The Souther The Souther The Souther n GalacticPlaneSur n GalacticPlaneSur n GalacticPlaneSur n GalacticPlaneSur n GalacticPlaneSur page 35 vey vey vey vey vey

Astronomy reports page 36 A cross-section of the Milky Way as seen at a wavelength of 21 cm. The upper figure is an image made figure as seen at a wavelength of 21 cm. The upper of the Milky Way cross-section A Figure 27 of 14 observing the 21 cm line with an angular resolution by the Parkes telescope with the multibeam receiver and latitudes of –1.5 to +1.5 Galactic longitudes of 266 to 280 degrees, is from covered The area arcminutes. as area per second. The lower image shows the same velocity of +73 kilometres of rest at a local standard degrees In both of 2 arcminutes. data, with an angular resolution Array seen with a combination of Parkes plus Compact while black shows no atomic hydrogen, to bright emission from images, the light yellow colour corresponds the disk is warped toward where far outside the solar circle, emission. This velocity plane traces the outer Galaxy, latitude). The broad, with zero negative latitudes in this longitude range (note that the bright ridge does not align from giant shells resulting dark channel that bisects the disk on the right-hand side is a superposition of many stellar winds and explosions. From the SGPS data we have measured the rotation measured curve have of we the SGPS data From Figure 29. This in shown the inner Galaxy, of a number produced; it shows curve sampled HI rotation densely is the most ever In new results. particular see strong departures we associated with the spiral smooth circular rotation from arms, which theory gas expect that we a to spiral density wave According approaching with dotted lines. are marked spiral arm the arm before in circular velocity a decrease the inner Galaxy side should show from and then an increase as the gas passes through the arm. This in the Milky see is almost exactly we what Way.

Astronomy reports enters aspiralarmandthenbegins toincrease asthegaspassesthrough thearm. (N), Scutum-Cruxarm(Sc)and theSagittarius-Carinaarm(Sa).Therotational velocitydecreases asthegas shows theapproximate positionsand widthsofthespiralarmswhichare labelledfrom lefttorightasNorma arm Figure 29 degrees. Sagittarius-Carina spiralarmisapparent asaloopofstrong emission(very pink)crossing nearlongitude280 outer edgeoftheHIdisk(atlarge positivevelocities).We are alsoabletotracetheoutermostspiralarms.The solar circle, whereas negativevelocities showgasintheinnerGalaxy. Usingthisimagewecansearch forthe There are approximately 10,000pixelsalongthelongitudeaxis.Positivevelocitiescorrespond togasoutsidethe Figure 28 HI rotation quadrant), sampledevery arcminute. fortheinnerGalaxy(fourth curve Thedottedline Longitude–velocity imageoftheHIemissioninGalacticplane over theentire SGPSIregion. page 37

Astronomy reports Lightning strike near one of the Compact Array antennas Photo: ©Robert Della-Piana 2002

page 38 Compact Ar Compact Ar A A developments developments Ar Ar Compact Ar place intheseareas. During 2002, considerabledevelopment work took to thetelescopehardware, software andoperation. changes a myriadof requires the millimetreupgrade As well asdeveloping thenew receiver packages, antennas andinterimsystemsonly. during 2002continued tobeavailable withthree expected tofollow in2004.Millimetreobserving antennas isduein2003withthe3-mmsystems thefinal12-mmreceivers onall Installation of thefinalsystems. of design andconstruction to concentrateengineeringdevelopment onthe interim systemtoallantennasitwas decidedin2002 with thesethreeantennas. thanextendthe Rather weremillimetre images obtainedusingdatataken installed onantennas2,3and4thefirst interim 12-and3-mmreceiver were packages using two antennas onasinglebaseline. In2001, takeninNovember were Array Compact 2000 millimetre-wave atthe first The observations 1997(MNRF-1997). in February Research underacontractsigned Facilities program, the Commonwealth Government’s MajorNational hasbeenfundedunder upgrade and 3mm.This frequencies, bandsat12 withtwo newobserving high(millimetre-wave) at tooperate the array hasbeentoupgrade years foranumber of Array development focusattheCompact primary The developments Ar A reports Observatory developments developments Ar Ar Compact Ar Compact Ar A A ustralia T ustralia T ustralia T ustralia T ustralia T ray upgradesand ray upgradesand ray upgradesand ray upgradesand ray upgradesand elescope elescope elescope elescope elescope ray ray ray ray ray page 39 configurations configurations New stationsandar New stationsandar configurations New stationsandar lengths thedataqualityisreduced atlow elevations atlow elevations—at sources thesewave-observe millimetre wavelengths whereitisundesirable to considerationhours. at Thisisanimportant Fourier coverage tobeachieved inlessthan12 compact configurations, andallows areasonable five antennastations. very isintendedfor This spurline, 214-mlongwith anorth of construction the alsoincludes millimetreupgrade The 360 m. approximately EW367, withmaximum spacings of configurations, EW352and complementary andtwo 214 m, has amaximum spacingof configuration includeconfigurationEW214,which new The theMNRF-1997program. of part as haveantenna stations beenconstructed brightness sensitivity ninenew observations, high for andtoprovidemetres) betterarrays (with antennaspacingsuptoseveral hundred To configurations optimisetheCompactArray configurations configurations New stationsandar New stationsandar Observatory Dr BobSault,Officer-in-Charge PaulWild attheNarrabri ray ray ray ray ray

Observatory reports ucture ucture ucture ucture ucture Antenna str Antenna str Antenna Antenna str Antenna The efficiency of antennas depends the telescope partly the accuracy on of At their surfaces. optical surfaces the antenna millimetre wavelengths within tolerances that are 10 need to be maintained stringenttimes more at than centimetre This is a challenging engineering wavelengths. has an ongoingrequirement. The program ATNF the surface accuracies of and monitor to improve the antennas. factors are important good in achieving beam Two the antenna efficiency and beam shape: firstly, be set to within a specified surfacepanels must be made of account must tolerance; secondly, the in the gravitationalchange deformation of the antennas as a function of The elevation. deformations of interest include changes to the of as movement as well main dish shape the During the year package. subreflector and receiver initiated to understand these were studies two issues. A holographic image of the surface of antenna 2 obtained using a 30 GHz geostationarywas that the signal. as a reference Thissatellite showed aligned to an accuracy (rms)panels were of 0.21 mm, with the poorest accuracy occurring in the innermost ring of panels. One of the shortcomings of standard holography is that it uses geostationary This satellite signals. means that the holography is performed at a method of An alternative elevation. fixed single, surveying using the antenna optical surfaces is by This form photogrammetry. is an advanced of surveying where reflectors are placed at many points The three-dimensionalon an antenna surface. positions of the reflectors by can be deduced photographing surface and reflectors the from of An advantage aspects. many photogrammetry can be performed it is that at arbitrary elevation, and so the gravitational effects on the antenna can be studied. Antenna str Antenna str Antenna page 40 Signal distribution Signal distribution A major task of the MNRF-1997 program the was upgrade of signal distribution the system throughout the array as an upgrade as well of the local oscillator system. The upgraded signal paths replace which use single-mode optical fibres, coaxial cables fibres. and multi-mode copper wires, distributesThe system now local oscillator two references: at frequency one used frequency a low and a high frequency one wavelengths centimetre millimetre for use in conjunction with the new packages. receiver The installation of the new single-mode optical completed fibre signal distribution system was completed on all was Fibre splicing work mid-year. as to a as well antennas and to all station posts, panel in the screened room.patch Upgraded installed to eliminate a fibre modems were that problem had previouslysynchronisation caused an occasional loss of data. Shortlyall six thereafter to regular operations over switched antennas were using the new reference frequency distribution system.the end of By all signals, the year including time frame, ethernet communications and intermediate-frequency return were data links, running on the new fibres. The one remaining task for the signal distribution system, making the high frequency local oscillator is due for completion reference system tuneable, 2003. in May Signal distribution due to increased atmospheric opacity and poorer opacity and increased atmospheric due to phase stability. the completion ofFollowing on optical fibre work new in the new antenna stations 2002, several April and EW367, EW214, H75 array configurations, used dur- and successfully were scheduled H168, to October period. The reconfigurationing the June the first was 2002, on 12 August to the H75 array, astronomical use of north the new spur. Signal distribution Signal distribution

Observatory reports Early morningatthe Australia Telescope Compact Array adjustmentsystem. subreflector was initiatedduringtheyeartodesignatwo-axis thesubreflector. Following thesefindings, astudy of a two-axis adjustmenttotheaxialandtiltmotions canberecovered,shape degradation however, with astronomically.observed lossandbeam gain The withthose agreed implied by thesedeformations effects andgain/elevation beam shapechanges Additionally,location. analysisshowed the that toitsdesign remainsclose the subreflector surface, while elevations inthemainreflector occurs atlow showed themainantennadeformation that elevations results between The 15and90degrees. forantenna onantenna2, was undertaken examination 2002,aphotogrammetric In February page 41 Antenna controlcomputers Antenna controlcomputers were 2002. taken inSeptember computers usingthenew scientific observations software were achieved inMarch 2002andthefirst usingthenewcontrol interferometric observations hardware.outfitted withthenew first The programming. During2002allantennaswere software rewrittenusingobject-oriented andthecontrolcomputers arebeingreplaced, systems.millimetre Asaconsequencethese requirementsneededforthenew more stringent the insupporting reliability andtheirinflexibility of machines) interms showing theirage are (PDP11/73 antennacontrolcomputers The existing Antenna controlcomputers Antenna controlcomputers Antenna controlcomputers Photo: DavidSmyth

Observatory reports ray data archive ray data archive ray data archive ray data archive ray data archive y improvements y improvements y improvements y improvements y improvements vator vator vator vator vator Obser Obser Compact Ar Compact Ar project project broadband analogue system was signal transmission broadband Thisof is capable developed. transferring the 4 to intermediate-frequency12 GHz first signals from central to the The site. the millimetre receivers correlator analogue the 4 GHz bandwidth used was as part ofcorrelator ATNF by developed the it is planned Eventually prototype project. AMiBA to replace this unit with a new analogue correlator the full 4 to 12 GHz band. capable of processing The on the Compact Array installed system was in 2002 as a survey instrument.July It used a 30-m baseline in the 12-mm band and east-west operated as a transit instrument. the This avoided The and phase tracking. requirement for delay in September employed 2002 in a system was successful point source survey observation. Since the start of operation of the Compact Array, been routinely almost all observations have Although there are frequent requests for archived. is a valuable the archive from this archive, data index of During 2002, an asset that is under-used. the list ofmade was in the archive files available with the online “projects” Together online. available archive this has allowed and “positions” database, In collaboration with requests to be more specific. Mathematical and InformationCSIRO Sciences, data online with began to place the archive work a web-based interface. via access to be provided the end of by advanced well This was process 2002. facilities will be further In 2003 the archive adding a data reduction front-end to by improved integration some and by ofthe online archive, the “virtual Australian with the developing archives observatory” projects. Obser amount ofA significant took place building work The the site amenities. to improve during the year laboratory extended so that all receiver was members of and their the Electronics Group, The equipment, can be located in a single building. Compact Ar project Obser Obser Compact Ar Compact Ar project project page 42 relator relator relator relator relator ray wideband ray wideband ray wideband ray wideband ray wideband analogue cor analogue cor Compact Ar Compact Ar Millimetre operations Millimetre operations Millimetre analogue cor With the advent of the advent With and the the millimetre receivers it became feasible single-mode optical fibres, new a very wideband interferometer at the to develop The challenges major technical were Compact Array. the transfer of broadband (up to 8 GHz) signals from the antennas to the central site and the ofdevelopment a correlator to process these Both ofsignals. met by these challenges were resorting A to purely analogue techniques. Compact Ar During the winter observingDuring the winter to May period from interim 12- and 3-mm systems October 2002, the to observers. offered were on three antennas 17% ofApproximately the observations use made of optimise the antenna To the 3-mm systems. the three antennas were spacings and sky coverage “shuffled” with the array in some configurations, north as a shunting yard. spur used The initial millimetre observations testing essential provided of the arrayperformance and system capabilities whilst also enabling observers at mm-wavelengths to gain millimetre-observing experience. against robustness some poor weather provide To during millimetre a flexible observations, a tried. In this scheme, was scheme scheduling millimetre observing with a program swapped was program for observations centimetre at wavelengths too poor to obtain good was when the weather millimetre data. The program millimetre then was later. a few days rescheduled 1996 to An analysis of meteorological data from that during the winter months the 2002 showed the was expected to improve scheme swap probability of observing in good from weather 65% to 85%. In practice the swap approximately with only successful, reasonably proved scheme three hours of millimetre observing lost due to poor A total ofweather. six out of 27 swaps a possible than expected from lower initiated. This was were analysis and reflected the extremethe weather in the Narrabridrought conditions experienced region in 2002. Millimetre operations Millimetre analogue cor analogue cor Compact Ar Compact Ar Millimetre operations Millimetre operations Millimetre

Observatory reports Mopra Mopra Operations Operations Staff Staff VSOP project. The millimetre single-dish millimetre The VSOP project. aswell asinconjunctionwiththe Baseline Array theLong of were takenobservations aspart VLBI to VLBIandmillimetreobservations. Mopra thisyearcontinued toberestricted Use of Mopra CSIRO.new postdoctoralpositionfromCorporate have increasedby oneperson,withfundingfora numbers Narrabri at Overall, staff during 2002. were appointed members intheelectronicsgroup A newsystemsscientistandthreestaff area. asastorage and rebuilding agarage thesitehouses inmany of insectscreens replacing safety standards, work drainage aroundtheLodge, building Centreuptocurrent building andVisitors thecontrol in theLodge, bringingsomeaspectsof on siteincludedrefurbishing themen’s bathroom more welcoming entrance. Othersignificantjobs available space, andto give a to make betteruseof was inthecontrolbuilding renovated area reception Operations Staff Operations Operations Staff Staff Mopra Mopra The smallerantennaisusedfor 12GHzholographicmeasurement ofthemaindishsurface. ofMopraRockinthe background.The Mopraantenna,withSiding SpringMountainandpart page 43 Staff Staff upgrades. focus onassistingwithMopraoperationsand witha but position willbestationedinNarrabri, Mopra operationsscientistwas appointed.This 2002,a assistants. Attheendof casual observing theTelescope” andtwo ATNF-funded “Friend of by aUNSW-funded supported astronomers were season, visiting During the3-mmobserving functions. housekeeping perform andto VSOPobservations basis tosupport were employed area people intheMopra onacasual problems attheobservatory. three Additionally allowed for amoretimelyresponsetominor notice.This atshort limited engineeringsupport toprovide with theAnglo-Australian Observatory and Sydney. was established In2002anarrangement isprovidedthe engineeringsupport fromNarrabri atMopra.Mostof staff arenopermanent There Staff Facility andUNSWobservations. was theyear National usedfor total, 39%of SouthWales New (71days). In to theUniversity of (41days)Facility andtimeallocated observations 2002, was splitbetweentimeallocatedforNational time, scheduled inJune –Novemberobserving 3-mm SISreceiver millimetre system.The were takenusingthe for allprograms observations Staff Staff

Photo: University of New South Wales

Observatory reports © CSIRO © User feedback User feedback Elevation drive Elevation drive refurbishment refurbishment Theof period telescope had a shutdown six weeks in September – October 2002 to allow time for major refurbishment of system. drive the elevation gearboxes, parts elevation All moving two in the ofmany replaced and the two were them original, large sector gears reground were hand into the by correct This only the second occasion figure. was in the 40 year life of the telescope that the had been removed. gearboxes The web-based user feedback and fault reportingThe user feedback web-based tool for the successful systems is an essential In total,26 user operations at the observatory. in 2002, slightly were received feedback responses the previous than for in part (34), year due to lower The shutdown. maintenance responses the lengthy generally were with radio veryreceived positive, frequency interference again emerging as the single most important issue flagged observers. by committed each areConsiderable resources now eliminating, year to identifying, and where possible sources of interference. User feedback Elevation drive refurbishment User feedback User feedback Elevation drive Elevation drive refurbishment refurbishment page 44 Dr John Reynolds, Officer-in-Charge at the Parkes Observatory Dr John Reynolds, Officer-in-Charge mance and time use mance and time use mance and mance and time use mance and mance and time use mance and time use mance and for for for for for arkes arkes arkes arkes arkes er er er er er P P P P P The fraction of for all observations time scheduled 82.0%, unchangedin 2002 was from the two better than expected,Thiswas years. previous during maintenance shutdown a lengthy given September and October for telescope time for refurbishment. Some additional observations scheduling made possible by was night-time observingfor a during the shutdown specialised zenith-strip HI survey (HIPARK). The fraction of time lost to equipment faults in 1.4%, a slight increase on the previous 2002 was extraordinary an period of However, year. bad the end of towards weather resulted in a the year of 3.8%, total time lost due to high winds recent year. significantly higher than in any with problems There technical no outstanding were Minor problems importantany telescope systems. receiver with the heavily-used multibeam of culminating in a failure continued, one of the of A refurbishment 26 channels. is this receiver planned for 2003. P P P P P

Observatory reports The Parkesradiotelescope page 45 page 45 © CSIRO

Observatory reports Photo: John Sarkissian John Photo: A new-generation recording baseband was system as CPSR2 Known late in the year. commissioned Swinburne 2), the new Recorder Parkes (Caltech ofsystem is an order in magnitude leap forward capable of baseband recording technology, recording rate of a data one Gigabit second for per The new system extends the very sustained periods. measurements currentlyprecise pulsar timing larger of number being made to a much fainter leading international and maintains Parkes’ pulsars, position in this area. The wide-bandwidth, high time-resolution in 2002, April correlator, initially installed at Parkes its firstproduced spectrum pulsar 2002. in October This instrumentband- provide will eventually frequency widths up to 2 GHz with up to 1,024 By the end capability. and full polarisation channels of 2002 the correlator was operating somewhat but upgrades to be its ultimate capability, below this situation. installed in early 2003 should redress This instrument will become the main observatoryfor timing, pulsar “workhorse” where polarisation are more critical than and sensitivity high time resolution. project with the UrumqiA collaborative Astronomical Observatory a very in China reached with the in successful conclusion August commissioning of a cryogenically-cooled 18-cm staff on the Urumqi ATNF telescope. receiver to China to assist in the installation. travelled

One of the new zenith axis gears, manufactured by Crown One of the new zenith axis gears, manufactured Engineering of Brisbane. Photo: John Sarkissian John Photo: page 46 Major activities Major activities One of the cleaned Parkes radio telescope zenith cleaned prior to a dye axis racks. The racks were being applied that highlighted the elevated regions on the rack teeth for later grinding. The Parkes multibeam pulsar survey, a major pulsar survey, multibeam The Parkes survey of the Galactic plane using the 20-cm and dedicated pulsar filter banks, receiver multibeam 2002. nominally completed on 14 March was Bank, Jodrell a collaboration between This survey, of and the University ATNF Bologna, commenced in 1997 and has been one of the observatory’s in the intervening activities five principal research years. The success of the survey all has exceeded of with the discovery expectations, more than 600 to be new pulsars and another 100 or so expected when the data are reprocessed.revealed The the number roughly doubled survey will then have of thirds of with around two known, pulsars all telescope. with the Parkes pulsars discovered known observations ofFollow-up the newly-discovered into 2003. well pulsars will continue Major activities This work went extremely smoothly and the new extremely smoothly went This work many more years of give systems should useful life the period, During the shutdown to the telescope. put to goodnights were observing use by a narrow strip of with the telescope parked the sky repeatedly, The zenith. and pointed at the aim of this project image of sensitive is to create an extemely neutral emission. hydrogen Major activities Major activities

Observatory reports NA NA Steve Broadhurst (right)andJonCrocker (left) replacing oneofthebearingszenith axisgears. Robert Semlitzky(centre), SeniorProject EngineerwithSvenskaKullagerFöreningen (SKF) Australia, • • • • are: thisagreement of was signedin August majorcomponents 2002.The NASAspacecrafttrackingin2003/4 of support Parkes for anduseof theupgrade NASA, for of withCTIP,An agreement actingonbehalf with two visitingChineseengineers. working Parkes at was constructed by localstaff telecope, and be installedonthe25-metreUrumqi newreceiver receiverThe isthefirstcryogenic to NA NA NA September 2003toMarchSeptember 2004. Up toninehoursperday tracking intheperiod Antenna acceptancetesting. anew8.4GHzreceiver. Provision of 54 mdiameterrange. antenna providing newpanelsinthe44to theParkes of thesurface of An upgrade S S S S S A Marstrackingsupport A Marstrackingsupport A Marstrackingsupport A Marstrackingsupport A Marstrackingsupport page 47 Future developments Future developments in otherareas, such astheNASAcontract. more slowly thanexpected,owing tocommitments 2003.Work onthisprojecthasproceeded of half willbecommissionedinthesecond observations receiver designedforpulsartiming specifically In additiontotheNASA-related work, anew Future developments contract isapproximatelyA$3M. the manufacture isproceeding. totalvalueThe of other components, thedesigniscompleteand the and successfullytestedinOctober. Of is proceeding. feedwasmanufactured The thereceiver designandmanufacture of The panelsisscheduled thenew inMarch 2003. of in August withSydney Engineeringandinstallation thepanelswas signed of A contract forthesupply Future developments Future developments

Photo: John Sarkissian

Observatory reports roposals and scheduling roposals and scheduling roposals and scheduling roposals and scheduling roposals and scheduling VSOP VSOP P P Operations Operations observations. This providedobservations. Host under a time, Country agreement in a will be used NASA, with service observing mode for spectroscopic This to advertised observations. new facility was and internationalthe Australian with community service observations expected to start in the first observing term of 2003. P strong continued There demand for proposal was over- in 2002, with an effective the LBA ofsubscription rate similar to previous about two, A significant amount ofyears. scheduled time was astrometric program. for the ATNF-USNO access to the Tidbinbilla facilities remains However, difficult, especially for the 70-m antenna. Operations observingThere werethree major LBA sessions in as usual of2002, with an allocation per one week an 89% success achieved term. the LBA Overall years. on the previous two a 5% improvement rate, Most of with success rates the telescopes continued a single system failure of 97%. However, over a at Ceduna led to significant time losses motor drive array the overall in one session and affected performance. VSOP The to operate VSOP satellite continued its into NASA support was However, sixth year. in Februarydiscontinued 2002 and operation and Mitaka only at the Penticton continued Thecorrelators. main VSOP program has been the mission-led survey of galactic this and nuclei active recording has been done using primarily S2 data been the main Mopra and Hobart have systems. one Operations in 2002 involved ground antennas. short observationsor two (up to six hours) per week The provided Mopra antenna with these antennas. supportreduced for VSOP during the southern to winter months because of commitments millimetre observing. VSOP support Continued is each contingent on the scientific case been approved Time termAssignment Committee. the ATNF by P P Operations Operations VSOP VSOP page 48 ustralian ustralian ustralian ustralian ustralian ray ray ray ray ray Long Baseline Long Baseline Ar Ar The A The A The 22 GHz operations 22 GHz operations LBA report 2002 LBA report 2002 LBA report In 2002 a technical problem with the 22 GHz problem In 2002 a technical system on the 70-m Tidbinbilla antenna receiver and the telescope became available resolved was observations in the 12-mm sensitive for extremely (22 GHz) observing band. The new 22 GHz greatlyfacilities of the operation enhanced the LBA most the in this band. Tidbinbilla is now network radio telescope in the southern hemisphere sensitive for observationsat 22 GHz. A large proportion of observations during LBA at 22 GHz, utilising the 2002 were – August May Hobart Tidbinbilla, Mopra, Parkes, Compact Array, and Ceduna. A new observing tried mode was two successfully for one project. In this mode, and recorded simultaneously, maser lines were water around four pairs ofthe system switched spectral recorded line data were In addition, spectral lines. at the Compact Array and autocorrelations were recorded all telescopes. at the end ofTowards arrangements 2002, put were in place for a fraction of time on the Tidbinbilla 70-m antenna to be allocated for single-dish Long Baseline Ar 22 GHz operations The Australian Long Baseline ArrayThe (LBA) Australian operates as a verylong baseline interferometer (VLBI) array utilising most radio telescopes around antennas (Parkes, It includes all the ATNF Australia. Mopra,Array), Compact the Hobart and Ceduna antennas of of the University and Tasmania, Canberra Deep Space antennas of NASA’s ComplexCommunications at Tidbinbilla. It also with overseas operates in collaboration frequently especially the Hartebeesthoek antenna in antennas, antenna in Park South Africa and the Kokee Hawaii. The A The 2002 LBA report 22 GHz operations 22 GHz operations LBA report 2002 LBA report 2002 LBA report Long Baseline Long Baseline Ar Ar The A The A The

Observatory reports group report group report Astrophysics Astrophysics Staff Staff staff andstudents. staff andRSAA betweencollaborations ATNF staff communities in Australia andtoincrease interactions between theradio andoptical research istostimulate Mount Stromlolocation themove tothe ATNF Oneaimof andtheRSAA. the withjointfundingfrom group Canberra years. alsojoinedthe Frank Professor Briggs astrophysics positionin anumber of permanent positionatCSIRO,new permanent thefirst In October2002JimLovell was toa appointed Astrophysics MountStromloObservatory. (RSAA), Astronomy and at theResearch School of staff COSSA officestolocatedwiththeANU Jauncey and JimLovell moved theirCSIRO from membersDave duringtheyear.reorganised Staff ATNFThe were astrophysics activities inCanberra University. atSwinburne manager left theATNF totake upapositionastheSKA theyear, Steven Tingay Netherlands.At theendof The to postdoctoral positionandreturned jointCSIRO/Indonesiancompleted aone-year Wales, Cardiff.University DiahSetia-Gunawan of took upaPPARC Advanced Fellowship the at ErwindeBlok postdoctoral fellows alsodeparted. VLBIinDwingeloo.Insititute for Several BonnandChrisPhillipsfromtheJoint University of Manchester (Jodrell Bank), Juergen Ottfromthe Hobbsarrived fromtheUniversity of George theirchoice. of outresearch programs to carry BoltonfellowsATNF new joinedthe Three in2002 group report Astrophysics activities Current Staff Staff Staff group report group report Astrophysics Astrophysics page 49 CSIRO awards CSIRO awards A A scholarships in2002.Bothstudentsthenjoinedthe Aidan HotanandHaydon received Knight, University, Swinburne studentsfrom postgraduate top-upscholarship award.a prestigious Two initiative, studentsreceive exceptional postgraduate scholarships was Underthis introducedin 2002. CSIROA new scheme toprovide postgraduate meetings. universities through seminarsandscientific Australian with interactions encouraging stimulating ATNF for staff, areusefulfor but Such notonly Windhorst (ArizonaState). visitsare RussHulst (Kapteyn), Taylor andRogier (Calgary) van der Thijs the ATNF from visitorprogram, astrophysics-related visits, undertheauspicesof ATNFThe tohave was fortunate several extended CSIRO awards A CSIRO awards CSIRO awards A A Head, ATNF AstrophysicsGroup Dr ListerStaveley-Smith TNF visitorprogram TNF visitorprogram TNF visitorprogram TNF visitorprogram TNF visitorprogram

Photo: Kristen Clarke

Current activities orld coordinate systems orld coordinate systems orld coordinate systems orld coordinate systems orld coordinate systems Linux operating system Linux operating system Linux operating W W During 2002 an Australian AIPS++ Users Group AIPS++ Users an Australian During 2002 formedwas with group members drawn from a ofnumber radio astronomy groups. The Australian group discusses AIPS++ usage and advises the team on priorities for AIPS++ development and implementation. further software development A highlight of the publication of the year was a systems for coordinate describing the world paper representing celestial coordinates in the commonly- used astronomical data format as FITS known aspect System). A key Image(Flexible Transport of FITS-formatfiles is the use of “header” information that describes the kind of data that software should files in the and how exists interpret It is of the data. great importance to have a standard format representing for celestial This publication, the result ofcoordinates. years of staff by ATNF work member Mark Calabretta, is the result of international collaboration, much mathematical and software development, excellent internationaland extensive negotiations to get a general acceptance of standard. the new Linux operating system Linux operating The is system Linux open-source operating becoming increasingly important in ATNF of for a wide variety is available Linux computing. laptop machines to personal computers from In 2002 ATNF cluster systems. multiprocessor efforts a uniform concentrated on providing set Linux users and dealing with the conflictingup for requirements of rapid support for new hardware and stable operation. W Linux operating system Linux operating system Linux operating W W page 50 . This vices vices vices vices vices Detecting the Epoch of Reionisation Computing Computing AIPS++ AIPS++ Marsfield computer ser Marsfield computer ser Astrophysics events Astrophysics events Astrophysics AIPS++ is an astronomical data processing an international by being developed environment consortium of radio observatories. The package has using “object-oriented” software been developed and presents users and applicationstechniques with a toolkit ofdevelopers astronomy-oriented has four staff The ATNF functions. members of contributing part-time to the development AIPS++. The ATNF provides information provides technologyThe ATNF (IT) and manages support users, for National Facility computing at the Marsfield The site. ATNF-specific IT infrastructure the CTIP is managed by computer services group (CSG). AIPS++ Computing Marsfield computer ser There were several astrophysics events in 2002. A events astrophysics several There were series of held during an talks was research Dick 2002 to celebrate June “astrofest” on 5 60th birthday his outstanding and Manchester’s An inaugural Bolton career in pulsar astronomy. of activities the research Symposium, showcasing postdoctoral (and some other staff fellows ATNF On held on 11 December 2002. and students) was 18 December 2002, as part of the growing interest was project (page 64), a workshop in the LOFAR held on Astrophysics events Astrophysics ATNF studentship scheme with joint supervision with scheme studentship ATNF Significant Swinburnebetween and the ATNF. for in other new initiatives also shown interest was postdoctoralfellowships, and ARC-CSIRO CSIRO appointments are expected in 2003. and several provided an opportunityprovided for interested astronomers to start engaging in the promising, but challenging, field of research. radio astronomy low-frequency a joint Other meetings held during the year included symposium. symposium and a student ATNF-AAO AIPS++ AIPS++ Marsfield computer ser Marsfield computer ser Astrophysics events Astrophysics events Astrophysics Computing Computing

Current Activities 2002/2003 ATNF summervacationstudents program program Summer vacation Summer vacation em aho thestudentsworked forabout12 team. Each of toexperienceworkingan opportunity inaresearch provides thestudentswith vacation program The Observatory. Narrabri withtheothertwo headquarters atthe Marsfield ATNF the the studentswere locatedat Six of positions, eightwiththe ATNF and11withCTIP. Over received were for19 300 applications was heldjointly withCTIP. 2002/2003program The theirdegrees. have of completedatleastthreeyears studentswho forundergraduate vacation program EachATNF summerthe asummer coordinates program Summer vacation program program Summer vacation Summer vacation page 51 them to consider further studyorresearch careers.them toconsiderfurther hadattracted environment theprogram andthat enjoyed theCSIRO hadgreatly they work thestudentscommentedthat experience, manyof theirwork diverse research topics.At theendof the givenwith apresentation oneachof withastudentsymposium, concluded The program at theobservatories. provided by staff students alsoreceived safetyandtelescopetraining provided byATNF postdoctoralfellows. The support with thetelescopes, withobserving allocated approximately 10hoursforobservations projects. was Each group teams onobserving andworked insmall Parkes Observatory orNarrabri eitherthe where thestudentsspentfour daysat trip was anobservatory theprogram a highlightof a research scientistorengineer. years, As inprevious weeks from onaresearch projectwithsupervision

Photo: Barnaby Norris

Current activities used by the Division ofthe Division used by and the Radiophysics ATNF. made thorough assessment was In 2001 – 2002, a of the entire collection to of the contents determineparts and the retaining, which are worth relocated to a purpose-builtcollection was room humidity are the temperature where and relative maintained at accepted for long-term levels conservation of photographic material. Following the assessment, in 2002 approximately 2,500 the years 1939 to 1964, were covering images, using a high-quality digital files, scanned to create for the project. film scanner purchased page 52 This photograph, taken in 1964, is one of thousands available in the ATNF photoarchive. The photoarchive. ATNF This photograph, taken in 1964, is one of thousands available in the TNF TNF TNF TNF TNF photoarchive photoarchive A A Sheep in the paddock Parkes 64-m and Kennedy 18-m radio telescopes can be seen. The Kennedy antenna was transferred from Fleurs to the from was transferred Parkes 64-m and Kennedy 18-m radio telescopes can be seen. The Kennedy antenna Parkes site in 1963. photoarchive A dates photographic historic The archive ATNF to the mid-1990s and comprises over 1939 from and negatives or slides, 100,000 individual The imagesincludes collection associated prints. of ofmany radio in Australian figures the key photographic records ofastronomy, in events key the history of radio and astronomy Australian images of stations the radio telescopes and field photoarchive photoarchive A A

Current Activities A A observers at the Narrabri Observatory. attheNarrabri observers tocollectfeedback from forms online survey overseas, going and forstaff facilitate arrangements their owncreate web pages, to atravel form New onlinetoolsincludefacilitiesforstaffto metadata“tags”inweb files. example intheuseof web standards, compliance tocurrent for as greater newsandevents aswell current dynamic listingof and technological the changes. include These significantstructural newdesignincorporates The central siteinMarch 2002. the ATNF of withthereplacement website, the anddesignof put intoimproving thestructure After consultation withusers, was amajoreffort observatories. the of which criticaltotheoperations are of technical documentsandonlineapplications, some website andcomplex,withmany isextremely large research andfuturedevelopment work.ATNF The activities publicoutreach promote andtodocument the ATNF’s facilities. web The isalso usedto astronomerswho use community of international thenationaland for andresources information to provide communications tool,inparticular ATNFThe isusedasaprimary website A databaseprogram, management usinganasset- andorganised are catalogued highresolutiondigitalfiles The per image. 10millionpixels approximately resolution of negatives arescannedata photographic The mg rhv fmorerecentimages. archiveimage of Australia. In2002, work onaseparate alsobegan radioastronomy in sixdecadesof representing and willprovide atleast6,000digitalimages archiveThe isbeingsystematicallyextended and forexhibitions, andpublic relations. education Australian astronomy of for research onthehistory digitalarchiveThe isbeingdeveloped asaresource database. enteredintothe ontheimages detailed information A A TNF website TNF website TNF website TNF website TNF website Cumulus , page 53 with Abbotsleigh SchoolusingtheSEARFE equipment Catriona Rafael(left)andEileenLee(right)from Public outreach Public outreach SEARFE andtheSK SEARFE andtheSK public relationsactivities heldduringtheyear. the followingThe sectionsdescribesomeof andspecialeventsinterviews, such asOpenDays. promotional materials, publictalksandmedia and publications educational programs, located attheParkes Observatories, andNarrabri Centres Visitors which of includetheoperation activities of outreach through arange ispromoted relations withourlocalcommunities. Public andtomaintainfostergood in Australia, science people intoscience, theprofile of toraise for theATNFoutreach goals aretoattractyoung public primary profile.The maintain, astrong public career. ATNF The has, andwillcontinue to studentstowards ascience-based of generation promoting scienceandtoencouragingthenext interest.Assuch public itisideallysuitedto of ahighlevel Astronomy isasubjectthatgenerates and theirstudents. Thestudentsmonitorand equipment tohighschools monitoring andlogging providesEnvironment. project spectrum This Exploring Australia’s Frequency Radio SEARFE—Students launch inJune 2002of A signficanteducational initiative in2002was the Public outreach SEARFE andtheSK SEARFE andtheSK SEARFE andtheSK Public outreach Public outreach A A A A A

Current activities The Festival of (detailing a and the Nine Elyseum 7 Catalyst Getaway!

, have proved popular with proved , have weekend, the Mopra radio weekend, telescope rabri and Mopra rabri and Mopra rabri and Mopra rabri and Mopra rabri and Mopra Nar Nar outreach outreach was open to the public on 27 October 2002. open to the public was 110 visitors touredApproximately the telescope vertex room and control room. During the year a ofnumber tours of the Mopra telescope were student groups. conducted for As part of Coonabarabran the annual the Stars Invisible Universe Nar outreach The Narrabri Centre hosted approximately Visitors more than in 10,300 visitors in 2002, somewhat The Centre also ran Visitors years. previous groups for community star-gazing evenings several Theand official delegations. observatory featured television programs during the year—thein two science program ABC’s Revenue taken through the through the Visitors Centre has taken Revenue of in line with the number increased A new visitors. show, three-dimensional spaceflight to Mars), and another audiovisual visitors. A dramatic new cafe and associated visitors. graces now barbecue area the site of the old hexagonal adjacent to the barbecue shelter ConstructionVisitors Centre. started in work earnest The to Christmas 2002. just prior building of for the motivation the cafe is to broaden the range of bring visitors to the attractions that for them when more activities provide observatory, length of are and to extend the average they there, their stay. Network’s travel programtravel Network’s Nar Nar outreach outreach page 54 This site

. www.atnf.searfe.au arkes outreach arkes outreach arkes outreach arkes outreach arkes outreach P P P In 2002, the number of visitors public to the The centre to rise. hosted Visitors Centre continued up the 2002 calendar year, 135,000 visitors over a long-termfrom of average around 55,000 prior 2000 (pageto the year The rate of 13). increase the very dry over Christmas 2002 period slowed its momentum. With has since recovered but ofthe increasing public profile the observatory comes a steady flow of requests to host special Highlights in 2002 included a concert for events. around 500 attendees at a national meeting of car a Easter 2002 and over enthusiasts held in Parkes in Local dinner for more than a hundred Women in May. representatives Government provides informationprovides also hosts and to the schools discussion forum teachers for students, an active Theand project organisers. project is ofgrowing with a number to join schools expected in 2003. supportThe project SEARFE and receives ofsponorship from the University Sydney, of of University University Sydney, Technology Perth Systems Australia, BAE IBM Australia, NSW, Observatory Geographic. In 2002 and Australian project including joined the schools several College (NSW), Dickson Abbotsleigh (ACT), Narrabri (NSW) and Kimba Area High High School (SA). School analyse the radio spectrumanalyse the areas and in their local their results other groups with compare of students the SEARFE time, Over in the country. elsewhere a database of radio frequency project will build up and around Australia, usage levels and interference contribution this information a valuable will make (pageto the SKA project 60). are The the schools acquired SEARFE results by posted on the website, P P

Current Activities management management Spectr Spectr ♦ ♦ ♦ ♦ ♦ ATNF involved arecurrently include: for more than30years. areas inwhichThe the astronomy radio andtheprotectionof management involved inactivities tospectrum related Radiophysics ATNF, andlaterthrough hasbeen CSIRO, theDivisionof through initially management Spectr management management Spectr Spectr awareness inthisregion. significantly theradioastronomy and profile Telescope (APT)meetingsin2002andhasraised activelyAsia-Pacific in RAFCAP participated astronomy. radio committeefor management regional spectrum anew (RAFCAP), Frequency CommitteeintheAsiaPacific region AstronomyParticipation intheRadio and WRC deliberations. and hashadasignificantimpactonStudyGroup activeIUCAF hasbeenvery inITUmeetings theIAU,a committeeof URSIandCOSPAR. Frequencies) Commission for theAllocationof Participation inIUCAF(Inter-Union theOECDscienceministers. meeting of toafuture was producedin2002andwillgo interference andprotectionmeasures.A report force was setuptoinvestigate radiofrequency task where aninternational forum megascience theOECD Working meetingsof Party ATNFParticipation bythe Directorinthe Meeting,withfocusonWRC 2003. Preparatory andin2002theConference (Science Services) include regularmeetingsofITUStudyGroup7 TelecommunicationsThese Union(ITU). theInternational meetings undertheauspicesof Participation inregional andinternational (WRC) in2003. the World Radiocommunication Conference theactivities for was thepreparations focus of Communications Authority (ACA). In2002the protectionAustralian activitiesthroughthe planningand Participation in nationalspectrum um um um um um page 55 future. frequency signalscouldbecontrolledintothe low,signals are increaseinradio any andwhere radiofrequency levels existing of an area where aradio-quietreserve, establishment inAustralia of the ACA andATNF thepossible regarding discussionshaveIn addition, beenheldbetween between theACA andtheATNF onthisissue. toallparties.acceptable Meetingsarecontinuing committed toachieving anoutcomein2003thatis ACA, withkey inconsultation stakeholders, is radioastronomyinterference riskat facilities. The appropriate guidelinestoassistwithmanaging toconsult withthe undertaken ATNF todevelop forward by theProductivity Commissionandhas put thesuggestion manner from in adifferent the recommendationwillneedtobeimplemented Australian Parliament. ACAThe hasadvisedthat Government’s responseweresubmittedtothe The Productivity Commission’s andthe report report: (Recrecommendation 10.4)intheCommission’s resultedinthefollowing This the Commission. produced asubmissionandappearedbefore into theRadioCommunications Acts. ATNF the Australian Commissioninquiry Productivity event in2002was management A majorspectrum footnote AUS87. or partiallywithinthebandsspecifiedin user hasappliedforatransmitterlicencewholly These facilitiesmustbenotifiedthatanother Australian Radio-frequencySpectrumPlan. designated as“radiosensitivesites”underthe Radio astronomyfacilitiesshouldbe

Current activities Occupational Occupational and safety health and safety health Occupational and safety health occupational health site has its own ATNF Each meets at least four which and safety committee, issues and identify any new times a year to review a by is assessed annually workplace Each hazards. member of and a formal the local committee, programs of report a number in Training made. areas correct as ergonomics, such lifting techniques, are offered driving and defensive electrical safety throughout the year. of a number Over rate of years the ATNF’s has been occupational health and safety incidents ofin line with that as the such similar institutions, ObservatoryAnglo-Australian Large Very and the staff In 2002, ATNF Array. and visitors recorded a lost of 2.1 total of 22 incidents with a total time and six compensation claims acceptedweeks by Comcare. Occupational Occupational and safety health and safety health page 56 Insight Staff Satisfaction Insight Staff www.atnf.csiro.au/overview/ . vey vey vey vey vey placed the ATNF as the top Division of as the top Division placed the ATNF Equal Equal Employment Employment Opportunity Opportunity Staff satisfaction Staff satisfaction Staff sur sur The ATNF has an active EEO group EEO has an active five with The ATNF are two are based in Sydney, Two contact officers. Staffat Narrabri and one is at Parkes. of any at the sites can contact any of the EEO officers and are assured that all discussions will be held in The to promote confidence. EEO officers work information to provide good relations, workplace and advice to staff and management on EEO and to support staffpolicies, in complaints involved ofat each EEO talks are given procedures. the to summer vacation also given sites and are ATNF The group staff. students and to new maintains pages web at extensive Equal Employment Opportunity management/eeo/ Staff satisfaction Staff sur of is an employer The ATNF In 2002, choice. responses to a CSIRO Survey CSIRO while staff CSIRO is satisfaction within the ATNF the comparative higher than across considerably Global R&D Norm surveyed consultants the by International The staff Survey Research. responses to the survey especially favourable were questions and for questions associated with “leadership management” and “job security and organisational stability”. High staff morale is one of the ATNF’s greatest strengths. Equal Equal Employment Employment Opportunity Opportunity Staff satisfaction Staff satisfaction Staff sur sur

Current Activities Marsfield engineering Marsfield engineering developments developments P P Executive Special Executive Special components for a number of ATNF projects, but components foranumber of inproviding notonly successful, state-of-the-art ExecutiveThe SpecialProjecthasproved highly 3-mmreceiversCompact Array toabove 112GHz. the coveragepotential toextend thefrequency of Initial testsindicatethatthisamplifierhasthe indium phosphideHEMTlow noiseamplifier. new designfora3-mmbandcoplanarwaveguide CSR15alsoincluded a from 2000, initial CSR8run proven the MMICdesignsfrom quantities of AswellCSR15. ascontainingproduction third andfinal TRW labelled run, wafer fabrication thedicedchips fromthe delivery inApril2002of project wasThis effectively completedwiththe high-speed digitisercircuits. microwave circuits (MMICs)and integrated monolithic include produced undertheprogram process. Devices indium phosphidefoundry TRWUSA by thefoundry usingtheirleadingedge within ATNF andCTIParefabricatedinthe communications. developed designsare circuit The astronomy radio circuits for and tele- CTIP todevelop highfrequency integrated ATNF the and projects was ajointproposal of these research teamswithinCSIRO. Oneof by large projectstobeundertaken number of Officer, announceda DrMalcolmMcIntosh, ExecutiveIn December1997CSIRO’s Chief P Executive Special developments Technology Marsfield engineering developments P P Executive Special Executive Special Marsfield engineering Marsfield engineering developments developments roject roject roject roject roject page 57 developments developments 12- and3-mmreceiver 12- and3-mmreceiver manufacturing the3-mmfeedhorns, using Array,the Compact methodof anew tothe3-mmsystemsat theupgrades of As part thisandfuture projects.reliability offered for and potential enhancementsinperformance worthwhile given the savings involved andthe techniques, was tobe considered theeffort indeveloping curve thebasic significant learning cabling costs.Although thisapproach involved a reducingpackaging and functions, withtheaimof intomodulescombininganumber of integrated thesystemwere significantsectionsof in which 12-mmreceivers.Array A new was approach taken the final conversion systems for thenewCompact was put intothedetaileddesignof A majoreffort developments 12- and3-mmreceiver high frequencyMMICs. of awiderange inthedesignof develop expertise also ingiving ATNF to engineerstheopportunity developments developments 12- and3-mmreceiver 12- and3-mmreceiver Head, ATNF EngineeringDevelopmentGroup Dr Warwick Wilson

Photo: Kristen Clarke

Technology developments Photo: David Smyth David Photo: Y Y Y Y Y ARADA ARADA ARADA ARADA ARADA F F ATNF engineer Russell Bolton with the wideband-prototype 3-mm, the wideband-prototype engineer Russell Bolton with ATNF systems 12-mm receiver and production-phase F project, the European funded by The FARADAY program is a co-operative Union, the UK, between that Australia Italy and Poland, The Netherlands, aims to produce prototypes of integrated focal plane arrays large and to study arrays for future implementation. collaboration,As part the ATNF of the FARADAY 40% ofacquired access to approximately an indium phosphide HEMT fabrication run to be undertaken of Part in early 2003. TRW at this allocation will be production quantities ofused to provide previous Special under the Executive designs developed (pageProject 57). of In addition, a number new undertaken,designs were in response both to as a 50 GHz such immediate requirements, frequency doubler for the 3-mm LO system, but also aimed at possible future requirements of a The latter included a 60 – nature. speculative more noise amplifier90 GHz low and broadband low F F page 58 arkes 10/50 cm arkes 10/50 cm arkes 10/50 cm arkes 10/50 cm arkes 10/50 cm P P receiver receiver Local oscillator upgrade Local oscillator upgrade Local oscillator Most of design and manufacture the mechanical of completed by was the 10/50 cm pulsar receiver the end of This 2002. included a dual frequency which was coaxial feed, designed by CTIP, successfully tested after integration with other to installation A test designed components. ATNF interface to the telescope will the mechanical check place in early 2003. take P receiver As part of the Compact Array upgrade to operate a new local oscillator (LO) at 3-mm wavelength, to produce a reference near is being developed chain the observing frequency from the signal distributed phosphide MMIC indium Two from the central site. for under the this LO chain developed chips packaged and tested. Project were Special Executive These were separating a sideband and a mixer case performance In each was frequency doubler. within specifications. to be well shown Three other components required for the 3-mm a 25 – 50 GHz frequencyLO chain, a doubler, amplifier and a 100 GHz power 50 GHz power to be difficult to source from amplifier proved A gallium arsenidecommercial MMIC suppliers. fabrication run undertaken was in July with TRW 2002 to address this problem. The designs for the the CTIP, by provided amplifiers were power from this run were Wafers doublerATNF. by returned tests Initial on-wafer in October 2002. that the performanceshowed of the MMICs was although final results will not adequate, probably in early until the designs are packaged be available 2003. This has significantly delayed development the installation of is now which the 3-mm systems, mid-2004. place before to take unlikely Local oscillator upgrade Local oscillator precision than electro-forming, rather machining has significantly successful and to be very proved reduced complexity of the cost and manufacture. A new design for a 3-mm OMT (orthomode Thetransducer) polariser was completed. design in performance a significant improvement gives the commercial used in the 3-mm devices over prototype receivers. P P receiver receiver Local oscillator upgrade Local oscillator upgrade Local oscillator

Technology developments Arecibo 21-cmmultibeam Arecibo 21-cmmultibeam AMiBA prototypecor AMiBA prototypecor A new8GHzbandwidth A new8GHzbandwidth receiver receiver spectrometer forMopra spectrometer forMopra meeting at Arecibo in September 2002. meeting at Arecibo inSeptember CTIP. ATNF personnelattended adesignreview hasbeensubcontracted to thefeed array design of andthereceiveramplifiers mechanism.The rotation feed array, thelow system, noise thecryogenic supply thefront-endreceiver package, includingthe successful Parkes multibeam receiver. ATNF will the receiverThe of design willbeanadaptation multibeam receiver forthe Arecibo radiotelescope. aseven-beam 21-cm 2002 forthesupplyof Center,Ionisphere April USA(NAIC)wassignedin AstronomyA contract and withtheNational October 2002. were obtainedin andfirstfringes September telescope was installedonMaunaLoain was delivered toTaiwan prototype April. The in system CMB Prototype correlator telescope. The system toASIAAfor thetwo-element AMiBA acquisition anddata prototype analoguecorrelator ATNFASIAA Taiwan, and ATNF provided a between acollaborative agreement of As part mid-2004. system isplannedtobeinstalledandoperatingin The project. upgrade broadband Compact Array designs beingdeveloped fortheMNRF-2001 ATNF usingthepolyphasedigitalfilterbank willbebuiltbyadditional funding. instrument The and Sydney and MonashUniversities providing a collaborative withUNSW, project, ATNF willbe spectrometer fortheMopratelescope.This an8GHz enable thedevelopment of successful inobtainingfundingfromtheARC to NSWwas In October2002,theUniversity of cm-wave systems. the ATCA for future upgrade apossible context of broadband inthe were low noiseamplifiers devised The inthe1to12GHz range. noise amplifiers Arecibo 21-cmmultibeam AMiBA prototypecor A new8GHzbandwidth receiver spectrometer forMopra Arecibo 21-cmmultibeam Arecibo 21-cmmultibeam AMiBA prototypecor AMiBA prototypecor A new8GHzbandwidth A new8GHzbandwidth receiver receiver spectrometer forMopra spectrometer forMopra relator relator relator relator relator page 59 receiver phaseinMarsfield duringitsconstruction ATNF technicalofficerPatSykeswiththeParkes10/50cm MNRF MNRF of a new innovation anew statement,anew of In early2001theGovernment announced,aspart The Way Ahead National Research Facilities MNRF astronomical community in the report astronomical communityinthereport priorities,These asidentifiedbyAustralian the intooneproposalforMNRFfunding.growth combine theirtwo future highestprioritiesfor Australian communitydecidedto astronomical A$23.5M. singleallocation, thelargest proposal was granted ATNF-led thesethe successful proposals. Of to15 A$155M undertheMNRF-2001program Nick Minchin,announcedtheallocation of Industry, Science,andResources, Senator August On21 2001. theMinisterfor 2001, inMay wasproposal submitted toAusIndustry radiotelescope. MNRF-2001 The generation theSKA—thenext- and development of optical/infrared telescopesoftheGeminiproject MNRF MNRF , are additionalaccesstothe are , -2001 -2001 -2001 -2001 -2001 program. The program. Beyond 2000: Major

Photo: David Smyth Technology developments ray ray ray ray ray A antennas A antennas A antennas A antennas A antennas The Square The Square Kilometre Ar Kilometre Ar SK SK so doing will profitso doing from important extensions to its observational In the short capabilities. to a access term,will have users Facility National enhanced instrument,significantly the longerwhile term goals of addressed. the SKA are The upgrade the bandwidth of will increase the Array a factorCompact of by 16 to a total of 8 digital filter bank GHz. A new polyphase structure frequency increased will provide in a highlyresolution flexible format. This is a replacing the major upgrade Array, to the Compact the samplers, systems, existing frequency conversion system and the correlator. the delay transfer, the data SK in the Antennas are the highest profile components The SKA concept SKA goal designs. is to various widely separated beams many simultaneous, have can be “placed” in different on directions which Three types ofthe sky. antenna design are being Luneburg These involve considered in Australia. cylindrical reflectors, and phased- lens antennas, In 2002, goodarray progress antennas. continued to be made in a joint project between four Molecular Science CTIP, (ATNF, divisions CSIRO to Science & Technology) and Manufacturing low-loss, composite, and develop investigate dielectric material for use in Luneburg lenses and The engineering applications. other electromagnetic within CSIRO primarily is being developed material and InfrastructureManufacturing and Technology mid-2003. Thea patent will be finalised by current design will determine on antenna prototype work ofthe choice technology SKA for Australian will be made demonstratorantennas; this choice mid-2004. by The Square Kilometre Ar in the player a very is active The ATNF SKA consortiumsinternational and, and Australian and universities with Australian in collaboration major is making across CSIRO, other Divisions to the design ofcontributions the array in several the the antenna elements, areas including key site investigations, signal processing, receivers, array configurations and interference mitigation. SK SK The Square The Square Kilometre Ar Kilometre Ar page 60 ray broadband ray broadband ray broadband ray broadband ray broadband The MNRF funds will be used Increase share Australia’s in the International Telescopes Gemini (currently 5%). initially to purchase an additional share of share additional an to purchase initially ThisGemini. programprovide will not only astronomers with a biggerAustralian share of Gemini observing but will also improve time, ofthe capabilities and Gemini telescopes, the expertise in instrument Australia’s advertise building. for the SKA. technologies enabling Develop is one ofThe ATNF a consortium of major countries institutions in eleven radio astronomy next-generation large the world’s planning now the SKA. This instrument’s radio telescope, area one million square metres of collecting as the best as sensitive it 100 times will make instruments:present-day be will area this perhapsdistributed across many hundreds, of thousands, kilometres in a location yet to be Using a combination ofdecided. technologies, frequency ranges from 100 the SKA will cover 10 GHz. The SKA project is MHz to above largest radio astronomy currently the world’s and will cost around A$2B. initiative Construction of the instrument is expected to start 2012. by are coordinated SKA activities Australian SKA Consortium the through Australian This committee aims Committee (ASKACC). Australia a single interface between to provide achieve and the international SKA project. To coordinates SKA research and this ASKACC with the within Australia, development ofestablishment groups working for national also consults ASKACC different SKA activities. astronomical with the wider Australian promotes the SKA to the public community, and appoints and industry, and to Government members to the International SKA Australia’s Steering Committee. upgrade project upgrade project Compact Ar Compact Ar ♦ ♦ This has the aim of project new signal developing for the SKA and technologies processsing applying in a significant upgrade them of the The Compact Array will become, Compact Array. but in in effect, a test bed for SKA developments, upgrade project Compact Ar ♦ The of specific aims program the MNRF-2001 to: are ♦ ♦ ♦ upgrade project upgrade project Compact Ar Compact Ar

Technology developments SK SK proposal during2003. aninitialAustralian SKAsiting submission of the site inWestern of part Australia willform these two sitesandthewell-characterised Mileura South Wales.The combinedsiteinvestigations from New site testingisalsoplannedforainwestern Further analysis toolswillneedtobeundertaken. usingmoresensitivesurvey equipmentand although adetailedradiofrequencyinterference tobeanexcellentMurnepowie site radio-quiet have measurements interference shown Australia.outback Radiofrequency South in at apotentialSKAsitenearMurnpeowie, made interference measurementswere preliminary December 2002,afirst-roundinspectionand Australia (ATNF Annual 2001).In Report inWestern outattheMileuraStation carried Extensiveon theAustralian testshave agenda. been investigations atpossible SKAsitesremainshigh Radio frequencyinterferencetestingandsite SK prototypes.laboratory collaborators andwillbeusedwithSKA amplifier. hasbeendelivered This tointernational uncooled widebandGaAsMMIClow-noise ATNFin 2002the completedadesignforan thiswork, of and itsdemonstratorantennas.As part receiver theSKA solutionsfor highly-integrated of ATNFThe isalsocontributingtothedevelopment SK SK A siteinvestigations A siteinvestigations A siteinvestigations A siteinvestigations A siteinvestigations possible locationfortheSKA. The MurnpeowiesiteinSouth Australia isoneofseveral Australian sitesbeingtestedasa page 61 SK SK Geraldton, WesternGeraldton, Australia, inJuly 2003. SKAworkshop willbeheldin An international to 10beams. atfrequenciesnear10GHzusingup observations offer acompromisesolutionwithoptionsfor view.Australian antennadesignsmay The favouring of multiplefields and othergroups favouring observations highfrequency groups dividedscience community with some iscurrently issueiscomplex;theSKA This but notboth. view, taken usingmultiple fieldsof observations (>20GHz)orfor high frequencyobservations available antennadesignsprovide foreither The design meetsalltheprojectsciencegoals. was nosingle at SKAantenna present evidentthat it Inparticular Groningen. from thediscussionsat requirements. Several issuesemerged data transport andSKA submissions onnew receiver concepts processing.Australian included Other contributions designs fromtheantennasthroughtodata “end-to-end” descriptions, giving representative Bothproposals were solution. cylindrical reflector Luneburg lensantennasandtheotherdescribinga one based on Australian SKAConsortium, Papers. Two WhitePapers were presentedby the proposals, SKAconcept orWhite discussion of themeetingwas thepresentationand highlight of Netherlands, The Groningen, inAugustA 2002. SKAmeetingwas heldin An international SK SK SK A meetings A meetings A meetings A meetings A meetings

Photo: Robert Jenkins

Technology developments o page 62page 62 was commissioned by the ATNF in 2002 for the international SKA workshop to be in 2002 for the international SKA ATNF was commissioned by the , by Charmaine Green , Emu in the Sky, , Emu in the Sky, produce parallel interpretations of the sky, presenting both the indigenous and astrophysics views together. produce parallel interpretations of the sky, Emu in the Sky © 2002 Charmaine Green This painting held in Geraldton, Western Australia in July 2003. The original painting is acrylic on canvas. The original painting Australia in July 2003. Western held in Geraldton, Art Collective t is working with the Marra ATNF The Art Collective in Geraldton. Charmaine Green is a local member of the Marra Technology developments Warlu time,theconstellation ofPleiades(sevensisters) islowabovethehorizon. shape appearsto besitting,andthelocal Aborigines, the Yamaji people,know thatthisisthetimetocollect emueggsforea This storyrefers tothefactthatobscuring dustcloudsintheMilky Way maketheshapeofanemu. At a certain timeofye called Warluis eggs. This Time. In ourregionthe Yamaji peopleusethestars(sevensisters)andMilky Way (emuimage) toknowwhenistimegooutfor Warlu Time (storyprovidedbyCharmaineGreen) page 63 ting. At ar, theemu emu

Technology developments is , . . A second two- www.lofar.org The low frequency Universe The low frequency AR AR AR AR AR OF OF OF OF OF L L As a result of in submission White an initial Paper Consortium short- 2001, the international LOFAR other along with two Australia, listed inland Western sites (in the USA and The as a Netherlands), in collaboration The ATNF, site. possible LOFAR ofwith the Government Australia, Western proposal in submitted a second, more detailed, the many October 2002; this proposal outlined ofadvantages Australia. in a location Western The scientific potential of discussed was LOFAR in December 2002: at a meeting held at the ATNF Detecting the epoch of reionisation L Array)Frequency (LOw is the first ofLOFAR the next-generation radio telescopes based on geographically systems but connected, distributed, of designed to is being LOFAR array stations. operate at frequencies from 10 to 250 approximately in initial formMHz and will be operational within array will contain The years. LOFAR five the next thousands of a 400-km distributed over antennas is a low- many In region. respects LOFAR of prototype version frequency the SKA, and is a direct step of in the development the SKA. are designed to antennas the LOFAR However, smaller much frequencies and over lower operate at for systems simpler receiving allowing bandwidths, is expected to start initial LOFAR than the SKA. next solar operations around the time of the in 2006 – 2008, with an estimated cost minimum of A$200M. Further from information is available at website the LOFAR day meeting,day scheduled for of 2003 at January Thescheduled University Sydney. In February a delegation 2003, from the LOFAR to discuss possible Consortium will visit Australia with involvement collaborations and Australian The delegation will also visit the potential LOFAR. and will meet with the Australia Western site in ofrepresentatives of the Government Western as well as advisers in the Australia, Australian A decision on the location of Government. a site the end of is expected to be made by for LOFAR 2003. L L page 64 y collaboration y collaboration y collaboration y collaboration y collaboration Industr Industr The proposal includes industry MNRF-2001 Technologies Powder partnershipsAdvanced with Pty Ltd and Dell Pty Ltd, CEA Technologies Computers 2002, a new partnership Pty Ltd. In agreement with in a collaborative established was Ltd, one of Pty largest Connell Wagner Australia’s This agreementengineering consultancies. provides additional SKA funds of $A0.5M for SKA research will Connell in 2003. Wagner and development of resources in a variety contribute engineering including an engineering infrastructureareas, study of In making Australia. possible SKA sites within NSW regional Connell Wagner’s the offer, noted that will the SKA Barry, manager, Tony many opportunitiesprovide for Australian as leading to engineering in coming years as well The new in radio astronomy. achievements exciting programcollaborative will be directed Steve by Hall (ATNF). and Peter (Connell Wagner) Negus Industr Industr Industr

Connell Wagner Pty Ltd NSW Regional Manager Tony Barry Pty Ltd NSW Regional Manager Tony Connell Wagner right) sign the Ron Ekers (front Director left) and ATNF (front in December 2002. Standing: collaborative agreement SKA left) and Peter Hall (ATNF). Negus (Connell Wagner, Steve Photo: Dietrich Georg and Engineers Australia Magazine Australia Engineers and Georg Dietrich Photo:

Technology developments A A Revenue (actual)2001-2002 Revenue (actual)2001-2002 Expenditure (actual)2001-2002 Expenditure (actual)2001-2002 6. The shortfallinrevenue isfundedfrom ATNF reserves whichincludeMNRF-1997deferred revenue. 5. Excludes A$4.8M depreciation appropriation. 4. The ATNF shares itsSydneyheadquarterswithCSIRO Telecommunications andIndustrialPhysics. 3. Includestheoperationofobservatory’s Visitors Centre. 2. Includestheoperationofobservatory’s Visitors Centre andtheMopraObservatory. 1. Expenditure includescapitalbutexcludesdepreciation. Notes: Direct appropriation Revenue (actual)2001-2002 (PaulWild) Observatory theNarrabri Operation of Expenditure (actual)2001-2002 A Appendices OA 17,308 329 1,066 359 990 103 892 708 1,558 3,790 TOTAL andmaintenance repairs Corporate Square KilometreArray MNRF-2001 MNRF-1997 National Facility support Computing Astrophysics program Office ofDirector Engineering anddevelopment Research (ATNF Marsfield support contribution) theParkes Observatory Operation of te xenlrvne299 160 1,308 1,338 TOTAL andmaintenance repairs Corporate draw down reserve Asset replacement revenue Other external Research revenue andservices Revenue (actual)2001-2002 Revenue (actual)2001-2002 Expenditure (actual)2001-2002 Expenditure (actual)2001-2002 A A : F : F : F : F : F 6 inancial infor inancial infor inancial infor inancial infor inancial infor 5 3 page 65 mation mation mation mation mation 4 2 1 1 1 1 1 A$1,000s A$1,000s A$1,000s A$1,000s A$1,000s 12,959 16,064 2,119 2,497 2,897

Appendices elecommunications and elecommunications and elecommunications and elecommunications and elecommunications and Staff shared with CSIRO Staff shared with CSIRO T T Industrial Physics Industrial Physics Administration Administration JSM Lie (Receivers) (Administration) Little S (Computing) Macquarding I Magri (Electronics) RG (Electronics) Manchester (Astrophysics) Manchester A PA) Manefield (Engineering D McConnell (LBA) N (Head, Computing) McConnell V McClure-Griffiths (Bolton Fellow/Astrophysics) G McIntyre (Computing) R Moorey (Receivers) R Norris (Acting Director) W Ojha (Astrophysics) J Support) (National Facility Orchiston SE Fellow/Astrophysics) Ott (Bolton (Administration) O’Toole C PA) (Director’s Pacey D Phillips (Bolton Fellow/Astrophysics) G (Bolton Fellow/Astrophysics) Pisano L (Receivers) Powell P (Receivers) Reilly N (Electronics) Roberts S (Administration) Rolph H Saunders (Electronics) L Support) Facility Sim (National M (Head, Astrophysics) Staveley-Smith P Storey (SKA site Studies/PASA) B (Receivers) Sykes A Thomas (Engineering Research) M (Astrophysics/LBA) Tzioumis G Fellow) Research (ATNF/USyd Walker B SKA) Fellow, Postdoctoral (ATNF/USyd Warr W Wilson (Administration) T Wilson (Head, Electronics) A Astrophysics) (Bolton Fellow, Wong Support) (National Facility Wright Staff shared with CSIRO Administration SO Clark C D’Amico C Duffy K Hodges B Lambert Wrbik T Industrial Physics Administration Administration Staff shared with CSIRO Staff shared with CSIRO T T Industrial Physics Industrial Physics page 66 y to December y to December y to December y to December y to December Manager) Astrophysics) Fellow, Postdoctoral Research) TNF staff TNF staff TNF staff TNF staff TNF staff B: Staff list, 2002 list, B: Staff 2002 list, B: Staff A A Januar Januar Sydney Sydney TJ (Electronics) Adams PJ (Administration) Archer Axtens (Receivers) RR PA) Barends (Astrophysics/Computing Beresford (SKA) M Bolton (Receivers) M (Receivers) Bowen J Support) Bromley (National Facility W (Assistant Director, Brooks & Engineering M (Astrophysics/Computing) Brouw G Calabretta (Computing) J Carrad (Receivers) AJ (Astrophysics) Caswell Chandra (Computing) RA Support) (Head, National Chapman Facility Chekkala (Electronics) D Chippendale (SKA) E (Electronics) Craig E (Electronics) Davis V Astrophysics) Blok (Bolton Fellow, de A Support) (National Drazenovic Facility J Dunning (Receivers) RT (Office of Ekers Director) Director) (ATNF Ekers R Elton (Electronics) G (Electronics) Ferris T (Receivers/overseas) Gay R Getts (LBA) G Gough (Receivers) E (Receivers) Graves P Hakvoort (Receivers) G Hall (Head, SKA Program) P (Bolton Fellow/Astrophysics) Hobbs S Secretary) (Divisional Howson P (Receivers) Jackson E (Computing/LBA) Jones H Support) (National Facility Kachwalla L Kanoniuk (Receivers) (AAO/ATNF Kedziora-Chudczer M (Astrophysics/Engineering Kesteven NB Killeen (seconded to CTIP) M (Astrophysics) Koribalski (Electronics) Leach B: Staff list, 2002 list, B: Staff A Januar Sydney Januar Januar Sydney Sydney A A B: Staff list, 2002 list, B: Staff 2002 list, B: Staff

Appendices Nar Nar Librar Librar Engineering ser Engineering ser Reynolds (Administration) Rees (Lodge) A Reddall (Electronics) M Oestreich (Electronics) B Murphy (Antennas&SiteServices) M Munting(Electronics) C McFee (GeneralServices) McFee (Electronics) S M Leven (Antennas&SiteServices) J Kennedy (VisitorsCentre) C Johnson (Antennas &SiteServices) (GeneralServices) Houldsworth T B Hiscock(Electronics) J Hill(Electronics) B Guest(Lodge) M Gordon (Antennas&SiteServices) Giovannis (Computing) M T Gay (Administration) Gates (Antennas&SiteServices) J C Forbes (Administration) J Dowd (Antennas&SiteServices) K Day (Electronics) O (Antennas& SiteServices) Darcey A Cunningham(Computing) E Campbell(Antennas&SiteServices) S Brooke (Electronics) D Brodrick (Computing) D Behrendt(Electronics) D Aboltin(Electronics) R D van derLeeuw Joos C A Librar Wright Wilcockson (AssistantEngineeringManager) Uden M B Sharp J Parsons (AssistantEngineeringManager) P Moncay B McDonald R Iannello M Huynh O Hughes T Finch G W Cooper BEgan Cook P Bonvino G Bourne P M Engineering ser Nar Librar Librar Engineering ser Engineering ser Nar Nar rabri rabri rabri rabri rabri y y y y y vices vices vices vices vices page 67 P P Canber Canber Walker Centre) (Visitors Centre) Unger (Visitors R Twardy (VisitorsCentre) K Turner (SiteServices) R Turner (SiteServices) S Spratt(Computing) B Smith(RFsystems) Sarkissian(Operations) G M Ruckley (Research Support) Reynolds (Officer-in-Charge) J T Reeves (SiteServices) J Price (Visitors Centre) K Preisig (Electronics/Servo) L Munday (Administration) B Centre) (Visitors Milgate L Mader(Operations) L Lees(SiteServices) Services) S (Lodge/Site Ingram R Hunt(Electronics/Servo) S Hoyle (Computing) Hockings (PA/Visitors Centre) A S Grimshaw Centre) (Visitors J Freeman (Administration) M Eslich (SiteServices) G Dawson (RFSystems) Crocker (SiteServices) R Cole(Lodge) B J Cathin(RFsystems) J Manager) Officer-in-Charge/HR Ball(Deputy D L Lovell (Astrophysics/Tidbinbilla) Jauncey (Astrophysics) J ANU/ATNF (Astrophysics/SKA) Briggs D F P Canber Wilson (Lodge) (Computing) Wieringa (Library) Wieringa C M (GeneralServices) Wheaton J Wark (Operations) V Troup (Computing) R (BoltonFellow) Tingay Stump(Library) E S Sunderland(Antennas&SiteServices) J Subrahmanyan(Operations) Stump(Library) G R Saripalli(Astrophysics) J Sault(Officer-in-Charge) L Ryan (Electronics) R Rowe-McDonald (GeneralServices) A D P P Canber Canber arkes arkes arkes arkes arkes ra ra ra ra ra

Appendices y Committee y Committee y Committee y Committee y Committee page 68 man man man man man echnical Advisor echnical Advisor echnical Advisor echnical Advisor echnical Advisor y y y y y man man man man man TNF Steering Committee 2002 TNF Steering Committee 2002 TNF Steering TNF Steering Committee 2002 TNF Steering TNF Steering Committee 2002 TNF Steering Committee 2002 TNF Steering C: Committee membership C: Committee membership C: Committee MNRF T MNRF T A A Secretar Secretar Members Members Deputy Chair Deputy Chair Chair Chair Dr S Guilloteau, Institut de Radio Astronomie Millimetrique (France) National Observatory Astronomy Dr P Napier, Radio (USA) Observatory Mullard Radio Astronomy Dr R Padman, (UK) (Australia) and Industrial Physics Telecommunications CSIRO Dr A Young, Organisation Netherlands (The Netherlands) Dr N Whyborn, Space Research MNRF T Secretar ATNF Mrs A Barends, Members Ex-Officio Prof ATNF Director, R D Ekers, and Industrial Physics Telecommunications CSIRO W King, Chief, Dr Prof of University Mt Pleasant and Ceduna Radio Observatories, Director, P McCulloch, Tasmania Dr R L Sandland, Deputy Chief CSIRO Executive, Astronomers of University Dr E Sadler, Sydney of Swinburne University Dr M Bailes, Technology International advisers Dr N Kaifu, National Astronomical Observatory Director General, Japan of Tokyo, Japan, Bonn, Germany Max Plank Institue for Radioastronomy, Dr K M Menten, Director, USA Science Institute, Directors Space Telescope Dr R E Williams, Industry Med, North Res Ryde President Innovation, Vice Dr R H Frater, Australia Cable & Optus, Wireless Networks Managing Director, Dr S Rotheram, Prof Observatory Anglo-Australian B J Boyle, Deputy Chair Prof Observatory R D Cannon, Anglo-Australian Chair C: Committee membership C: Committee A Secretar Secretar Members Members Deputy Chair Deputy Chair Chair Chair MNRF T MNRF T A A C: Committee membership C: Committee membership C: Committee

Appendices A A Members Members Secretar Secretar Chair Chair Dr SJohnston Mr MMeyer Dr S Tingay Mr DLewis rMZan nvriyo Melbourne Dr MZwaan, University of Dr T Wong, ATNF SydneyDr MWalker, (untilApril2002) University of # * Newmemberin2002 Dr FBriggs Melbourne Dr DBarnes, University of Members Mr VMcIntyre, ATNF Secretar Astronomy &Astrophysics,Dr CJackson, Australian University National Research School of Sydney (ChairuntilApril2002) Dr AGreen,University of Chair A Ms TGetts Tasmania Dr SEllingsen,University of (untilApril2002) Anglo-AustralianDr ECorbett, Observatory Dr TWong Dr MHunt University Dr BGibson,Swinburne Mr DMitchell Dr NMcClure-Griffiths Members Members Secretar Secretar Chair Chair A A Student member ustralia T ustralia T ustralia T ustralia T ustralia T # *, *, * * y y # y * y y nvriyo NSW , University of , University of Sydney (untilApril2002) , University of eerhSho fAstronomyAstrophysics, & Australian NationalUniversity , Research School of # , ATNF, ATNF , University of Tasmania , University of nvriyo Melbourne , University of # * nvriyo Sydney , University of nvriyo Sydney , University of elescope UsersCommittee2002 elescope UsersCommittee2002 elescope UsersCommittee2002 elescope UsersCommittee2002 elescope UsersCommittee2002 * , ATNF, page 69

Appendices page 70 elescope Time Assignment Committee Assignment Time elescope Committee Assignment Time elescope elescope Time Assignment Committee Assignment Time elescope elescope Time Assignment Committee Assignment Time elescope Committee Assignment Time elescope y y y y y man man man man man ustralia T ustralia T ustralia ustralia T ustralia ustralia T ustralia T ustralia cting Chair cting Chair cting Chair cting Chair cting Chair A A 2002 2002 Members Members A A Secretar Secretar Chair Chair * non-voting members Dr J Chapman*, ATNF Members of University Dr R Balasubrahmanyan, 2002) (to March Wales New South ofUniversity Dr A Melatos, 2002) MelbourneNovember (from Prof 2002) (Acting Director to March ATNF R Norris, Observartory, ATNF Parkes Officer-in-Charge, Dr J Reynolds*, Observatory Anglo-Australian Dr S Ryder, Narrabri ATNF Dr R Sault*, Officer-in-Charge, Observatory, National University RSAA, Australian Dr B Schmidt, Prof of 2002) University November (from J Storey, New South Wales 2002) (from November ATNF Dr L Staveley-Smith, of University 2002) Dr M Wardle, (to July Sydney A (Acting Chairman 2002) 2002 and July ATNF forin March meetings held Dr R Manchester, Secretar Chair Prof (Chairman 2002) ATNF until July Director, R Ekers, Prof 2002) (Chairman National University RSAA, Australian from November B Schmidt, A 2002 Members Members A A Secretar Secretar Chair Chair A A 2002 2002

Appendices D: Obser D: Obser Januar Januar Obser Obser Januar Obser D: Obser Januar Januar Obser Obser D: Obser D: Obser awl TFRs n alo a HmsrfaeC0 16 C906 anOHmaserflare of Riseandfall NCSA/UIL 11.5 UMin, RAIUB, 239 ATNF 98 C834 C918 C894 LMC with the ATCA 111.5 in edge-on late-type galaxies ATNF, UIL, UIL, UIL, the of 5-and8.6-GHzSurvey A C890 Measuringthepolarisationof Plante OMs, fromquasarjets ATNF, dark matter halos Dickey, The shape of Klein, RSAA ATNF, CfA, ATNF, UMar ATNF, Meixner, Dickel, Chu, Sault, 23.5 radio-bright x-ray transients Milne, Staveley-Smith, McIntyre, ATNF/RSAA, RSAA, Radio, X-ray andopticalemission A Group theCen of survey Caswell C858 ATNF, JPL, JPL, a very young PN of The radio properties Staveley-Smith, Kalnajs ATNF, MIT, ATNF, O’Brien, Freeman,Bosma, NRAL, NRAL spiral galaxies disks of CNR,UCatania Perlman Schwartz, 12 UTas 113 Tingay, Murphy, Preston, Jauncey, Lovell,Marshall, C779 C819 Trigilio, Umana, Cerrigone RSAA in unusual X-ray states Spencer, McCormick UMont, JHU 24 Anextendedhigh-resolutionHI NAPA Triaxial halosandtheouterHI C652 C751 UVIC, AITub, RSAA,CLMBA, ATNF ATNF,Ellingsen UMelb, KI, Carignan, Meurer Mass-lossratesoftheWRstars Bureau, Freeman, emissionfrom Continuumradio Beaulieu, NAPA 27.5 Freeman C651 de Blok, Zwaan, Briggs, NRC/DRAO, UCL, ATNF NFRA, CfA, 15.5 11.5 C634 Wilms, Tzioumis inthemassive Wd1 cluster ATNF, 276 C611 ray ATNFbursts UAm,ATNF UCardiff, C393 HartRAO Radio afterglows gamma from 26 Gaensler,Stappers,Getts RSAA, RSAA, ATNF, NRAO, Caltech, Caltech, C596 remnants(SNRs)in Supernova Waters,Chapman Goodwin, USyd 52 Dougherty, Clark, C186 densitycalibration Absoluteflux the Clouds Magellanic Wark, 103.5 Hours ATNF, Subrahmanyan MPE, MPE, Monitoring observations of Wieringa, Price, Schmidt, Number C530 62.5 Berger, Frail, Kulkarni, C015 MIT, Galacticplane ATNF, southern PKS0405-385(cont) The phaseII survey: MPIfR Pannuti, Staveley-Smith, Wolleben C539 Haberl, Filipovic,Pietsch, ATNF, ATNF,ATNF, ATNF, ATNF, KI Nicolson galaxies IRAS radio-loud Intermediate High-spatial-resolution Reynolds, Wieringa, Tzioumis, ATNF CfA, CfA, UCal, ATNF, UMinn, Kedziora-Chudczer, Jauncey, RSAA,RSAA Green HIinellipticalgalaxies 25 Taylor,Haverkorn, Title Program Gaensler, Dickey, McClure-Griffiths, ATNF, USyd, NFRA, UMar Dopita McGregor, Drake, C184 SNR 1987A van derHulst Sadler, Oosterloo,Morganti, 1978supernova The inNGC1313 Affiliations Reynolds AAO, ATNF, ATNF, MIT, SAO ATNF, ATNF White Duncan, USyd, ATNF, ATNF Ryder,Schlegel Staveley-Smith, Kesteven,Reynolds Wheaton, Staveley-Smith, Tzioumis, Manchester, Gaensler, Observers edr al,Poe,Um TF RO AAcrua oaiaino 87NAPA C857 10.5 NAPA circular polarisation of C846 UAm, ATNF, MRAO, MagneticfieldintheGalacticCentre: TIFR, TIFR, ATNF NAPA Fender, Pooley, Sault, C767 Roy, Rao,Subrahmanyan GX339-4 NAPA of observations CEA, UAm, JILA, Fender, Corbel, Nowak, vations madewiththeA vations madewiththeA vations madewiththeA vations madewiththeA vations madewiththeA y toDecember2002 y toDecember2002 y toDecember2002 y toDecember2002 y toDecember2002 ving programs ving programs ving programs ving programs ving programs ustralia T ustralia T ustralia T ustralia T ustralia T page 71 of the ATCA the of EtaCarina of observations RM observation of extragalactic sources extragalactic of RM observation 6.7 GHzmethanolmasers poweredaccretion MSPs elescope CompactAr elescope CompactAr elescope CompactAr elescope CompactAr elescope CompactAr ray ray ray ray ray

Appendices binary systems galaxy NGC 6872 in star formation regions ofand the evolution omega-HI the Magellanic Clouds page 72 van Gorkom, Mulchaey Gorkom, van UClmba, CarOgroupsof poor galaxies Perlman, Tzioumis Perlman, Dubner, Giacani, Dickel, GreenReynoso, Sault, McClure-Griffiths,plus 9 studentsUIL,IAFE, IAFE, Sault,Kedziora-Chudczer, ATNF UMar, Macquart, RickettATNF ATNF, Zabludoff, Pisano, Wilcots, Studyof the HI in the environs ofATNF, USyd, USyd AAO/ATNF, UArzna, of BL Lacerate objects ofATNF, variability radio UWis, Intraday C1011 Narrabri student Vacation of Evolution the HI content of KI, UCSD 12.5 the SNR G315.1-2.3 C1013 C1015 C1012 50.5 97.5 sources at 22 GHz 36 observing session Manchester, Manchester, Staveley-Smith, CfA, ATNF, SNR 1987A at 12mm DishoeckWong, Hunstead, Sadler Cotter, Buttery, USyd CL, USyd, CL, Ryder, Dahlem, Ehle, Haynes Landt, Perlman,Padovani, with SUMSS Cluster searches Bignall Tzioumis, C981 LO ATNF, Landt,Bignall, Padovani, AAO,ESA, ESO, UMar,STScI, STScI, 43 C1004ofobservations ATCA the STScI, STScI, UAd, ofobservations HI galaxies UAd 72 ATNF, disks at 3mm UTasofimaging ATCA samplefaint a C1009 C1005 C1010 jet of MH 2136-428 13 13 27.5 with radio halos Gaensler, Gaensler, Kesteven, Tzioumis Corbel, Fender,Brocksopp, ATNF, Tingay ATNF, ATNF, SchaudelBecker, CEA,UAm, LivJMU, Filipovic, Weisskopf,Jones, Aschenbach Radio jets in recurrent transients x-ray Wright, Wilner, Bourke, C989 NAPA MPE, MPE, MSFC, UWS, CfA, ADFA, CfA, ATNF UWS, MPE Observations ofofx-ray follow-up pre-planetary radio A C996 C992 selected SNR candidates 43 25 Saripalli, Hunstead, SubrahmanyanATNF USyd, ATNF, ATNF, Setia Chapman,Gunawan, Duncan, ATNF, ATNF, White, CheungKoribalski, galaxycandidatesradio giant SUMSS Millimetre observations of Eta CarinaHorellou, Koribalski C977 C978UAd UMar, ATNF, 24 8 ATNF OSO, HI in the gigantic interacting C979 26 Boyce, de Blok, GarciaBoyce, Beasley, Staveley-Smith,Claussen, Marvel, Boboltz ClarkBrocksopp, UCardiff UBr, ATNF, USNO AAS, ATNF, CaltechOv, NRAO, Magellanic Clouds in the masers Water UCL LivJMU, Radio jets in supergiant x-ray C973 74 C974 23 Rosenberg, Putman, Stocke,Rosenberg, Shull, Ryan-Weber McClure-Griffiths, Dickey,CASA,CASA, CASA, GreenGaensler, Zwaan, Drinkwater An HI study of the Lyman alphaUMinn, ATNF, ChurchwellJohnson, Indebetouw, UMelb CASA, UWis UWis, UWis, C960 Minchin,Disney, Knezek, Kilborn, Freeman, Studies of Galactic chimneys:USyd CfA, UMelb UMelb, HII regions in Ultracompact Grossi,Gallagher, Davies, 44.5 absorber/galaxy connection RSAA, JB, KPNO, UCardiff, UWis, UCardiff, C961 The HI content of high Z galaxies C967 UCardiff, UCardiff,resolution gas-rich high galaxies 97 C966 36 ofevolution The extreme 60.5 C970 12 EkersCaswell ATNF ATNF for 1720 MHz OH masers Search C952 35.5 Tingay, Tzioumis, Dodson Tzioumis, Tingay, Corbel, Fender, Kaaret,Tomisck, Tzoumis UTas ATNF, ATNF, Green, Dubner, Reynoso, Goss Johnston, Giacani, Morganti, Oosterloo, Sadler, Barnes,Koribalski, de Blok, IAFE, USyd, USyd, der Hulst, van Staveley-Smith, UAm, CEA, CfA/SAO, CASA/UCSD, transients state in the low-hard NFRA,NFRA, USyd, NRAO USyd, IAFE, ATNF,KI, ATNF, Swinb, ATNF, Theinterstellar towards medium An unbiased study of the HI peculiar neutron stars properties of ATNF early-type galaxies observations of NAPA soft x-ray C940 C950 C932 36 NAPA 42 Bignall, Jauncey, Rayner, Lovell, Kedziora-Chudczer, ATNF, ATNF, ATNF, Macquart, McCulloch, Nicolson, polarisation ofRAO,Hart, flat spectrum UTas, USyd, radio sources ATNF, UAd/ATNF, Microarcsecondstructure and C927 186

Appendices coe OaroundRSculptoris 220.5 C1049 A Centaurus 53.5 C1048 galaxies field ratio mass-to-light LO 47 139 pilot20GHzsurvey A C1045 C1046 ATNF, SISSA, USyd, ATNF, RSAA, ATNF, ATNF, ATNF RSAA, ATNF, 25 thedetached Imaging shell USyd ATNF, galaxy nearthegiantradio HIgas ATNF,Subrahmanyan, Walker, Wilson, 13 Ricci, Sadler, 24.5 Staveley-Smith, C1040 nearby Kedziora-Chudczer,high Kesteven, HI ATNF, The nature of OSO, StO, Ekers,Jackson, Dopita, C1044 C1043 RSAA/ATNF,ATNF, Schoier Wong, Lindqvist, Olofsson, ATNF, KI, Staveley-Smith the 5000-yr-old A new pulsar: Warren,Jerjen, Koribalski, contemporary Multifrequency 75 Johnston ATNF CfA, UClmba, Koribalski, van theeclipsing der, Hulst, of observations NGC1291 C1039 Manchester OABol,Camilo,Gaensler, OABol, CAO, ATNF, ATNF, 24 the Moon 36 ATNF Polarised emissionfromManchester, Johnston WIlson, ISAF-CNR ISAF-CNR, ATNF, ATNF,Possenti, Burgay,NIRFI, D’Amico, C1038 IRA-CNR,ISAF-CNR, 27 52.5 merging complex A3558 polarisationat6and20cm C1033 Vinyajkin, Krotikov, Nicastro galactic of Observations Sault, Kesteven, Bernardi, C1037 C1036 RSAA IRA-CNR IRA-CNR, OAB, NFRA, USyd, Poppi, Cortiglioni, Carretti, 38.5 IRA-CNR, IRA-CNR, Search HIemissioninthe for ImagingthePSR1706-44pulsar gravitationally candidate Observing Poppi, Kesteven Sault, Sironi, C1034 IRA-CNR, IRA-CNR, theringgalaxy Cortiglioni, Carretti, Bernardi, of dynamics The UMelb,UMelb, UMelb 4 178.5 Tzioumis variability spectral the Determining 38 RSAA, Hunstead, RSAA, RSAA, Morganti, C1035 FieldSouth Deep theChandra Bardelli, Venturi,Dallacasa, C1032 C1030 UMelb,ATNF, Wayth,USyd Webster, Trott GLOBALSTAR S2 observations of UTas 48 Kalnajs ATNF, RSAA of imaging Freeman, Perez, Fux, radio Ultra-deep GOODSCollaboration The CGJ1720-67.8 group in galaxies gas-rich Enigmatic C1028 Webster, Cram, Norris, STScI, ATNF, ATNF Koekemoer,Dickinson, Mobasher, 24 of 3cmcontinuumandlinemaps 51 48 ATNF,UCardiff HI Tingay, roleof deKool The - ingroups C1026 C1027 C1025 Dodson UCL UCL, UCL, Swinb,Swinb, UBir A* variability inSgr galaxies andevolution Formation of IAI thecompactgalaxy HIcontentof III part Mitchell, Sault GalacticfountainHIinNGC253, southern Kuhr sources of galaxies bluecompactdwarf Davies de Blok, LivJMU, 48 LivJMU, 67.5 70 Barlow, Liu, 39 Yates KI, OAB/KI 24.5 UYonsei, ATNF IAI,ATNF, C1018 C1023 ATNF,Ponman Barnes, SISSA KI, NFRA, McKay,Forbes, Mundell, C1019 MIT clouds C1024 bright-rimmed C1016 observations 18.5GHzpolarisation Weinberger Staveley-Smith, Temporin, of andkinematics HIenvironment 26.5 van Sancisi derHulst, andX-ray Connectedmillimetre A new GRBhostgalaxies: Oosterloo, Boomsma, RSAA, ATNF, RSAA, HI theextended of A survey C1017 McIntyre IAP,Rhee, IAP, IRA, UKC, UKC Staveley-Smith,Sung, Freeman, KI, ATNF, UCLA, Sault, Ricci Caltech, Caltech, Zotti, Prandoni, Gruppioni, Bafanoff ATNF, UWis of survey A20cmimaging Morris, Sault, Macquart, Frail Kulkarni, Berger, UKC, UKC, UKC, Miao White, Urquhart, Morgan, Thompson, Pisano,Wilcots eZtiOAP de Zotti SdmillisecondpulsarJ1740-5340 USyd NIRFI, ISAF-CNR UMila, ATNF, ATNF perspective intocosmicstarformation NRAO page 73 and polarisation characteristics of characteristics and polarisation wind nebula satellite interference nearby groups NGC 7009and6153 ESO39-2 environment of “Mouse” counterpart? “Mouse” lensed radiolobes PKS 1718-649

Appendices N in C1084 30 3 OH and HC 3 G1.6-0.025 nearest L-dwarf neighbour (NAPA) supernovae cloud G291.3-0.7 Cloud-cloud collision or outflow in Centaurus A Southern Galactic Plane Survey correlator/interferometer distinguish SFR from SNR the circumstellar nebulae of four stars Wolf-Rayet dwarfs and brown page 74 Wong, HillWong, Purcell, Burton,Minier, Hunt, Balasubramanyam, HillWong, Cannon, Sadler, Jackson, Couch, Deeley UNSW, UNSW, UNSW, UNSW, UNSW, Hunt, Whiteoak High resolution observations ofRSAA, AAO, USyd, UNSW ATNF, hot molecular cores C1082 PKS0019-338 and the AGN- UNSW ATNF, 27.5 UNSW UNSW, clusters ATNF UNSW, C1083connection starburst CH SiO, 12 Godfrey, CraggGodfrey, Whiteoak,Lazendic, Slane, GreenWardle, Hunt-CunnighamJones, CfA, ATNF, CfA, Monash Monash, UNSW ATNF, toward Methanol maser search USyd, USyd C1078 Star formation in molecular 13.5 1720-MHz OH sites in SNRs C1079 12 Weiler, StathakisWeiler, de Blok, Dejonghe,Baes, Davies Wu, Tzioumis, Spencer, Fender, Jonkervan der Klis, Johnston, UCL, ATNF, JB, UAm, SOGB, ATNF, SOGB, Manchester, Hendrick, Gaensler, ofjet Theultrarelativistic X-1Cir BorkowskiReynolds, IoA UAm, USyd, TheATNF, mass distribution and AAO NRL,NCSU, CfA, Martin, Koribalski, Madersupernova pulsar-powered new A C1073 ATNF ATNF, UHawaii, 87.5 NCSU NCSU, C1074 C1069 UCardiff 2001ig Radio emission from our 39 70 remnant in the LMC C1075 dynamical history of disk galaxies 23 Rantakyro, Murphy, WebbMurphy, Rantakyro, Subrahmanyan,Dwarakanath, Mohan, SrinivasanUNSW UNSW, ESO, Subrahmanyan,ATNF, Sadler, RRI,Ryder, damped Lyman alpha absorbers ATNF, USyd, AAO, supernovaradio-luminous The RRI RRI, the towards absorption OH C1066 C1064 104.3 Galactic Centre 12 MacquartWebb, Curran,Wong, PihlstromMurphy, Burgasser, PutmanUNSW, ATNF, UNSW, Highly redshifted molecular lines inNRAO UNSW, KI UCLA, CASA C1061 16.5 damped Lyman alpha absorbers emission in cool dwarf Radio stars C1062 83.5 Price, Schmidt,Salvo, Kulkarni, Frail, Subrahmanyan ATNFWong, Jones, Caltech, NRAO, Hunt, Burton, Minier, for A search GRB signatures in RSAA, RSAA, RSAA, What makes a gamma-ray burst? :UWS, UNSW, C1076Hunt-Cunnigham Jones, UNSW, UNSW, ATNF, NAPA medium Ellingsen, Burton,Minier, Biomolecules in the interstellarUNSW ATNF, UNSW,UTas, UNSW, C1077 Dust emission from protostellar Kinematics of G291.3-0.7: 41.5 C1081 C1080 16 12 OrchistonLeach,Kesteven, Wilson, et alRoberts, ATNF, ATNF, ATNF, and initial testing of Installation ATNF/AAO ATNF stars active 3.5 GHz analogue C1057 39 GaenslerKoribalski CfA ATNF HCO+ emission and absorption C1054 27.5 Caswell, Caswell, McClure-Griffiths,Cheung McClure-Griffiths, Dickey, ATNF, ATNF, UMin, ATNF, SNR G292.2-0.5: youngA faint Galactic HI polarimerty UAd C1052 9 C1053 74.5 remnant supernova Cheung, McClure-GriffithsBudding, Drake, Slee, ATNF UAd, CO, GSFC, ATNF, Caswellthefrom remnants Supernova Duncan, Koribalski of Verification list of the Parkes C1055 Lovell,Bignall, Jauncey, C1056Kedziora-Chudczer,Tzioumis, 14 ATNF ATNF, ATNF, ATNF, 43 ANTF,ATNF, UAd, ATNF Measurement of velocity the ISM PKS 1257-326 the IDV High-dynamic-range towards imaging ofCurran, Staveley-Smith, C1060 C1059 ATNF, lines to UNSW, Recombination 10 35 Millimetre fluxes of QSOs illuminating C1063 C1058 28 16.5

Appendices aedcUy/TFcloudassociatedwithN113 11 13 C1116 USyd/ATNF regions star forming C1118 A search forwater inCarina masers 24.5 A NGC1052andCentaurus 12 12 C1111 ImagingtheHCO+molecular CaltechOv,NRAO UAd/ATNF ESO(Chile) C1115 ATNF, UNSW, ATNF, C1112 CASA, ATNF, inhighvelocity fields Magnetic clouds Lazendic 25 24 Search massive excited for OHin ionisedcontentof The Whiteoak, Wong, Hunt, JIVE Beasley,Claussen ATNF, UWis, C1109 C1110 Johnston-Hollit H southern of UChi, Ekers, Putman, analogueforLGG93 NRAO, NFRA, Benjamin, 12.5 McClure-Griffiths, highredshiftquasars Brooks Follow-up continuum imaging Garay, Bronfam, Faundez, C1108 ATNF, JPL, CfA J0352-6602 48 Sky polarisation at 5GHz Langevelde van Vermeulen, Pihlstrom, CfA, CfA, ATNF, UNSW, NCRA ISAF-CNR, ISAF-CNR, C1107 ATNF Jauncey, Kuiper, linesin Molecular absorption Moran 66.5 Kondratko, Lovell, Greenhill, ATNF, 73 ATNF, UNSW, ATNF, UNSW, HIintheLocalGroup Intragroup 22 KI, RSAA IXO 37-apossibleintermediate C1106 Poppi Cotiglioni, Carretti, 48 8 ATNF UMelb, C1105 McConnell, Subrahmanyan, ATNF, Swinb, 11 Murphy,Kanekar HIPASS C1097 Unravelling of thenature C1103 Wong,Curran, Webb, 36 C1104 C1098 Staveley-Smith 12 NFRA, USyd, NFRA, of scaleHIdistribution Large Barnes,Pisano, Gibson, galaxy spiral masers methanol HIintheleadingarm C1101 Radiopulsationsfromisolated Ferguson, Jerjen ATNF ‘Antof Mz3 Nebula’, observations C1102 Multi-transition URuhr, URuhr, Oosterloo,OSO Sadler,Morganti, UNSW, UTas, USU, Monash, 13.5 UNSW, UNSW, UAl, AnHIstudyofG318.9+0.4 AAO, UMelb Manthey, Huttemeister, Aalto C1094 Wong of kpcscalemorphology The the of Radio observations Sobolev, Cragg, Ellingsen, Purcell, Minier,Burton, JB,UHerts Boeing, NRAO, JHU, USyd Rings USyd,USyd molecular The Lords of Ryder, Buta, Meyer UHerts, JB, galaxies UCL, barred 36 of 52 Tingay 8.5 Punsly, Clarke, Colbert, C1093 C1092 UNSW, ATNF NAPA Gledhill Meaburn, Bains, C1091 Redman,Bryce, C1090 theLMXBX1624-490 24 ESA, UTas Reynoso,Green 1630-47 4U Magneticfieldsincentralregions Bright-rimmedclouds:tracing 37 in outflow thepossible Studying Johnston C1088 ATNF, of Catching outburst thenext MSSL/UCL UTS, MPIfR, UTas, C1089 UKC, UKC, UKC Whiteoak Hunt, HerbigAe/Besystems USouth, JB Resolving thedustydisksinsouthern White Thompson, Urquhart, young stellarobjects inthe Massive starformation Ehle, Haynes UBir,UBir, UHel, ESA, Beck,Harnett, Peart, 117 DRAO, ATNF Spencer Hannikainen, Balucinska-Church, ULeeds, Church, ULeeds, UAm, C1087 CfA, Fornaxcluster Red Galaxy: MSXsources MIT, 22 MIT Sault, Wu UNSW ULeeds,ULeeds, Kuulkers, Hannikainen, holeCTEJ1550-564 theblack ATNF thedisksaroundtwo Imaging around jet/ISMinteractions The Dougherty,Tzioumis C1085 Waters,Ancker, vanden ATNF, CfA, UCSD, ATNF, UWol King. Oudmaijer, Burton CEA, UAm, ATNF, Lumsden, Hoare, Miller, Wijnands UNSW, RRI, Tomsick, Mitchell,Kaaret, Fender,Corbel, Tzioumis, Galaxy evolution in the Subramanyan UMelb,Schultz, UMelb, UMelb, Balasubramanyam, Ekers, Nulsen Waugh,Webster, Drinkwater, ye A N01gC0362.5 CX033 SN2001ig AAO Ryder IAR-CNR page 75 neutron stars? in theNucleusofNGC4945 their ionisedrims with theDSN luminositymergers moderate NGC 4622 hole mass black 2 O masersdetected 18 19 C1086

Appendices P352 10.6 P360 14.1 P361P366 2.1 10.3 P236 9.69 P262 3.03 P263 5.82 P268 15.4 P276 18.6 P282 4.23 P294 10.4 P303 14.3 P138 1.08 P140 33.5 O maser survey P368 1.25 2 observations of Stars post-AGB of PSR J0045-7319 page 76 arkes radio telescope arkes radio telescope arkes radio telescope arkes radio telescope arkes radio telescope y to December 2002 y to December 2002 y to December y to December 2002 y to December y to December 2002 y to December 2002 y to December vations made with the P vations made with the P vations made vations made with the P vations made vations made with the P vations made with the P vations made Januar Januar Obser Obser Kitamura ISAS southern YSOs (II) towards Hotan McLaughlin, Joshi,Burgay, Lyne, Kramer, Pearce, Manchester, Possenti, D’Amico, CamiloATNF, UBol, UBol, JB,UMan, UBol, Furuya, Cesaroni,Testi, JB, JB, JB, multibeam Parkes high-latitude OAAI, OAAI, OAAI, Swinb Multi-epoch H survey UClmba Forbes, BarnesForbes, Staveley-Smith, Koribalski,Henning, Kraan-Kortweg,Harnett, Schroeder, Sadler, Stewart, Green Price, ATNF, ATNF, Ord, Bailes, Jacoby, UM, UGuan,Kulkarni, AndersonNice, USyd, UTS, Swinb, Straten,van Ord, LivJMU, Bailes, bulge A extension to the UNM, USyd ULeic, survey ZOA Swinb, Swinb, Caltech, Swinb, Swinb, galaxies in groups Swinb, - the role of Caltech, HI Caltech A high-latitude millisecond pulsar Studies of binary a relativistic pulsar P357 survey 7.65 Sarkissian, Possenti, Sarkissian, CamiloPossenti, Lyne, Stairs, Athanasiadis, ManchesterKramer, UBol, UClmba ATNF, Pivovaroff,Crawford, Kaspi, Manchester in globular clusters JB, JB, JB, Mundell,McKay, ATNF JB, MIT, Haverford, UMcGill, ATNF Magnetospheric changes in LivJMU, LivJMU, of Timing discoveredpulsars B1828-11 PSR in a search of SNRs of Formation and evolution P340 P342 1.06 0.54 Januar PossentiKaspi, D’Amico, Lyne, Camilo, Kramer,D’Amico OABol OABol, UMcGill, Kaspi, Manchester, Crawford, Lyne JB, UClmba, JB, Lyne, D’Amico, Manchester, ATNF,JB, UBol, UMcGill, Timing and searching for pulsars ATNF, JB UBol LMCorp, and timing of Search pulsars Timing and confirmation of Magellanic Cloud pulsars Kulkarni, Edwards, Bailes, Stapper Manchester, Kramer, Lyne, Hobbs, Stairs, Camilo, UAm, Swinb, Caltech, Kaspi, Possenti, D’Amico, JoshiATNF, JB, JB, Lyne,Camilo, Manchester, Stairs, Hobbs, Kramer, UMcGill, OABol, OABol, UMan, UClmba, NRAO, UClmba,JB, ATNF, Pulsar multibeam survey Lorimer, Manchester, Freire, UAm NRAO, UMan, JB, Timing of pulsar discoveries multibeam NAIC, ATNF, JB, UMan Tucanae 47 in Sarkissian, Anderson, KulkarniLyne, Han, Manchester, Caltech Caltech, ATNF, Hoyle Sarkissian, Lewis, Manchester, Kaspi, BailesJB, ATNF, ATNF, UTas, NAO(Beij), Knight, Straten, Ord, van ATNF, rotation and Farady Polarisation of Timing pulsars young Swinb, Swinb, Swinb, Baseband searching for ultrafast pulsars UMcGill, Swinb ATNF of southern pulsars Obser ObserversKaspi , Manchester UMcGill, ATNF Affiliations Long-term monitoring Program Title Number Days LewisBoyleHannikainenHarnett UTas UHel AAO UTS PSR 1055-52 XTE J1450-603 X-ray lens candidate Gravitational Radio observations of NGC 986 CX039 CX1001 CX040 12 12 10 CX038 8.5 Tingay, McClure-GriffithsTingay, Deacon, ChapmanATNF ATNF, ATNF USyd/ATNF, Henz-90 22.235 GHz maser CX036Straten,Ord, van Bailes, Knight, Hotan, Manchester, CX034 12 ATNF, Swinb, Swinb, Swinb, Swinb, Swinb, 6 Precision pulsar timing Januar Januar Obser Obser

Appendices r wn radiopulsars Supernova from 1987A 3.41 P420 Swinb Interstellarscintillationstudiesof forpulsations 20-cmsearch Adeep ray pulsar ATNF JB USyd, CNR-IFCAI, UMcGill, UMcGill, 2.14 Moremembersofanewclasspulsars P414 UMcGill Ord hemisphereregions JB,UBol, UMan, Johnston, Nicastro, sub-millisecondgamma- Apossible JB, JB, UAO, Manchester ATNF, nebulae planetary NRAO, Kaspi, Ransom, origin The of UClmba, Lorimer UMcGill, UMcGill, Joshi, Hobbs, Possenti, USyd, USyd, ATNF Manchester, Stairs, Camilo, Kramer, Lyne, Wang, SN1006 ATNF of dishobservations Single DiffusepolarisationfromtheGalactic 7.06 0.83 main-sequencestar singledishobservations plane: Deacon, Green,Chapman P406 IAFE, ATNF IAFE, southern of GalacticHIimaging Kaspi P407 Roberts,USyd Ransom, UMinn, ULeid, boxes EGRET error HighresolutionprofilesofOHlinesP402 3.85 Haverford sourcesintheGalactichalo inmid-latitude pulsars Asearch for ATNF, CfA, Mader Dubner, Why noradiopulsationfromCastelletti, SAX 0.21 ATNF, ATNF, J1808.4-3658sofar? UMcGill, UMcGill, Dickey,Haverkorn, Green Gaensler, McClure-Griffiths, UMcGill, P401 UMcGill, ATNF 0.96 UAm, UAm, UBol, Filipovic apulsarcompanionto A search for UBol, CAO, ATNF Staveley-Smith, Anderson, P404 Possenti,D’Amico, UMcGill, Manchester UWS NRAO (GB), JB, JB, Salvo,Di Burderi, Burgay, Egret A pulsarsearch four for the fo observations Multifrequency Crawford pulsars 10.2 eclipsingmillisecondpulsarJ1740-5340 Tam, Ransom, Roberts, Kaspi, UMcGill UMcGill, P399 UBol, ATNF,Manchester ATNF, USyd Lyne, Kramer,Stairs, GeodeticprecessioninPSRJ1141-6545 3.37 0.59 ATNF/USyd Manchester, Wilson, Johnston Possenti,Burgay, D’Amico, JB, P398 P393 JB, NRAO (GB), loosegroups Stootman AnHIstudy of ATNF, McGill, UClmba Vela the pulsar Intrinsicpolarisationof Tam ATNF, RSAA insouthern Monitoringscintillation ATNF, Deep Roberts,searches Kaspi, for young and Swinb, Swinb, Manchester,Kaspi, Camilo USyd,ATNF, UCSD, Kramer, Lyne, Stairs, pulsars “radio-quiet” ATNF 1.06 Staveley-Smith, Freeman from emission radio for search A UClmba, GSFC, Pisano,Barnes, Gibson, P383 magnetars CfA, UMan, ATNF Walker ATNF Johnston, Ball, Rickett, Timingtwo pulsars young andenergetic Vacation session studentParkes observing JB, UMcGill, UMcGill, alpha absorbers Gaensler, Lorimer, Machester ATNF, UClmba, Spectraof1720-MHzOHmasers ATNF connection absorber/galaxy bandobservations Narrow Camilo, Arzoumanian, JB,Sarkissian JB,Manchester,Camilo, JB, Manchester ATNF, ATNF UNSW, NCRA Tam, Lorimer, Kaspi, HIindampedLyman search A for UMelb,UMelb Lyne, Kramer, McLaughlin, UNSW,UNSW, UMelb UNSW, Manchester ATNF Sault McClure-Griffiths, CASA HIPASS of Completeness&reliability UMelb, UMelb, 2.23 Kanekar Flambaum, Webb, Curran, Murphy, FisherlawwithaHIPASS sample P372 Webster Meyer, UMelb,UMelb, HIPASS team Meyer, Ryan-Weber, AnHIstudyoftheLymanalpha Webster,Zwaan, Drinkwater, ATNF, RSAA CASA, CASA, CASA, Tully- theBaryonic Investigating Caswell Shull RSAA, ATNF, RSAA, Rosenberg, Stocke, Putman, Jerjen Staveley-Smith, Gurovich, deBlok,Freeman, page 77 fHIPASS spirals edge-on of inSFRs morphology at 20cm 491.56 P419 3 P417 0.23 0.3 P413 P410 1.14 1.6 P409 P408 0.5 P405 1.17 P400 11.8 3.82 P396 P395 2.95 P394 1.54 P392 4.11 P391 9.53 P389 18.3 P387 4.85 P370

Appendices P423 0.17 M122 19 O masers V137 20 2 1934-638 jet interaction regions (part A) in Circinus the LBA star formation regions the youngest protostars in Ophiuchus ISOGAL field - m18.63+00.35 page 78 vations vations vations vations vations y to December 2002 y to December 2002 y to December 2002 y to December 2002 y to December y to December 2002 y to December 2002 y to December y to December 2002 y to December 2002 y to December 2002 y to December 2002 y to December vations made with the Mopra radio telescope vations made with the Mopra radio telescope vations made vations made with the Mopra radio telescope vations made vations made with the Mopra radio telescope vations made with the Mopra radio telescope vations made Januar Januar VLBI obser VLBI obser Januar Januar Obser Obser Lewis Reynolds, Tzioumis, Tingay, Jauncey ATNF, ATNF, ATNF, Morganti, Tzioumis,Oosterloo, et al.Tingay, Reynolds, activity and proper motions in Core NFRA, NFRA, ATNF,Tingay HI absorption around the young V160 ATNF ATNF, UTas 14 V161 ATNF 24 radio galaxy PKS 1549-79 ATNF PSR B1259-63 GPS galaxies PKS 1718-649 and PKS high resolution imaging of Wide field, V165 24 Drake, McGregor,Norris Drake, TzioumisOjha, Tingay, ATNFRSAA, RSAA, OjhaATNF ATNF, Corbett, Norris, Kewley, Intermediate ATNF, radio-loud IRAS GalaxiesDopita, Smith V143 of NGC 7552 with Wide-field imaging Reynolds, Johnston, Dodson, V150 ATNF,AAO, CfA, 22 ATNF,USyd, UTas, 12 Do mergers stop monsters? Distance and proper motion ofCfA RSAA, ATNF V156 V155 44 30 in the Hubble Deep Field South Reynolds, TzioumisReynolds, Greenhill, Moran, Norris, et al.CfA, ATNF CfA, ATNF ATNF, the acceleration of Tracking H Januar Observers Legge,Dodson, Reynolds, Lewis Fey,Ojha, Reynolds, Jauncey, Tzioumis, Johnston, UTas, ATNF, UTas, Dodson, et al.McCulloch, Corbett, Dopita, Norris, et al. ATNF, ATNF, USNO, PSR proper motions from hemisphere ICRF sources USNO, Affiliations UTas UTas, ATNF, RSAA ATNF, ATNF, AAO, Astrometry/imaging of southern imaging of LBA bright Cola galaxies two V133 UTas V088 V131 Program Title 14 44 203 observations with the LBA Number Hours Tzioumis, Tingay, et al.Tingay, Tzioumis, ATNF ATNF, VLBI obser survey observations Claussen, Ellingsen,Beasley, UTas, NRAO, CaltechOV, - II Measuring the mass of the Galaxy V135 24 Huynh, Norris, JacksonRSAA ATNF, RSAA, Phase referenced observations of galaxies V153 14 Januar BurtonKing, Oudmaijer, Hirabayashi, Edwards, Lovell, ATNF,ISAS, ISAS, ULeeds, ULeeds, UNSW red MSX sources Continued use of Moprafor VSOP Observers Burton,Myers, Walsh, BarnesEllingsen, Cragg, Godfrey,MinierLadd, FullerCfA,UNSW, CfA, Monash, Monash, UTas, Bright class II methanol masers Affiliations Do starsform stationary by collapse M116 M117 UNSW 12.92 UBuck, UMIST Program Title UNSW 2 The of evolution dense cores forming or moving accretion? M118 7.71 Number Days Barnes, Staveley-Smith ATNF UMelb, Obser II:a mini Malin I Wombat Caswell ATNF for 13 GHz OH masers in Search Jiang, Balasubramanyam, Omont IAP RRI, NAO(Beij), P421 Hoare, Lumsden, for SiO maser stars Search in an 1.08 M119 ULeeds, ULeeds, 2.96 star formation Massive in the Galaxy: M121 10.67 Januar Januar VLBI obser VLBI obser Januar Januar Obser Obser

Appendices E: A E: A CEA Centre d’Etudesd’Astrophysique, Centre CEA SpaceCommunications Deep Canberra Colorado, USA University CASA, of CDSSC Cagliari Astronomical Observatory, CASA CAO Technology, Instituteof California Caltech Association, Berkeley-Illinois-Maryland Observatory, BeijingAstronomical BIMA BAO Australia Telescope Facility, National Taiwan AcademiaSinica,IAA, ATNF Czech Sciencesof ASIAA Academy of Russia Astrospace Centre, ASCR Observatory, Armagh UK ASC ArO Uppsala, AstronomiskaObservatoreit, Kiev, AstronomicalObservatory AOUpp AreciboObservatory, USA AOK Australia NationalUniversity,Australia AO ANU Astronomy, University of Insitituteof Czech AstronomicalInstitutePrague, AITub AIPr Australian DefenceForceAcademy, Telescope, Anglo-Australian Australia ADFA Observatory, Anglo-Australian AAT AAO E: A E: A E: A ffiliations ffiliations ffiliations ffiliations ffiliations Saclay, France Australia Complex, Italy USA USA China Australia Republic Czech Republic, Sweden Ukraine Tubingen, Germany Republic Australia Australia page 79 IAG Instituto Astronomico eGeofisico, Instituto Institutod’AstronomiayFisicadel IAG deCanarias,Astrofisica Institutode IAFE IAC RadioObservatory, HatCreek USA University, Harvard USA HatCreek Harvard Astronomical Radio Hartebeesthoek SpaceFlightCenter, Goddard USA HartRAO GSFC Gray Data Consulting, USA Mason University, George USA Gray Data Telescope, GreenBank USA GMU GBT ESTECAstrophysics Division, Observatory, Southern European ESTEC ESO Astrophysical DominionRadio DRAO d’EtudesdelaMatière Département CSIRO Telecommunications & DEMIRM SpaceResearch, Centerfor USA CTIP CSR deLyon, France CRALObservatoire CRALOL SpaceScience& of CSIRO Office University, Cornell USA Observatory, NewZealand Carter COSSA Cornell CO Technology, New Instituteof Central Astrophysics, Centerfor Harvard CITNZ CfA Brazil Espacio, Argentina Spain Observatory,Africa South Netherlands The Germany Observatory, Canada France deParis,Millimétrique l’Observatoire et enInfraRouge interstellaire Industrial Physics, Australia Applications, Australia Zealand University, USA

Appendices Physik, GermanyPhysik, Germany Germany UK Observatory, USA Centre, Japan TheNetherlands in Astronomy, USA Observatory, USA tory, Italy Italy Italy Italy Italy France MonashMPE Australia Monash University, MPIfA Inst. für Extraterrestrische Max Planck Inst. für Astrophysik, Max Planck MPIfRRadioastronomie, Inst. für Max Planck MRAO Radio Astronomical Mullard NAIC and Ionosphere National Astronomy NAOJObservatory, Astronomical National NASA-RCUSA Center, Research NASA Ames NFRA for Research Netherlands Foundation NOAO National Optical Astronomical NRAO Radio National Astronomy Observa- NRLNROUSA Laboratories, Research Naval NWU Japan Nobeyama Radio Observatory, OAAI USA Northwestern University, Osservatorio Astrofisico di Arcetri, OABol Osservatorio Astronomico di Bologna, OARome Osservatorio Astronomico di Roma, OATOCat Osservatorio Astronomico di Trieste, OHP Osservatorio Astronomico di Catania, OMs Observatoire de Haute Provence, ON ObservatorireFrance de Marseille, Observatorio Nacional, Brazil page 80 Radioastronomica, Argentina France Italy Brazil Espaciais, Bologna, Italy USA Laboratory, Germany Interferometry Network, UK USA IAPIAR France Paris, Institute d’Astrophysique Argentino Instituto de IASpIFCTR Institut d’Astrophysique Spatiale, Fisica Cosmica - CNR, Instituto de ImColINPE Imperial College London, UK Instituto Nacional de Pesquisas IoAIPAC Institute ofUK IRA-CNR Astronomy, Caltech, USA IPAC, Institute of CNR, Radio Astronomy, ISAISU Japan ISAS, JAC USA State University, Iowa JBO USA Hilo, Astronomy Centre, Joint JHU UK Bank Observatory, Jodrell JILA USA Hopkins University, John JPL of JILA, University USA Colorado, KI USA Propulsion Laboratory, Jet KPNOLivJMU Kapteyn Netherlands Institute, USA National Observatory, Kitt Peak LLNLUK Moores University, John Liverpool National Livermore Lawrence LOLSW The Netherlands Leiden Observatory, MSFC Landessternwahrte Heidelberg, MERLIN USA Space Flight Center, Marshall Multi-element Radio Linked MIT Institute of Massachusetts Technology,

Appendices BsBostonUniversity, USA Germany Bonn, University of UBos UK Birmingham, University of UBonn Amsterdam, University of UBir USA Alabama, University of UAm Australia Adelaide, University of UAl Tata Astronomy, Radio Institutefor UAd Tokyo University, Gakugei Japan TIFR Technology, TGU University Swinburne of SpaceTelescope ScienceInstitute, USA Swinb Stockholm Observatory, Sweden STScI StO SuperiorediStudi ScuolaInternazionale Observatory, Shangai China SISSA SETIInstitute, USA ShO SETI Astronomy & Research Schoolof RamanResearch Institute, India RSAA Scotland Edinburgh, Royal Observatory RRI Belgium Belgium, of Royal Observatory ROE Royal Canada College, Military ROB RMC RadioAstronomy Institute, University QueensUniversity, Canada RAIUB Queens Pontificia Universidad CatolicadeChile, Mountain Observatory, Purple China PUCC PhillipsLab, USA PMO OnsalaSpaceObservatory, Sweden PLab deParis, Observatoire France Meudon, OSO OpenUniversity, UK OPM Open The Netherlands The India Australia Avanzati, Trieste, Italy Astrophysics, Australia Germany Bonn, of Chile page 81 KooUiest fKyoto, Japan University of Kyushu Tokai University, Japan UKyoto UKT Telescope, UnitedKingdomSchmidt Kokugakuin University, Japan UKST Iowa State University, USA UKok Illinois, USA University of UIow PRChina HongKong, University of UIL Hilo, USA University of UHK UK Hertfordshire, University of UHilo Finland Helsinki, University of UHerts University deGuanajuato, Mexico UHel University, Eotvos Lorand Hungary UGuan Edinburgh, UK University of UEot Durham,England University of UEdin UDur SanDiego, California, University of UCSD SantaCruz, California, University of SantaBarbara, UCSC California, University of UCSB Lick California University of ColumbiaUniversity, USA UCLO London,UK University College UClmba Chicago, USA University of UCL Chile, Chile University of UChig USA Champagne-Urbana, University of UChi Cardiff, UK Universiy of UCha Berkeley, California, USA University of UCardiff Calgary, Canada University of Colorado, USA University of UCB UCal Bristol,UK University of UC UBr Australia USA USA USA Observatory, USA

Appendices Australia Australia USydUTas of University Australia Sydney, UTex of University Australia Tasmania, UTor of University USA Texas, UTS of University Canada Toronto, UVir of Sydney, University Technology, UW of University Virginia, USA UWA of University UK Wales, UWash of University Australia, Western UWis of University USA Washington, UWol of University Wisconsin, USA UWS of University Australia Wollongong, Yale of Australia University Sydney, Western YU USA University, Yale China Observatory, Yunnan page 82 alia ederal University, Brazil ederal University, Science and Technology, UK Science and Technology, Mexico Mexico, Australia ULeedsULeic of University UK Leeds, UMac of University UK Leicester, UMan Australia Macquarie University, UMar of University UK Manchester, UMaur of University Maryland, USA UMcGill of University Mauritius Mauritius, UMelb Canada McGill University, UMinn of University Melbourne, Australia UMIST of University Minnesota, USA of University Insitute of Manchester, UMontUNag of University Montreal, Canada UNAM Japan University, Nagoya de Nacional Automa Universidad UNMUNSW of University USA Mexico, New of University New South Wales, UOxUPenn of University Oxford, Oxford UPitt USA State University, Pennsylvania UQld of University USA Pittsburgh, of University Queensland, Austr URhURuh of University South Africa Rhodes, USMF Germany Ruhr-Universitaet, USNA Santa Maria F USNO USA Academy, US Naval USouth USA Observatory, US Naval UStan UK Southampton University, UStern USA Stanford University, USU Germany Sternwarte University, USuss Russia State Ural University, of University UK Sussex,

Appendices G: 2002publications G: 2002publications F F P P June PASA, 2001, (2002). 29. 19, Frederick White Workshop onAGN Variability CSIRO ATNF, AcrosstheElectromagnetic Spectrum, 25-29 NICOLSON, G.D. radiosources” intraday Elizabeth and variable anATCA “New resultsfrom studyof RAYNER, D.P., TINGAY, S.J., TZIOUMIS, A.K., CLAY, R.W., DODSON, R.G., McCULLOCH, P.M. & JAUNCEY, H.E., *BIGNALL, D.L., L.L., LOVELL, KEDZIORA-CHUDCZER, J.E.J., MACQUART, J.-P., 567, 342.(2002). BHAT, N.D.R. & GUPTA,Y. “Pulsar scintillation inthelocal interstellarmedium:LoopIandbeyond”.ApJ, Parkes multibeam pulsars”. J. of observations Astrophys. 23, 53. (2002). Astron., BHAT, N.D.R., CAMILO, F., CORDES,J.M., D.J., NICE, D.R.LORIMER, CHATTERJEE,& S.“Arecibo D.D. (2002). 83. 391, A&A, atlas”. The I. &THIERBACH, galaxies inbarred fields “Magnetic M. SHOUTENKOV,BECK, R., V., HARNETT, EHLE, M., J.I., HAYNES, R.F., SHUKUROV, SOKOLOFF, A., MyCn18”. MNRAS, nebula, (2002). ‘Engraved Hourglass’ 337,401. *BAINS, I.,BRYCE, M.,CALABRETTA, M.&STIRLING, the A.M.“A radiocontinuum studyof by anasterisk. indicated are PapersATNF authors which include P G: 2002publications October 04 September 06 17May ATNF mediareleasescanbefoundontheweb at Mini black holesmay helpexplainmassive ones August 02 CSIRO tohelpeaseNASA’s jam” “traffic 14February heart of change galaxies’ Black holes’ fatal attractiontriggers 16 May toChina Equipment builtat“thedish”goes solved:Gamma-ray explodingstarstheculprit burstmystery Astronomers findstarstretchedtobursting point F P P G: 2002publications G: 2002publications F F apers usingA apers usingA apers usingA apers usingA apers usingA : A : A : A : A : A TNF mediareleases,2002 TNF mediareleases,2002 TNF mediareleases,2002 TNF mediareleases,2002 TNF mediareleases,2002 TNF data,publishedinrefereedjour TNF data,publishedinrefereedjour TNF data,publishedinrefereedjour TNF data,publishedinrefereedjour TNF data,publishedinrefereedjour page 83 http://www.atnf.csiro.au/news nals nals nals nals nals

Appendices page 84 BIRKINSHAW, M., WORRALL, D.M. & HARDCASTLE, M.J. “The of jet and halo X-ray M.J. & HARDCASTLE, PKS 0521-365”. D.M. M., WORRALL, BIRKINSHAW, 335, (2002). 142. MNRAS, “Cassini and VLA observations of radia- R.J. emission from Jupiter’s synchrotron SAULT, & S.J. *BOLTON, 415, 987. (2002). Nature, tion belts”. “The spectrum of and variability D.C. & BACKER, circular R.J. H., SAULT, FALCKE, G.C., *BOWER, 571, 843. (2002). A* from 1.4 to 15 GHz”. polarization in Sagittarius ApJ, “The ofdiscovery R.N. BRACEWELL, strong extragalactic Radio Telescope”. polarization using the Parkes Astron. History 5, & Heritage, 107. (2002). J. & CORTIGLIONI, C. R., SBARRA, CARRETTI, E., FABBRI, V., M., TUCCI, M.,BRUSCOLI, NATALE, of behaviours “The power-law S. angular spectra of 7, polarized Galactic synchrotron”. New Astronomy, 171. (2002). radio and optical study “A J.F. & DONATI, SLEE, O.B. M.W., MENGEL, B.D., E., CARTER, *BUDDING, of 527. (2002). 19, 35850)”. F star HR 1817(=HD PASA, young the active observations of “Correlation & WHITE, in microwave S.M. effects O.B. SLEE, E., LIM, J., *BUDDING, 35. 7, (2002). stars”. Astronomy, New selected RS CVn-like M., IARIA, R., VANDERKLIS, N.R., ROBBA, L., FIORE, STELLA, F., T., L., DiSALVO, BURDERI, M. “A & BURGAY, S. REBECCHI, G., GENNARO, S., CAMPANA, MENDEZ, M., M.T., MENNA, BeppoSAX observation of KS 1731-260 in its quiescent state: constraints on the magnetic field of the neu- 574, 930. (2002). tron star”. ApJ, of “Representations coordinates celestial E.W. in FITS”. A&A, 395, M.R. & GREISEN, *CALABRETTA, 1077. (2002). “Heartbeat of & LORIMER,D.R. B.M. GAENSLER, MANCHESTER, the Mouse: R.N., a F., *CAMILO, 579, L25. (2002). ApJ, radio pulsar associated with the axisymmetric nebula G359.23-0.82”. young “PSR J1124- J. & SARKISSIAN, D.R. LORIMER, GAENSLER, B.M., MANCHESTER, R.N., F., *CAMILO, of5916: discovery 567, L7. (2002). remnant G292.0+1.8”. ApJ, energetic in the supernova pulsar a young “Mid-infrared, Halpha and R.D. & CANNON, MADER, S. Q.A., PARKER, A.J., GREEN, M., *COHEN, images continuum ofradio 336, 736. (2002). H II region, G308.70+0.60”. MNRAS, an unusual R., M., BRUSA, FIORE, F., MAIOLINO, P., SEVERGNINI, COMASTRI, M.,A., CILIEGI, MIGNOLI, P., G.C. PEROLA, & G. MATT, R.,F., VIGNALI, LA FRANCA,C., MORGANTI, A., MOLENDI, S., BALDI, observations of II. Multiwavelength “The HELLAS2XMM survey. bright, optically inactive P3: an X-ray 571, 771. (2002). galaxy”. ApJ, “The 2000 periastron & McCONNELL, D. MANCHESTER, R.N. S., JOHNSTON, T.W., *CONNORS, passage of 1201. (2002). 336, PSR B1259-63”. MNRAS, WIJNANDS, J.M., MILLER, J.A., OROSZ, A.K., TOMSICK, J.A., TZIOUMIS, FENDER, R.P., *CORBEL, S., jets from the microquasar XTE J1550-564”. X-ray relativistic “Large-scale, decelerating P. & KAARET, R. 298, 196. (2002). Science,

Appendices MNRAS, (2002). 336,39. “VariableSPENCER, R.E. circularpolarizationassociatedwithrelativistic ejectionsfromGRS1915+105”. *FENDER, R.P., RAYNER, D., D.G., McCORMICK, MUXLOW,T.W.B., POOLEY, G.G., SAULT, R.J. & (2002). EYRES, S.P.S. Sakurai’s radioemissionfrom “The Object(beyondAstrophys. 1MM)”. SpaceSci.,279,69. (2002). variability intheglobularcluster47Tucanae”. withlarge-amplitude pulsar opticalcounterpart ApJ, 579,741. EDMONDS, P.D., GILLILAND,R.L., CAMILO, F., C.O. HEINKE, GRINDLAY,& J.E.“A millisecond (2002). MNRAS, variable stars”. luminousblue four 63. 330, *DUNCAN, S.M. of &WHITE, R.A. images “Radio theyoungsupernova SN1006(G327.6+14.6)”. A&A, 387,1047.(2002). remnant environment of DUBNER, G.M., GIACANI, E.B., GOSS,W.M., GREEN, A.J. & NYMAN, neutralgas “The L.A. medium aroundthesupernova remnantG320.4-1.2”.AJ, 123,337.(2002). G.M.,DUBNER, B.M., GAENSLER, GIACANI, E.B., GOSS,W.M. &GREEN, A.J. interstellar “The DRINKWATER, M.J. 2001Australian “The GalaxyClusterWorkshop”. PASA, 19, 265.(2002). (2002). MNRAS,DODSON, G343.1-2.3andPSRB1706-44”. L1. 334, &GOLAP, R. of “Ontheassociation K. MNRAS, regions”. (2002). 333,307. star-forming DODSON, R.G. &ELLINGSEN, S.P. “A insouthern search 4750- and4765-MHzOHmasers for A&A, 392,417.(2002). DE HEIJ,V., BRAUN, R.&BURTON, W.B. compact,isolatedhigh-velocity clouds”. “An study of all-sky (2002). 43. 382, A&A, low-mass galaxies”. onthespacedensityof -constraints andSculptorGroups the Centaurus *DE BLOK, W.J.G., ZWAAN, M.A.,DIJKSTSRA,M.,BRIGGS, F.H. &FREEMAN, K.C. “An of HIsurvey A&A, 385,816.(2002). *DE BLOK, W.J.G. low surfacebrightnessgalaxies”. of curves A.“High-resolutionrotation &BOSMA, ApJ, (2002). 570,L89. forahighmass-to-lightratio intheclustercore”. millisecondpulsarsinNGC6752: evidence J. “Timingof *D’AMICO, N., MANCHESTER,R.N.,A., L., FICI, POSSENTI, LYNE, A.G., CAMILO,F. &SARKISSIAN, PASA, (2002). 455. 19, quasars”. thebackground densitiesof systemsandradioflux dampedLymanalphaabsorption catalogue of CURRAN, S.J., WEBB,J.K., MURPHY, M.T., &FLAMBAUM, BANDIERA, E. CORBELLI, R., V.V. “A 650. (2002). ApJ, “. COLAgalaxies 564, insouthern andcompactradiocores correlation Project: theradio-far-infrared T., MARSTON, CHARMANDARIS,A., V., KEWLEY, &ZEZAS, L. results theCOLA from “First A.L. *CORBETT,NORRIS,E.A., R.P.,APPLETON, DOPITA,HEISLER, C.A., M.A., P., C.,STRUCK, MURPHY, page 85

Appendices O maser 2 page 86 O maser emission in seven active galactic and at high nuclei active O maser emission in seven 2 velocities in the Circinus galaxy”. ApJ, 582, L11. (2002). galaxy”. in the Circinus ApJ, velocities of M.R. “Representations & CALABRETTA, coordinates in FITS”. world A&A, 395, E.W. *GREISEN, 1061. (2002). magnetic “Counterclockwise fields in the G.J. & QIAO, A.G. LYNE, MANCHESTER, R.N., J.L., *HAN, Norma 570, L17. (2002). spiral arm”. ApJ, MANCHESTER, R.N., F., I.H., CAMILO, KRAMER, STAIRS, M., JOSHI, B.C., A.G., LYNE, G., *HOBBS, very 333, large MNRAS, in PSR J1806-2125”. glitch “A POSSENTI, & KASPI, A. V.M. N., D’AMICO, L7. (2002). OHNISHI,A.K., K. & FUKISHIMA, TZIOUMIS, T. J., REYNOLDS, D.L., M., JAUNCEY, *HOSOKAWA, fluctuation of“Possible the position of 580, to extragalactic radio sources”. ApJ, Sagittarius A* relative L43. (2002). KANONIUK, H. & CHU, GOUGH, R.G., H., SINCLAIR, M.W., WANG, C.-H., LIEN, Y.-J., *HWANG, 78-114 GHz monolithic subharmonically IEEE Microw. pumped GaAs-based HEMT diode mixer”. “A T.-H. & Wireless Components Lett., 12, 209. (2002). M.R.S. K.I., & HAWKINS, HOOK, I.M. KELLERMANN, P.A., SHAVER, J.V., WALL, C.A., JACKSON, quarter-Jansky“The flat-spectrum Parkes I. Sample selection and source sample. identifications”. A&A, 386, 97. (2002). 19, 277. (2002). “Single dish polarisation calibration”. PASA, S. JOHNSTON, 332, 109. (2002). pulsars”. MNRAS, for giant pulses in search Vela-like R. “A & ROMANI, S. JOHNSTON, *FENDER, R.P., RAYNER, D., TRUSHKIN, S.A., O’BRIEN, K., SAULT, R.J., POOLEY, G.G. & NORRIS, G.G. POOLEY, R.J., K., SAULT, O’BRIEN, S.A., TRUSHKIN, D., RAYNER, R.P., *FENDER, time-lag properties polarization and “Spectral, of 330, 212. R.P. oscillations”. radio GRS 1915+105 MNRAS, (2002). NOHEJL,K.& P.A., JONES, L., STAVELEY-SMITH, W., REID, T., BOHLSEN, M.D., *FILIPOVIC, study of radio-continuum ATCA the Small Magellanic “An - I. Source catalogues at Cloud G. GOLDSTEIN, 335, 1085. (2002). 8.64 GHz”. MNRAS, 1.42, 2.37, 4.80 and A.L., H. ANDERNACH, ROY, RUDNICK, L., SLEE, O.B., KEMPNER, C.L., J.C., SARAZIN, Y., *FUJITA, observations& EHLE, M. “Chandra of the disruption of 575, 764. (2002). cool core in A133”. the ApJ, star- massive “Two M.G. & BURTON, R.P. NORRIS, D., MARDONES, K.J., BROOKS, G., *GARAY, forming regions at early evolutionary 579, 678. (2002). stages”. ApJ, a “Towards J. & TAUBER, J.L. K., JONAS, GORSKI, K.M., BENNETT, A.J., BANDAY, G., GIARDINO, model of intensity and linear polarisation: full-sky a re-analysis of Galactic synchrotron data”. Parkes the A&A, 387, 82. (2002). SINCLAIR, GOUGH, R.G., McGREGOR, P.J., R.P., NORRIS, S.P., ELLINGSEN, *GREENHILL, L.J., H search for “A J.M. & MORAN, J.R. HERRNSTEIN, C.J., PHILLIPS, D.P., RAYNER, M.W., galacticemission in southern and star-forming nuclei active galaxies: discovery of in the edge-on a maser 565, 836. (2002). galaxy IRAS F01063-8034”. ApJ, JAUNCEY, J.M., MORAN, KUIPER, T.B.H., J.E.J., LOVELL, P.T., KONDRATKO, L.J., *GREENHILL, “The of discovery H G.P. & BAINES, D.L.

Appendices 179. (2002). V. MINIER, R.S. &BOOTH, “A 387, A&A, toward regions”. methanollinesurvey high-mass star-forming 1310. (2002). *MERRITT, D. &EKERS, R.D. “Tracing Science, 297, black throughradiolobemorphology”. holemergers ApJ, HIshells”. large 578,176.(2002). distribution of *McCLURE-GRIFFITHS, N.M., DICKEY, J.M.,B.M. GAENSLER, &GREEN,A.J. Galactic “The PASA,1990-2001”. (2002). 207. 19, BIZUNOK, N.S., SN1987A: KESTEVEN, M.J. theradioremnantof &REYNOLDS, J.E. “Evolution of R.N.,*MANCHESTER, GAENSLER, B.M., WHEATON, V.C., STAVELEY-SMITH, TZIOUMIS, L., A.K., (2002). 615. GRO 396, A&A, J1655-40”. of emission duringthe1994outburst *MACQUART,J.-P., WU, K.,SAULT, R.J. &HANNIKAINEN, D.C. “Rapidly evolving circularlypolarized 572, 786.(2002). *MACQUART, J.-P. &JAUNCEY, D.L.ApJ, synthesis”. usingEarth-orbit imaging radio “Microarcsecond 1452-517 andPKSB2148-555”.MNRAS, 331,717. (2002). *LLOYD, B.D. &JONES, P.A. PKSB1234-723, MRC “Jets galaxies Iradio class intheFanaroff-Riley H positions of *LAZENDIC, J.S.,WHITEOAK, J.B., HARBISON, KLAMER,I., P.D. &KUIPER, T.B.H. “Accurate Pulsar”. MNRAS, 523.(2002). 334, JOHNSTON,KRAMER, M., S. &VAN STRATEN, W. theVela “Highresolutionsinglepulse studies of 887. (2002). Way. Milky behind thesouthern Hydra/AntliaThe region I. (l KRAAN-KORTEWEG, R.C., HENNING, P.A. galaxies &SCHRODER, A.C. “Parkes of HIobservations supernova remnantN206”.AJ, 124,2135.(2002). *KLINGER, R.J., J.R., DICKEL, FIELDS,B.D. &MILNE,D.K. “A featureinthe peculiarlinearradio from 86.1to92.1GHz”. PASA, (2002). 19, 505. H.D.,KIM, BALASUBRAMANYAM, &BURTON, R. IRAS17470-2853 M.G. “A of linesurvey spectral AJ, sky”. 124,690. (2002). of from thesouthcelestialcapregion EKERS, R.D., FREEMAN, K.C., GIBSON, B.K., HENNING, P.A. HI-selectedgalaxies etal.“A catalog of BARNES, D.G.,W.J.G., DEBLOK, BHATHAL, R., BOYCE, P.J., DISNEY, M.J., DRINKWATER, M.J., *KILBORN, V.K., R.L., STAVELEY-SMITH, WEBSTER, MARQUARDING, L., BANKS, M., G.D., (2002). Astrophysics, 448. 45, survey”. KARACHENTSEV, I.D. theRFGCcatalog detectedintheHIPASS &SMIRNOVA, of galaxies “Flat A.A. AGN A&A,388,113.(2002). background andtheLMCgas”. N logSof KAHABKA, P., log The theLMC-III. K.S. DEBOER, &BRUNS, C. “ROSAT X-ray of inthefield sources (2002). &CAMILO, M. KRAMER, F. “A Proc. Soc. searchAstron. highGalacticlatitude pulsars”. 687. for 3, India, B.C.,*JOSHI, BURGAY, M., LYNE, A.G., MANCHESTER, R.N., D’AMICO,POSSENTI, A., N., 2 O masers in the Large Magellanic Cloud”.MNRAS, Magellanic 969.(2002). O masersintheLarge 331, page 87 ≈ 266 degrees to 296 degrees)”. A&A,391, to296degrees)”. 266degrees

Appendices page 88 MISANOVIC, Z., CRAM, L. & GREEN, A. “A search for young Galactic supernova remnants”. Galactic supernova for young search MNRAS, A. “A Z., CRAM, L. & GREEN, MISANOVIC, (2002). 335, 114. MUCKE, S.V., MARCHENKO, G., SKALKOWSKI, I.R., STEVENS, M.F., CORCORAN, A.F.J., *MOFFAT, 573, 191. et al. starburst “Galactic NGC 3603 from to radio”. X-rays ApJ, B.S. KORIBALSKI, A., A., PTAK, (2002). POSSENTI, MANCHESTER, R.N., F., I.H.,CAMILO, STAIRS, A.G., LYNE, G., HOBBS, D.J., *MORRIS, & KRAMER, M. “The Parkes F. CRAWFORD, N.P.F., McKAY, N., D’AMICO, KASPI, V.M., A., BELL, J.F., Multibeam Pulsar Survey of and timing - II. Discovery 335, 275. (2002). 120 pulsars”. MNRAS, I.R. “Australia STEVENS, & M.F. CORCORAN, A.F.J., MOFFAT, B.S., *MUECKE, KORIBALSKI, A., Compact Array radio imaging ofTelescope objects in the giant H II region NGC 3603”. the proplyd-like (2002). 571, 366. ApJ, L., “The & SMITH, R.C. HI environment of three STAVELEY-SMITH, B., GROVES, M.S., *OEY, 123, 255. (2002). superbubbles in the Large Magellanic Cloud”. AJ, “Extended HI N. & CALDWELL, D. R., SADLER, E.M.,VERGANI, MORGANTI, T.A., OOSTERLOO, 123, 729. (2002). disks in dust lane elliptical galaxies”. AJ, Heights the Dover radio astronomy: in Australian “Ingenuity and initiative B. & SLEE, O. W. *ORCHISTON, Astron. History 5, & Heritage, 21. (2002). hole-in-the-ground antenna”. J. observations of “Multiwavelength three P. short- BRADY, & B.E. A., WOOD, BROWN, R.A., OSTEN, 138, (2002). 99. EI Eridani”. ApJS, CC Eridani, and binary systems: ER Vulpeculae, period active M.I., L., ANDERSEN, AMATI, P., SOFFITTA, GARMIRE, G., J., GOROSABEL, FRAIL,D.A., , L. *PIRO, M.R., HJORTH, GARCIA, G., GANDOLFI, J., FYNBO, F., E., FRONTERA, ANTONELLI, L.A., BERGER, “The et al. burst of bright gamma-ray J. 2000 February 10: a case study of an optically gamma-ray dark 680. (2002). 577, burst”. ApJ, HI/optical atlas of “An isolated galaxies”. 142, 161. ApJS, C.T. E.M. & LIU, WILCOTS, D.J., *PISANO, (2002). B.M., GAENSLER, S.F., ANDERSON, F., L., VERBUNT, HOMER, W.H.G., LEWIN, D., POOLEY, of M. “Optical identification DER KLIS, & VAN KASPI, V.M. D.W., FOX, MILLER, J.M., B., MARGON, cataclysmic variables”. sources in the globular cluster NGC 6752: numerous evidence for faint X-ray multiple (2002). 569, 405. ApJ, R.M., R., WARK, SUBRAHMANYAN, KULKARNI, S.R., D.E., E., REICHART, BERGER, *PRICE, P.A., S.D., K.,RYDER, E.,GUNN, CORBETT, B., BOYLE, J., BAILEY, WIERINGA, M.H., FRAIL, D.A., 572, L51. (2002). star progenitor”. K. ApJ, et al. “GRB 011121: a massive KOVIAK, SEYMOUR, N., L. “Probing the HI kinematics of the E. & STAVELEY-SMITH, RYAN-WEBER, J.X., *PROCHASKA, Large interpreting Magellanic quasar absorption-line Cloud: observations of toward protogalactic velocity 114, 1197. (2002). fields”. PASP, B.K., GIBSON, K.C., R., FREEMAN, L., BRAUN, STAVELEY-SMITH, V., M.E., DE HEIJ, *PUTMAN, DISNEY, P.J., BOYCE, R., DE BLOK, W.J.G., BHATHAL, G.D., BANKS, D.G., BARNES, W.B., BURTON, clouds: high-velocity properties of et al. “HIPASS R.D. the compact EKERS, M.J., DRINKWATER, M.J., 123, 873. (2002). and extended populations”. AJ,

Appendices hydrogen nearthesupernova remnantW28”.AJ, 2145.(2002). 124, VELAQUEZ, P.F., G.M., DUBNER, GOSS, W.M. neutral thelarge-scale &GREEN, A.J. of “Investigation -IV.ring galaxies Parkes (2002). 140. 386, A&A, observations”. VAN W., DRIEL, COMBES,F., &SPARKE, M. ARNABOLDI, polar L.S. “A of hydrogen survey neutral 841.(2002). A&A, 392, observations”. JONES,M., D.,VLBI the : sources radio LOVELL, Spectrum J. CompactSteep southern “A etal. sampleof REYNOLDS, J., JAUNCEY, D., PRESTON, P., McCULLOCH, R., TINGAY, S., EDWARDS, P., COSTA, *TZIOUMIS, KING, A., DALLACASA,MORGANTI, E., R., D., TADHUNTER, C., FANTI, C., arcminute scales”.ApJ, 579,607.(2002). J.M. Galacticsynchrotron &McCLURE-GRIFFITHS, emissionon N.M. “Polarization angularspectra of S.,*TUCCI, M.,CARRETTI,E.,CECCHINI, NICASTRO, L., FABBRI, R.,GAENSLER,B.M., DICKEY, radiosources”. ApJS, hemisphere southern 141,311.(2002). VLBIinvestigations of VLBI andgeodetic *TINGAY, S.J., REYNOLDS, J.E., TZIOUMIS, JAUNCEY,A.K., D.L., LOVELL, J.E.J. “VSOPspace etal. 652. (2002). *TINGAY, S.J. &EDWARDS,AJ, PKS0521-365”. P.G. 124, andevolution of structure parsec-scale “The J. Astron.&Astrophys., (2002). 26, 158. SU, B.M., LI, Y.S., GAO, Y.F., &FU, Chinese H.W. several IRASgalaxies”. ultra-luminous “Radiospectraof MNRAS, 335,1079.galaxies”. (2002). starburst*STEVENS, I.R.,FORBES, D.A. indwarf superstarclusters &NORRIS, R.P. of observations “Radio MNRAS, galaxies”. 337,981.(2002). GHz peaked spectrum SNELLEN, I.A.G., LEHNERT, M.D., M.N. BREMER, R.T. &SCHILIZZI, “A Parkes half-Jansky sampleof high-velocity clouds”.ApJ, (2002). 572,178. SEMBACH, GIBSON, K.R., B.K., FENNER,Y. &PUTMAN, compact M.E.“A limitonthemetallicity of ApJ, J0116-473”. galaxy 256.(2002). giant radio 565, *SARIPALLI, SUBRAHMANYAN, L., &UDAYA R. N. SHANKAR, “A activity casefor renewed inthe AJ, newlycatalogued galaxies”. 1954.galaxies: (2002). 124, DISNEY, M.J., DRINKWATER, M.J., EKERS, R.D., FREEMAN, 1000brightestHIPASS K.C. etal. “The R.C., RYDER, S.D., BARNES, D.G., DEBLOK, W.J.G., KILBORN,V.A., BHATHAL, BOYCE, R., P.J., *RYAN-WEBER, KORIBALSKI, E., B.S., STAVELEY-SMITH, JERJEN, L., KRAAN-KORTEWEG, H., (2002). JOHNSTON-HOLLITT, M.“Multiplemergingevents inthedoubleclusterA3128/A3125”.AJ, 123,1216. J.A.,*ROSE, GABA, A.E., CHRISTIANSEN, W.A., DAVIS, D.S., CALDWELL, N., HUNSTEAD, R.W. & densityinquasarPKS0405-385”.ApJ, flux 103.(2002). polarized 581, *RICKETT, B.J., &JAUNCEY, L. KEDZIORA-CHUDCZER, the D.L. of “Interstellar scintillation ATNF, 25-29June PASA, 2001, (2002). 100. 19, Elizabeth andFrederick WhiteWorkshopAGN on Variability CSIRO Spectrum, AcrosstheElectromagnetic inintraday interstellarscintillation variations atcentimeterwavelengths”:RICKETT, B. role of “The page 89

Appendices page 90 TNF data, published in conference proceedings TNF data, published in conference proceedings TNF data, published in conference TNF data, published in conference proceedings TNF data, published in conference TNF data, published in conference proceedings TNF data, published in conference proceedings TNF data, published in conference apers using A apers using A apers using A apers using A apers using A P P P *ANDERNACH, H., SLEE, O.B., ROY, “Extreme relic radio sources in four southernM. A.L. & EHLE, ROY, O.B., H., SLEE, *ANDERNACH, India, 1999, Nov/Dec Pune, Radio Frequencies, at Low Symposium 199: The Universe clusters”. In: IAU Gopal-Krishna), (2002). Swarup, Pramesh Rao, 153. (eds. in the “Merging clusters & MOLENDI, S. DE GRANDI, S. VENTURI,T., ZUCCA, E., S., BARDELLI, 2000, Sesto Pusteria, 2-7 July with Galaxy Clusters, Cosmic Evolution Shapley Concentration”. In: Tracing (2002). Borgani, & Valdarnini), 268, Mezzetti 143. (eds. Ser., ASP Conf. “ATCA D. & BOBOLTZ, M.J. CLAUSSEN, K.B., L., MARVEL, STAVELEY-SMITH, A.J., BEASLEY, Observations of Masers in the Magellanic Clouds”. American Astronomical 201, Society Meeting Water (2002). “High-resolution radio polarimetry of A.J. X”. & GREEN, Vela MILNE, D.K. R.J., SAULT, *BOCK, D.C.J., 271, 187. Ser., 2001, ASP Conf. 14-17 August Boston, Mass., Remnants, In: Stars in Supernova Neutron (2002). Slane & Gaensler), (eds. Narrow-band L. “The HI Survey Parkes of the Magellanic & STAVELEY-SMITH, J. KERP, C., BRÜNS, System”, Seeing Through the Dust: The Detection of of HI and the Exploration ASP the ISM in Galaxies, & Willis), (2002). Landecker Taylor, 276, 365. (eds. Ser., Conf. methanol masers to hot molecular cores”. R., “From & BALASUBRAMANYAM, A. WALSH, M., BURTON, III: the earliest of phases In: Hot Star Workshop 267, 355. star birth, (ed. Crowther), Ser., ASP Conf. massive (2002). VENTURI, T., BARDELLI, S., ZAGARIA, M., PRANDONI, “Radio R. I. from emission ZAGARIA, MORGANTI, & S., BARDELLI, VENTURI, T., cluster complex:the A3571 stage the final of a cluster merger?”. 385, 39. (2002). A&A, M.E. “HI fine structure& PUTMAN, in Magellanic AJ, tidal debris”. T.A. OOSTERLOO, B.P., WAKKER, 123, 1953. (2002). BARNES, V.A., L., KILBORN, WEBSTER, R.L., STAVELEY-SMITH, M.J., M., DRINKWATER, *WAUGH, K.C., FREEMAN, R.D., EKERS, M.J., DISNEY, P.J., BOYCE, R., BHATHAL, DE BLOK, W.J.G., D.G., H. et al. “The large-scale JERJEN, distribution of P.A., in the neutral hydrogen HENNING, B.K., GIBSON, 337, 641. (2002). MNRAS, region”. Fornax A.R. & PATNAIK, J.N., HEWITT, FLETCHER, A.B., H.-W., CHEN, J.E.J., LOVELL, J.N., *WINN, a gravitationally “PMN J0134-0931: radio morphology”. lensed quasar with unusual ApJ, SCHECHTER, P.L. 564, 143. (2002). A.R., PATNAIK, J.E.J., LOVELL, C.S., KOCHANEK, J.N., HEWITT, N.D., MORGAN, J.N., *WINN, R.A. “PMN J1632-0033: & SCHOMMER, a new gravitationally lensed P.L. SCHECHTER, PINDOR, B., 10. 123, (2002). quasar”. AJ, 19, 475. A. PASA, “Millimetre science with the upgraded Telescope”. Australia & MELATOS, T. *WONG, (2002). & J.P. HALPERN, J., TRUMPER, MANCHESTER, R.N., D., SANWAL, G.G., PAVLOV, V.E., *ZAVLIN, 569, 894. (2002). “X-radiation from the millisecond pulsar J0437-4715”. ApJ, BECKER, W. P P

Appendices Slane &Gaensler),(2002). inSupernovaNeutron Stars Remnants, Mass., Boston, 14-17August ASPConf. 2001, Ser., 271,387.(eds. FILIPOVIC, M.D., STUPAR, JONES, M., P.A.WHITE, G.L. & In: “GalacticSNRsinthePMNSurvey”. (2002). Supernova Remnants, Boston, Mass., 14-17AugustASP Conf. 2001, Ser., (eds. 271,395. Slane&Gaensler), FILIPOVIC, M.D., JONES, P.A. in Stars &WHITE, G.L. Neutron In: Clouds”. “SNRsintheMagellanic 37. (eds. Taylor, Landecker, Willis), (2002). theISMinGalaxies, Penticton, B.C. 20-25 October 2001,ASPConf. of HIandtheExploration Ser., 276, of *EKERS, R.D. advances Detection Through theDust:The In: “Observational inradio astronomy”. Seeing Frequencies, Pune, Nov/Dec India, 1999,498.(eds. Pramesh,Swarup, Ghopal-Krishna), (2002). *EKERS, R.D. &BELL,J.F. IAU In: Universe LowThe interference”. 199: at Radio “Radiofrequency AugustASP Conf. 2001, Ser., (eds. 271,415. Slane&Gaensler),(2002). inSupernova In:NeutronStars supernova Remnants, remnantswithneutronstars”. Boston,Mass., 14-17 G.,DUBNER, GIACANI, B.M., GAENSLER, E., GOSS,W.M. bilateral &GREEN, “Environsof A. Ser., (ed.Slane&Gaensler),(2002). 271,195. NeutronStarsinSupernova Remnants,SNR B0540-693”. In: Boston,Mass., 14-17August 2001,ASP Conf. R.N., STAVELEY-SMITH, KESTEVEN, L., M.J. thecomposite &GALLANT, Y. of “Radio observations J.R.,*DICKEL, MULLIGAN, R.J., M.C., KLINGER, B.M., GAENSLER, D.K., MILNE, MANCHESTER, Mass., 14-17August ASPConf. Ser., 2001, (eds. 37. 271, (2002). Slane&Gaensler), campaign at Parkes tofindyoung radiopulsarsat20cm.”. In:NeutronStars inSupernova Remnants, Boston, *CRAWFORD, F., PIVOVAROFF, M.J.,V.M. KASPI, R.N. &MANCHESTER, “A sensitive search targeted 41. (eds. Slane&Gaensler), (2002). 6127”. In:NeutronStarsinSupernova Remnants, Boston,Mass., AugustASP Conf. 14-17 2001, Ser., 271, PIVOVAROFF, M.J. aradio supernova “SNRG292.2-0.5: remnantassociatedwiththeyoung pulsarJ1119- *CRAWFORD, F.,B.M.,V.M., GAENSLER, KASPI, R.N., MANCHESTER, CAMILO, F., LYNE,A.G. & Marina, Italy, May, ASPConf. Ser., 199.(eds. .258, Maiolino, (2002). Marconi&Nagar), Active Marciana GalacticNuclei, of IssuesinUnification In: P3”. thecaseof optically quietgalaxies: R., FIORE, F., LAFRANCA,F., MATT, G., PEROLA, G.C., BALDI, A.&MOLENDI, S. “X-ray bright BRUSA,A., CILIEGI, M., P.,COMASTRI, C., VIGNALI, SEVERGNINI, M., MIGNOLI, P., MAIOLINO, Radio Science(WARS 2002), 20-22February, Leura, 2002,(2002). *CHIPPENDALE,A.P. “Technology SKAreceiver issuesfor In:Workshop design”. of onApplications URSI XXVIIthGeneralAssembly, Maastricht, 17-24August, 2002,(2002). *CHIPPENDALE,A.P. Array”. In: theSquareKilometre “SiGeLNAnoisetemperatureprojectionsfor Symposim 206,331.(eds. (2002). Reid &Migenes), AGB In:CosmicMasers: From stars”. ProtostarstoBlack Holes, RiodeJaneiro, 4-11March, 2001,IAU post- *CHAPMAN, J.M. ATCA/VLA Identification &SEVENSTER,M.“The of OH1612MHzSurvey: to Black Holes, RiodeJaneiro, 4-11March, 2001, IAU 1.(eds. Symposim206, &Reid), (2002). Migenes J.L.*CASWELL, From Protostars CosmicMasers: between themaserspecies”.In: relationship “Starformation: page 91

Appendices page 92 *GAENSLER, B.M., DICKEY, J.M., McCLURE-GRIFFITHS, N.M., BIZUNOK, N.S. & GREEN, A.J. “High A.J. & GREEN, BIZUNOK, N.S. N.M., McCLURE-GRIFFITHS, J.M., DICKEY, B.M., *GAENSLER, polarimetryresolution of on the inner Galaxy”. Backgrounds: In:Workshop Polarized Astrophysical et al.), (2002). Cecchini Bologna, 9-12 October 2001, 20. (eds. Backgrounds, Polarized Astrophysical “New views of A.J. & GREEN, the J.M. DICKEY, N.M., McCLURE-GRIFFITHS, *GAENSLER, B.M., 2002. (2002). 17-24 August, Maastricht, Southern Galaxy”. In: URSI XXVIIth General Assembly, spline-profile “Smooth-walled millimetre- G.G. & MOOREY, R.J. BOLTON, G.L., JAMES, C., *GRANET, horn 375. (2002). 2002, France, In: JINA 2002, Nice, astronomy”. for radio wave the “Investigating L. H., DE BLOK, & STAVELEY-SMITH, E. K., JERJEN, FREEMAN, S., GUROVICH, Structure In: The sample”. Dynamics, & History of with a HIPASS Law Baryonic Tully-Fisher Galaxies: A in Honour of Da Costa & Jerjen), (2002). 273, 375. (eds. Workshop Ser., ASP Conf. Freeman. Professor Ken of on Applications “The directions”. Kilometre Array - Square In: Workshop Australian Radio P.J. *HALL, 2002. (2002). 2002), Leura, February, 20-22 Science (WARS “Square - an overview”.Array (SKA) prototyping in Kilometre XXVIIth URSI Australia In: P.J. *HALL, 1326. (2002). 2002, 17-24 August, Maastricht, Assembly, General “The gigantic barred Meeting of galaxy B.S. NGC 6872”. Proc. In: & KORIBALSKI, C. the *HORELLOU, Combes & Barret), 2002, 177. (eds. (2002). d’Astronomie et d’Astrophysique, Societe Francaise G.D., NICOLSON, J.-P., MACQUART, J.E.J., KEDZIORA-CHUDCZER,LOVELL, L., D.L., *JAUNCEY, BIGNALL,A.K.,M.A.& WIERINGA, “Intra-day H.E. TZIOUMIS, J.E., R.A., REYNOLDS, PERLEY, In: origins and implications”. proceedings ofParticles Galaxies: and Fields in Radio variability, the Oxford Laing & Blundell), (2002). 123. (eds. 250, Ser., 2000, ASP Conf. 3-5 August Oxford, Galaxy Workshop, Radio “A B.J. & WALLACE, GAENSLER, C.M., B.M. OLBERT, J.W., KEOHANE, C.G., WAITE-JONES, S., JIN, morphological of In: analysis The High G292.0+1.8 with Chandra remnant ATCA”. the supernova and (2002). Schlegel & Vrtilek), 262, 343. (eds. Ser., ChandraASP Conf. Science, Energy at Sharp Focus: Universe & B.M. R., GAENSLER, M., ROMANI, A., ROBERTS, M.,GREEN, DOHERTY, S., JOHNSTON, of imaging “Radio and X-ray near 1=312 degrees”.F. EGRET sources two In: Neutron Stars CRAWFORD, Slane & Gaensler), 271, 209. (eds. Ser., 2001, ASP Conf. 14-17 August Boston, Mass., Remnants, in Supernova (2002). “The R.W. WIERINGA, M.H. & HUNSTEAD, R.D., EKERS, R.W., M., CLAY, *JOHNSTON-HOLLITT, dual radio relics of India, Nov/Dec Pune, at 199: Radio Frequencies, Low The A3667”. In: Universe IAU Ghopal-Krishna), (2002). Pramesh, Swarup, 1999, 157. (eds. “The of cluster environment R.W. Abell 3667”. & HUNSTEAD, R.D. M., EKERS, *JOHNSTON-HOLLITT, Particles and Fields in Radio Galaxies:In: of proceedings 3-5 Oxford, the Oxford Radio Galaxy Workshop, Laing & Blundell), (2002). 250, 432. (eds. Ser., 2000, ASP Conf. August all sky Measure estimated Rotation “An R.D. & EKERS, C.P. M., HOLLITT, *JOHNSTON-HOLLITT, 2002, 2172. (2002). 17-24 August, Maastricht, In:map”. XXVIIth General URSI Assembly,

Appendices 17-24 August, (2002). 2002. “Wide-field HIimagingwith theAustralia Telescope”. In:URSIXXVIIth GeneralAssembly, Maastricht, *McCLURE-GRIFFITHS, N.M., STANIMIROVIC, S., DICKEY, J.M.,B.M. GAENSLER, &GREEN, A.J. & Willis),(2002). theISMinGalaxies,ASP Conf. Ser., 276,58.(eds.Taylor, of HIandtheExploration Landecker Detection of *McCLURE-GRIFFITHS, theDust:The SeeingThrough In: “. N.M. GalacticPlaneSurvey Southern “The Mass., 14-17August ASPConf. Ser., 2001, (eds. 31. 271, (2002). Slane&Gaensler), Parkes inSupernova Neutron Remnants, Stars andtheirassociations”.In: MultibeamPulsarSurvey Boston, B.C., CRAWFORD, F., D’AMICO, N., POSSENTI, A., V.M., KASPI, STAIRS, I.H. “Young pulsars from the R.N.,*MANCHESTER, J.F., BELL, CAMILO, F., LYNE, M.I., A.G., KRAMER, HOBBS, G.B., JOSHI, Frequencies, Pune, Nov/Dec India, 1999,355.(eds. Pramesh,Swarup, Ghopal-Krishna), (2002). *MANCHESTER, R.N. In:IAU overview”. Universe 199:The atLow “Pulsars:anobservational Radio Rodriguez), (2002). Workshop,40”. In:NewviewsonMicroquasars:4thMicroquasars 2002,224.(eds. Durouchoux, Fuchs& *MACQUART, J.-P.,WU, K.,SAULT, R.J. &HANNIKAINEN, D.C. polarization inGRO “Circular J1655- (2002). Oxford RadioGalaxyWorkshop, 3-5August ASPConf. Oxford, 2000, Ser., (eds. 250,137. Laing&Blundell), the “Circular polarizationinscintillatingsources”.In: andFieldsinRadioGalaxies:proceedingsof Particles *MACQUART, J.-P., JAUNCEY, L., KEDZIORA-CHUDCZER, D.L., SAULT, &RAYNER, R. D.P. Slane Gaensler),(2002). supernova remnantshocks”.ASP Conf. In:Neutronstarremnants Series, 271,399.(eds. diagnostics of LAZENDIC, J.S.,WARDLE, M.,GREEN, A.J., WHITEOAK, J.B. &BURTON, M.G., “Molecular & Willis),(2002). theISMinGalaxies,ASP Conf. Ser., 276,72.(eds.Taylor, of HIandtheExploration Landecker Detection of *KORIBALSKI, B.S. (HIPASS)”.The HIParkes Survey theDust: “The SeeingThrough All-Sky In: &Fich),August, (2002). 21-23 2002,59.(eds. Curry Waterloo, StarFormation, Ont., asaDiagnosticof Corona Australis cloud”.In:SFChem2002:Chemistry KONTINEN, S., HARJU, J., P., CASELLI, &WALMSLEY,A. HEIKKILA, “Dustandmoleculesinthe M. ASP Conf. Ser., (eds. 271,419. Slane&Gaensler),(2002). StarsinSupernovasupernova remnantN206”.In:Neutron Remnants, Boston,Mass.,August 14-17 2001, *KLINGER, R.J, DICKEL,J.R., FIELDS, B.D. &MILNE,D.K.“A inthe feature peculiarlinearradio et al.),(2002). Workshopgrounds: Astrophysical on Polarized (eds. 9-12October 2001,156. Bologna, Backgrounds, Cecchini *KESTEVEN, M.J. “AMiBA: Microwave for Astrophysical Array Polarized In: Anistropy”. Back- Background Blundell), (2002). GalaxyWorkshop,the Oxford Radio August Oxford, 3-5 ASP Conf. 2000, Ser., 250,128.(eds. Laing& extreme intraday variable quasarPKS0405-385”.In:Particles andFieldsinRadioGalaxies:proceedingsof TZIOUMIS,WIERINGA, M.H., A.K., PERLEY, the R.A.&REYNOLDS, J.E. monitoringof “Longterm *KEDZIORA-CHUDCZER, JAUNCEY, L., D.L., LOVELL, J.E.J., WALKER, M.A., MACQUART, J.-P., page 93

Appendices page 94 MINIER, V., BURTON, M.G. & HILL, T., “Evolutionary stagessequence for the early of & HILL, T., M.G. star massive BURTON, MINIER, V., 24-29, EDP June France, formation”. Paris, meeting, Francaise In: SF2A-2002: Semaine de l’Astrophysique Combes & Barret), (eds. 465. (2002). Ser., Conf. de Physique, Editions Sciences, M.R. “Methanol masers & PESTALOZZI, and the earliest M.G. BURTON, BOOTH, R.S., MINIER, V., stages of star formation”. massive Proceedings of 25-28 June. Symp., VLBI Network European the 6th (2002). & Zensus), Lobanov Porcas, Ros, (eds. 205. Bonn, Germany, correlation “Post RFI real-time adaptive versus M.J. & KESTEVEN, R.J. SAULT, *MITCHELL, D.A., 2002, 115. (2002). 17-24 August, Maastricht, XXVIIth General Assembly, cancellation”. In: URSI a by R. “Powered I. & DODSON, HARRUS, A., SLANE, P., GREEN, GAENSLER, B.M., D., MOFFETT, 2001, ASP 14-17 August Mass., Boston, Stars Remnants, pulsar? G291.0-0.1”. In: Neutron in Supernova (2002). Slane & Gaensler), 271, 221. (eds. Ser., Conf. “HI N. KILLEEN, & C. TADHUNTER, G., MOORSEL, VAN T., OOSTERLOO, R., *MORGANTI, India, Pune, Nov/Dec Frequencies, at Low Radio 199: Theabsorption Universe in radio galaxies”. In: IAU Gopal-Krishna), (2002). Pramesh, Swarup, 1999, 118. (eds. “A E.B. & FOMALONT, R.D. R., H.R., DE RUITER, EKERS, FANTI, P., M.,PARMA, *MURGIA, study ofmulti-frequency the radio galaxy and Fields in Radio Galaxies: proceedings NGC 326”. In: Particles Laing & 250, 380. (eds. Ser., 2000, ASP Conf. of 3-5 August Oxford, the Oxford Radio Galaxy Workshop, Blundell), (2002). century and politics in nineteenth passion, power vs Russell: Australian “Tebbutt W. *ORCHISTON, Kyoto, Historyastronomy”. IAU, of Discussion 17, 23rd General Assembly, Joint Proc. Astronomy: Oriental (2002). 169. (ed. Ansari), 1997, 25-26 August, F. & CAMILO, A.G. LYNE, J., SARKISSIAN, MANCHESTER, R.N., N., *POSSENTI, A., D’AMICO, Summer 2001 further clustersmillisecond pulsars in globular for results”. In: at Parkes: ACP “Searching 2001. (2002). Aspen , 26 June Compact Objects in Dense Star Clusters, Workshop: L. “Local column density distribution function E., WEBSTER, R. STAVELEY-SMITH, & *RYAN-WEBER, Mulcahey 254, 209. (eds. from HI selected galaxies”. Ser., ASP Conf. In: Extragalactic Redshift, Gas at Low (2002). & Stocke), structure R. “The & MORGANTI, dymanics, & history of T. SADLER, E.M, OOSTERLOO, Galaxies: A of in honour workshops Da Costa & Jerjen), 273, 215 (eds. Ser., In: ASP Conf. Freeman”. Professor Ken (2002). V., BURWITZ, V.E., ZAVLIN, GARMIRE, G.P., O.Y., KARGALTSEV, G.G., PAVLOV, D., *SANWAL, spectrum R. “X-ray pulsations and of & DODSON, MANCHESTER, R.N. pulsar”. In: Neutron the Vela Slane & 271, 353. (eds. Ser., 2001, ASP Conf. 14-17 August Boston, Mass., Remnants, Stars in Supernova Gaensler), (2002). frequency “Low planetary 199: at Radio Low radio astronomy”.The Universe In: IAU R.J. *SAULT, Ghopal-Krishna), (2002). Pramesh, Swarup, 1999, 407. (eds. India, Nov/Dec Pune, Frequencies, Radio Frequencies, at Low 199: TheUniverse “Wide field IAU frequencies”. In: imaging at low R.J. *SAULT, Ghopal-Krishna), (2002). Pramesh, Swarup, 1999, 508. (eds. India, Nov/Dec Pune,

Appendices Krishna), (2002). Low Frequencies, Radio Pune, India,Nov/Dec IAU 1999, (eds. 161. Symposim199, Pramesh,Swarup, Ghopal- Universe In:The Concentration”. theShapley at A.K. “Active remnantsinthecoreof andcandidate galaxies T.,*VENTURI, BARDELLI, S.,DALLACASA, D., HUNSTEAD, R.W., MORGANTI,TZIOUMIS, & R. Bologna, 9-12October2001,AIP Conf. Ser., 60.(eds. 609, Cecchini etal.),(2002). Astrophysical Polarized Workshopscales”. In: Backgrounds: onAstrophysical Polarized Backgrounds, J.M. &McCLURE-GRIFFITHS, synchrotron arcmin polarized N.M. emissionat galactic “Angular of spectra *TUCCI, M.,CARRETTI,E.,CECCHINI,S., NICASTRO, FABBRI, L., GAENSLER,B.M., R., DICKEY, (2002). A”. Centaurus Assembly, In:URSIXXVIIth General evolution of 17-24 August, Maastricht, 2002,2156. *TINGAY,S.J., PRESTON, JAUNCEY, R.A., D.L. &MURPHY, D.L. and structure subparsec-scale “The theISMinGalaxies,ASP Conf. Ser., (eds. 68. 276, Taylor, of the Exploration (2002). LandeckerWillis), & LOCKMAN, HIand F.J. Detectionof The theDust: “. In:SeeingThrough VLAGalacticPlaneSurvey “The *TAYLOR, J., STIL, A.R., DICKEY, J., McCLURE-GRIFFITHS, N.M., MARTIN, P.,ROTHWELL, T. & Assembly,August Maastricht, (2002). 17-24 2002,710. *SUBRAHMANYAN, &EKERS, R. R.D. usingtheSKA”. “CMBobservations In:URSIXXVIIthGeneral Anistropies,Missing Baryons, andCMB ASP Conf. Ser., 257,251. (eds. Chen etal.),(2002). *SUBRAHMANYAN, theCMB withtheAMiBA”. R.“Observing AMiBA In: 2001:High-Z Clusters, and CMBAnistropies, ASPConf. Ser., 257,289. (eds. (2002). Chenetal.), *SUBRAHMANYAN,“ATCA R. AMiBA High-ZClusters, In: 2001: andCMBanisotropies”. MissingBaryons, AIP Conf. Ser., 616,102.(eds. DePetri (2002). &Gervasi), atMillimetreWavelengths,Experimental Cosmology Valle Breuil-Cervinia, d’Aosta,Italy, 9-13July, 2001, *SUBRAHMANYAN, 2K1BCWorkshop “Cross-talkinclosepacked In:The R. interferometer arrays”. on Krishna), (2002) Radio Frequencies, PuneIndia,Nov/Dec1999, IAU 58.(eds. Symposium199, Pramesh,Swarup, Ghopal- *SUBRAHMANYAN, Universe “Cosmicmicrowave R. Low The low at frequencies”.In: at background ASP Conf. Ser., (eds. 276,391. Taylor, Landecker (2002). &Willis), theISMinGalaxies, Penticton, B.C., HIandtheExploration 20-25October2001, of Dust: theDetectionof the SeeingThrough In: Cloud”. Magellanic theLarge *STAVELEY-SMITH, of scalestructure large L. “The (eds. &Reid), (2002). Migenes Cosmic Masers: From ProtostarstoBlack Holes, RiodeJaneiro, 4-11March 2001,IAU Symposim206,179. E.C., WATSON, W.D., ELLINGSEN, S.P. In: IImethanolmasers”. class &CASWELL,J.L. “Modelsof *SOBOLEV, OSTROVSKII, A.M., A.B., MALYSHEV, A.V., CRAGG, D.M., GODREY, P.D., SUTTON, France, 23-27July,ASP Conf. 2002, Ser., 290,45. (eds. Collin,Combes&Schlosman), (2002). Activeradio jets”.In: GalacticNuclei: From CentralEnginetoHostGalaxy, Meudon, of Chandra survey J.E.J., JAUNCEY, D.L., PERLMAN, E.S., MURPHY, D.W. & PRESTON, “ResultsR.A. a from complete *SCHWARTZ, D.A., MILLER, H.L., B.P., MARSHALL, WORRALL, D.M., BIRKINSHAW, M., LOVELL, Polarized (eds. 9-12October2001, 150. Backgrounds, Bologna, Cecchini etal.),(2002). Telescope Polarized Workshop In:Astrophysical Backgrounds: CompactArray”. onAstrophysical *SAULT, R.J., RAYNER, D.P. &KESTEVEN, M.J. withthe Australia andwidefieldpolarimetry “Precision page 95

Appendices , 2002 , 2002 , 2002 , 2002 , 2002 TNF TNF TNF TNF TNF page 96 vised by the A vised by the A vised by the A vised by the A vised by the A -super -super -super -super -super Theses of students co Theses of students co Getts, T., “Dynamical study of “Dynamical T., Getts, southern Macquarie University interacting galaxies”, MSc thesis, M., “Molecular spectral line observationsHunt, of sourthern PhD thesis, molecular clouds”, ofUniversity Sydney Western astrometry of “Accurate ofLegge, University southernD., radio pulsars”, PhD thesis, Sydney galaxies “Nearby in the Zone of ofS., Juraszek, University PhD thesis, Avoidance”, Sydney into radio emission from SNR 1987A in investigation models and an “Hydrodynamical Wheaton, V., of University the Large Magellanic Cloud”, MSc thesis, Sydney Theses of students co VENTURI, T., BARDELLI, S., HUNSTEAD, R.W. & MORGANTI, R. “The & MORGANTI, effects of R.W. cluster mergers on HUNSTEAD, S., BARDELLI, VENTURI, T., the properties of radio galaxies”. Presented at Cluster Mergers Sources: to Radio and their Connection 24th England. In: Highlights of 2000,Manchester, 10, 7- 18 August Discussion Joint meeting of the IAU, (2002). (ed. Rickman), 12, 536. Astronomy, R. “Radio M., from emission PRANDONI, I. ZAGARIA, & MORGANTI, S., BARDELLI, VENTURI, T., with Galaxy Evolution Cosmic the A3571 cluster complex in the Shapley Concentration “. In:Tracing Borgani, 268, 455. (eds. Mezzetti & Valdarnini), 2000, Ser., ASP Conf. Sesto Pusteria, 2-7 July Clusters, (2002). “The COMASTRI, R. A., & VIGNALI, C. MORGANTI, PELLEGRINI, accretion S., VENTURI, T., ofthe nucleus in process the radio galaxy PKS1333–33”. of In: Proceedings VLBI Net- the 6th European & Zensus), (2002). Porcas Ros, Symposium, 165. (eds. work A.J., GREEN, R.G., CRAM, L.E., DAVISON, D., CAMPBELL-WILSON, J.D., BUNTON G.B., *WARR., & SADLER, E.M. “Prototyping SKA technologies at A.J. PARFITT, MITCHELL, D.A., R.W., HUNSTEAD, on Applications of 20-22 2002), Leura, radio telescope”. In: Workshop the Molonglo Radio Science (WARS 2002. February, TEAM “The cosmological R.L. & HIPASS WEBSTER, L., MEYER, M.J., M.A., STAVELEY-SMITH, ZWAAN, mass density of Astronomical Society Meeting 201.American (2002) neutral gas from HIPASS”, Theses of students co Theses of students co

Appendices co co H: H: Name, projecttitleandaffiliation Name, projecttitleandaffiliation As ofDecember2002 As ofDecember2002 Name, projecttitleandaffiliation Melbourne theFornaxWaugh, cluster”,University of Meryl “Galaxypopulations, dynamicsandevolution of Australian University nearby galaxies”, National highHImass-to-lightradiofield Warren, Bradley of Nature “The Australian University National diskgalaxies”, thinedge-on darkhalosof Jess theshapeof O’Brien,“Probing Sebastian Gurovich, “Investigating theBayonic Tully-Fisher Australian relationship”, NationalUniversity region withsensitive data”,Australian radio National University FieldSouth Deep intheHubble galaxies of history thestarformation Minh Hyunh, “Constraining Sydney inradioastronomy”, UniversityDaniel Mitchell, mitigation of “Interference Tasmania young pulsars”, University of Dion Lewis, “Timingof Montreal,Canada University spheroidal galaxies”, of Antione Bouchard, for “Search HIindwarf Melbourne thelocalUniverse”, University of Emily Ryan-Weber, functionof “Columndensitydistruction Bonn,Germany University of system andotherhigh-velocity theMagellanic clouds”, of arms gaseous “The Christian Bruens, Sydney Paul Roberts, inradioastronomy”, “Componentsforwidebandwithsignalprocessing University of Wollongong University Bridge”, theMagellanic of of Erik Muller, kinematicsandstructure “The Sydney supernova remnantshocks”, University of Jasmina Lazendic, of “Moleculardiagnostics Adelaide University of Melanie Johnston-Hollitt, through Faraday “Examiningmagneticfields rotationmeasures”, Adelaide blazars”,University of Hayley Bignall,“Multiwavelength studiesof Queensland University galaxies”, of Boris Babic, “Massdistributionsinrich clustersof Queensland A multiwavelength ininteractinggalaxies: study”,UniversityScott Gordon,“Starformation of Western Australia University of timedseriesanalysis”, Matthew Young, usingimproved pulsardynamics “An methodsof investigation of As ofDecember2002 co H: Name, projecttitleandaffiliation Name, projecttitleandaffiliation As ofDecember2002 As ofDecember2002 co co H: H: -super -super -super P P -super -super P P P ostgraduate students ostgraduate students ostgraduate students ostgraduate students ostgraduate students vised bytheA vised bytheA vised bytheA vised bytheA vised bytheA page 97 TNF TNF TNF TNF TNF

Appendices page 98 Rachel Deacon, “Planetary Deacon, Rachel - origin of nebulae morphology”, of University Sydney observationAidan Hotan, “Pulsar of and timing”, Swinburne University Technology Gianni Bernardi, radiation as foreground polarised CMB experiments”, synchroton “Diffuse Galactic for ofUniversity Bologna/CNR, Italy of pulsars”, Swinburne for millisecond Knight,“Baseband searching University Haydon Technology of evolution “Galatic distribution and Vranesevic, Natasa of pulsars”, University Sydney Ricci, “TheRoberto frequency Compact Array high radio sky Italy survey”, SISSA/ISAS, “High dynamic range synthesis interferometry”, imaging with many baseline Aaron Chipendale, ofUniversity Sydney “Intermediate Drake, Catherine National University IRAS galaxies”, radio-loud Australian

Appendices I: Abbreviations I: Abbreviations INeutralHydrogen. HIParkes Survey. AllSky MobilityTransistor. HighElectron Gamma-rayBurst. GalliumArsenide. Flexible Transport Image System. EqualEmployment Opportunity. Focal-planeAccess andYield. forRadioAstronomy: Design, Arrays HIPASS HI HEMT GRB Caltech-Parkes-Swinburne Recorder. Group. ComputerServices GaAs FITS FARADAY CommitteeonSpaceResearch. Association. Berkeley-Illinois-Maryland EEO Australia Telescope Committee. Users Australia Telescope Facility. National CTIP Australia Telescope CompactArray. CSIRO CPSR Australian Research Council. Committee. Australian SKAConsortium CSG Asia-Pacific Telescope. COSPAR Microwave for Array BIMA Anisotropy. Background Array. Millimetre AtacamaLarge ATUC ProcessingSystem. Image Astronomical ATNF L-bandFeed Arecibo Array. ATCA AsymptoticGiantBranch. ASKACC Australian Communications Authority. ARC Telescope. Anglo-Australian APT Observatory. Anglo-Australian AMiBA ALMA AIPS ALFA AGB ACA AAT AAO I: Abbreviations I: Abbreviations I: Abbreviations of CSIRO partly co-locatedwiththeATNF. CSIRO partly of CSIROTelecommunications andIndustrialPhysics –aDivision Commonwealth andIndustrialResearch Scientific Organisation. page 99

Appendices page 100 adio Astronomy Frequencyadio Astronomy Committee in the Asia Pacific Region. Major National Research Facilities. Major National Research agency. SEARFESESTSGPSSISSKASUMSSTAC Radio Environment. Frequency Students Exploring Australia’s TCSURSI (Chile). Submillimetre Telescope Swedish-ESO USNO Southern Galactic Plane Survey. VLBIVSOP Semiconductor-Insulator-Semiconductor. SquareWMAP Kilometre Array. Sky Molonglo Survey. University Sydney WRC Time Assignment Committee. ZOA Control System. Telescope International Union of Radio Science. Observatory. United States Naval Long Baseline Interferometry. Very VLBI Space Observatory Program. Anisotropy Probe. Wilkinson Microwave Radiocommunication Conference. World Zone of Avoidance. IAUISMITITUIUCAFJIVELBALOLOFAR International Union. Astronomical MIRIAD Interstellar Medium. MMIC Information Technology. MNRF Union. International Telecommunications Commission for the Allocation of Inter-Union Frequencies. NASA Institute for VLBI in Europe. Joint OECD VLBI observations. used for Australian Long Baseline Array, OMT Frequency Array. Low Local Oscillator. PPARC Multichannel Image Reconstruction Image Analysis and Display. RAFCAP Integrated Circuit. Microwave Monolithic National Aeronautics and Space Administration. The US space Organisation for Economic Cooperation and Development. Orthomode Transducer. Council. Research and Astronomy Physics Particle R

Appendices