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ATNF News
Issue No. 65, October 2008 ISSN 1323-6326


ATNF outreach
Rob Hollow (ATNF)

PULSE@Parkes project
The PULsar Student Exploration online at Par kes (PULSE@Par kes) project is now up and r unning successfully on a regular basis. We host one high school per month at Mar sfield for student obser vations. Schools receive a preobser ving visit by a project staff member to learn about radio astronomy, pulsar s and what an obser vation session involves. A successful demonstration session involving 15 students from three Per th schools was held at the SPICE Centre at the Univer sity of Western Australia in March 2008. Talks about the program were presented at the American Astronomical Society/ Astronomical Society of the Pacific Joint Meeting in St Louis in the USA in June 2008, as well as the Astronomical Society of Australia annual meeting in Per th, the national science teacher s' conference, CONASTA, in Queensland in July 2008 and the NSW Science Teacher s' Conference in late November 2008. ATNF's Education Officer, Rob Hollow visited the Univer sity of Texas, Brownsville in June as par t of the project collaboration. He spent a week at their Summer School for High School Students presenting several sessions and learning more about the programs r un there including the Arecibo Remote Control Centre. For more information visit the project webpage: http://outreach.atnf. csiro.au/education/pulseatparkes/

Students from Caroline Chisholm College observing for the PULSE@Parkes project. Photos: Robert Hollow, CSIRO

Cover page images
Photo: David McClenaghan, CSIRO (See page 9) Photo: Carole Jackson, CSIRO (See page 9) Image: Emil Lenc, CSIRO and Steven Tingay, Curtin University of Technology (See page 23) Image: Richard Dodson, University of Western Australia (See page 26)
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Contents
ATNF outreach ........................................................................................................................ 2 From the Director .................................................................................................................. 4 Dr John Paul Wild AC CBE MA ScD (Cantab.) FRS FTSE FAA 17 May 1923 ­ 10 May 2008................................................................................................. 5 Parkes achieves world-beating pulsar timing precision .................................................. 6 ASKAP update ......................................................................................................................... 9 New Postdoctoral Fellows and Research Scientist ......................................................... 12 ATNF Graduate Student Program ...................................................................................... 13 ATNF distinguished visitors .................................................................................................. 14 8th ATNF Synthesis Imaging School ..................................................................................... 14 Twenty years of the Compact Array ................................................................................... 16 Memorandum of Understanding (MOU) ........................................................................... 19 The scattered debris of the Magellanic Stream................................................................ 20 The nuclear region of NGC 4945 revealed ...................................................................... 23 Polarisation obser vations with the LBA ............................................................................ 26 ATNF Operations ................................................................................................................... 28 ATNF Science Operations .................................................................................................... 29 Time assignment information ............................................................................................... 30 ATNF Engineering Operations............................................................................................. 31 ATNF publications list ............................................................................................................ 32 ATNF outreach ........................................................................................................................ 38

Editorial
Regular reader s of the ATNF News will not have failed to notice that this is the fir st issue in our new format, with the adoption of a standardised CSIRO format for the design and layout. This year also mar ks a change from three to two issues a year, nominally in April and October. This issue contains an obituar y for Dr Paul Wild, who passed away in May 2008. Paul Wild was instr umental in the design and establishment of the Culgoora Solar Radio Obser vator y in the 1960's, ser ved as Chief of the Division of Radiophysics in the 1970's, and was Chairman of CSIRO from 1978 to 1985. The Culgoora Obser vator y is now home to the Australia Telescope Compact Array (ATC A), and elsewhere in this issue Helen Sim looks back over 20 year s of the ATC A and identifies a number of its strengths and successes. One of the strengths is the solid grounding students receive in obser ving with the ATC A, and Phil Edwards repor ts on the 8th Synthesis Imaging School at the ATC A . A repor t on the Par kes Pulsar Timing Array, and ar ticles describing studies of the Magellanic Stream, the starbur st galaxy NGC 4945, and polarisation obser vations with the Long Baseline Array, illustrate the breadth of science being under taken with ATNF facilities. The recent changes to the str ucture for managing telescope operations are outlined, and ongoing planning for future operations, incorporating ASKAP, are presented. This issue is the last with Mar y Mulcahy at the helm as Mar y will move on to a new position in another division of CSIRO in the new year. We thank Mar y for her enthusiasm and attention to detail in her role as ATNF Communications Manager. Mary Mulcahy and Jo Houldsworth The ATNF Newsletter Production Team (newsletter@atnf.csiro.au)

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N

EWS

From the Director
Brian Boyle CSIRO ATNF Director

As I write this I am struck by a tremendous sense of what has been achieved in Australian radio astronomy during 2008 by ATNF and CSIRO more broadly, together with our many partners.
The list of specific milestones that come to mind includes the following: · Duringthefir sthalfoftheyearthere was a specific focus on proactively engaging with the ATNF user community to discuss the plans for changes to ATNF operations. The need for change is undeniable given the commitment to operating a new wor ld-class obser vator y, the Australian Square Kilometre Array Pathfinder (ASKAP), in a few year s time in an environment where costs are growing faster than recurrent funding. The engagement with the community involved significant effor t from a number of senior ATNF staff, including roadshows to most major cities in Australia to engage with our user base to discuss planned operational changes, the development of a set of Science Priorities for the ATNF telescopes for the 2010­2015 period, the development of the User Policy for ASKAP, and the call for Expressions of Interest for the major Sur vey Science Projects for ASKAP. Together these effor ts have been ver y positive in securing a strong and healthy engagement between ATNF and the astronomy community. The response to the call for Expressions of Interest in ASKAP sur vey science has provided an outstanding demonstration of the vibrancy of the international astronomy community,
4 ATNF Ne ws , Issue 65, October 2008

and of the potential for ASKAP to deliver groundbreaking science. Thir ty eight expressions of interest have been received, from a total of 608 investigator s (354 independent) based in 23 countries. Over the coming weeks these will be assessed, and then invitations will be extended to groups to develop full proposals. Given that it is likely that there will be just five or so ASKAP sur vey science projects over the fir st five year s of operation, this degree of interest at this ear ly stage augur s well for great science. · From1July2008theorganisationof ATNF Operations changed from a strong obser vator y alignment to a "Science Operations" and "Engineering Operations" str ucture that extends across all ATNF obser vatories, and which will include ASKAP once scientific operations begin in 2012. The new str ucture is already resulting in a positive sharing of knowledge across the wide range of ATNF activities. The transition from leader ship by our excellent Officer s in Charge, John Reynolds (Par kes) and Phil Edwards (Narrabri) to the Head of Engineering Operations, Brett Dawson, and of Science Operations, Phil Edwards, has been effected seamlessly. · InAugusttheASKAPteamachieved fir st light with the chequerboard Phased Array Feed designed by John O'Sullivan on the newlycommissioned 12-m testbed antenna at Par kes. The results were and continue to be ver y encouraging, with a remar kable degree of agreement between the measured and predicted performance which under lines the team's deep under standing of the physics of these systems. While there are still many challenges to

be solved with these systems the results achieved to date are ver y promising and indicate the retirement of some of the greatest technical risk involved in the ASKAP project. · The signing of the ASKAP antenna contract with CETC54 was another major milestone for the year. CETC54 will deliver thir ty six 12-m antennas, including an innovative third rotation axis judged necessar y to achieve the ver y high dynamic range target for ASKAP, for under A$10M meeting a cost target considered by many to be a major commercial challenge for the project, and even for the SKA itself. · Morebroadly,theAustralianSKA Industr y Cluster has played a key role in fur thering industr y par ticipation in the ASKAP project. A number of strategic par tner ships have been forged, and the release of the Industr y Oppor tunities Register in October was a significant highlight. · Theapprovalon3Decemberin the Australian Federal Par liament of the expediency motion for the constr uction of ASKAP following the completion of its consideration by the Par liamentar y Standing Committee for Public Wor ks (PWC) amounts to the "green light" for the star t of constr uction. The PWC submission involved a great deal of effor t across CSIRO, with suppor t from the Commowealth and WA State governments. It stands as a testament to the ability of CSIRO to under take large, unique, capital intensive scientific developments in Australia. Moreover, it ser ves as an appropriate conclusion to a highly successful year for "Team Australia" which began with the highly successful international SKA For um in Per th.


Dr John Paul Wild AC CBE MA ScD (Cantab.) FRS FTSE FAA 17 May 1923 ­ 10 May 2008
Geoff Garrett, CSIRO Chief Executive

· Thecontinuedsuccessfuldevelopment and testing of the Compact Array Broadband Backend (C ABB) correlator during 2008 has been ver y pleasing. Recent months have been regular ly punctuated by repor ts of the progressive solution of technical challenges, and of successful tests of an increasingly capable system. Once operational, C ABB will revolutionise the scientific capability of the Compact Array and maintain its competitiveness in the Expanded Ver y Large Array (EVLA) and the Atacama Large Millimeter Array Project (ALMA) era. The fact that these milestones, have been achieved while continuing to operate three ver y complex scientific obser vatories 24 hour s a day, 7 days a week, facilitating the remar kable scientific discoveries outlined in this newsletter and detailed elsewhere , is a tribute to the effor ts of all the staff involved within ATNF and elsewhere in CSIRO. The scientific productivity of the ATNF's telescopes remains outstanding, and the ar ticles in this Newsletter give a taste of the quality of the science that continues to be delivered through the exper tise of the user s of the ATNF. Finally I'd like to welcome all the new appointees to the ATNF, some of whom are featured in this newsletter. The ATNF has an outstanding pool of talent in its staff and its greatest strength derives from the knowledge and dedication of those people, be they engineer s, scientists, technicians or exper ts in some other area that is integral to achieving CSIRO's goals in the field of radio astronomy. Best wishes to ever yone at the end of 2008, and here's to a happy and prosperous 2009.

CSIRO deeply regrets the passing of Dr John Paul Wild, distinguished scientist and former Chairman of CSIRO. Dr Wild died on Saturday, 10 May 2008.
Dr Wild was one of Australia's most respected and inspirational scientist and engineer s. Dr Wild was best known for his contributions to Solar Science. He was par t of the team that built and operated the original solar radiospectrographs and later the Radioheliograph at Culgoora in NSW. The Radioheliograph was a ground breaking instr ument producing real time images of solar activity across a range of altitudes from the sun's surface. In the late 1960's and ear ly `70's the Culgoora group led the wor ld in solar research attracting prominent solar physicists from around the wor ld. Dr Wild successfully applied his considerable initiative and exper tise to the development of ground breaking technology for industr y and the community. As Chief of the CSIRO Division of Radiophysics from 1971 until 1978 he led the team that developed the Inter scan aircraft landing system that was adopted in 1978 as the international standard. Colleagues appreciated his generosity in sharing ideas. He was extremely approachable and had the magical ability to reduce the most complex of concepts to simple terms under stood by all. His colleagues appreciated the fact that when these concepts were realised in practice he never failed to acknowledge the role they played in developing them. Dr John Paul Wild Photo: CSIRO As Chairman of CSIRO from 1978 to 1985, Dr Wild was a national science leader. He led the Organisation through the restr ucture designed in 1978 to modernise the Organisation and bring it closer to the industries and community which it ser ves. He recognised that CSIRO needed to adapt and provide scientific and technological leader ship in a changing wor ld. And, as he wrote in 1984 "Yet, whatever the changes, one characteristic must remain inviolate: a high standard of excellence and originality. Without excellence and originality, research achieves nothing." During this period he was instr umental in securing funding for major national research facilities including the oceanographic research vessel, the Australian Animal Health Laborator y and the Australia Telescope, and he established a new Division of Information Technology. He has left a rich inheritance which will continue to bring enormous benefits to Australia. On behalf of his colleagues and friends at CSIRO, I would like to extend our condolences and best wishes to his family and friends.

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Par kes achieves wor ld-beating pulsar timing precision
Dick Manchester (ATNF)

The Parkes radio telescope has a well-founded reputation for pulsar astronomy, with about two-thirds of the approximately1800 known pulsars having been discovered there. While discovering pulsars is important, the most significant science comes from the followup studies, especially pulse timing observations. Now Parkes can lay claim to achieving world-beating pulsar timing precision using the Pulsar Digital Filterbank (PDFB) systems developed at ATNF.
Pulsar s are remar kable objects, tiny spinning neutron star s formed in supernova explosions at the death of massive star s. They have super-strong magnetic fields and the combination of this with ver y rapid rotation ­ the fastest known pulsar spins 716 times ever y second ­ means that pulsar s are highly efficient dynamos, generating enormous electric fields in the "magnetosphere" surrounding the neutron star. These electric fields accelerate charged par ticles to ultra-relativistic energies resulting in the emission of powerful beams of

radiation. These beams sweep across the sky as the star spins, generating a periodic train of pulses for any obser ver in their path. Because of the huge moment of iner tia and small radius of a neutron star, the pulse periodicity is extraordinarily stable, making pulsar s mar vellous celestial clocks. Timing of pulsar s has many applications ranging from studies of neutron-star interior s to testing of theories of gravitation. Pulsar timing can also be used to establish a so-called "pulsar time" and to check for irregularities in the international timescales based on atomic clocks. Although pulsar timing obser vations were made over many year s at Par kes using the analogue filterbank systems used for pulsar searches, precision pulsar timing really began in 1993 with the Fast Pulsar Timing Machine, a collaborative effor t between Caltech and ATNF. Since then, several generations of baseband recording systems giving increasing timing precision have been developed in collaboration with Swinburne Univer sity of Technology and used, especially for pulsar astrometr y and the study of binar y pulsar s. In 2003, the Par kes Pulsar Timing Array (PPTA) project was established with the principal goal of making a direct detection of gravitational waves using pulsar timing. To have a chance of reaching this ambitious goal, regular obser vations of at least twenty millisecond pulsar s over 5 ­ 10 year s with unprecedented timing precision are required. In order to reduce the per turbing effects of propagation through the inter stellar medium, obser vations at relatively high radio frequencies are best for precision

Figure 1: Greyscale plot of intensity of PSR J0437-4715 as a function of pulse phase and frequency. The one-hour obser vation was made on 6 September 2008 using the 10-cm receiver with a total bandwidth of 1024 MHz and PDFB2 in folding mode. The plot is of the raw spectral data and has been clipped at 20% of the peak to better show the low-level structure.

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pulsar timing. But pulsar s, especially millisecond pulsar s, are relatively weak and steep-spectr um radio sources, so wide bandwidths are required to give the necessar y sensitivity and radio frequencies of a few GHz are optimal. The 10/50-cm receiver was designed with these ideas in mind, with the 10-cm system having a bandwidth of 1 GHz between 2.6 and 3.6 GHz. Such bandwidths place severe demands on the signal processing system. The PDFB system was designed to meet this challenge . It has 8-bit digitisation of either two or four input signals and a maximum bandwidth of 1024 MHz. A polyphase filterbank is used to split each input signal into a maximum of 2048 frequency channels. Channel outputs are correlated to give four polarisation products per channel. These are then synchronously folded at the apparent pulsar period and integrated in a pulsar binning memor y with a maximum of 2048 bins per period. These maximum specifications can be reached for pulsar s with periods of four milliseconds or more . The system is based on the signal processor board developed for the Compact Array Broadband Backend (C ABB) system which contains 10 high-performance Field Programmable Gate Array (FPGA) chips and a large amount of memor y. The PDFBs have several modes of operation. Normally they are used with two inputs to produce full-polarisation pulse profiles in each channel across the band. Figure 1 shows a typical obser vation of the strong southern millisecond pulsar, PSR J0437-4715, illustrating the high time and frequency

resolution of the obser vations. They can also operate in "search" mode where data from each frequency channel is integrated for a time, typically 100 microseconds, and then dumped to disk, and in spectral-line mode which is similar except that integration times are typically longer. For fold-mode and search-mode data, files are written in PSRFITS format, whereas spectral-mode files use RPFITS format. The PDFB system can also operate as a front-end for the next-generation baseband system, ATNF Par kes Swinburne Recorder (APSR), currently being developed in conjunction with Swinburne Univer sity of Technology. A system for real-time mitigation of

radio frequency interference (RFI) using adaptive filtering is also provided. To determine pulse times-of-arrival (TOAs), the calibrated total intensity pulse profiles are correlated with a standard profile template giving the phase of a reference point on the template relative to the star t time of each obser vation. These TOAs are then corrected for offsets in the Par kes time system and for delays due to inter stellar disper sion. These are then referred to solar-system bar ycentre, correcting for both the propagation time and the change in gravitational potential, giving infinite-frequency TOAs in what

Figure 2: TEMPO2 plot of post-fit timing residuals over one year for 10-cm observations of PSR J0437-4715 using PDFB2. There are a total of 147 TOAs, each from a 1-hour observation, and a total of 10 model parameters were fitted for.

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is assumed to be an iner tial reference frame. These TOAs are then compared with predicted TOAs based on a model for the pulsar, including its position, proper motion, pulse frequency and its derivatives and binar y parameter s if appropriate . The difference between the obser ved and predicted TOAs are known as timing "residuals" and are the basic product of pulsar timing. Systematic variations in these residuals can be used to improve the parameter s of the pulsar model and to search for un-modelled effects such as relativistic per turbations in binar y parameter s or pulse frequency per turbations due to gravitational waves passing over the pulsar or the Ear th. To make a significant detection of the stochastic gravitational-wave background in the Galaxy, we need to have rootmean-square (rms) timing residuals of order 100 nanoseconds for most of our sample . This is a ver y demanding requirement which has not even been approached in previous pulsar timing obser vations. However with the PDFB systems we are approaching this level of precision. Figure 2 shows our best result to date , an unprecedented 56 nanosecond rms timing residual over one year for PSR J0437-4715 using the 10-cm receiver and PDFB2. Data processing made use of the PSRCHIVE and TEMPO2 software systems. While our current results constitute the most accurate pulsar timing results ever obtained for such a large pulsar sample , they are not yet sufficiently precise to detect the predicted gravitationalwave background in the Galaxy. We are continuing to wor k on removal of systematic error s in the data and on improving our processing algorithms. We have also established collaborations with the European and Nor th American pulsar timing array projects (EPTA and NANOGrav, respectively) to form Figure 3: Commissioning of the five export PDFBs at Parkes on 13 October 2008. From left, the people are Hongfei Liu (National Astronomical Observatories, Chinese Academy of Sciences (NAOC), Beijing), Zhiyong Liu (NAOC, Urumqi Observatory), Tim Ikin (Jodrell Bank Centre for Astrophysics, University of Manchester), Maozheng Chen (NAOC, Urumqi Observatory), Dick Manchester (ATNF), Andrew Brown (ATNF), George Hobbs (ATNF) and Warwick Wilson (ATNF). Photo: John Sarkissian, CSIRO

the International Pulsar Timing Array (IPTA). The increased sky coverage and number of obser vations afforded by the IPTA will considerably enhance the chances of a successful detection of gravitational waves. Looking fur ther into the future, the enormous sensitivity of the Square Kilometre Array will allow obser vations of a much larger sample of pulsar s, making possible not only detection of gravitational waves, but detailed study of both the waves and the sources that emit them. The outstanding performance of the PDFB systems is a tribute to the ATNF engineer s and scientists who designed and constr ucted them. As an illustration of the impact of the development

of these systems, the ATNF has just completed constr uction and testing of five systems under contract to other obser vatories around the wor ld, three in Europe and two in China. Before shipment, these systems were all tested at Par kes. Figure 3 shows five systems in the Par kes tower with the team of ATNF and visiting engineer s and scientists involved in the commissioning. The design and constr uction of the PDFB systems was led by ATNF engineer s Grant Hampson, Andrew Brown and Warwick Wilson, with major contributions from John Reynolds, Evan Davis, Paul Rober ts, Michael Kesteven and Mar k Calabretta.

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ASKAP Update
Diana Londish (ATNF)

Commonwealth Parliamentary Standing Committee on Public Works
The Commonwealth Par liamentar y Standing Committee on Public Wor ks is tasked with reviewing proposed expenditure of public money, and preparing and presenting repor ts and recommendations for Par liament. Documentation on the Australian Square Kilometre Array Pathfinder (ASKAP) was submitted by CSIRO to the committee in June 2008 and the in camera and public hearings took place on 1 October in Geraldton. The Committee's repor t was tabled in the Commonwealth Par liament on 1 December, expressing suppor t for the ASKAP project as par t of the continued development of radio astronomy in Australia. The motion was approved by Par liament on 3 December.

ASKAP Science
An ASKAP User Policy Taskforce has been set up to determine access policies for both large sur veys and small general science experiments. Issues dealt with include user suppor t, open access policies, and the interaction with the international Vir tual Obser vator y community. A wor kshop to discuss synergies between proposed ASKAP sur veys and planned optical and infrared sur veys was held in Melbourne from 24 ­ 26 September, hosted by Swinburne Univer sity of Technology. A call for Expressions of Interest (EoI) to be involved in designing and implementing an initial set of Sur vey Science Projects for ASKAP was issued on 1 November, with submission deadline 15 December. This has resulted Above: The 5x4 chequerboard-design phased array feeds installed at the focus of the Parkes Testbed Facility antenna. Photo: David McClenaghan, CSIRO in 38 submissions from Principal Investigator s in10 different countries. Information relating to ASKAP science, call for EoIs and User Policy can be found on the ASKAP web pages at http://www.atnf.csiro.au/projects/askap/ Below: ASKAP team members enjoy a 3-D show of the antenna build process. (See also front cover.) Photo: Carole Jackson, CSIRO Wide-field Array (MWA) project and the old MWA caravan was removed. Other upgrades and activities included placement of a por table generator for temporar y additional power, upgrading of air-conditioner s on the MWA hut, dressing of cables to MWA tiles, installation of additional receiver s in the MWA hut to suppor t more tiles (up to 32), installation of beamformer s, testing of the 8-tile (8T) system and general data collection. By the end of November, 26 MWA tiles were operational, and

MRO
At the end of September a new temporar y hut was deployed on site at the Murchison Radio-astronomy Obser vator y (MRO) for the Murchison

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the remaining six tiles will be brought on line in Januar y. Following the installation of the system test science obser vations were made of the Sun, and the data were processed at Cur tin Univer sity of Technology in Per th.

review (CDR) was held 17-19 December, in China at CETC54's premises.

Parkes Testbed Facility
The ASKAP project has developed the Par kes Testbed Facility (PTF) based on a 12-m diameter prime focus antenna built by Patriot Antenna Systems at Par kes Obser vator y. Its purpose is to test the CSIRO-developed phased array feeds (PAF). The Par kes 64-m dish provides a platform for deeper, more sensitive testing of the PAF in tandem with the PTF. The PTF pedestal houses an ASKAPstyle beamformer, antenna control and monitoring systems. In addition a trial forced-air ventilation system was installed, providing cooling to these sensitive components. In mid-May a group of 30 ASKAP team member s travelled to Par kes to view the PTF and plan for the PAF tests. As well as being able to check out the antenna and the facilities installed at Par kes to suppor t the PTF (including a new RFI-screened room in the woolshed), the team enjoyed the 3-D show of the antenna build process and a "hay ride" on the 64-m dish capped off the day. A major milestone was reached on 24 July when the fir st prototype PAF was hoisted onto the antenna, and testing began the following Sunday. On Tuesday 29 July the team captured signals from eight of the total 40 por ts and "fir st light" was thus declared. Testing of the PAF, as well as the analogue, digital and computing systems is continuing. In September this included interferometr y between the 12-m dish and the Par kes 64-m dish using all 40

elements of the PAF, a major step in demonstrating that the array performs as expected. The PAF was returned to Mar sfield in late November for refitting with upgraded components.

RQZ
Fur ther protection for the MRO radio-quiet zone (RQZ) was put into place during 2008 with the Western Australian (WA) government adopting the technical standards and assessment procedures recommended by CSIRO to manage its declared Mineral Resource Management Area (MRMA) under the WA Mining Act. The conditions require the licensee or lessee of all new mining leases and licences within 80 km of the centre of the MRO to submit a plan of activities to the WA Government for approval. A duly approved Radio Quiet Management Plan must hencefor th be included with any Program of Wor k or mining proposal submitted to government, for those mining activities that fall within the MRMA zone .

Digital signal processing/Computing
The architecture for the digital system has been completed, and the team is developing the details and path to deliver y. The Concept Design Review is completed, and the Preliminar y Design Review was held on 5 December. The ASKAP project is preparing a call for Expressions of Interest to collaborate on the development of a single digital backend with the ASKAP project; this will be opened on AusTender in ear ly 2009.

Industry Engagement ramps up for ASKAP
Phil Crosby and Carole Jackson (ATNF) As ASKAP focuses on the establishment of the MRO site in readiness for the deliver y of the Boolardy Ear ly Test Array (BETA) in mid-2010, there has been a corresponding increase in industr y engagement activities over the past six months. The focus is now shifting from over view and planning briefings for industr y, to practical engagement and involvement. Highlights of the past period are: · Neworincreasedcollaborative R&D activities established with IBM, Cray, Intel, Mesaplexx and PPM. · AnSKApowergeneration wor kshop held at CSIRO Energy

Antenna tender
The ASKAP antenna Request for Tender (RFT) closed in May 2008 and a tender evaluation process was r un to the plan set out in the Tender Header Document, with visits being made to shor tlisted tenderer s. On 3 November CSIRO announced that the major contract for the antennas was awarded to the 54th Research Institute of China Electronics Technology Group Corporation (known as CETC54). CETC54 will supply thir ty-six 12-m antennas for under A$10 million, meeting a key cost target of under $300,000 per delivered antenna. A critical design

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Technology in November to examine technologies and distil options for ASKAP and SKA sustainable power requirements. The wor kshop was suppor ted by Solar Systems, Horizon, Spectrolab, Wor ley Par sons, as well as Government stakeholder s. · ASKAPhassub-contracted strategically-impor tant wor k packages to: · SKM, Par sons Brinckerhoff, and WT Par tner ships to prepare elements of the submission, design and costings for the (now successful) submission to the Par liamentar y Standing Committee for Public Wor ks; · AARNet for the design study for the fibre optic link from Geraldton to the MRO. Both of these are now complete , and planning for the next phase activities is underway.

The ASKAIC group visit the ASKAP test-bed at Parkes: left to right (as much as one can tell under the hard hats!) Davin Gibb (Cisco), Peter Elford (Cisco), Charlie Williams (RFS), Michael Matthews (RFS), Dan Credazzi (Visionstream/Leightons), Tony Combes (SGi), Shane Braendler (BAE Systems Australia), Bruce Robbins (DOIR, WA), John Reynolds (CSIRO ATNF), Dane McCormack (Boeing), John Humphreys (GIC), Chris Farrow (IBM), Glen Welby (Cicso), Matthew Francis (Telstra), Grant Wilson (DIISR), Peter Shelley (Raytheon), Brett Preisig (CSIRO ATNF), Carole Jackson, (CSIRO ATNF), Glen Wightwick (IBM), Brendan Bourke (Horizon Power), Janice Humphreys (GIC). Photo: John Sarkissian, CSIRO

· Two editions of the Australian SKA
Industr y Capabilities Director y have been published to showcase Australian based businesses with SKA relevant capabilities. The Director y is available on-line , with new businesses able to register at any time . The Director y currently has over 350 businesses registered. · ReleaseoftheASKAP Industr y Oppor tunities Register (IOR) and the companion pamphlet, the Australian Industr y Par ticipation Plan (AIPP) is also publicly available from the ASKAP website . Both have received ver y positive feedback from industr y and other stakeholder s.

in ASKAP and the SKA, continues to suppor t the project and meet regular ly to plan collaborative, selffunded activities to suppor t the Australian SKA bid. ASKAIC provides a for um for industr y engagement issues to be raised and addressed. · MinisterCarrhostedthe2nd"CEO's dinner" at Par liament House on Tuesday 11 November. Brian Boyle, Phil Crosby and Carole Jackson attended from CSIRO. Feedback has been positive, and it seems that this will now be a permanent fixture on ASKAIC's annual calendar of events. · OnMonday17November,18ASKAIC member s visited Par kes Obser vator y to view the ASKAP test-bed, the

64-m dish and hold a regular ASKAIC steering committee meeting. John Reynolds and Brett Preisig contributed to the success of this visit, showing all our visitor s the professional, dedicated obser vator y team. General industr y briefings have continued and are complemented by regular editions of the ASKAP Industr y Newsletter. Copies of all information distributed to industr y stakeholder s, presentations and updates can be found at: www.atnf.csiro.au/projects/ askap/industr y.html

· The Australian SKA Industr y
Consor tium (ASKAIC), a group of companies with a strong interest

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New Postdoctoral Fellows and Research Scientist
Robert Braun and Naomi McClure-Griffiths (ATNF)

From the top: Dr Dr Dr Dr Dr Dominic Schnitzeler, James Green, Bjorn Emonts, James Urquhart, Shami Chatterjee.

Dr Dominic Schnitzeler star ted at the ATNF on 18 August 2008 as a postdoctoral fellow. Dominic studied undergraduate astrophysics at Leiden Univer sity, where he also completed his PhD in May 2008 wor king on how Rotation Measure Synthesis can be applied to study the magnetised Galactic warm inter stellar medium (ISM). At the ATNF Dominic will wor k with Naomi McClure-Griffiths on how we can probe the Galactic magnetic field using the Zeeman effect, and he is also interested in collaborating with people who want to use Rotation Measure Synthesis. Outside office hour s Dominic can be spotted hiking in the countr yside. Dr James Green joined the ATNF on 7 August 2008 as a postdoctoral fellow. Jimi studied undergraduate astrophysics at Cardiff Univer sity, before completing his PhD in 2008 at the Jodrell Bank Centre for Astrophysics, studying high-mass star formation and Galactic str ucture through the Methanol Multibeam Sur vey. Jimi will be wor king in Naomi McClure-Griffiths's group on the Galactic distribution of regions of high-mass star formation together with their magnetic field str ucture. Jimi is an avid Liverpool Football Club suppor ter, as well as keenly pur suing a wor ldwide exploration of beer s. Jimi has moved to Australia with his wife Alison. Dr Bjorn Emonts began his Bolton Fellowship at the ATNF on 1 September 2008. Bjorn did both his undergraduate wor k and PhD research at the Univer sity of Groningen, where he completed his thesis, entitled Nearby Radio Galaxies: the interplay of gas, star formation and active nucleus, in 2006. Subsequently he was awarded a Rubicon post-doctoral fellowship to continue his research at Columbia Univer sity. At the ATNF, Bjorn

plans to concentrate on under standing the cold ISM in low- and high-redshift radio galaxies, making extensive use of the millimetre capabilities of the ATC A. Dr James Urquhar t star ted at the ATNF on 15 September 2008 as a CSIRO Office of the Chief Executive post-doctoral fellow. James completed his undergraduate wor k at the Univer sity of Sussex and went on to complete his PhD at the Univer sity of Kent, where he completed his thesis, on Radio Surveys of Triggered Star Formation within Bright-rimmed Clouds, in 2004. Since that time he has been wor king as a post-doctoral research assistant at the Univer sity of Leeds. James will be continuing his study of massive star formation in the Galaxy at the ATNF in the context of his Star Formation through Cosmic Time post-doctoral appointment, in collaboration with Kate Brooks and Rober t Braun. James has come to Australia with his par tner, Lucy, and they are looking forward to a great deal of bush-walking. Dr Shami Chatterjee began his appointment as Astrophysics Research Scientist at the ATNF on 8 December 2008. Shami completed his PhD at Cornell Univer sity in 2003 and has subsequently held a Jansky Fellowship at the Har vardSmithsonian Center for Astrophysics and National Radio Astronomy Obser vator y in Socorro and most recently a Postdoctoral Fellowship at the Univer sity of Sydney. His current research interests cover : (a) the radio transient sky, (b) compact objects: neutron star s and black holes, and (c) high precision astrometr y. He brings a wide range of interests and exper tise to our Astrophysics group and we look forward to wor king together. Please join us in welcoming Dominic, Jimi, Bjorn, James and Shami to the ATNF.

Photos courtesy of those pictured.

12 ATNF Ne ws , Issue 65, October 2008


ATNF Graduate Student Program
BÄrbel Koribalski (ATNF)

ATNF would like to officially welcome the following students into the ATNF cosupervision program:
· SarahBur ke(SwinburneUniver sity of Technology) The Symbiosis between Cosmological Evolution Models and Millisecond Pulsars with super visor s Prof Matthew Bailes (Swinburne Univer sity of Technology), Dr David Barnes (Swinburne Univer sity of Technology), Dr Simon Johnston (ATNF) and Dr Dick Manchester (ATNF). · JoanneDawson(NagoyaUniver sity) Supershells as Molecular cloud factories in the Evolving ISM with super visor s Prof Yasuo Fukui (Nagoya Univer sity) and Dr Naomi McClure-Griffiths (ATNF). · AndresGuzman(Univer sidadde Chile) Ionised jets and molecular outflows in high-mass young stellar objects with super visor s Prof Guido Garay (Univer sidad de Chile) and Dr Kate Brooks (ATNF). · AquibMoin(Cur tinUniver sityof Technology) e-VLBI science with the LB A ­ exploring science applications for the long baseline component of ASKAP with super visor s Prof Steven Tingay (Cur tin Univer sity of Technology) and Dr Chris Phillips (ATNF). · MinnieMao(Univer sityofTasmania) Cosmic Evolution of Radio Sources with super visor s Dr Jim Lovell (Univer sity of Tasmania), Dr Rob Sharp (Anglo Australian Obser vator y) and Prof Ray Norris (ATNF). · Anne-MarieBrick(Univer sity of Tasmania) Galactic Structure

and Methanol Masers with super visor s Dr Simon Ellingsen (Univer sity of Tasmania), Dr Jim Lovell (Univer sity of Tasmania) and Dr Chris Phillips (ATNF). · KateRandall(Univer sityofSydney) Discriminating between AGN and SFG in ATLAS with super visor s Dr Andrew Hopkins (Univer sity of Sydney) and Prof Ray Norris (ATNF). · ChristopherHales(Univer sityof Sydney) Radio Polarisation and the Origin of Galactic and Intergalactic Magnetic Fields with super visor s Prof Br yan Gaensler (Univer sity of Sydney), Dr Enno Middelberg (Univer sity of Bochum, Germany) and Prof Ray Norris (ATNF). · ElizabethMahony(Univer sityof Sydney) Understanding the HighFrequency Radio Source Population with super visor s Prof Elaine Sadler (Univer sity of Sydney), Dr Scott Croom (Univer sity of Sydney), Prof Ron Eker s (ATNF) and Dr Ilana Feain (ATNF). · KeithBannister(Univer sityofSydney) Archival and Future Searches for Radio Transients with super visor s Prof Br yan Gaensler (Univer sity of Sydney) and Dr Tim Cornwell (ATNF).

propagation of pulse signals in interstellar medium and their effect on the detection of gravitational waves. · JaninevanEymerenonthesuccessful submission of her Univer sity of Bochum (Germany) PhD thesis on Gas Kinematics in the Haloes of Nearby Irregular Dwarf Galaxies, and · VickySafourisonthesuccessful submission of her Australian National Univer sity PhD thesis on Environmental Influence on the Evolution of Jets from Active Galactic Nuclei. Dr Janine van Eymeren is now at the Univer sity of Manchester, UK, andDrXiaopengYouattheSchool of Physical Science & Technology, Southwest Univer sity, China.

The following students recently submitted their PhD Thesis:
· AdamDeller(SwinburneUniver sity of Technology): Precision VLBI astrometr y: Instrumentation, algorithms and pulsar parallax determination. · MarcellaMassardi(International School for Advanced Studies (SISSA), Trieste): The extragalactic sources at mm wavelengths and their role as CMB foregrounds. · EmilLenc(SwinburneUniver sityof Technology): Studies of Radio Galaxies and Starburst Galaxies using Wide-field, High Spatial Resolution Radio Imaging.

Congratulations to:
· Mar tinLeungonthesuccessful submission of his Univer sity of Sydney PhD thesis on A wideband feed for a cylindrical radio telescope. · XiaopengYouonthesuccessful submission of his Chinese Academy of Sciences PhD thesis on The

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ATNF distinguished visitor s
Robert Braun (ATNF)

8th ATNF Synthesis Imaging School
Phil Edwards (ATNF)

Over the past months we have enjoyed wor king visits from Cesar Estaban (Instituto de AstrofÌsica de Canarias), Jay Lockman (National Radio Astronomy Obser vator y), Jayanne English (Univer sity of Manitoba), Mar tin Cohen (Univer sity of California, Ber keley), Simon Driver (Univer sity of St Andrews), Peter Kalber la (Univer sity of Bonn), Patrick Hennebelle (Paris Obser vator y), D J Pisano (National Radio Astronomy Obser vator y) and Barney Rickett (Univer sity of California, San Diego). Current visitor s include Ingrid Stair s (Univer sity of British Coumbia). Upcoming visitor s we expect include Mar ta Burgay (Univer sity of Cagliari), Leo Blitz (Univer sity of California, Ber keley) and Jim Cordes (Cornell Univer sity). The Distinguished Visitor s Program remains a ver y productive means of enabling collaborative research projects with local staff, adding substantially to the vitality of the ATNF research environment. Visits can be organised for periods ranging from only a few weeks up to one year. For more information please see www.atnf.csiro.au/people/ distinguished_visitors .html. Prospective visitor s should contact the local staff member with the most similar interests.

The ATNF held its 8th Synthesis Imaging School from Monday 29 September to Friday 3 October 2008 at the Australia Telescope Compact Array (ATCA). The format was similar to previous Schools, with lectures by radio astronomers and engineers as well as practical sessions involving ATCA observing and data reduction. A total of 32 students attended the school, with about a quarter of these being members of the Australian SKA Pathfinder (ASKAP) team.
The fir st day commenced with an introduction to the ATC A by Phil Edwards, followed by lectures on the principles of interferometr y by Ron Eker s and Rick Per ley. Ron's illustration of the impor tance of phase and amplitude using Fourier transforms of a duck and a cat was par ticular ly memorable! After lunch Graeme Carrad spoke on receiver systems and Dick Ferris gave an introduction to correlator s and the Compact Array Broadband Backend (C ABB), before Ilana Feain gave an over view of ASKAP and the SKA. The day concluded with the conference dinner at the Outback Shack in Narrabri. Rober t Braun opened proceedings on Tuesday with an enter taining description of Fourier transforms, which Mar k Wieringa put into practice during talks on calibration and editing, and imaging and deconvolution. Andrew Walsh rounded out the morning with a description of spectral line obser ving. The Tuesday, Wednesday and Thur sday afternoons were devoted to tutorial sessions. During these sessions all par ticipants were given a tour of an antenna and the screened room, introduced to the ATC ASCHED scheduling tool, shown how to obser ve with the ATC A, and given the oppor tunity to reduce one (or more) example datasets. In addition, on the Tuesday afternoon Tara Murphy gave a talk on the Radio-Astronomers IT Toolkit, describing various tools and strategies for dealing with data.

Top: The wood-fired pizza oven proved a popular choice. Bottom: Andrew Walsh with a spellbound audience during his after dinner talk Complex Molecules in Space, and Can We Make Beer out of them? Photos: Joanne Houldsworth, CSIRO

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Participants and helpers from the synthesis imaging school outside the Visitors Centre in front of two antennas from the Compact Array. Photo: Jock McFee, CSIRO

Wednesday morning's program star ted with Bob Sault describing sensitivity and Steven Tingay explaining selfcalibration. After coffee , Ron Eker s gave a talk on error recognition, and Cormac Reynolds extended the imaging techniques to continental and intercontinental baselines. Wood-fired pizzas were cooked on-site Wednesday evening, and diner s enter tained by Andrew Walsh's exposition on Complex Molecules in Space , and Can We Make Beer out of them? Bob Sault introduced mosaicing on Thur sday morning, which was followed by a talk on data analysis by Naomi McClure-Griffiths. A 20th bir thday cake was wheeled in for the coffee break, and a rousing ver sion of Happy Bir thday was sung to the ATC A. After the break, Jessica Chapman introduced OPAL (Online Proposal Applications & Links) and ATOA (Australia Telescope Online Archive ) and gave some tips on proposal

writing. Dave McConnell impressed the audience with his manual dexterity in combining rotating polarisation vector s, and par ticipants literally had a ball with his example of a PoincarÈ Sphere! Rick Per ley followed Dave's introduction to polarimetr y with a more detailed study of the topic as a tutorial for the more advanced students after lunch. The School finished on Friday with an introduction to advanced data reduction by Maxim Voronkov, and a flying tour of telescopes of the wor ld by Phil Edwards. Par ticipants were then invited to complete a questionnaire on the School, with the feedback received being overwhelmingly positive. A common theme was the appreciation of lectures that were interesting and engaging, with lots of pictures and examples and containing practical advice that couldn't be learnt by simply reading a book. The hands-on experience provided by the tutorial sessions was similar ly valued.

Tutorial sessions were ably led by Christoph Brem, Kate Brooks, Jock McFee, Scott Munting, Robin War k and Tobias Westmeier, with contributions from a number of lecturer s. The effor ts of all Narrabri staff in preparing for the school and ensuring it ran smoothly are greatly appreciated, with the tireless behindthe-scenes wor k of Jo Houldswor th and Marg McFee par ticular ly notewor thy. Financial assistance from the Donovan Tr ust and Cur tin Univer sity of Technology is gratefully acknowledged. As always, a vital ingredient in the School's success was the attendance and active par ticipation of students from across Australia and from over seas. As they are representatives of the next generation of array user s, we can be confident the ATC A's future is in capable hands!

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Twenty year s of the Australia Telescope Compact Array
Helen Sim (ATNF)

The Australia Telescope Compact Array turned twenty this year. (On 2 September, to be precise.) Twenty, if you're a telescope, is a good age at which to reflect: to look both backwards and forwards. The Compact Array Science Day on 11 June 2008 largely looked to the future. But what is that future based on? Where is the Compact Array now, and where has it come from?

paper s (Tingay et al. and Schwar tz et al.) included both Ver y Long Baseline Interferometr y (VLBI) data that the Compact Array contributed to, and stand-alone Compact Array data. And, not surprisingly, the target-of-oppor tunity paper s ­ in fact, all 12 paper s ­ are in the list by vir tue of the Compact Array being both in the Southern Hemisphere and having high angular resolution (i.e. being an interferometer). The rest of the list is diver se, and perhaps less predictable, covering obser vations of ultracompact HII regions, methanol maser s, and quasar scintillation. "It's not all continuum, it's not all hydrogen," said Phil. "There's a ver y wide range of science topics in that top twelve." "Two of the most cited and influential paper s are the hydrogen (HI) mosaic images of the Large Magellenic Cloud (LMC) and Small Magellenic Cloud (SMC)," added Ron Eker s, former ATNF Director. "These were the most dramatic examples of the use of the mosaicing technique, which was really introduced into the astronomy community by the Compact Array." Two of the paper s represent obser vations that lay outside the obvious range of the Compact Array's capabilities. "The 6.7 GHz obser vations of methanol maser s are interesting, because 6.7 GHz is outside the nominal range of frequencies the Compact Array can obser ve at," said Phil. (Methanol maser s were unknown at the time the Compact Array was designed). "Apparently the engineer s took some convincing to allow obser vations to be made at 6.7 GHz," said Phil. "But it was tried and indeed proved to be possible." The obser vations of intra-day variability from the quasar PKS 0405-385 were not technically challenging, he said, but represented a

mode of obser ving that wasn't envisaged when the Compact Array was built. The recently completed AT20G sur vey is too new on the scene to be a candidate for the "top 12" list, but it too has taken the Compact Array into unchar ted technical water s by mapping the sky with continuous slewing. It also used an innovative wideband analogue correlator developed by ATNF engineer s for a completely different purpose ­ a cosmic microwave background experiment. A few other notable pieces of Compact Array research haven't made it into the "top 12" because they were fair ly specialised. One is the ground-breaking obser vation of SNR1987a in 1991. This was the fir st imaging of the bir th of a radio supernova remnant, and provided the impetus to get the 6-km antenna of the Compact Array wor king. A second instance is the 3-D tomographic images of Jupiter's radiation belts. These obser vations, led by former Narrabri Officer-in-Charge Bob Sault in 1995, were "perhaps the most innovative" that have ever been made with the Compact Array, according to Ron Eker s. And obser vations exploiting the Compact Array's exceptional polarisation purity have been small in number, but excellent. The obser vations of circular polarisation in BL Lacs by PhD student David Rayner have never been bettered, said Ron Eker s, and those of circular polarisation in the intra-day variable source PKS 1519-273 by J-P Macquar t "might turn out to be one of the most impor tant Compact Array discoveries", he said. The last time anyone looked (Trimble & Ceja 2008 AN, 329, 623-647), the Compact Array ranked second in the wor ld in terms of the total number of citations (this was for the year s 2001-

The Compact Array: Greatest Hits
Phil Edwards, the ATNF's Head of Science Operations, has plucked from the Astrophysics Data System (ADS) the top twelve most highly cited paper s using Compact Array data, all with more than 100 citations. While cautioning that this sample will be biased towards paper s more than five year s old, he describes the results as "ver y interesting". Three of the top four paper s use targetof-oppor tunity obser vations, and date from the late 1990s. "This was the era when satellites were star ting to pinpoint gamma-ray bur sts with sufficient accuracy that they could be followed up at radio wavelengths," Phil said. In fact, the most highly cited paper was not just an obser vation of a gamma-ray bur st, but cr ucial evidence that these bur sts were linked to supernovae . The three most highly cited paper s, and another two in the list (Corbel et al. and Schwarz et al.) are multiwavelength. Two of the

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2003), second only to the VLA (Par kes was a close third). It is a proud record, built on good design choices, excellent engineering, operational efficiency, and the openness of a National Facility to the best obser ving proposals.

The 12 most highly cited Compact Array papers
· Kulkarni,S.R.;Frail,D.A.;Wieringa, M. H.; Eker s, R. D.; Sadler, E. M.; War k, R. M.; Higdon, J. L.; Phinney, E. S.; Bloom, J. S. Radio emission from the unusual supernova 1998bw and its association with the -ray burst of 25 April 1998. 1998 Nature 395, 663. · Harrison,F.A.;Bloom,J.S.;Frail,D. A.; Sari, R.; Kulkarni, S. R.; Djorgovski, S. G.; Axelrod, T.; Mould, J.; Schmidt, B. P.; Wieringa, M. H.; War k, R. M.; Subrahmanyan, R.; McConnell, D.; McCar thy, P. J.; Schaefer, B. E.; McMahon, R. G.; Mar kze , R. O.; Fir th, E.; Soffitta, P.; Amati, L. Optical and Radio Obser vations of the Afterglow from GRB 990510: Evidence for a Jet. 1999 ApJ 523, L121. · Kim,S.;Staveley-Smith,L.;Dopita, M. A.; Freeman, K. C .; Sault, R. J.; Kesteven, M. J.; McConnell, D. An HI Aperture Synthesis Mosaic of the Large Magellanic Cloud. 1998 ApJ 503, 674. · Tingay,S.J.;Jauncey,D.L.;Preston, R. A.; Reynolds, J. E.; Meier, D. L.; Murphy, D. W.; Tzioumis, A. K.; McKay, D. J.; Kesteven, M. J.; Lovell, J. E. J.; Campbell-Wilson, D.; Ellingsen, S. P.; Gough, R.; Hunstead, R. W.; Jones, D. L.; McCulloch, P. M.; Migenes, V.; Quick, J.; Sinclair, M. W.; Smits, D.. Relativistic motion in a nearby bright X-ray source. 1995 Nature 374, 141. · Stanimirovic,S.;Staveley-Smith,L.; Dickey, J. M.; Sault, R. J.; Snowden, S. L. The large-scale HI structure of the Small Magellanic Cloud. 1999 MNRAS 302, 417. · Walsh,A.J.;Bur ton,M.G.;Hyland, A. R.; Robinson, G. Studies of ultracompact HII regions - II. High-resolution radio continuum and methanol maser sur vey. 1998 MNRAS 301, 640. · Morganti,R.;Killeen,N.E.B.;Tadhunter, C . N. The Radio Structures of Southern 2Jy Radio Sources. 1993 MNRAS 263,1023. · Schwar tz,D.A.;Mar shall,H.L.;Lovell,J. E. J.; Piner, B. G.; Tingay, S. J.; Bir kinshaw, M.; Char tas, G.; Elvis, M.; Feigelson, E. D.; Ghosh, K. K.; Harris, D. E.; Hirabayashi, H.; Hooper, E. J.; Jauncey, D. L.; Lanzetta, K. M.; Mathur, S.; Preston, R. A.; Tucker, W. H.; Virani, S.; Wilkes, B.; Worrall, D. M. Chandra Discover y of a 100 kiloparsec X-Ray Jet in PKS 0637-752. 2000 ApJ 540, L69.

Growth and learning
The Compact Array has had three major technical upgrades, says Dave McConnell, Officer-in-Charge of the Paul Wild Obser vator y during 1997­2001 and now the ATNF's Assistant Director : Operations. The most obvious to user s has been the outfitting of the Compact Array to handle 12- and 3-mm wavelengths. This was a major overhaul, funded by the fir st round of the Commonwealth Government's Major National Research Facilities (MNRF) program over several year s, and involved creating new receiver s, building the nor th spur track, resurfacing the antennas, and reconfiguring the Local Oscillator (LO) distribution system. The second upgrade , completed in 2008 and done in collaboration with NASA, has given the Compact Array an additional 7-mm capability for both astronomy and spacecraft tracking. The third upgrade , which will be completed next year, is the Compact Array Broadband Backend (C ABB) project (described at http:// www.narrabri.atnf.csiro.au/obser ving/C ABB . html). C ABB was funded by a second round of the MNRF program. Both the millimetre-wave upgrade and C ABB competed successfully in their respective MNRF rounds against bids from all areas of Australian science , not just astronomy. These upgrades were on a natural development path for the Compact Array. For instance , for the LO system, modified under the fir st-round MNRF program, "the eventual need for higher

· Norris, R. P.; Whiteoak, J. B.; Caswell,
J. L.; Wieringa, M. H.; Gough, R. G.. Synthesis images of 6.7 GHz methanol masers. 1993 ApJ 412, 222. · Corbel,S.;Nowak,M.A.;Fender,R.P.; Tzioumis, A. K.; Mar koff, S. Radio/X-ray correlation in the low/hard state of GX 339-47. 2003 A&A 400, 1007. · Frail,D.A.;Goss,W.M.;Reynoso,E.M.; Giacani, E. B.; Green, A. J.; Otr upcek, R. A Sur vey for OH (1720 MHz) Maser Emission Toward Supernova Remnants. 1996 AJ 111, 165. · Kedziora-Chudczer,L.;Jauncey,D.L.; Wieringa, M. H.; Walker, M. A.; Nicolson, G. D.; Reynolds, J. E.; Tzioumis, A. K. PKS 0405-385:The Smallest Radio Quasar? 1997 ApJ 490, L9.

Above: The Compact Array in a compact configuration

Photo: Phil Edwards, CSIRO

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bandwidth had been foreseen," said Dave . "We took advantage of new technology when it became available ." C ABB, which will provide the Compact Array with much greater sensitivity, has arisen for the same reasons. The millimetre-wave upgrade too was foreseen, or at least provided for in the initial specifications: the antennas were originally specified to operate at frequencies well above the 8 GHz upper frequency allowed for in the constr uction budget. However, the antenna designer s were careful not to push the requirements above 7 mm to avoid cost over-r uns. The decision to upgrade the Compact Array for 3-mm obser vations was carefully considered in the mid 1990s in light of the site's characteristics, but "I think it has been wor th the risk," said Dave . This extension of the Compact Array's capabilities opened the instr ument up to new uses: for instance , studies of higher-frequency maser s and molecular species such as carbon monoxide (CO) in high-redshift galaxies. The changes fostered the development of specific capabilities within the ATNF. The receiver group took on the challenge of designing high-frequency receiver s, "and developed their capability enormously," said Dave . And in the area of correlator s, the ATNF came to grips with high-speed data transpor t: technologies that flow directly through to ASKAP. " Again, a ver y strong group, but they had to extend themselves," said Dave. CSIRO, he says, wants to identify the capabilities the ATNF has "that are unusual and give us an advantage in par ticular areas of science and technology. The drive [throughout CSIRO] is to recognise the capabilities that CSIRO has that might be valuable , and to do our best to maintain and extend them."

The Compact Array is also a "learning instr ument" for obser ver s, par ticular ly students. There are a dozen new students joining the ranks of obser ver s each year, Phil said. "And they find it ver y inspiring to come to the telescope." The Duty Astronomy scheme keeps ATNF staff current with the telescope, he says. Because project proposer s are also the obser ver s, there is a steep learning cur ve for fir st-time obser ver s, but "we also learn from them," said Phil. "They ask questions such as `why can't I do this?' ". Remote obser ving has accounted for about 15% of all obser ving with the Compact Array for the past five year s. As this propor tion increases, there will have to be other ways found to maintain interactions with obser ver s, Phil suggests.

The next five years
What of the future? The new Compact Array Broadband Backend, to be installed in March/April 2009, will hugely enhance Compact Array science and enable projects that were not feasible before. This is par ticular ly tr ue for millimetre-wave projects, which will benefit from increased sensitivity and bandwidth. Combined multiline and wideband continuum obser vations will be the Compact Array's standard obser ving mode in the future. The Compact Array will soon be operating in an environment where the Atacama Large Millimeter Array Project (ALMA), the Australian Square Kilometre Array Pathfinder (ASKAP) and the Expanded Ver y Large Array Project (EVLA) will give the wor ld's astronomer s new obser ving possibilities, but there are several areas ­ for instance, wide and deep continuum sur veys, niche HI sur veys, studies of radio transients, and 3-D imaging of magnetic fields ­ in which the Compact Array will continue to do excellent science.

What will be the most highly cited paper s of the future? The Compact Array's deep sur veys will be among them, predicts the ATNF's Ray Norris. The Compact Array has been used for four deep sur veys: PHOENIX,ATESP,theradiocounterpar tof the Hubble Deep Field South, and ATLAS, which builds on the multiwavelength data available in fields such as the Chandra Deep Field South. All have gone deep; ATLAS has also gone wide, covering seven square degrees. Such radio sur veys, says Ray, have become par ticular ly impor tant at the current time, when our under standing of galaxy evolution, and of the star-formation histor y of the univer se, is changing rapidly. "As an east-west array, the Compact Array is par ticular ly good for viewing wide fields, and of cour se it has had an excellent correlator," said Ray. "Those factor s have made it one of the wor ld's best radio sur vey instr uments." Radio monitoring of transient sources (such as gamma-ray bur sts, supernovae and other s) is also likely to be a future source of highly cited paper s, predicts BÄrbel Koribalski, Deputy Leader of the ATNF's Astrophysics Group. "With C ABB, follow-up of such events will be faster and deeper than before," she said. The immediate future promises rich pickings for the Compact Array in follow-up detections from new satellites such as Fermi (which monitor s gamma-ray sources) and Planck (which will operate in the millimetre and submillimetre bands). But the mostly highly cited Compact Array paper s will result from new discoveries made possible by the expanded "parameter space" C ABB will provide, BÄrbel says. "Flexibility" and "variety" are likely to remain the watchwords for success in the future ­ along with the in-depth knowledge and imagination of the obser ver s.

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Memorandum of Under standing (MOU)
Kate Brooks (ATNF)

CSIRO's Australia Telescope National Facility and Universidad de Chile signed a memorandum of understanding in April 2008 to facilitate collaboration between astronomers of the Australia Telescope National Facility (ATNF) and the Universidad de Chile (UChile). Working together, these two institutions can have a major impact in observational astronomy in the Southern Hemisphere.

The main method for encouraging collaboration between ATNF and UChile will be through the interchange of researcher s, professor s and students. Astronomer s who come from one institution will be appointed as Visiting Scientist in the host institution. Joint ATNF/UChile research projects utilising Australian facilities and those built in Chile will be par ticular ly encouraged. The Depar tment of Astronomy at UChile has a strong tradition of astronomical research and education, with a total of 30 academic staff and researcher s as well as more than 20 post-graduate students. A major par t of the astronomical research carried out by UChile utilises the international obser vatories built in the nor thern par t of the Chile , which are home to the wor ld's best optical, infrared and millimetre telescopes including ALMA, the Atacama Large Millimetre Array. Once ALMA is operational in 2012 it will offer unprecedented millimetreobser ving capabilities for the Southern Hemisphere . Under the MOU a program of joint postdoctoral fellowships has been established. The fellowship takes the name of Australis Fellow, with Australis being a Latin word referring to the south, which is meant to symbolise the astronomical research in the Southern Hemisphere that the ATNF/ UChile Australis Fellow will carr y out.

Left to right: Professor Guido Garay (UChile), Dr Kate Brooks (CSIRO ATNF) and Andres Guzman (UChile and CSIRO ATNF co-supervised student) on the grounds of the Calan Observatory at the University of Chile. Photo: Courtesy Kate Brooks, CSIRO

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ARTICLES
The scattered debris of the Magellanic Stream
Tobias Westmeier and BÄrbel S Koribalski (ATNF)

Spanning more than half the sky, the Magellanic Stream and the Leading Arm are among the most prominent gaseous structures in the neighbourhood of the Milky Way. They are widely believed to be the result

of tidal interaction between the two Magellanic Clouds and the Milky Way (Yoshizawa & Noguchi, 2003), although rampressure interaction could have played a significant role in their formation and evolution

(Mastropietro et al., 2005). The Magellanic Stream was first studied over its entire extent by Mathewson et al. (1974), who also noticed its association with the Magellanic Clouds.

Figure 1: HI column density map of high-velocity gas in a large area on the sky based on the Leiden/Argentine/Bonn survey. The high-velocity clouds (HVCs) found in HIPASS are overprinted as the black contour lines. The identified HVC filaments are labelled with the capital letters A­E. For this project we studied the region of 0h00m to 1h30m in right ascension and -30° to +25° in declination.
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Here we repor t on the detection of an extended, filamentar y population of compact neutral hydrogen (HI) clouds most likely connected with the Magellanic Stream (Westmeier & Koribalski, 2008). The original aim of our project was to search the HI Par kes All-Sky Sur vey (HIPASS) for a diffuse cosmic

web filament connecting the nearby Sculptor group with the M31 group. To do this we searched a large area on the sky (see Figure 1) for diffuse H emission in HIPASS. The studied area cover s about 3% of the entire sky.

I

We did not find any evidence for a diffuse HI filament connecting the groups

but there are numerous high-velocity clouds (HVCs) in this region of the sky (see also, e.g., Putman et al., 2002 and 2003) that appear to be associated with the Magellanic Stream that r uns across par t of the area studied. We identified 153 potential HVCs, most of which are fair ly compact with typical angular diameter s of only 20 to 30 arcminutes (full width at half maximum). An HI column density map of high-velocity gas in the entire region, based on the Leiden/ Argentine/Bonn sur vey, is shown in Figure 1 with the detected HVCs overprinted as the black contour s. Apparently, their distribution is not homogeneous, but concentrated in filamentar y groups which have been labelled with capital letter s in Figure 1. Most of these filaments have approximately the same orientation, r unning from the nor th-west to the south-east parallel to the Magellanic Stream. This morphology suggests a common origin of the HVCs and a possible association with the stream. Fur ther evidence for a connection between the detected HVCs and the Magellanic Stream is provided by the kinematics of the clouds. Figure 2 shows the radial velocity distribution of the HVCs as a function of declination. In the local standard of rest frame (LSR, upper panel) we obser ve a strong velocity gradient of about 3 kms-1 per degree. After conver sion into the Galactic standard of rest (GSR, lower panel) this gradient completely disappear s, demonstrating that the velocity gradient obser ved in the LSR frame has simply been caused by the projection of the rotation of the Galactic disc. In fact, all

Figure 2: Position-velocity diagrams of the detected HVCs (dots) in the Local Standard of Rest (LSR, top) and Galactic Standard of Rest (GSR, bottom). Five Sculptor Group galaxies found in the region are also plotted. The crosses show the velocities at eight positions along the nearby Magellanic Stream. The solid line is a linear fit to the data, and the capital letters indicate the declination ranges of the filaments outlined in Figure 1.
Articles 21


HVCs have approximately the same GSR velocity with a mean value of vGSR = -203.0 kms-1 and a remar kably small disper sion of only 43.5 km s-1. Fur thermore , the velocities of the HVCs are ver y similar to those obser ved along the Magellanic Stream (crosses in Figure 2), suggesting an association of the clouds with the Magellanic Stream. A comparison of our results with the numerical simulations of Gardiner & Noguchi (1996) provides additional evidence for the origin of the HVCs. In their simulations, the Magellanic Stream and the Leading Arm were formed during the previous perigalactic passage of the Small Magellanic Cloud about 1.5 Gyr ago which approximately coincided with a close encounter between the two Magellanic Clouds. Their model stream consists of two separate par ts, a denser main stream which can be identified with the one obser ved in neutral hydrogen, and a secondar y stream with lower surface density which is not obser ved in HI. A comparison with figure 6 of Gardiner & Noguchi (1996) reveals that the location of the secondar y stream coincides with the population of HVCs that we found in HIPASS. Therefore , the discovered HVC filaments could be the neutral par t of the faint secondar y stream predicted by the simulations of Gardiner & Noguchi (1996). In this case , they would have formed about 1.5 Gyr

ago together with the main filament known as the Magellanic Stream. In addition, Sembach et al. (2003) detected high-velocity ionised oxygen (OVI) absorption against three quasar s in the nor thern par t of our field. In all three cases, the radial velocities of the OVI absorber s are similar to those of the HVCs found in HIPASS, suggesting that the HVCs are condensations within a much more extended filamentar y networ k of diffuse and mainly ionised gas. In the case of collisional ionisation, OVI reaches its highest ionisation fraction at a temperature of about 3 â105 K (Suther land & Dopita, 1993). Therefore, the OVI absorber s probably trace the interface region between the warm neutral gas of the Magellanic Stream and the highly-ionised Galactic corona. In summar y, our results suggest that the detected HVCs are par t of an extended networ k of neutral and ionised gas filaments associated with the Magellanic Stream. Consequently, the Magellanic Stream would be much more extended than generally believed, with some of the clouds being as far away as 20° from the original stream. A more extensive study of HIPASS data is under way to map the entire extent of the HVC filaments and investigate

their connection with other HVC complexes on the sky. In addition, we are planning to follow up obser vations of some of the clouds with higher angular and spectral resolution using the ATC A. This will allow us to derive the physical parameter s of the HVCs and possibly to estimate their distances.

References
Gardiner, L.T. & Noguchi, M., 1996, MNRAS, 278, 191. Mastropietro, C ., Moore, B., Mayer, L., et al., 2005, MNRAS, 363, 509. Mathewson, D.S., Clear y, M.N., & Murray, J.D., 1974, ApJ, 190, 291. Putman, M.E., de Heij, V., StaveleySmith, L., et al., 2002, AJ, 123, 873. Putman, M.E., Staveley-Smith, L., Freeman, K.C ., et al., 2003, ApJ, 586, 170. Sembach, K.R., Wakker, B.P., Savage, B.D., et al., 2003, ApJS, 146, 165. Suther land, R.S. & Dopita, M.A., 1993, ApJS, 88, 253. Westmeier, T. & Koribalski, B.S., 2008, MNRAS, 388, L29. Yoshizawa, A.M. & Noguchi, M., 2003, MNRAS, 339, 1135.

22 ATNF Ne ws , Issue 65, October 2008


The nuclear region of NGC 4945 revealed
Emil Lenc (ATNF) and Steven Tingay (Curtin University of Technology)

The central regions of nuclear starbursts are typically obscured by dense clouds of gas and dust, making them notoriously difficult to study at optical wavelengths. However, radio obser vations provide a means to unveil the shrouds of gas and directly image sources hidden behind them. The recently upgraded Long Baseline Array (LBA) and the Australia Telescope Compact

Array (ATCA) have been used to observe the nuclear region of the starburst galaxy NGC 4945 with unprecedented sensitivity and detail. By processing the LBA data with wide-field Very Long Baseline Interferometry (VLBI) techniques, the entire nuclear region was imaged with a resolution of 15 milli-arcseconds (0.3 pc). The resulting images reveal a population of compact

radio sources shrouded by dense ionised gas and a jet-like feature that may be associated with a supermassive black hole. These are the "engines" that drive larger-scale features obser ved at other wavelengths in this galaxy.
NGC 4945 is a near ly edge-on spiral galaxy associated with the Centaur us group of galaxies at a distance of 3.8 Megapar secs (Mpc). The galaxy has been classified as SB(s)cd or SAB(s)cd and

Figure 1: A composite, multi-wavelength view of NGC 4945. Light grey indicates K-band infrared (Jarrett et al. 2003); dark/grey/ black Chandra soft X-ray (Schurch et al. 2002); and mid-grey indicates H (Rossa & Dettmar 2003). Inset: LBA 2.3-GHz image with ATCA 23-GHz contours overlaid. Circles give an indication of the degree of absorption in the vicinity of the source, with the diameter of the circle being directly proportional to the absorption. (See also cover page.)

Articles 23


Figure 2: High-resolution LBA image of the jet-like feature discovered in NGC 4945.

has an optical extent of 17 arcminutes. While it is classified as a Seyfer t 2 galaxy, it exhibits both starbur st and Seyfer t characteristics. Evidence of an Active Galactic Nucleus (AGN) comes fromstrongandvariablehardX-ray emission (Isawa et al. 1993) and the detection of a water megamaser in the nuclear region (Greenhill et al. 1997). NGC 4945 hosts a large number of massive star s that quickly evolve to form supernovae . These supernovae drive activity in the nuclear region over time-scales of 20-30 million year s and produce strong winds out of the disk ofthegalaxythatarevisibleinX-ray and H images (see Figure 1). In NGC 4945, gas is funnelled into the nuclear region by dynamical processes associated with bar instabilities, providing material that feeds the star-forming activity. The supernova activity in the starbur st region is generally hidden from view by dense ionised gas. However, direct obser vation of supernova remnants

in this region is possible at radio wavelengths. Fur thermore, Ver y Long Baseline Interferometr y can provide ver y high angular resolution. Such obser vations enable us to investigate the remnants themselves, using them to reconstr uct the supernova and star formation histor y of the galaxy. They also provide a link between the largescale dynamical effects in the galaxy, activity in the star forming region itself, and the energetic phenomena that are in turn driven by the starbur st. Motivated by the existence of compact radio sources (supernova remnants and HII (ionised hydrogen) regions) and strong indicator s of free-free absorption in similar starbur st galaxies, such as NGC 253 (Lenc & Tingay 2006) and M82 (Pedlar et al. 1999), we embar ked on a program of LBA and ATC A obser vations of NGC 4945. The galaxy was obser ved at 2.3 GHz over two epochs (separated by 1.9 year s) using the LBA to produce the highest resolution images of the

nuclear starbur st region of this galaxy to date (see Figure 1). Multi-epoch images allowed us to monitor for new supernovae and to check the evolution of existing supernovae and supernova remnants. The LBA obser vations were complemented with additional data between 8.64 and 23 GHz obser ved with the ATC A (the 23-GHz image is shown in Figure 1) to determine the spectral indices of the sources and to model the effects of free-free absorption. A total of 15 compact radio sources were detected with the LBA and 13 of these were associated with sources in the higher frequency ATC A images. Nine sources exhibited spectra that were consistent with free-free absorption, suggesting that they were embedded deep within the nuclear region (the degree of absorption is illustrated with circles in Figure 1). Ten sources had steep intrinsic spectra typical of supernova remnants. In the highest resolution images (15 milli-arcsecond beam), four

24 ATNF Ne ws , Issue 65, October 2008


supernova remnants were resolved into shell-like str uctures with diameter s ranging between 1.1 and 2.1 par secs (pc.) The detection of the supernova remnants allowed us to take a number of different approaches towards estimating the type-II supernova rate of the starbur st region of the galaxy. An upper limit can be derived from the absence of any new sources between epochs. A lower limit can be determined based on the number of supernova remnants, their sizes and an assumed expansion rate for the remnants. Finally, the supernova rate can also be determined from an estimate of the median age of the remnant population based on the obser ved flux variation between two epochs. Our preliminar y results, based on only two obser ving epochs, suggest that the type­II supernova rate is between 0.1(v/104) and 15.3 per year, where v is the radial expansion velocity of the supernova remnant in km per second. We obser ved no significant variation between epochs in the detected sources above our error limits. However, if we assume that the median variation in the strongest of sources is real then we find an upper limit of 0.8% per year to the fading rate in NGC 4945. If the supernovae are assumed to fade as the -0.7 power of time (Weiler et al. 1986) then we estimate that the median age of the supernova remnant population of ~85 year s. This would imply a supernova rate of ~0.12 per year, a value that falls within the limits determined above . With only two obser ving epochs our supernova rate estimates are not highly constrained. The upper limit can be improved with more frequent obser vations of the source . The lower limit can be fur ther refined once the

age of the remnants can be more accurately determined­either by obser ving expansion in the remnants themselves and thus pinning down the expansion velocity or by obser ving their fading with a greater degree of cer tainty. Nonetheless, it is promising that these independent estimates are consistent with each other and are also consistent with similar results obtained from farinfrared, H, radio-recombination line and radio continuum obser vations. A surprising discover y in the LBA images is that of a one-sided jet-like source in the centre of the nuclear region (see Figure 2). The source extends for approximately 5 pc and has a width of <1.5 pc. A chance alignment of several compact sources in such a linear arrangement is highly unlikely. If it is a jet then it is likely that the source is associated with a supermassive blackhole. The one-sided nature of the jet would suggest that it is either relativistic (with the side facing us being Doppler boosted) or that one side is heavily obscured by the accretion disc surrounding the central blackhole. Similar jet features have been obser ved in other nearby Seyfer ts, however, this would be one of the nearest discovered to date. Interestingly, the jet-like source is offset from the assumed location of the AGN (based on the detection of a water megamaser) by approximately one arc-second - an offset that is well outside the positional error s of both obser vations. The jet-like nature of the source can be confirmed in future obser vations of the source if motion in the suggested jet is detected. A detailed analysis of the wor k presented here has been submitted to the Astronomical Journal for publication

and is par t of a larger on-going study of the sub-par sec-scale proper ties of local, bright southern starbur st galaxies. Other galaxies in the sample include M83, NGC 55, NGC 253 (Lenc & Tingay 2006), NGC 1313 and NGC 5253. A subsidiar y focus of this project is to achieve high sensitivity, high fidelity, high resolution, and computationally efficient imaging over wide fields of view (at least compared to traditional VLBI imaging techniques). The associated exploration of the relevant techniques is a step toward the much larger task of imaging with next generation radio telescopes such as the Square Kilometre Array (SKA).

References
Greenhill, L.J., Moran, J.M., & Herrnstein, J.R. 1997, ApJ, 481, L23 Iwasawa, K., Koyama, K., Awaki, H., Kunieda, H., Makishima, K., Tsur u, T., Ohashi, T., & Nakai, N. 1993, ApJ, 409, 155 Jarrett, T.H., Chester, T., Cutri, R., Schneider, S.E., & Huchra, J.P. 2003, AJ, 125, 525 Lenc, E., & Tingay, S.J. 2006, AJ, 132, 1333 Pedlar, A., Muxlow, T.W.B., Garrett, M.A., Diamond, P., Wills, K.A., Wilkinson, P.N., Alef, W. 1999, MNRAS, 307, 761 Rossa, J., & Dettmar, R.-J. 2003, A&A, 406, 505 Schurch, N.J., Rober ts, T.P., & Warwick, R.S. 2002, MNRAS, 335, 241 Weiler, K.W., Sramek, R.A., Panagia, N., van der Hulst, J.M., & Salvati, M. 1986, ApJ, 301, 790

Articles 25


Polarisation obser vations with the LBA
Richard Dodson, University of Western Australia (UWA)

Work has been on-going for the development of full polarisation processing of Ver y Long Baseline Interfometry (VLBI) data using the Australian Long Baseline Array (LBA) antennas. The results from this analysis are available (Dodson 2007) but we present a summar y here to encourage others to use the facility.
Polarisation calibration entails the solving for the fractional polarisation impurities of the right and left handed (or alternatively the two linear) receiver s on each antenna (these are the D-terms in the data reduction package, AIPS). This is then included in the calibration application for the formation of the Stokes products (I, Q, U and V). We have extended AIPS to allow the suppor t of two new mount types; the left-handed and right-handed Nasmyth antennas (Pico Veleta in the Global millimetre VLBI Array (GMVA) and Yebes in the European VLBI Networ k (EVN)) and the EW-mount (Hobar t in the LBA). A great deal of testing has now been performed, and the updates required

have been included in the latest ver sions of AIPS. A summar y of some of the outcomes of these tests are: The comparison of Australia Telescope Compact Array (ATC A) and LBA was repor ted in Dodson (2008), which presented LBA obser vations of the 6.7GHz methanol maser G339.8-1.26. These are the fir st ever polarised VLBI images of methanol maser s, and also the fir st polarisation VLBI imaging from the LBA. The telescopes involved were Par kes, ATC A, Mopra, Ceduna (all requiring conventional feed solutions) and Hobar t (requiring the solution for the EWmount type). The target, G339.8-1.26,

Figure 1: Polarisation angle and fraction for G339.8-1.26, as observed by the LBA (Dodson 2008, open squares), and the ATCA (Ellingsen, priv. comm., closed circles). The spectra is scalar summed across the image (Stokes I,Q and U), and shows good agreement between the VLBI and the connected array results. The errors are the absolute errors based on the confidence in the polarisation calibration (2 % and 0.4 % respectively), not the relative errors. Where errors are not shown they could not be calculated.

26 ATNF Ne ws , Issue 65, October 2008


Figure 2: a) The polarised flux from 3C273, as observed by the LBA and the VLBA (smoothed) in 2008. The black contours are the VLBA polarised intensity, the grey those of the LBA with the LBA polarisation vectors overlaid. b) The polarised flux from 3C279, as obser ved by the LBA and the VLBA in 2008. The black contours are the VLBA polarised intensity, the grey those of the LBA with the LBA polarisation vectors overlaid. was (at the time of the experiment) one of the best candidates to show methanol maser s forming in the dusty disk surrounding a massive forming star. Using unpublished results from Simon Ellingsen we compared the polarised flux and position angle averaged over the maser for both these LBA obser vations and those from ATC A (made the year before). The position angle and polarised flux by velocity channel for both the ATC A data and the LBA data are shown in Figure 1. This shows pleasing agreement between the polarised fluxes and position angles by velocity channel. A comparison of the VLBA and the LBA has also been performed. We recently (March 2008) obser ved a number of sources at 8.4 GHz: 3C273, 3C279, 1921293 and 1934-638. The fir st two are regular ly monitored under the MOJAVE project (Monitoring Of Jets and AGN with VLB A Experiments , Lister & Homan 2005). The telescopes involved were the same as before . After the smoothing of the VLBA data to the LBA resolution (~3 milli-arcseconds) we were able to compare the two datasets (see Figure 2). The total fluxes are in good agreement and the polarised fluxes and angles are in reasonable agreement. The problems which remain are related to known problems with the data, not with the procedure. Mopra, for example, had D-terms of 35% where normally we would expect D-terms to be better than 10%. The hybrid tuning, which was the source of this problem, has been rectified. The fir st focus for use of these new capabilities will be to follow-up the results from G339.8-1.26, and test the prediction of the magnetic field directions from the model of methanol maser s arising in disks in a significant number of sources. Fur thermore, if sufficiently good calibration can be achieved, we will use the Stokes V magnitudes to estimate the field strengths and recover the full three dimensional magnetic field in these massive star forming regions. The magnetic fields are a significant influence in these regions, and have not been fully considered in current modelling. These questions can only be answered with VLBI resolution, and the LBA obser vations are opening up this field for investigation. Results from polarisation imaging with the LBA of Active Galactic Nuclei (AGNs) and their jets will follow up the wor k done by the MOJAVE sur vey in the Nor th. The polarisation of the ejection components, and their dynamic development with time and with jet position, are a delicate probe of the conditions therein. We would encourage anyone interested to test out their own science ideas with the new capability, as the more obser vations made, the better we will under stand the system and therefore improve the outcomes.

References
Dodson, R. 2007, Polarisation gain terms for VLBI with Nasmyth or EW IT-OAN2007-16,http://www1.oan.es/informes/ archivos/IT-OAN-2007-16.pdf, Dodson, R. 2008, First VLBI observations of methanol maser polarisation A&A, 480, 767 Lister, M.L. & Homan, D.C . 2005, MOJAVE I. 1st-Epoch 15 GHz Polarization Images AJ, 130, 1389

Articles 27


REGULAR
ATNF Operations

ITEMS

Jessica Chapman and David McConnell (ATNF)

By 2012 the Australia Telescope National Facility (ATNF) will be operating four world-class obser vatories: the Australia Telescope Compact Array (ATCA), the Parkes and Mopra radio telescopes, and the Australian SKA Pathfinder telescope (ASKAP) ­ currently under development. These facilities will also be operated together for ver y high angular resolution observations as the Long Baseline Array (LBA). Astronomers will also have access to some time on the Tidbinbilla 70-m and 34-m antennas.

Planning for future ATNF operations began in ear ly 2007. In December 2007, a document Future ATNF Operations (Version 1) was prepared for discussion with the ATNF Steering Committee and this document was made available to the user community in Febr uar y 2008. This document has now been substantially revised and ver sion 2 was be made available around the end of October 2008. Since Febr uar y 2008, much progress has been made in ATNF Operations. We would like to highlight: Community consultation: An extensive process of seeking input and consulting with the user community on the operations plans and the ATNF science priorities has taken place during 2008. This has been extremely valuable and has had a big impact on the development of the ATNF's plans for the future . Operations restructure: The ATNF Operations theme has now been restr uctured into two groups, for science and engineering operations.

Science Priorities: An essential par t of the planning process has been to clear ly identify the ATNF Science Priorities for the period 2010 ­ 2015. A discussion paper on these is now available. ASKAP user policy: Good progress has been made towards establishing the user policies for ASKAP through the effor ts of an international taskforce and a draft policy is now available. ASKAP 12-m testbed antenna: A new 12-m testbed antenna for ASKAP has been successfully commissioned at the Par kes Obser vator y, with extensive input from operations staff, resulting in ver y promising fir st light tests with the new phased array feed receiver for ASKAP. A new 12-mm receiver at Parkes: A new and far more sensitive 12-mm receiver has now been commissioned at Par kes with excellent fir st science results obtained in September 2008. These have all added up to a busy and productive period, especially as

all of this wor k has been in addition to the core daily tasks of operating ATNF's facilities and providing obser ving and other suppor t to our many visitor s and obser ver s. It is a great credit to all of our operations staff that this has been possible. Input from the community on any aspect of the operations plans, and on the science priorities, is always welcome. This should be sent either through available web for ums, or by email to Jessica.Chapman@csiro.au, Lewis.Ball@csiro.au or David.McConnell@csiro.au. For all web links on ATNF operations planning, please see www.atnf.csiro.au/observers/planning/.

28 ATNF Ne ws , Issue 65, October 2008


ATNF Science Operations
David McConnell and Phil Edwards (ATNF)

In July 2008 the ATNF adopted a new structure for managing telescope operations and the two organisational entities, Science Operations and Engineering Operations, were established. Broadly speaking, Engineering Operations deal with the hardware (telescopes, instrumentation, infrastructure) and Science Operations deal with software and "live-ware": the users, their support, proposals, allocation to the telescopes, and the operational and data reducing software and associated computing. Science Operations includes the running of the specialised accommodation ser vices at the observatories and the visitors' lodge at Marsfield. Science Operations is divided into four areas:

Telescope Operations and Science Services (TOSS): Coordination with Engineering Operations; Telescope calibration and systems analysis; Time Assignment Committee; usage statistics; calibration sources and catalogues; off-line data verification; user friend suppor t (all stages); user guides and all user suppor t; suppor t for Target-of-Oppor tunity requests and queue scheduling. Computing Infrastructure (CI): Operating systems; site-site communications (conference links etc); obser ver s' environment (terminals etc); user and email accounts and passwords; data back ups and management; infrastr ucture (networ ks, ser ver s, data storage); networ k ser vices (email systems, authentication, etc). Scientific Computing and Archives (SCA): Telescope control and monitoring software; data reduction, image analysis.

The Australia Telescope Online Archive (ATOA); Online Proposal Application system (OPAL); scheduling software. Visitors Services (VS): Visitor administration, accommodation bookings and invoices; Lodge ser vices; office allocations. ATNF user s have been accustomed to Officer s-in-Charge at the Par kes and Narrabri obser vatories being critical links and contact points for many issues related to their obser vations, directly while obser ving, and indirectly when preparing proposals or reducing data. In future, user s should contact member s of the TOSS group that is led by Phil Edwards.

Phil will be suppor ted, from ear ly in 2009, by newly appointed Senior System Scientists at each of Par kes and Narrabri: Ettore Carretti and Jamie Stevens respectively. The other groups are led by Shaun Amy (CI), Mar k Wieringa (SC A) and Vicki Drazenovic (VS).

Regular items 29


Time assignment information
Philip Edwards and Jessica Chapman (ATNF)

The 2009 APRS
For Par kes, Mopra, the LBA and Tidbinbilla the 2009 April Semester (2009 APRS) will r un for a six-month period from 1 April until 30 September 2009. For the Australia Telescope Compact Array, there will be a sixweek shutdown from 1 March until mid April 2009 for the installation of the full Compact Array Broadband Backend (C ABB). For the Compact Array only, the 2009 APRS will r un for a three-month period from 15 April 2009 until 14 July 2009. Compact Array proposals submitted for the 2009 APRS will be considered for this period only. For this semester, C ABB will be available with 2-GHz bandwidths with a single obser ving mode as described below. We strongly recommend that proposals for this semester include an ATNF staff member. Please note that because of the need for local knowledge in using the new C ABB systems, remote obser ving is expected to be more restricted in this semester. A separate call for Compact Array proposals will be announced on 15 April 2009, with a deadline of 15 May 2009 for a "2009 JULS" semester. The 2009 JULS will r un from 15 July 2009 until the end of September 2009. Compact Array proposals not scheduled in the 2009 APRS should be resubmitted for consideration in the 2009 JULS. It is expected that one or more C ABB zoom modes will be available for this semester.

correlator will be permanently removed to allow for the installation of the full C ABB system on all six antennas. 2009 APRS will be the fir st semester to offer the C ABB capability. For 2009 APRS, C ABB will be available with a single coar se resolution mode with a bandwidth of 2 GHz and a spectral resolution of 1 MHz, corresponding to 2048 spectral channels. In the 12-, 7- and 3-mm bands, two frequencies may be selected: the spacing between the two frequencies may be larger than the current limit of 2.7 GHz, but must be less than 6 GHz and will depend on the obser ving frequencies chosen. Obser ving will be possible with the standard 12-mm (16 ­ 25 GHz) and 7-mm (30 ­ 50 GHz) systems on all six antennas, and 3-mm systems (83.5 ­ 105.0 GHz) on five antennas. Obser ver s planning 3-mm obser vations in an extended array (H214 or EW352) are encouraged to consider also requesting time in more compact configurations as many 3-mm sources are weak and extended and the longer baselines may not detect all of the emission. In the 6- and 3-cm bands the existing front-ends allow a 2-GHz bandwidth to be used, with 4.5 to 6.5 GHz and 8.0 to 10.0 GHz being the nominal ranges. Simultaneous 6/3-cm obser ving will continue to be possible. In the 20- and 13-cm bands the usable bandwidth is limited by the front-ends to around 500 MHz, though radio frequency interference (RFI) will reduce the usable bandwidth, par ticular ly at 20 cm. Simultaneous obser vations at 20/13 cm will not be possible. Proposer s are reminded that the primar y flux density calibrator at

7 mm and 3 mm is Uranus, which for 2009 APRS will be at a Right Ascension of 23 h 45 m and declination of -2 d 30 m. Obser vator y staff will calibrate a number of bright active galactic nuclei (AGN) spread over the full range of right ascensions, against Uranus at the standard continuum obser ving frequencies throughout the semester for use as secondar y flux density calibrator s if Uranus is not visible, or is resolved out. Proposer s requiring their own obser vations of Uranus (at special frequencies, for example), should make this clear in the justification of their proposal. Proposer s for multi-source obser vations are reminded that it is extremely useful for the justification to include a clear statement about how the obser vations can be optimally scheduled. A statement along the lines of "six blocks of ten hour s duration scheduled anywhere between 4:00 and 16:00 LST" both indicates to the Time Assignmnent Committee (TAC) that you have carefully thought about the scheduling of your proposed obser vation, and makes the scheduling of the obser vations much easier.

Support for Tidbinbilla observations
Access to antennas at the Canberra Deep Space Communications Complex (CDSCC) at Tidbinbilla is provided under the Host Countr y agreement with NASA and made available to the astronomical community though the ATNF. The 70-m antenna provides the most sensitive system in the southern hemisphere for this band, with a system temperature of 60 Jy. Tidbinbilla has been used with considerable success for sensitive single-dish obser vations

Compact Array Broadband Backend
During the six-week shutdown of the ATC A the existing array backend and

30 ATNF Ne ws , Issue 65, October 2008


ATNF Engineering Operations
Brett Dawson (ATNF)

using the 70-m antenna in the 12mm band. The new 12-mm receiver at Par kes has a sensitivity three times that of its predecessor but Tidbinbilla remains the most sensitive southern hemisphere antenna for this band. Tidbinbilla single-dish obser vations are taken in a ser vice obser ving mode with typically 200 hour s of obser ving time available in a year. The level of suppor t to be provided by the ATNF for single dish spectroscopy at Tidbinbilla has been uncer tain until recently. An arrangement has now been set up in which ser vice obser vations will be taken by the CDSCC Radio Astronomy Engineer, Shinji Horiuchi, while the ATNF will provide in-kind suppor t. This will include announcements of oppor tunity and time allocation processes, the maintenance of Tidbinbilla-related web information and engineering suppor t for specialised ATNF equipment. Jimi Green, from the ATNF, will liaise with and provide advice to Shinji in his role of astronomy suppor t and is now the ATNF point of contact for Tidbinbilla enquiries. For enquiries relating to single dish obser vations with Tidbinbilla, please contact Jimi Green (Jimi.Green@csiro.au).

July 2008 saw the introduction of a new operational structure for the ATNF. The Engineering and Science Operations groups were formed to run the National Facility instruments. These changes have in part been made to facilitate the transition to ASKAP operations and to consolidate operations in ways which reduce duplication of functions across sites and aim to more efficiently run our facilities.
Par kes and Narrabri now each have a Site Manager and Technical Coordinator. In addition, four technical project groups were formed across the Par kes and Narrabri operations groups. Site Manager and Technical Coordinator for Narrabri and Mopra is Brett Hiscock. At Par kes the Site Manager is Brett Dawson and the Technical Coordinator is Brett Preisig. At each facility Site Manager s have overall responsibility for continuity of operations. Technical coordinator s have a specific role related to instr ument configuration and fault rectification. Project leader s are responsible for the planning and deliver y of projects in their respective areas. The new project groups are Mechanical, Drives and Electrical (MDE project leader is Tim Wilson), Digital, Ser vo and Electronics (DSE project leader is Peter Mir tschin), Receiver s, LO and Conver sion (RLOC project leader is Jock McFee) and Cr yogenics (CRYO project leader is John Wilson) 2009 will see Engineering Operations become substantially more project driven. In par ticular, projects which suppor t the automation and remote operation of Par kes, and preparations for the establishment of a Science Operations Centre in Sydney, will continue to be high priorities for Engineering Operations.

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ATNF publications list
Publication lists for paper s which include ATNF data or ATNF author s are available on the Web at http://www.atnf.csiro.au/research/publications. Please email any updates or corrections to this list to Christine.VanDerLeeuw@csiro.au. This list includes published refereed paper s compiled since the April 2008 newsletter. Paper s which include ATNF staff are indicated by an asterisk. ARCHIBALD, A.M., KASPI, V.M., LIVINGSTONE, M.A. & McLAUGHLIN, M.A. "No detectable radio emission from the magnetar-like pulsar in Kes 75". ApJ, 688, 550-554 (2008). *BEKHTI, N.B., MURPHY, M., RICHTER, P. & WESTMEIER, T. "Ca II and Na I absorption signatures from the circumgalactic gas of the Milky Way". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 273-274 (2008). *BEKHTI, N.B., RICHTER, P., WESTMEIER, T. & MURPHY, M.T. "Ca II and Na I absorption signatures from extraplanar gas in the halo of the Milky Way". A&A, 487, 583-594 (2008). *BEKKI, K., CHIBA, M. & McCLURE-GRIFFITHS, N.M. "The Magellanic impact: collision between the outer Galactic H I disk and the leading arms of the Magellanic Stream". ApJ, 672, L17-L20 (2008). *BELLOCHE, A., MENTEN, K.M., COMITO, C ., MULLER, H.S., SCHILKE, P., OTT, J., THORWIRTH, S. & HIERET, C . "Detection of amino acetonitrile in Sgr B2(N)". A&A, 482, 179-196 (2008). *BENAGLIA, P., VINK, J.S., MARTI, J., MAIZ-APPELLANIZ, J., KORIBALSKI, B.S. & JOHNSTON, S. "Radio evidence on the mass loss bistability jump". In: Mass Loss from Star s and the Evolution of Stellar Cluster s , Lunteren, The Nether lands, May 29 - June 1, 2006, ASP Conf. Ser., 388, 141-142 (2008). BEUTHER, H. et al. "ATC A 3 mm obser vations of NGC 63341 and I(N): dense cores, outflows, and an UCH II region". A&A, 481, 169-181 (2008). BHAT, N.D., TINGAY, S.J. & KNIGHT, H.S. "Bright giant pulses from the Crab Nebula pulsar : statistical proper ties, pulse broadening, and scattering due to the Nebula". ApJ, 676, 1200-1209 (2008). *BHATNAGAR, S., CORNWELL, T.J., GOLAP, K. & USON, J.M. "Correcting direction-dependent gains in the deconvolution of radio interferometric images". A&A, 487, 419-429 (2008). *C AMILO, F., REYNOLDS, J., JOHNSTON, S., HALPERN, J.P. & RANSOM, S.M. "The magnetar 1E 1547.0-5408: radio spectr um, polarimetr y, and timing". ApJ, 679, 681-686 (2008). *C ASWELL, J.L. & PHILLIPS, C .J. "Water maser 353.273+0.641, the prime example of a class dominated by a blueshifted outflow". MNRAS, 386, 1521-1526 (2008). CERRIGONE, L., HORA, J.L., UMANA, G. & TRIGILIO, C . "IC 4406: a radio-infrared view". ApJ, 682, 1047-1054 (2008). *CHAMPION, D.J. et al. "An eccentric binar y millisecond pulsar in the Galactic plane". Science , 320, 1309-1312 (2008). *CHAMPION, D.J. et al. "The discover y of an eccentric millisecond pulsar in the Galactic plane". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More, Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 448-452 (2008). CHEN,X.etal."ATC AandSpitzerobser vationsofthebinar yprotostellarsystemsCG30andBHR71".ApJ,683,862-875(2008). *CLUVER, M.E., JARRETT, T.H., APPLETON, P.N., KRAAN-KORTEWEG, R.C ., WOUDT, P.A., KORIBALSKI, B.S. et al. "The hidden H I-massive luminous infrared galaxy HIZOA J0836-43: inside-out galaxy formation". ApJ, 686, L17-L20 (2008). *CORONGIU, A., POSSENTI, A., D'AMICO, N., BURGAY, M., LYNE, A.G., MANCHESTER, R.N., C AMILO, F. & SARKISSIAN, J.M. "Par kes obser vations of radio pulsar s in globular cluster s". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 601-603 (2008). *CORTESE, L., MINCHIN, R.F., AULD, R.R., DAVIS, J.I., C ATINELLA, B., MOMJIAN, E., ROSENBERG, J.L., TAYLOR, R., GAVAZZI, G., O'NEIL, K., BAES, M., BOSELLI, A., BOTHUN, G., KORIBALSKI, B.S., SCHNEIDER, S. & VAN DRIEL, W. "The Arecibo Galaxy Environment Sur vey. II. A H I view of the Abell cluster 1367 and its outskir ts". MNRAS, 383, 1519-1537 (2008). CRAWFORD, E.J., FILIPOVIC , M.D. & PAYNE, J.L. "Radio continuum study of the Large Magellanic Cloud - SNR J0519-6926". Serb. AJ, 176, 59-63 (2008). CRAWFORD,F.HESSELS,J.W.&KASPI,V.M."Asearchforsingleradiopulsesandbur stsfromsouthernAXPs".In:40Year sofPulsar s:Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 259-261 (2008). *CUNNINGHAM, M.R., LO, N., KRAMER, C ., BAINS, I., JONES, P.A., BURTON, M.G., MULLER, E. & OSSENKOPF, V. "Large scale str ucture and turbulence: the Mopra G333 sur vey". In: Far-Infrared and Submillimeter Emission of the Inter stellar Medium Wor kshop, Bad Honnef, Germany, 5-7 November 2007, EAS Pub. Ser., 31, 9-14 (2008). *CURRAN, S.J., KORIBALSKI, B.S. & BAINS, I. "The large-scale atomic and molecular gas in the Circinus galaxy". MNRAS, 389, 63-74 (2008). DA COSTA, G.S., JERJEN, H. & BOUCHARD, A. "ESO540-032: a transition-type dwarf in the Sculptor group". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 123-126 (2008). *DAWSON, J.R., MIZUNO, N., ONISHI, T., McCLURE-GRIFFITHS, N.M. & FUKUI, Y. "The `Carina Flare' super shell: probing the atomic and molecular ISM in a Galactic chimney". MNRAS, 387, 31-44 (2008). DICKEN, D., TADHUNTER, C ., MORGANTI, R. et al. "The origin of the infrared emission in radio galaxies. I. New mid- to far-infrared and radio obser vations of the 2 Jy sample". ApJ, 678, 712-728 (2008). *DOBASHI, K., BERNARD, J.-P., HUGHES, A. et al. "Extinction and dust/gas ratio in LMC molecular clouds". A&A, 484, 205-223 (2008).

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DODSON, R. "Fir st VLBI obser vations of methanol maser polarisation, in G339.88-1.26". A&A, 480, 767-773 (2008). *DODSON, R., FOMALONT, E.B., WIIK, K., HORIUCHI, S., HIRABAYASHI, H., EDWARDS, P.G. et al. "The VSOP 5 GHz Active Galactic Nucleus Sur vey. V. Imaging results for the remaining 140 sources". ApJS, 175, 314-355 (2008). DUBNER, G., GIAC ANI, E. & DECOURCHELLE, A. "High resolution radio study of the pulsar wind nebula within the supernova remnant G0.9+0.1". A&A, 487, 1033-1040 (2008). ECKART, A. et al. "Prospects for obser ving the Galactic Center : combining LBT LINC-NIRVANA obser vations in the near-infrared with obser vations in the mm/sub-mm wavelength domain". In: Optical and Infrared Interferometr y, Mar seille , France , 23 June 2008, Proc. SPIE, 7013, 70134L (2008). *ELLINGSEN, S.W., HAMPSON, G.A. & CHILDERS, R.K. "Argus: an L-band all-sky astronomical sur veillance system". IEEE Trans. Antenn. Propag., 56, 294-302 (2008). EMONTS, B.H., MORGANTI, R., OOSTERLOO, T.A. et al. "Enormous disc of cool gas surrounding the nearby powerful radio galaxy NGC612 (PKS0131-36)". MNRAS, 387, 197-208 (2008). *ENOMOTO, R., HIGASHI, Y., YOSHIDA, T., TANIMORI,T., BICKNELL, G.V., CLAY, R.W., EDWARDS, P.G. et al. "Cangaroo-III search for gamma rays from Kepler's supernova remnant". ApJ, 683, 383-388 (2008). ESAMDIN, A. et al. "Timing obser vations of rotating radio transient J1819-1458 at Ur umqi obser vator y". MNRAS, 389, 1399-1404 (2008). FAUCHER-GIGUERE, C .-A. & KASPI, V.M. "Bir th and evolution of isolated radio pulsar s". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More, Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 607-609 (2008). *FEAIN, I.J., CORNWELL, T.J., EKERS, R.D., NORRIS, R.P., GAENSLER, B.M., OTT, J., JOHNSTON-HOLLITT, M., MURPHY, T., MIDDELBERG, E. & BLAND-HAWTHORN, J. "A long overdue synthesis image of Centaur us A". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 287-288 (2008). *FERDMAN, R.D., STAIRS, I.H., KRAMER, M., MANCHESTER, R.N. et al. "The double pulsar : evolutionar y constraints from the system geometr y". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 474-478 (2008). FILIPOVIC ,M.D.etal."NewXMM-Newtonobser vationsofsupernovaremnantsintheSmallMagellanicCloud".A&A,485,63-70(2008). *FORD, H.A., McCLURE-GRIFFITHS, N.M., LOCKMAN, F.J., BAILIN, J., C ALABRETTA, M.R., KALBERLA, P.M., MURPHY, T. & PISANO, D.J. "H I clouds in the lower halo. I. The Galactic All-Sky Sur vey pilot region". ApJ, 688, 290-305 (2008). *FREUDLING, W., C ATINELLA, B., C ALABRETTA, M. et al. "The ALFA Ultra Deep Sur vey (AUDS)". In: The Evolution of Galaxies Through the Neutral Hydrogen Window, Arecibo Obser vator y, Puer to Rico, 1-3 Febr uar y 2008, AIP Conf. Proc., 1035, 242-245 (2008). *GAENSLER, B.M., TANNA, A., SLANE, P.O., BROGAN, C .L., GELFAND, J.D., McCLURE-GRIFFITHS, N.M. et al. "(Re-)discover y of G350.1-0.3: a young, luminous supernova remnant and its neutron star". ApJ, 680, L37-L40 (2008). *GIROLETTI, M., GIOVANNINI, G., COTTON, W.D., TAYLOR, G.B., PEREZ-TORRES, M.A., CHIABERGE, M. & EDWARDS, P.G. "The jet of Mar karian 501 from millions of Schwarzschild radii down to a few hundreds". A&A, 488, 905-914 (2008). *GONZALEZ-NUEVO, J., MASSARDI, M. et al. "Statistical proper ties of extragalactic sources in the New Extragalactic WMAP Point Source (NEWPS) catalogue". MNRAS, 384, 711-718 (2008). *GRANET, C ., KOT. J.S., HAY, S.G. & O'SULLIVAN, J.D. "A study of optimized dual-reflector systems with phased array feeds for `ASKAP' ". In: Wor kshop on Applications of Radio Science (WARS 2008), Broadbeach, Qld, 10-12 Febr uar y 2008, 6 pp. (2008). GRCEVICH, J., PUTMAN, M. & PEEK, J.E.G. "H I in local group dwarf galaxies". In: The Evolution of Galaxies Through the Neutral Hydrogen Window, Arecibo Obser vator y, Puer to Rico, 1-3 Febr uar y 2008, AIP Conf. Proc., 1035, 159-162 (2008). *GREEN,J.A.,C ASWELL,J.L.,FULLER,G.A.,BREEN,S.L.,BROOKS,K.,BURTON,M.G.,CHRYSOSTOMOU,A.,COX,J.,DIAMOND,P.J.,ELLINGSEN, S. P., GRAY, M. D., HOARE, M. G., MASHEDER, M. R. W., McCLURE-GRIFFITHS, N., PESTALOZZI, M., PHILLIPS, C ., QUINN, L., THOMPSON, M. A., VORONKOV, M. et al. "Multibeam maser sur vey of methanol and excited OH in the Magellanic Clouds: new detections and maser abundance estimates". MNRAS, 385, 948-956 (2008). *HALPERN,J.P.,GOTTHELF,E.V.,REYNOLDS,J.,RANSOM,S.M.&C AMILO,F."Outbur stofthe2sanomalousX-raypulsar1E1547.0-5408".ApJ, 676, 1178-1183 (2008). *HAVERKORN, M., BROWN, J.C ., GAENSLER, B.M. & McCLURE-GRIFFITHS, N.M. "The outer scale of turbulence in the magnetoionized galactic inter stellar medium". ApJ, 680, 362-370 (2008). *HAY, S.G., O'SULLIVAN, J.D. & MITTRA, R. "Analysis of connected patch arrays using the characteristic basis function method". In: IEEE International Symposium on Antennas and Propagation (AP-S 2008), San Diego, Calif., 5-12 July 2008, ar t. no. 4619541, (2008). *HAYMAN, D.B., BERESFORD, R., BUNTON, J.D., C ANTRALL, C ., CORNWELL, T., GRANCEA, A., GRANET C ., JOSEPH, J., KESTEVEN, M.J., O'SULLIVAN, J.D., PATHIKULANGARA, J., SWEETNAM, A.W. & VORONKOV, M. "The NTD interferometer : a phased array feed test bed". In: Wor kshop on Applications of Radio Science (WARS 2008) : Australian SKA Pathfinder special session, Broadbeach, Qld, 10-12 Febr uar y 2008, 6 pp. (2008). *HENKEL, C ., BRAATZ, J.A., MENTEN, K.M. & OTT, J. "The kinetic temperature of a molecular cloud at redshift 0.9: ammonia in the gravitational lens PKS 1830-211". A&A, 485, 451-456 (2008).

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*HENNING, P.A., SPRINGOB, C .M., DAY, F., MINCHIN, R., MOMJIAN, E., C ATINELLA, B., MULLER, E., KORIBALSKI, B.S. et al. "The ALFA Zone of Avoidance Sur vey". In: The Evolution of Galaxies Through the Neutral Hydrogen Window, Arecibo Obser vator y, Puer to Rico, 1-3 Febr uar y 2008, AIP Conf. Proc., 1035, 246-248 (2008). *HESSELS, J.W., NICE, D.J., GAENSLER, B.M., KASPI, V.M., LORIMER, D.R., CHAMPION, D.J. et al. "PSR J1856+0245: Arecibo discover y of a young, energetic pulsar coincident with the TeV gamma-ray source HESS J1857+026". ApJ, 682, L41-L44 (2008). *HIGASHI, Y., KUBO, H., YOSHIDA, T., ENOMOTO, R., TANIMORI, T., EDWARDS, P.G. et al. "Obser vation of ver y high energy gamma rays from HESS J1804-216 with C ANGAROO-III telescopes". ApJ, 683, 957-966 (2008). *HOBBS, G. "Gravitational wave detection using high precision pulsar obser vations". Classical & Quantum Gravity, 25, 114032 (2008). *HOBBS, G., JENET, F., LOMMEN, A., COLES, W., VERBIEST, J.P. & MANCHESTER, R.N. "Using pulsar s to limit the existence of a gravitational wave background". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 630-632 (2008). *HOPKINS, A.M., McCLURE-GRIFFITHS, N.M. & GAENSLER, B.M. "Linked evolution of gas and star formation in galaxies over cosmic histor y". ApJ, 682, L13-L16 (2008). *HUGHES, A., WONG, T., OTT, J., MULLER, E., PINEDA, J.L. & MIZUNO, Y. "Atomic gas associated with GMCs in the LMC". In: Galaxies in the Local Volume, Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 293-294 (2008). *HUYNH, M.T., JACKSON, C .A., NORRIS, R.P. & FERNANDEZ-SOTO, A. "Radio obser vations of the Hubble Deep Field-South region. IV. Optical proper ties of the faint radio population". AJ, 135, 2470-2495 (2008). JACKSON, J.M. et al. "The Galactic distribution of infrared dar k clouds". ApJ, 680, 349-361 (2008). *JOHNSTON, S., KARASTERGIOU, A., MITRA, D. & GUPTA, Y. "Multifrequency integrated profiles of pulsar s". MNRAS, 388, 261-274 (2008). *JOHNSTON, S., TAYLOR, R., BAILES, M., BARTEL, N., BAUGH, C ., BIETENHOLZ, M., BLAKE, C ., BRAUN, R., BROWN, J., CHATTERJEE, S., DARLING, J., DELLER, A., DODSON, R., EDWARDS, P., EKERS, R.D. et al. "Science with ASKAP: the Australian Square-Kilometre-Array Pathfinder". Experim. Astron., 22, 151-273 (2008). JOHNSTON-HOLLITT, M., SATO, M., GILL, J.A., FLEENOR, M.C . & BRICK, A.-M. "Radio obser vations of the Horologium-Reticulum supercluster. I. A3158: excess star-forming galaxies in a merging cluster?" MNRAS, 390, 289-303 (2008). JONES, P.A., BURTON, M.G. & CUNNINGHAM, M.R. "A 3-mm molecular line study of the central molecular zone". In: Far-Infrared and Submillimeter Emission of the Inter stellar Medium Wor kshop, Bad Honnef, Germany, 5-7 November 2007, EAS Pub. Ser., 31, 77-80 (2008). JONES, P.A., BURTON, M.G. et al. "Spectral imaging of the Sagittarius B2 region in multiple 3-mm molecular lines with the Mopra telescope". MNRAS, 386, 117-137 (2008). JONES, P.A., BURTON, M.G. & LOWE, V. "A 3-mm molecular line study of the Central Molecular Zone of the galaxy". In: IAU 251: Organic Matter in Space, Hong Kong, 18-22 Feb. 2008, Proc. IAU, 4, 257-262 (2008). KALEMCI, E., TOMSICK, J.A., MIGLIARI, S., CORBEL, S. & MARKOFF, S. "Galactic black holes in the hard state, a multi-wavelength view of accretion and ejection". In: Obser vational Evidence for Black Holes in the Univer se: Proc. 2nd Kolkata Conf., Kolkata, India, 10-15 Febr uar y 2008, AIP Conf. Ser., 1053, 201-208 (2008). KAMP, I., FREUDLING, W., ROBBERTO, M., CHENGALUR, J. & KETO, E. "Probing protoplanetar y disk evolution with the HI 21 cm line". Physica Scripta, T130, 014013 (2008). *KATAOKA, J., MADEJSKI, G., SIKORA, M., ROMING, P., CHESTER, M.M., GRUPE, D., TSUBUKU, Y., SATO, R., KAWAI, N., TOSTI, G., IMPIOMBATO, D., KOVALEV, Y.Y., KOVALEV, Y.A., EDWARDS, P.G. et al. "Multiwavelength obser vations of the powerful gamma-ray quasar PKS 1510-089: clues on the jet composition". ApJ, 672, 787-799 (2008). *KATAOKA, J., STAWARZ, L., HARRIS, D.E., SIEMIGINOWSKA, A., OSTROWSKI, M., SWAIN, M.R., HARDC ASTLE, M.J., GOODGER, J.L., IWASAWA, K.&EDWARDS,P.G."ChandrarevealstwinX-rayjetsinthepowerfulFRIIradiogalaxy3C353".ApJ,685,839-857(2008). *KEITH, M.J., JOHNSTON, S., KRAMER, M., WELTEVREDE, P., WATTERS, K.P. & STAPPERS, B.W. "A high-frequency search for radio pulsar s in three EGRET error boxes". MNRAS, 389, 1881-1884 (2008). *KERN, K.M., KILBORN, V.A., FORBES, D.A. & KORIBALSKI, B.S. "H I mapping of galaxies in six Group Evolution Multiwavelength Study groups". MNRAS, 384, 305-315 (2008). *KIRBY, E.M., JERJEN, H., RYDER, S.D. & DRIVER, S.P. "Deep near-infrared surface photometr y of 57 galaxies in the Local Sphere of Influence". AJ, 136, 1866-1888 (2008). KOBULNICKY, H.A. & SKILLMAN, E.D. "Inflows and outflows in the dwarf starbur st galaxy NGC 5253: high-resolution H I obser vations". AJ, 135, 527537 (2008). *KOMUGI, G., SOFUE, Y., KOHNO, K., NAKANISHI, H. et al. "Molecular gas distribution in barred and nonbarred galaxies along the Hubble sequence". ApJS, 178, 225-246 (2008). *KORIBALSKI, B.S. & JERJEN, H., eds. Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., (2008). *KORIBALSKI, B.S. & the LVHIS team "The Local Volume H I Sur vey (LVHIS)". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 41-44 (2008).

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*KRAAN-KORTEWEG, R.C ., SHAFI, N., KORIBALSKI, B.S. et al. "Outlining the Local Void with the Par kes H I ZOA and Galactic Bulge sur veys". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 13-16 (2008). *KRAMER, M. & JOHNSTON, S. "High-precision geometr y of a double-pole pulsar". MNRAS, 390, 87-92 (2008). LANDT, H. & BIGNALL, H.E. "On the relationship between BL Lacer tae objects and radio galaxies". MNRAS, 391, 967-985 (2008). LI, J. et al. "The 3-mm flux density monitoring of Sagittarius A* with the ATC A". In: IAU 248 : A Giant Step: from Milli- to Micro-Arcsecond Astrometr y, Shanghai, China, 15-19 October 2007 248, 204-205 (2008). LONGMORE, S.N., BURTON, M.G., PURCELL, C .R. & OTT, J. "Determining the relative evolutionar y stages of ver y young massive star formation regions". In: Massive Star Formation: Obser vations Confront Theor y, Heidelberg, Germany, 10-14 September, 2007, ASP Conf. Ser., 387, 58-70 (2008). *LOPEZ-SANCHEZ, A.R. & ESTEBAN, C . "Interactions and star formation activity in Wolf-Rayet galaxies". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 299-300 (2008). *LOPEZ-SANCHEZ, A.R. & ESTEBAN, C . "Massive star formation in Wolf-Rayet galaxies". A&A, 491, 131-156 (2008). *LOPEZ-SANCHEZ, A.R., KORIBALSKI, B.S., ESTEBAN, C . & GARCIA-ROJAS, J. "Ionized and neutral gas in the starbur st galaxy NGC 5253". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 53-56 (2008). *LOPEZ-SANCHEZ, A.R., KORIBALSKI, B.S., ESTEBAN, C . & HIBBARD, J. "Interactions and starbur st activity in galaxy groups: the case of Tol 9 in Klemola 13 group". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 301-302 (2008). *LOVELL, J.E.J., RICKETT, B.J., MACQUART, J.-P., JAUNCEY, D.L. et al. "The Micro-Arcsecond Scintillation-Induced Variability (MASIV) Sur vey. II. The fir st four epochs". ApJ, 689, 108-126 (2008). LYNE, A.G. "Par kes 20-cm Multibeam Pulsar Sur veys". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 561-566 (2008). *MANCHESTER, R.N. "The Par kes Pulsar Timing Array Project". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 584-592 (2008). *MAO, S.A., GAENSLER, B.M., STANIMIROVIC , S., HAVERKORN, M., McCLURE-GRIFFITHS, N.M., STAVELEY-SMITH, L. & DICKEY, J.M. "A radio and optical polarization study of the magnetic field in the Small Magellanic Cloud". ApJ, 688, 1029-1049 (2008). MARSEILLE, M. et al. "Evolution of massive protostar s: the IRAS 18151-1208 region". A&A, 488, 579-595 (2008). *MASSARDI, M., EKERS, R.D., MURPHY, T., RICCI, R., SADLER, E.M., BURKE, S., DE ZOTTI, G., EDWARDS, P.G., HANCOCK, P.J, JACKSON, C .A., KESTEVEN, M.J., MAHONY, E., PHILLIPS, C .J., STAVELEY-SMITH, L., SUBRAHMANYAN, R., WALKER, M.A. & WILSON, W.E. "The Australia Telescope 20-GHz (AT20G) Sur vey: the bright source sample". MNRAS, 384, 775-802 (2008). *MASSARDI, M., LAPI, A., DE ZOTTI, G., EKERS, R.D. & DANESE, L. "Obser vability of the virialization phase of spheroidal galaxies with radio arrays". MNRAS, 384, 701-710 (2008). *MATTHEWS, D., STAVELEY-SMITH, L., DYSON, P., McCLURE-GRIFFITHS, N. & MULLER, E. "Characterising Magellanic Stream turbulent H I". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 309-310 (2008). *McCLURE-GRIFFITHS, N.M., STAVELEY-SMITH, L., LOCKMAN, F.J., C ALABRETTA, M.R., FORD, H.A., KALBERLA, P.M.W., MURPHY, T., NAKANISHI, H. & PISANO, D.J. "An interaction of a Magellanic leading arm high-velocity cloud with the Milky Way disk". ApJ, 673, L143-L146 (2008). *MIDDELBERG, E., NORRIS, R.P., CORNWELL, T.J., VORONKOV, M.A., SIANA, B.D., BOYLE, B.J., CILIEGI, P., JACKSON, C .A., HUYNH, M.T. et al. "Deep Australia Telescope Large Array Sur vey radio obser vations of the European Large Area ISO Sur vey S1/Spitzer wide-area infrared extragalactic field". AJ, 135, 1276-1290 (2008). *MIDDELBERG, E., NORRIS, R.P., TINGAY, S., MAO, M.Y., PHILLIPS, C .J. & HOTAN, A.W. "The fir st VLBI image of an infrared-faint radio source". A&A, 491, 435-439 (2008). MIETTINEN, O. et al. "Radio continuum imaging of the R Coronae Austrinae star-forming region with the ATC A". A&A, 486, 799-806 (2008). *MINAMIDANI, T., MIZUNO, N., MIZUNO, Y., KAWAMURA, A., ONISHI, T., HASEGAWA, T., TATEMATSU, K., IKEDA, M., MORIGUCHI, Y., YAMAGUCHI, N., JURGEN, O., WONG, T., MULLER, E. et al. 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PASA, 25, 115 (2008). *NAKAMORI, T., KUBO, H., YOSHIDA, T., TANIMORI, T., ENOMOTO, R., BICKNELL, G.V., CLAY, R.W., EDWARDS, P.G. et al. "Obser vation of an extended ver y high energy gamma-ray emission from MSH 15-52 with C ANGAROO-III". ApJ, 677, 297-305 (2008). *NAKANISHI, H. et al. "Kiso Outer Galaxy Sur vey: stellar radial distribution of the Galaxy". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 315-316 (2008).

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*NG, C .-Y., GAENSLER, B.M., STAVELEY-SMITH, L., MANCHESTER, R.N., KESTEVEN, M.J., BALL, L. & TZIOUMIS, A.K. "Fourier modeling of the radio tor us surrounding SN 1987A". ApJ, 684, 481-497 (2008). NIDEVER, D.L., MAJEWSKI, S.R. & BURTON, W.B. "The origin of the Magellanic Stream and its leading arm". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 243-246 (2008). *NOUTSOS, A., JOHNSTON, S., KRAMER, M. & KARASTERGIOU, A. "New pulsar rotation measures and the Galactic magnetic field". MNRAS, 386, 1881-1896 (2008). *O'BRIEN, J.T., JOHNSTON, S., KRAMER, M., LYNE, A.G., BAILES, M., POSSENTI, A., BURGAY, M., LORIMER, D.R., McLAUGHLIN, M.A., HOBBS, G. et al. "PSR J1410-6132: a young, energetic pulsar associated with the EGRET source 3EG J1410-6147". MNRAS Lett. 388, L1-L5 (2008). *OHISHI, M., MORI, M., ADACHI, Y., ASAHARA, A., BICKNELL, G.V., CLAY, R.W., DOI, Y., EDWARDS, P.G. et al. 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Proc., 321-322 (2008). *OTT, J., WONG, T., PINEDA, J.L., HUGHES, A., MULLER, E. et al. "The molecular ridge close to 30 Doradus in the Large Magellanic Cloud". PASA, 25, 129-137 (2008). *PAPADOPOULOS, P.P., FEAIN, I.J., WAGG, J. & WILNER, D.J. "A new twist to an old stor y: HE 0450-2958 and the ULIRG --> optically bright QSO transition hypothesis". ApJ, 684, 845-852 (2008). PAYNE, J.L. et al. "Optical spectra of radio planetar y nebulae in the Small Magellanic Cloud". Serb. AJ, 176, 65-70 (2008). *PINER, B.G., PANT, N. & EDWARDS, P.G. "The par sec-scale jets of the TeV blazar s H1426+428, 1ES 1959+650, and PKS 2155-304: 2001-2004". ApJ, 678, 64-77 (2008). *POPPING, A. & BRAUN, R. "The standing wave phenomenon in radio telescopes: frequency modulation of the WSRT primar y beam". A&A, 479, 903-913 (2008). *PROTHEROE, R.J., OTT, J., EKERS, R.D., JONES, D.I. & CROCKER, R.M. 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THOMPSON, D.J. "Gamma-ray pulsar studies with GLAST". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 56-63 (2008). TRIGILIO, C ., LETO, P., UMANA, G., BUEMI, C .S. & LEONE, F. "The radio lighthouse CU Virginis: the spin-down of a single main-sequence star". MNRAS, 384, 1437-1443 (2008). *TRINCHIERI, G., IOVINO, A., POMPEI, E., DAHLEM, M. et al. "Detection of a hot intergalactic medium in the spiral-only compact group SCG00184854". A&A, 484, 195-203 (2008). *TUDOSE, V., FENDER, R.P., TZIOUMIS, A.K., SPENCER, R.E. & VAN DER KLIS, M. "A decade of radio imaging the relativistic outflow in the peculiar X-raybinar yCircinusX-1"MNRAS,390,447-464(2008). UMANA, G., TRIGILIO, C ., CERRIGONE, L., BUEMI, C .S. & LETO, P. "ATC A obser vations of the ver y young Planetar y Nebula SAO 244567". MNRAS, 386, 1404-1410 (2008). URQUHART, J.S., BUSFIELD, A.L., HOARE, M.G., et al. "The RMS sur vey: 13CO obser vations of candidate massive YSOs in the nor thern Galactic plane". A&A, 487, 253-264 (2008). *VERBIEST, J.P., BAILES, M., VAN STRATEN, W., HOBBS, G.B., EDWARDS, R.T., MANCHESTER, R.N., BHAT, N.D., SARKISSIAN, J.M. et al. "Precision timing of PSR J0437-4715: an accurate pulsar distance , a high pulsar mass, and the limit on the variation of Newton's gravitational constant". ApJ, 679, 675-680 (2008). *WALSH, A.J., LO, N., BURTON, M.G., WHITE, G.L., PURCELL, C .R., LONGMORE, S.N., PHILLIPS, C .J. & BROOKS, K.J. "A pilot sur vey for the H2O Southern Galactic Plane Sur vey". PASA, 25, 105-113 (2008). *WANG,N.,YAN,Z.,MANCHESTER,R.N.&WANG,H.X."Dailyobser vationsofinter stellarscintillationinPSRB0329+54".MNRAS,385,13931401 (2008). *WELTEVREDE, P. & JOHNSTON, S. "The population of pulsar s with interpulses and the implications for beam evolution". MNRAS, 387, 1755-1760 (2008). *WELTEVREDE, P. & JOHNSTON, S. "Profile and polarization characteristics of energetic pulsar s". MNRAS, 391, 1210-1226 (2008). *WELTEVREDE, P., RANKIN, J., STAPPERS, B. & WRIGHT, G. "Pulsar B0656+14: highly unusual emission proper ties and a local RRAT". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 79-81 (2008). *WELTEVREDE, P., STAPPERS, B. & EDWARDS, R.T. "The subpulse modulation proper ties of pulsar s and its frequency dependence". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 43-46 (2008). *WESTMEIER, T., BRAUN, R., BRUNS, C ., KERP, J. & THILKER, D.A. "The relics of str ucture formation: high-velocity clouds around M 31". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 235-238 (2008). *WESTMEIER, T., BRUNS, C . & KERP, J. "Relics of str ucture formation: extra-planar gas and high-velocity clouds around the Andromeda Galaxy". MNRAS, 390, 1691-1709 (2008). *WESTMEIER, T. & KORIBALSKI, B.S. "The scattered debris of the Magellanic Stream". MNRAS Lett., 388, L29-L33 (2008). *WHITING, M.T. "Astronomer s! Do you know where your galaxies are?". In: Galaxies in the Local Volume , Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 343-344 (2008). *WHITNEY, B.A. et al., "Spitzer SAGE sur vey of the Large Magellanic Cloud. III. Star formation and ~1000 new candidate Young Stellar Objects". AJ, 136, 18-43 (2008). *WONG, O.I., WEBSTER, R.L., WAUGH, M., KILLBORN, V.A. & STAVELEY-SMITH, L. "Near-infrared proper ties of NOIRC AT". In: Galaxies in the Local Volume, Sydney, NSW, 8-13 July 2007, Astrophys. & Space Sci. Proc., 347-348 (2008). * WONG, T., LADD, E.F., BRISBIN, D., BURTON, M.G., BAINS, I., CUNNINGHAM, M.R., LO, N., JONES, P.A., THOMAS, K.L., LONGMORE, S.N. et al. "Molecular line mapping of the giant molecular cloud associated with RCW 106. II. Column density and dynamical state of the clumps". MNRAS, 386, 1069-1084 (2008). * WU, J.H.P., CHIUEH, T.H. et al., KESTEVEN, M.J., WILSON, W. et al. "AMiBA: fir st-year results for Sunyaev-Zel'dovich effect". Mod. Phys. Lett. A, 23 (1720), 1675-1686 (2008). *YAMAMOTO, H., ITO, S., ISHIGAMI, S., FUJISHITA, M., KAWASE, T., KAWAMURA, A., MIZUNO, N., ONISHI, T., MIZUNO, A., McCLURE-GRIFFITHS, N.M. & FUKUI, Y. "Aligned molecular clouds towards SS 433 and L=348o.5: possible evidence for a galactic "vapor trail" created by a relativistic jet". PASJ, 60, 715-729 (2008). *YARDLEY, D.R.B. "Correlations in the Par kes Pulsar Timing Array". In: 40 Year s of Pulsar s: Millisecond Pulsar s, Magnetar s and More , Montreal, Que ., 12-17 August, 2007, AIP Conf. Proc., 983, 636-638 (2008). *ZOU, W.Z., WANG, N., MANCHESTER, R.N., URAMA, J.O., HOBBS, G., LIU, Z.Y. & YUAN, J.P. "Obser vations of six glitches in PSR B1737-30". MNRAS, 384, 1063-1068 (2008).

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ATNF outreach

ATNF teacher workshops
Rob Hollow (ATNF) Two teacher wor kshops were r un by ATNF in the fir st half of 2008. Astrophysics for Physics Teachers was a one-day wor kshop at Mar sfield in April. Par ticipants heard talks about stellar evolution and explored useful classroom activities. A highlight of the wor kshop was the fir st Live from Gemini video conference session in which Gemini Outreach Scientist, Dr Scott Fisher, discussed modern optical/infra-red (IR) obser ving with the teacher s from the Gemini control room at Hilo in Hawaii. The annual three-day Astronomy from the Ground Up! wor kshop was a great success at Par kes in May. Clear skies allowed for plenty of viewing at night to complement the varied range of daytime talks and practical sessions. ATNF has expanded its collaboration with other organisations to offer teacher professional development around Australia. Wor kshops were held at the SPICE Centre at the Univer sity of Western Australia, the Victorian Space Science Education Centre and at the Univer sity of Southern Queensland at Toowoomba through the suppor t of the Queensland Depar tment of Education, Training and the Ar ts. Wor kshops were also held in regional Western Australia (WA) in Geraldton and Kalgoor lie in conjunction with Astronomy WA. Wor kshop sessions were also held at several Science Teacher state and national conferences including CONASTA at the Gold Coast in July.

ASKAP outreach
Rob Hollow (ATNF) Mar y Mulcahy and Rob Hollow visited Pia Wadjarri Remote Community School, near Boolardy in WA, in October for an activity-filled day of astronomy. They were accompanied by Professor Steven Tingay and Dr Megan Argo from Cur tin Univer sity. The Pia students were joined once again by those from Yalgoo Primar y School who came up for an overnight excur sion. Daytime activities included size and scale of the Solar System, constellations and sky pattern plus balloon and water rockets. Unfor tunately a cloudy night prevented the students from looking through the telescopes at the night sky but hopefully the next visit will be clearer. Whilst in Geraldton we briefed local teacher s and other interested par ties about the Australian Square Kilometre Array Pathfinder (ASKAP) and educational oppor tunities.

Art meets science at telescope open day
Helen Sim (ATNF) CSIRO's Australia Telescope Compact Array mar ked its twentieth bir thday on Saturday 19 July 2008 with an open day that drew more than five hundred visitor s. The radio telescope , near Narrabri NSW, is opened to the public only once ever y two year s. Visitor s were given guided tour s of the antennas, quizzed astronomer s in the control room, heard talks on different aspects of astronomy, and yarned with staff about the cosmos. In the two weeks leading up to the open day the Compact Array hosted an Ar tist-in-Residence, award winning ar tist Christine Hill. During the residency Christine painted pictures of people and daily life at the obser vator y, held wor kshops for school children who painted their interpretations of space, and culminated the residency at the open day with an exhibition and interactive public activities.

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Above and top right: Teacher and students enjoying the astronomy day activities at Pia Wadjarri Remote Community School, assisted by Megan Argo (Curtin University of Technology), Mary Mulcahy (ATNF) and Steven Tingay (Curtin University of Technology) respectively. Right: Participants from the annual Astronomy from the Ground Up! workshop held at Parkes in May get to experience the dish close-up. Photos: Robert Hollow, CSIRO Bottom right: Narrabri Artist-in-Residence Christine Hill with children and their artworks. Photo: Joanne Houldsworth, CSIRO Below:Vicki Fraser (ATNF) greeting visitors at the Compact Array open day. Photo: Phil Crosby, CSIRO

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For further information: C S IRO Australia Telescope National Facilit y E m a i l e n q u i r i e s : a t nf - e n q u i r i e s @ c s i r o . a u , E m a i l n e w s l e t t e r : n e w s l e t t e r @ a t nf . c s i r o . a u Web centr al : w w w. atnf.csiro. au Web newslet ter : w w w. atnf.csiro. au / news / newslet ter, Web ou tr each : ou tr each. atnf.csiro. au

Dr Phil Edwards preparing to light the candles on the 20th birthday cake at the ATNF Compact Array Open Day held in July 2008 at Narrabri. An eager crowd of children looks on. Photo: Phil Crosby, CSIRO