ATNF News Issue No. 70, April 2011 ISSN 1323-6326 CSIRO Astronomy and Space Science – undertaking world leading astronomical research and operator of the Australia Telescope National Facility. The Parkes Phased Array Feed (PAF) package, partially rotated, showing the chequerboard array minus the weather cover. The ability to invert the PAF package during and after assembly enables efficient final construction and, most importantly, safe transport and readiness for sky testing. Credit: Russ Bolton, CSIRO

Cover page image

Australian Pathfinder (ASKAP) antenna construction. Credit: Antony Schinckel, CSIRO

2 Issue No. 70, April 2011 Contents

From the Chief of CSIRO Astronomy and Space Science...... 4 New Deputy Chief for CASS...... 5 Distinguished Visitors...... 6 Graduate Student Program...... 7 Grote Reber Gold Medal Awarded...... 8 CSIRO Chief Visits Parkes...... 9 Ruby Payne-Scott: First in : Australia Day 1946...... 10 Operations Engineering Cadetship Experience...... 14 ASKAP and SKA News...... 16 Compact Array 20/13 cm and 6/3 cm Receiver Upgrade...... 20 CASS Teacher Scholarship...... 22 S-PASS: S-band Polarisation All Sky Survey...... 24 CABB Zoom Modes Produce New Science...... 28 ATCA Discovers an Ionised Jet Associated With a Young High-mass Star G345.5+01.5...... 30 SZ and X-ray Peaks Don’t Correspond...... 32 Education and Outreach...... 34 Operations...... 35 Publications List...... 37

Editorial

Welcome to this the April edition of In other science reports we feature As always, we provide our regular ATNF News for 2011. Once again we a report on the Sunyaev-Zel’dovich in-depth update on CSIRO’s bring you articles and news items effect in galaxy clusters and we ASKAP and SKA related activity. of interest, all associated with the look at some new science emerging It’s a busy year at the Murchison operation of our National Facility. via the new “zoom” modes of the Radio-astronomy Observatory Compact Array spectrometer. with the construction of support In a feature packed issue, Miller infrastructure and ASKAP’s Goss captures the past, detailing We then talk with new CASS remaining antennas both under way. Ruby Payne-Scott’s pioneering Deputy Chief Sarah Pearce who work in radio astronomy and the joins us from GridPP (the UK To conclude, we finish with our first use of a radio astronomical computing grid for particle physics, regular Operations report. interferometer at Dover Heights set up to deal with data from We hope you enjoy the issue. on Australia Day, 1946. CERN’s Large Hadron Collider). Your comments and suggestions Welcome aboard Sarah! We’re then back to the present are always welcome. If you’d day with a number of science In other news, Mark Bowen like to contribute to future articles focused on the latest reports on receiver upgrades editions of the ATNF News, please in radio astronomical research. at the Compact Array, CASS contact the newsletter team. This includes an article by CASS Teacher Scholar Stephen scientist Ettore Carretti who Broderick enjoys his week with Tony Crawshaw and provides his latest update on the the PULSE@Parkes project team, Joanne Houldsworth S-band Polarisation All Sky Survey and we report on this year’s The ATNF Newsletter Production Team (S-PASS). The survey has mapped Grote Reber Gold Medal Award ([email protected]) the diffuse polarised emission of recipient — . the entire southern sky with the Parkes at 2.3 GHz.

3 From the Chief of CSIRO Astronomy and Space Science Phil Diamond Chief of CASS

This, the 70th edition of the attendees from CSIRO, and not be final until the CSIRO Board ATNF Newsletter, again the Director of the Australian formally approves it on 29 June. Astronomical Observatory The second day of the meeting demonstrates the breadth of (AAO). The membership can be started with an update of the status found on the ATNF web site. science undertaken with the of the Square Kilometre Array (SKA) ATNF facilities; the quality of The Committee’s principal role is to project; this was enhanced by the the engineering that supports offer advice to the ATNF Director. I very welcome announcement by can safely say that they are not shy in the government in the previous the telescopes and the providing such advice, but it is always evening’s budget of $40.2m for professionalism of the operations done in a friendly and positive the pre-construction stage of manner. At the recent meeting the the SKA, scheduled to run from and other support staff that agenda covered those topics that January 2012 until December 2015. enables the whole endeavour to you would expect to be discussed, The delivery of the full amount work at a continuing high level. such as a report on recent science is contingent upon a successful results from the ATNF, an update outcome for Australia–New Zealand This sentiment is strongly supported on the status of engineering projects in the site selection process. and on operations. A major focus by the ATNF Steering Committee, I am sure that the highlight of the of the meeting was a presentation which met on the 10 – 11 May meeting for the Committee was the of the first complete version at Parkes. The Committee was so-called “hay ride” on the Parkes of the science and engineering keen to travel to one of the telescope itself. The telescope operations plan for the Australian telescopes, and will continue to was lowered to almost 0 degrees Square Kilometre Array Pathfinder do so in the future, ensuring that elevation, the committee stepped (ASKAP). It is expected that the it rotates around all CASS/ATNF onto the surface and were then plan will evolve as we receive sites in time. The Committee raised above the observatory input from bodies such as the has a varied membership, as the dish returned to point at Steering Committee, the Users’ with three astronomers from the zenith. The trick is to walk Committee, the ASKAP Science Australian institutes, three from down the dish surface as the local Survey Teams and CASS staff. the international community— horizontal changes! All Committee currently from China, Germany The Committee also received a members managed to do so and and the USA; two other members presentation, and entered into a were later seen safely to the bus are non-astronomers representing discussion on the proposed four- to whisk them off to the airport. the broader Australian community year budget for the ATNF and A great finale to the day! and there are two ex-officio CASS as a whole. This budget will

4 Issue No. 70, April 2011 New Deputy Chief for CASS Tony Crawshaw (CASS)

ATNF News Editor Tony Crawshaw spent some time speaking with Dr Sarah Pearce, new CASS Deputy Chief.

Hi Sarah. Welcome to CSIRO and more specifically to CASS. Thank you very much. I’m very happy to be here!

We’re happy as well. Could you tell us something of your background? I was project manager for GridPP, Dr Sarah Pearce which runs the UK computing grid Credit: Tony Crawshaw, CSIRO for particle physics, set up to deal with data from CERN’s (European Organisation for Nuclear Research) Large Hadron Collider. I worked It was fascinating to see behind And your inspiration in joining CASS? for them for six years, first of all in the scenes how politics worked, Working for GridPP, I really enjoyed a dissemination role and then as though in the end I found the being part of one of the world’s project manager. It was very exciting adversarial nature of the system largest science projects. I’d also to work as (a small) part of such a a bit limiting. So I moved back to been aiming to move back to large and high profile project, and science, where I think we all work astronomy: although I liked working I was impressed with how well together much more effectively. managed and organised the particle in particle physics, it was never physics community is. GridPP was You’re obviously well qualified. really “my” field. Living in Australia a distributed project, at 16 UK Where did you study? and looking to work in astronomy, sites and CERN, so it was good CASS was the obvious choice. As I have a degree in physics from preparation for working in CASS. well as the world-class work at Oxford, then a PhD from Leicester Parkes and the Compact Array, And prior to that? University. For my PhD I worked on there is ASKAP construction and calibrating the microchannel plate then operations to look forward to. Before I started with GridPP, detectors for the Chandra X-ray I worked in policy for the UK And if the SKA comes to Australia, observatory, using the Daresbury CASS will be at the centre of government and Parliament. synchrotron in the UK. I also went Parliament was particularly that process, playing a key role in to International Space University Australia’s largest science facility. interesting; I was a science adviser, for the summer session in 1994, writing briefing material on policy where I had an amazing 10 weeks in So in your role as CASS Deputy Chief questions to do with IT and physics. Barcelona—I’d highly recommend it what are your key responsibilities? I covered some controversial topics, to anyone who is interested in space including missile defence, internet science, engineering or astronomy. My position on the management regulation and nuclear power. team is focussed towards CASS

5 Distinguished Visitors Robert Braun (CASS)

as an organisation, rather than fields, whether that’s engineering, Over the past months we have externally. So I’m responsible for astronomy, or computer science, enjoyed working visits from Aris issues such as staffing, Health Safety and they are all keen to do an Karastergiou (University of Oxford, & Environment and communications. outstanding job that delivers UK) and Bill Coles (University I’m also working closely on the world-class science. I’m particularly of San Diego, USA) budget: we’re currently in the midst impressed with how long staff seem Upcoming visitors we expect of preparing a four year plan as part to work for CASS—there have include Patricia Henning (University of the Strategic Investment Process, been several long service awards of New Mexico, USA), Jose which takes in ASKAP construction since I got here! I also appreciate Gomez (Instituto de Astrofísica de and the start of operations, so it’s the collegiate atmosphere: Andalucía, Grenada, Spain), Dale a very useful time to join CASS everyone I’ve met has been Frail (National Radio Astronomy and work towards that goal. extremely helpful and welcoming. Observatory, USA), Paul Nulsen (Harvard-Smithsonian Center And what do you hope to Finally, what in particular for , USA), Martin achieve in the role? excites you about the field of astronomy and space science? Cohen (, I hope to help guide CASS through Berkeley, USA) and Jim Jackson the changes that are coming in the I’ve been fascinated with astronomy (Boston University, USA). next few years. With ASKAP, and in all its facets since I was in school. The Distinguished Visitors program potentially the SKA, this period It started with some of the popular remains a very productive means is a very dynamic one for radio books on , such as In of enabling collaborative research astronomy in Australia. This is an search of the by John projects with local staff, adding unprecedented investment, which Gribbin and Steven Weinberg’s substantially to the vitality of the will mean new ways of working and The first three minutes. I found, and research environment. Visits can be doing science. We need to make still find, the scale of astronomy organized for periods ranging from sure we can move towards this new compelling. As Douglas Adams only a few weeks up to one year. era without losing the expertise and said: “Space... is big. Really big. excellence that has led to CSIRO’s You just won’t believe how vastly For more information please see hugely mindboggingly big it is...” leading position in radio astronomy. www.atnf.csiro.au/people/ I think that’s what I like about it: distinguished_visitors.html I know it’s only been a short astronomy dwarfs all the other while, but what are your first sciences, both in scale and in some Prospective visitors should impressions of CASS? of the concepts it explores. contact the local staff member I’m very impressed with the with the most similar interests. Thanks for your time Sarah. dedication of all the staff at CASS. They are at the cutting edge in their My pleasure.

6 Issue No. 70, April 2011 Graduate Student Program Baerbel Koribalski (CASS)

We would like to officially welcome • Annie Hughes (University of the following students into the Swinburne)—Molecular Gas ATNF co-supervision program. in the Large Magellanic Cloud. • Paul Coster (University of • Joanne Dawson (University of Swinburne)—Accelerated Nagoya, Japan)—Supershells searches for the most relativistic as Molecular Cloud Factories in binary using next- the Evolving ISM: Observations generation instrumentation of HI and 12CO in the Galactic Natasa Vranesevic with supervisors Dr Willem Supershells GSH 287+04- van Straten (University 17 and GSH 277+00+36. of Swinburne), Dr Simon • Sarah Burke-Spolaor (University Johnston (CASS) and Dr of Swinburne)—Supermassive Mike Keith (CASS). Black Hole Binaries and • Phoebe de Wilt (University Transient Radio Events: of Adelaide)—Investigating Studies in Astronomy. the connection between star • Natasa Vranesevic (University forming regions and unidentified of Sydney)—Galactic distribution TeV gamma-ray sources with and evolution of pulsars. supervisors Dr Gavin Rowell (University of Adelaide), Dr Dr Annie Hughes is now a postdoc Kate Brooks (CASS) and at the Max Planck Institute in Dr Jill Rathborne (CASS). Heidelberg, Germany. Dr Sarah • Stuart Weston (University of Burke-Spolaor is now a Bolton Auckland, NZ)—Development Fellow at CSIRO Astronomy and and Astrophysical Applications Space Science. And Dr Jo Dawson Sara Burke-Spolaor of the High Performance Radio is now an Australian Research Astronomical Image Processing Council Super Science Fellow at Pipeline for e-VLBI with the University of . supervisors Dr Sergei Gulyaev Well done ! (University of Auckland, NZ) A summary of the ATNF Graduate and Dr Tim Cornwell (CASS). Student Program, current and Congratulations to the award past students,as well as new of their PhD degree and best application forms can be found at wishes for their future career http://www.atnf.csiro.au/research/ goes to the following students. graduate/scholars.html

7 Grote Reber Gold Medal Awarded Ken Kellerman (NRAO)

The 2011 Grote Reber Gold Medal for lifetime innovative contributions to radio astronomy will be awarded to Dr Jocelyn Bell Burnell who is currently a Professor of Astrophysics at Oxford University in . Burnell is being honored for her dramatic 1967 discovery of pulsars which has had a major impact on the second half of 20th century astrophysics and her continuing contributions to astrophysics and education.

Jocelyn Bell Burnell received her she noticed a peculiar form of a first degree in Physics in 1965 from signal which had a periodic pulse Glasgow University in Scotland rate close to one second. Like and her PhD from the University Grote Reber, she initially had to of Cambridge in 1968. Following a convince her better established two year Science Research Council colleagues that her observations Jocelyn Bell Burnell Fellowship, she held a Teaching were important for astronomy and Credit: University of Bath Fellowship at the University of not due to external interference or Southampton followed by research to a spurious instrumental effect. and management positions at She has previously been honored The 2011 Reber Medal will be the University College, London by many prizes and recognitions, presented to Dame Jocelyn in and the Royal Observatory in including the Albert Michelson August 2011 at the XXX URSI Edinburgh. After a ten year period Medal of the Philadelphia Franklin General Assembly in Istanbul, as a Professor of Physics at the Institute, the J Robert Oppenheimer Turkey. The Reber Medal was Open University of the United Memorial Prize from the Miami established by the Trustees of the Kingdom where she studied X-ray Center for Theoretical Studies, the Grote Reber Foundation to honor sources, she served as Dean of Tinsley Prize from the American the achievements of Grote Reber Science at the University of Bath. Astronomical Society, and the and is administered by the Queen Bell Burnell is best known for her Herschel Medal from the Royal Victoria Museum in Launceston, role in the discovery of pulsars. As Astronomical Society. She has Tasmania. Nominations for the a research student in Cambridge served as President of the Royal 2012 Medal may be sent to Martin she was heavily involved in the Astronomical Society, is a Fellow of George, Queen Victoria Museum, construction and operation of a long the Royal Society, is currently the Wellington St, Launceston, Tasmania wavelength radio telescope built to President of the Institute of Physics, 7250, Australia or by email to: study interplanetary scintillations and in June 2007, she was made [email protected] at 4-m wavelength. Later, while Dame Commander of the British to be received no later inspecting the output chart records, Empire (DBE) by Queen Elizabeth II. than 15 October 2011.

8 Issue No. 70, April 2011 CSIRO Chief Visits Parkes Erik Lensson (CASS)

CSIRO Chief Executive Megan Clark at Parkes. Credit: John Sarkissian, CSIRO

CSIRO Chief Executive Megan Clarke visited the Parkes for the analogue human interface. She was also interested in the new Observatory on 21 March 2011, accompanied by her husband Parkes backend switch, its impact Trent. The visit included an inspection of the refurbished Visitors on existing and future observing Centre, as well as discussion of astronomical observing trends and how remote observing might develop with systems providing with ATNF Science Operations and Astrophysics staff. tactile feedback and virtual reality technology. Ken Reeves took Trent A site tour with Engineering (MCP), a key achievement for the up the dark central column for Operations included the 12-m March 2011 a look at the “Cricket Pitch” on ASKAP Test Bed and a discussion shutdown. Megan appreciated the the surface of the Dish. Megan with Andrew Hunt and Tim Ruckley retro look whilst noting the all new and Trent then enjoyed informal about the new Parkes 64-m computer controllable electronics discussions and morning tea antenna Master Control Panel and agreed that there is still a place with staff at Parkes Quarters.

9 Ruby Payne-Scott: First Interferometry in Radio Astronomy: Australia Day 1946 Miller Goss (NRAO)

At sunrise on Australia Day 1946 (26 January), Ruby Payne- Scott (Figure 1) observed the sun at Dover Heights, the first use of a radio astronomical interferometer. She had been employed by the Council for Scientific and Industrial Research, Division of Radiophysics since 1941. Payne-Scott used a 200-MHz antenna, a portion of a shore defence radar system (Figure 2), constructed during the early years of World War II (WWII). By early 1946 the Australian Army had allowed the Radiophysics Laboratory Figure 1: Ruby Payne-Scott as a young student in the 1930s, possibly (RPL) to use the receiving aerial while she was a student at the University of Sydney 1929 – 1932, working for radio astronomy research. A on a BSc degree in physics. Goss and McGee have written a biography “Lloyds mirror” interference pattern : Under the Radar: The First Woman in Radio Astronomy: Ruby Payne-Scott, was observed by recording the published by Springer, 2009. The book was launched in Sydney and intensity variations as the rising sun Canberra in late 2009, sponsored by the University of Sydney School of appeared over the sea. Interference Physics and CSIRO. (Photo from the Bill Hall family collection) occurred between the direct and reflected rays from the sea, leading to a series of maxima and minima (“lobes”). With the cliff height of about 90 metres, the fringe of Dover Heights. During these correlated with the sunspot area as separation was slightly less than the observations (published in Nature in observed at the Commonwealth size of the quiet sun. The effective early 1946), the solar emission was Solar Observatory at Mt Stromlo. baseline of the interferometer detected with the single antenna On Australia Day 1946, the situation is twice the cliff height. system only. No fringes or lobes was quite different; a compact group were detected due to the wide Radio astronomical observations of sun-spots dominated the sun. distribution of the sunspots over of the active sun had, however, The lobe pattern was observed as the sun’s surface. The RPL group already begun in October, 1945. J L the sun rose shortly after 5 am local did determine that the brightness Pawsey, Ruby Payne-Scott and L L time. The radio sun actually rose temperature far exceeded the McCready had started observations about eight minutes earlier than expected temperature of the of the sun using the Royal Australian optical sunrise due to the increased quiet sun at 200 MHz. In addition, Air Force 200-MHz aircraft warning refraction at radio wavelengths the radio intensity was closely radar antenna at Collaroy, north compared to optical refraction. The

10 Issue No. 70, April 2011 Figure 2: RPL field station, Army Reserve, Dover Heights; the Fortress Fire Command Post was in this reserve, 2.2 km south of the Macquarie Lighthouse and 2 km north of Bondi Beach. The location is 7 km east of the centre of Sydney. Date, 18 February 1943. This 200-MHz antenna, associated with the main blockhouse, was used for the solar radio astronomy sea-cliff observations on Australia Day, 1946. The view is to the north with North Head clearly visible. Note the ships possibly waiting for the submarine net at the entrance to Sydney harbour. (ATNF historical photographic archive B81-1)

radio lobe pattern was observed solar surface was covered by the sun apparently coincident with the for about an hour due to the large spot). The 200-MHz radiation major optical sunspot. Based on primary beam of the radio antenna increased in intensity by a factor current knowledge, Type I bursts (about 10 degrees). The presence of ten compared to a few weeks were being detected. These can of deep minima implied a small earlier. Numerous observations be associated with fundamental angular size of less than about were obtained until the end of frequency plasma emission, 7 arc min, with a resultant March 1946. In addition to the in the presence of enhanced brightness temperature in excess limit on the size, the location of magnetic fields near sunspots. of a billion degrees. About two the radio emission from the sun The “Lloyd’s mirror” or sea-cliff weeks later (7 February 1946), a could be determined with an interferometer made use of the prominent sunspot appeared, one accuracy of a few arc min. The techniques used during World War of the major sunspots in recorded RPL group found that the emission II for “radio direction finding” using history (about 0.5 per cent of originated from a region on the radars for aircraft warning at metre

11 wavelengths. This remarkable radio interferometer consisted of a single antenna; a major drawback was that observations could only be carried out at sunrise or sunset when radio refraction effects were quite pronounced. The techniques used by Payne-Scott in early 1946 used the same methodology pioneered by numerous groups in Australia, the UK and the US during WWII for use in radar. In Australia, John Jaeger, an applied mathematician who worked at RPL, had worked out the theory of the lobe patterns in 1943. In the UK, both J A Ratcliffe and Fred Hoyle had independently carried out similar studies. In the publication of the exciting results from the sea- cliff interferometry from 1946 (publication August 1947), Pawsey, Payne-Scott and McCready suggested, for the first time, the Figure 3: The most commonly published photograph of Ruby Payne-Scott. principles of using This was taken at the Potts Hill Reservoir, likely in late 1948. “Chris” the method of Fourier summation. Christiansen is to the right with Alec Little in the middle. Payne-Scott and The other group that made rapid Little were working on observations of the sun at 97 MHz using the newly advances in the 1945 – 1946 era constructed swept-lobe interferometer. (ATNF Historical Photographic was the Cavendish Laboratory Archive: B14315 and Hall family collection) of the University of Cambridge, under the leadership of Ratcliffe and . After a remarkably short period of instrumental developments in early 1946, Ryle found that the solar emission was in the UK and Australia, Ryle and Vonberg were ready to observe less than 10 arc min in size, and and Vonberg detected circular the sun in July 1946, when another associated the radio emission with polarisation from Type I bursts prominent sunspot appeared. They the sunspot due to the compact size at this time. In the next decades, observed the sun at 175 MHz of the radio emission. In contrast the Michelson interferometer with a “Michelson” interferometer to the Sydney data, the position became the instrument of with a variable spacing up to 140 on the sun was not determined. choice for radio astronomers. wavelengths (240 metres). They In agreement with other groups

12 Issue No. 70, April 2011 Figure 4. A photo of a number of the RPL staff at Potts Hill circa 1950. From left to right, Ruby Payne-Scott (drinking a cup of tea), Alec Little, George Fairweather (a technician standing in the door), possibly Alan Carter and Joe Pawsey. The location is in front of one of the trailers used for instrumentation of the radio telescopes at Potts Hill. This photo is damaged with numerous spots, likely ink. Some colleagues that knew this group disagree with the identification of Alan Carter. (Bill Hall family collection)

The life of Ruby Payne-Scott has period of her career as a radio Advances in techniques in this recently been summarised by W astronomer was the period 1949 immediate post War period M Goss (NRAO) and R X McGee – 1951, working at the Potts Hill have had a major impact on the (Division of Radiophysics , retired). (Sydney) site with Alec Little as development of radio astronomy in Under the Radar: The First Woman they developed the swept lobe the 20th century. The major sunspot in Radio Astronomy: Ruby Payne- interferometer. The motions of the activity of 1946 – 1947 was a major Scott was published by Springer in Type IV outbursts were tracked stimulus as radio interferometry 2009. A number of highlights of her in real time by observing the sun development accelerated. life and career (CSIR and CSIRO 25 times per second. In Figures 3 A book about Payne-Scott for a from 1941 to 1951) are described, and 4, two group photos of some non-scientific audience is currently including a detailed account of the of the individuals at the Potts Hill in preparation by Goss: Making first recorded radio astronomy site from this period are shown. Waves: The Story of Ruby Payne-Scott: observations in Australia carried Prominent radio astronomers of Australian Pioneer Radio Astronomer. out in March 1944 by Pawsey and this era were present: Pawsey, Payne-Scott. The most innovative Christiansen, Payne-Scott and Little.

13 Operations Engineering Cadetship Experience Peter Mirtschin (CASS)

During the 2010 calendar bearing, the vibration signature access to these dataset buses. A year, Operations undertook a change can be detected and standalone RPC (Remote Procedure reported to operators in a timely Call) server application has been cadet engineer program. This manner. Currently this function completed which enables this program was targeted at giving is carried out by the observer to take place. In addition, it also noticing abnormal noises. With provides the option for Modbus (an two third year engineering automation and observers industry request and reply protocol) students industrial engineering being located remotely, this new controllers to monitor AT dataset work experience at CASS monitoring method becomes monitor points, if required. The important for maintaining the second stage of the project was to observatories. integrity of the structures. Her enable MoniCA to access Modbus efforts have been a great first step. devices directly. This has enabled An emphasis was for the cadets to MoniCA to very easily access any gain an “end-to-end” appreciation Ben McKay was the successful commercial off the shelf Modbus of operational radio astronomy cadet assigned to Narrabri and his equipment that may be installed at systems engineering under the project was to provide improved an observatory. Of course, there guidance of a professional mentor/ monitoring interfaces between the are the usual criteria, such as Radio supervisor. The project work was observatory computing environment Frequency Interference testing, that not limited to operational systems, and real world monitor points has needed to take place before but could involve engineering that are dispersed throughout installing commercial equipment. research or development work in the observatories. These points line with the development projects are crucial for the ongoing Specifically at Parkes, with the underway at the Observatories. operation of the observatory. completion of this software, MoniCA & LOboss software suites Another goal was to provide a Ben’s initial focus was to provide are now able to transparently and benefit to CASS operations in an improved methods for MoniCA simultaneously access the same area that might not otherwise occur to access Australia Telescope (AT) dataset buses with no perceived by carrying out a defined project serial dataset buses. MoniCA is a degradation in performance of that aligned with the interests software application used at the either application. LOboss continues of both the cadet and CASS. observatories for monitoring and to be the application for configuring Cathy Mitchell was the successful archiving of telescope monitor the Parkes conversion rack. candidate located at Parkes. Her points. AT datasets are interface project entailed some investigative hardware which enables computers At this point in time, Modbus work in the area of vibration to monitor physical measurements equipment that has been installed analysis. The ultimate aim of this of key parameters within the at the observatories includes work is to develop an automated observatory. AT datasets are generator and mains control and system which can monitor the integral in the existing observatories monitoring as well as several vibration signature of a telescope and there is a growing need for temperature and humidity sensors. in operation. Should something multiple stakeholder software The software developed is detrimental occur, such as a failed applications to have simultaneous designed to be sufficiently generic

14 Issue No. 70, April 2011 that it could be implemented on most Linux platforms. So thanks to the work of Ben we have seen several improvements. Firstly, the observatory software can now have reliable multiple access to the underlying monitoring hardware. At Parkes this has enabled the number of points monitored by MoniCA to be doubled whilst retaining the existing purpose written observing tools. Looking forward to the future it will facilitate a central monitoring system without complex integration into the observing software. Secondly, by enabling an industrial standard protocol to Cathy Mitchell be used with MoniCA the current Photo: Peter Mirtschin, CSIRO control and monitoring hardware can easily be expanded by the use of commercial equipment, These achievements have been a bonus for the Developmental Project, Parkes Equipment Control and Monitor (PECM), as it moves towards completion. There are plans to further extend the number of points monitored by MoniCA at Parkes in the coming months. Thanks to Euan Troup for some early work on this software and also to John Reynolds for software changes to LOboss to enable MoniCA access. I would also like to thank all those involved in enabling the Ben McKay cadetship program. It has been Photo: Peter Mirtschin, CSIRO a great success in its first year.

15 ASKAP and SKA News Flornes Conway-Derley (CASS)

2011 will be a critical year in the development of CSIRO’s Australian Square Kilometre Array Pathfinder (ASKAP). Following the successful construction of the first six ASKAP antennas at the Murchison Radio-astronomy Observatory (MRO) in 2010, the overall technical build of ASKAP continues to ramp up.

ASKAP Antennas During late 2010, five new ASKAP antennas were delivered and installed at the Murchison Radio- astronomy Observatory (MRO) in Western Australia, bringing the total number of antennas on site to six. At the same time, the first antenna (built in early 2010) Members of CETC54 in front of an ASKAP antenna at the MRO in underwent a number of retrofits October 2010. Credit: Terrace Photographers. to bring it as close as possible to the production design of the remaining ASKAP antennas. Comprehensive site acceptance tests and initial commissioning the antenna to be erected at the delivered dishes at the MRO has activities were also completed MRO, with no further adjustment been closer to 0.5 mm, which allows on the new antennas, including required, while maintaining a for astronomy-capable operation the fit-out of internal parts such specified surface accuracy. to be doubled to 20 GHz. as the support floor, mezzanine The reflector dishes are specified Not only does this design feature and internal cable trays. to a surface accuracy of 1.0 mm, allow for an increased range of An important feature of the which allows for astronomy- operation, but it also dramatically antenna design is the ability to set capable operation up to 10 GHz. saves on installation time. The reflector accuracy at the factory However, the surface accuracy guarantee of “in-the-field” surface acceptance test stage; this allows actually achieved on the first six alignment provides a reliable

16 Issue No. 70, April 2011 • Installation of 390 km of optical fibre cable between the MRO and Geraldton began in October 2010. In April 2011, one of four segments was fully completed, with partial completion in the other areas. The high capacity link will be used to transmit large volumes of data from the MRO for processing;

• A dry fit-up of the first full-sized Phased Array Feed (PAF) was completed in December 2010, and two full (analogue and digital) receiver systems are being assembled in preparation for preliminary system integration tests at the Parkes Testbed Facility (PTF) and on an ASKAP antenna at the MRO;

• Integration has commenced on the MATES (Marsfield ASKAP Test Engineering System) during Trench digging underway near the Boolardy homestead. the first half of 2011, which Credit: Barry Turner, CSIRO includes a skeletal PAF receiver with partial monitoring and control functions; dummy heat loads and temperature monitoring have provided a useful testbed for and fast build process for a to perform factory acceptance the PAF water cooling system; “traditional panel” style antenna. testing. The next batch of antennas will arrive at the MRO in May, • The first meeting of ASKAP All 36 ASKAP antennas are being with all 36 antennas expected PIs (Principal Investigators) manufactured by the 54th Research to be built by the end of 2011. for 2011 was held at Marsfield Institute of China Electronics in February. Following a Technology Group Corporation ASKAP General successful one year review in (known as CETC54) based in November, the teams have been Shijiazhuang, China. Members of Key ASKAP updates since the working on source finding and the ASKAP Antenna team recently previous issue of the ATNF simulation algorithms with the visited the CETC54 factory in China News went to print include: ASKAP Computing team ;

17 Aaron Saunders, Paul Cooper and Eliane Harkvoort with dry fit-up PAF. Credit: Wheeler Studios

• ASKAP was included as part ASKAP antenna contract to date representatives. At the conclusion of the Pawsey Centre’s early with CETC54’s capacity to fully of the Meeting, ILUA members adopters program, chosen as a assemble and precision align viewed, for the first time, the six large project that could use the all antennas in their factory in newly installed ASKAP antennas additional computing power to Shijiazhuang before shipping to on a tour of the MRO. The Wajarri open new avenues of research; Australia; resulting in a fast build- people have provided CSIRO time and with no adjustment of the a list of Wajarri names that will • A new version of the ASKAP reflector surfaces being required be used for key infrastructure software imaging package once on-site at the MRO. at the MRO in the future. (ASKAPsoft) was released in “This was an excellent opportunity February; the upgrade includes Industry Engagement enhancements to the virtual test to show the antennas to the CEO operating system, a weather of CETC and to continue to explore News station emulation and digital China’s expertise in producing low- The tender for the construction of receiver engineering GUI. The cost antennas at a cost-specification support infrastructure was recently test package will be used to test for the SKA,” says Carole Jackson. awarded to McConnell Dowell observations and measurements Also in late 2010, the MRO had Constructors (Aust.) Pty. Ltd., made during integration of the visits from the MRO Indigenous representing a significant milestone new full-sized PAF installed on Land Use Agreement (ILUA) in the ongoing development of the the PTF in the coming months. Liaison Committee as well as MRO site. The project commences students from Pia Wajarri, a remote immediately, and involves the At the MRO community located near Boolardy. construction of several kilometres of access roads and tracks, power In December 2010, senior staff The MRO ILUA Liason Committee and data infrastructure, a central from China Electronics Technology Meeting coincided with a visit to control building and 30 radio Group Corporation (CETC) visited the MRO by CASS chief Dr Phil antenna concrete foundations, the CSIRO Astronomy and Space Diamond and CSIRO’s ASKAP as well as ancillary works. Science headquarters in Sydney. Project Director Ant Schinckel, Both parties were keen to which provided the opportunity to The design tender for the recognise the success of the meet informally with the Wajarri Murchison Support Facility (MSF)

18 Issue No. 70, April 2011 Mr Tu Tianjie, President of CETC54, with Chief of CSIRO Astronomy and Space Science, Dr Philip Diamond. Credit: Tony Crawshaw, CSIRO.

at Geraldton was awarded to the development of the PAF SKA engineer. “This minimises the Aurecon and final detailing for Concept Descriptions, which will be number of external components the design works are underway. key inputs to the Concept Design needed to build a receiver, which Reviews (CoDRs) due to take place also leads to a reduction in size, The first two Redback-2 digital signal between April and October 2011. weight, power and cost.” processor boards will soon be ready for full integration testing over the Once fabricated, the chips will coming months. Puzzle Precision, First Silicon-on- be tested and integrated into a supplier of high-end digital Sapphire Prototype a demonstrator array that will systems, are currently delivering the SKA Receiver Chip perform the entire analogue major components of the ASKAP processing in the phased array digital systems, upon delivery the A significant milestone was achieved feed package, and contribute boards are fully tested and ready in the development of a radio significantly toward development for ASKAP systems integration. receiver on a chip, with the first of receivers for the SKA. chip design now fabricated as part of collaboration between CASS and Silanna (formerly Sapphicon SKA Activities Semiconductor). The chip is being Work Package manufactured at Silanna’s foundry in Sydney, and integrates much Discussions Continue of the electronics required to Discussions with international process one channel’s worth of partners on SKA Technology data in a Phased Array Feed (PAF) Work Packages (PrepSKA WP2) or Aperture Array (AA) receiver continue, focussed on SKA-related into a single integrated circuit. research and development such “The chip, which measures just 2.8 x as dish arrays, digital systems, 2.8 mm, also includes precision bias computing, signal transport and circuitry and digital control,” says systems. CASS is coordinating Suzy Jackson, ASKAP electronics

19 Compact Array 20/13 cm and 6/3 cm Receiver Upgrade Mark Bowen (CASS)

In December 2010 the installation of two upgraded 1 – 3 GHz receivers on the Compact Array heralded the substantive completion of the second phase of the Compact Array 20/13 cm and 6/3 cm receiver upgrade. Though the RF signal path of the receivers is complete, an upgrade of the receiver control and monitor electronics is still underway. The existing receiver electronics packages are over 20 years old and the upgrade will modernise them in line with the current millimetre-wave systems, ensuring our ability to support them into the future. This work will be completed during the first half of 2011 and can be accomplished on the antennas without removal of the receivers.

After the successful demonstration of a prototype 1 – 3 GHz receiver in late 2009, the roll out of fully upgraded receiver systems was commenced in June 2010. A further two receivers were installed in August, with the installation of these two receivers also bringing the first phase of the upgrade project to a conclusion. The 20/13 cm and 6/3 cm upgrade has three stages; the first of these included, among other things, the retrofit of new fins to the 20/13 cm receiver orthomode transducers (OMTs). The OMT refit was designed to improve the beam shape in the upper half of the receiver frequency range. The discovery of low frequency bias oscillation between pairs of Low Noise Amplifiers (LNAs) in some upgraded receivers during September resulted in a hiatus in the installation of the remaining receiver systems while a suitable fix was developed. Modifications to the LNA bias circuitry cured the problem and subsequent receivers were modified prior to installation. The remaining unmodified receivers Santiago Castillo installing an upgraded 1 – 3 GHz receiver system. Credit: Henry Kanoniuk, CSIRO.

20 Issue No. 70, April 2011 Initial testing of the gain stages, part of a 4 – 12GHz Low Noise Amplifier. Credit Alex Dunning, CSIRO.

are being retrofitted during cm receiver systems which will When completed, the upgrade the first half of 2011 as part of follow a similar development path of the existing Compact Array normal scheduled maintenance. to the 16-cm receiver systems. centimetre receivers will enable The provision of A$1.471M from the use of the full capability of The performance of the Astronomy Australia Limited (AAL) the Compact Array Broadband upgraded receivers has exceeded as part of the Education Investment Backend (CABB) at centimetre expectations. The system Fund (EIF) is funding the completion wavelengths. The upgrade will temperature (Tsys) has been of this phase of the project. The transform the piecemeal coverage of measured at ~ 20K over the band AAL funding will commence in July the 1 – 12 GHz observing spectrum 1.1 – 3.0 GHz, an improvement 2011 ending in June 2013 when delivering almost complete in overall noise performance of the project will be completed. The coverage in two frequency bands between 25% - 30% over the development of cryogenic 1 – 3 GHz and 4 – 12 GHz. original ATCA L/S receiver systems. 4 – 12 GHz LNAs is currently Jamie Stevens has also characterised underway. To ensure the feasibility the beam patterns of the upgraded of the third phase of the project, ATCA antennas between 1.1 – this work is being carried out 3.1 GHz. The primary beams are by CASS as part of the second symmetrical within 6%, independent phase. Substantial progress of frequency. These upgraded toward a suitable LNA has been receivers are now designated as made with testing of a prototype ATCA 16-cm receiver systems. scheduled for early 2011. The third and final phase of the project is an upgrade of the 6/3-

21 S-PASS: S-band Polarisation All Sky Survey Ettore Carretti (CASS)

Abstract The structure of the Galactic magnetic field is still largely The S-band Polarisation All Sky Survey (S-PASS) has mapped unknown. The observations show that the ordered component of the diffuse polarized emission of the entire southern sky with the the disc is aligned along the spiral Parkes radio telescope at 2.3 GHz with a resolution of 9’. Aimed arms, but several details of the at investigating the CMB Galactic foreground and the Galactic model are still under debate, like number and position of field magnetic field, the project has required a special setup to cover reversals (field reversal means that half a sky with such a resolution. The observations are now the field direction is preserved, but a complete reversal of the completed and the data reduction is in progress. With their huge heading occurs). Many data sets spatial dynamic range (360o to 9’) and high frequency, S-PASS are consistent with one reversal only, which would make our Galaxy maps deliver a completely new view of the polarised sky showing similar to the external galaxies interesting new features and structures at all Galactic latitudes. observed so far (e.g., Sun et al. 2008, van Eck et al. 2010), while some authors find that reversals Here we are again two years later powerful window to investigate the might occur at any spiral arm to to talk about the beautiful polarised magnetic field of our own Galaxy. inter-arm region transition, which sky of S-PASS (see April 2009 would make our Galaxy unique (e.g. But let’s step back a bit and issue). At that time S-PASS was 60% Han et al. 2006). Moreover, some introduce the project first. The complete and the data reduction recent results seem to challenge S-band Polarisation All Sky Survey still in an embryonic stage, but the the alignment with the spiral arms (S-PASS) is a project to map the first results were showing the high in the outer Galaxy where the field diffuse polarised synchrotron potentiality of this project already. could just take a ring-like shape emission of the entire southern sky Now, two years later, the survey (e.g. Van Eck al. 2010). The field at 2.3 GHz (Carretti et al. 2007). is completed and the resulting in the Galactic halo is even less Carried out with the Parkes radio maps show the diffuse polarised understood, essentially for lack of telescope, the survey is aimed sky with an unprecedented data in this low emitting region. at investigating two cutting-edge combination of angular scale Models have been proposed (e.g., cases of the present astrophysics dynamic range, sensitivity, and Han 2002, Sun et al. 2008) and research: the Galactic magnetic frequency, delivering a new view of the asymmetry recently discovered field, whose large scale structure the polarised sky. Unlike previous in the vertical component of the is still a puzzle, and the detection lower frequency surveys affected local field (Mao et al. 2010) has of the B-Mode of the Cosmic by severe Faraday depolarisation, suggested that a combination of Microwave Background (CMB) the diffuse emission from the dipole and quadrupole components polarised component, for which the Galactic disc is now unveiled might describe well the large scale synchrotron emission is one of the (expect for a few degree across field. However, all the proposed strongest foreground contaminants. the Galactic Plane) opening a new models are poorly constrained

22 Issue No. 70, April 2011 both by the lack of data and The CMB signal is weak, however A project like S-PASS has posed the contamination by large local (100 nK the current upper limit), several challenges, primarily to structures, like the big radio loops, weaker than the foreground minimise the ground emission that can introduce anomalies. Galactic synchrotron emission, contamination and to enable which thus needs to be removed absolute calibration, and a special More data are thus necessary for a successful detection of the scanning strategy based on long to understand how the Galactic cosmological signal. It is something Azimuth (Az) scans has been magnetic field is arranged. One of like peering through the fog of our developed to this purpose. Ground the goals of S-PASS is to help cover Galaxy to a have an unobstructed emission is mostly elevation this gap, measuring the polarised view of the far end of the visible dependent, and Az scans are synchrotron emission of the entire Universe. The goal of S-PASS is ideal to minimise it. Long azimuth southern sky. The diffuse polarised to measure with high precision s c a ns (115 o) can cover the entire emission encodes a wealth of the Galactic emission to make Declination range of interest in information on the magnetic field by possible CMB detections with just one go thus preserving the Rotation Measure (RM), polarisation the lowest possible error. information on all angular scales. angle, polarisation fraction, and RM- The mapping of all the desired synthesis, which can unlock how To realise such goals S-PASS has Right Ascension range is ensured the emission is organised along the observed the entire southern by the Earth rotation, that in line of sight delivering a 3D view of sky at 2.3 GHz with high signal- combination with AZ scans, lets the the interstellar medium (ISM). The to-noise ratio also in the lowest telescope draw zig-zag patterns in coverage of the entire southern sky emission regions of the halo. The the sky each day. The full coverage allows investigation of the field in all observations have been conducted of the sky is realised by precisely the possible environments: plane, from October 2007 to January 2010 timing the scan start each night, disc, halo, disc-halo transition. for a total of about 2000h, keeping so that day after day the zig- the team busy observing all night The other goal of S-PASS is to study zags are appropriately spaced to long for six months in two and a the polarised component of the ensure a uniform sky coverage. half years — almost a retreat! The CMB, which carries the signature of frequency is high enough to keep The vast area to observe and the the Gravitational Wave Background Faraday Rotation effects under small pixel size (4.5’) have required (GWB) emitted at the Inflation control down to disc latitudes, as a high scan speed to conduct the time (Kamionkowski & Kosowsky shown by the precursor project survey in a sensible time duration. 1998, Kinney et al. 2006, Boyle et Parkes Galactic Meridian Survey The scan rate has been pushed up al. 2006). This is the only radiation (PGMS, Carretti et al. 2010), to 15o/min, a significant fraction of that can travel the Universe from its while the high sensitivity enables the slewing speed (24o/min): not a very early stages (10-34 s after the both high efficient foreground bad performance for a 1000-tons Big Bang) up to us mostly untouched cleanings and sensitive rotation 64-m telescope nearly 50 years old! and gives us the chance to probe measute (RM) measurements the physics of the Big Bang at energy To recover the power on all angular (the expected sensitivity in the densities so high, that no particle scales a ”basket weaving” technique halo is some 2 rad/m2 when accelerator on Earth can parallel. (scan crossing) is required. Basket combined with 1.4 GHz data).

23 weaving is a tricky job with azimuth scans. However, the same Dec range can be observed either when the sky rises or sets, but with a different path in the sky. Two sets of scans has then been observed, one Figure 1: Combination of east and west scans. The two sets span the same eastward and one westward, whose Declination range but with a different path in the sky. The resulting crossing combination realises an effective enables an effective basket weaving. scan crossing (Figure 1). This, along with the modulation of the signal by parallactic angle variation along the scan, has permitted full recovery of the emission on all angular scales (for details see Carretti 2011, Carretti et al. 2011). As example, Figure 2 shows the final map of Stokes Q. This is absolutely calibrated and at full resolution delivering a spatial dynamic range of 2400 (360o to 9’), maybe one of the highest ever obtained in radio astronomy. Thanks both to the high resolution and high frequency that Figure 2: S-PASS Stokes Q map. Galactic coordinates centred at the Galactic reduce Faraday Rotation effects, Centre are used. Longitude increases leftward. the map shows an unprecedented amount of detail. The emission is smooth both at high Galactic latitude and in the disc down to 5o–10o from the plane even in the inner Galaxy, symptomatic that Faraday depolarisation is marginal almost down to the Galactic plane. This unveils the disc, which was strongly depolarised up to latitude |b| ~ 30o in previous surveys taken at 1.4 GHz (Figure 3). S-PASS thus opens a new window to investigate the magnetic field in the disc with polarised diffuse emission. Very large scale structures are visible at high Galactic latitudes. Figure 3: All-sky map of polarised intensity emission at 1.4 GHz. This image is The most obvious is the vertical combination of the Dominion Radio Astrophysical Observatory (north) and Villa structure along longitude l=0o that Elisa survey (south) and is in Galactic coordinates centred at the Galactic Centre. Longitude increases leftward.

24 Issue No. 70, April 2011 stretches from the south Galactic sky areas. Foreground emission S-Band Polarisation All Sky pole up to the north end of the map is also a strong contaminant for Survey, Parkes project P560. for a total length of nearly 150o. Epoch of Reionisation experiments Carretti E., Haverkorn M., Bright extended emission made of like Murchison Widefield Array, McConnel D., Bernardi G., several ridges is also obvious in the whose observations might be Cortiglioni S., McClure-Griffiths inner Galaxy at north latitudes conveniently pointed to the S-PASS N.M., Poppi S., 2010, MNRAS, (b ~ 0o–30o) and west of l=0o. lowest emission regions as well. In the outer Galaxy the polarised Carretti E., 2011, in The Dynamic Now the time of data analysis emission is detected down to the ISM: A celebration of the and investigations starts. A first Galactic plane, even if modulation CGPS, ASP Conf. Ser., 438 catalogue of nearly 5000 point by Faraday Rotation is obvious. source RMs has been extracted Carretti E., et., 2011, in preparation Prominent features in the disc are already, while RM analysis of two heavily depolarised regions Han J.L., 2002, in Astrophysical the diffuse emission and CMB on either sides of the Galactic Polarised Backgrounds, AIP foreground analysis will start soon. centre and the Gum nebula in the Conf. Ser., 609, 96 outer Galaxy. The formers well In summary, S-PASS observations Han J.L., Manchester R.N., Lyne match bright HII regions whose have been successfully completed A.G., Qiao G.J., van Straten high electron column density is the in two and half years of long W., 2006, ApJ, 642, 868 likely cause of the depolarisation. observing nights. The disc emission Kamionkowski M., Kosowsky The latter is centred at l~260o looks unveiled at last and promises A., 1998, PRD, 57, 685 and stretches for 30o–40o in new insights into the study of longitude and +/- 15o in latitude this part of the Galaxy, while the Kinney W.H., Kolb E.W., and closely follows the Hα high S/N at high latitude promises Melchiorri A., Riotto A., 2006, emission associated to the Gum both a big improvement in the Phys. Rev. D, 74, 023502 foreground cleaning efficiency Nebula. In the same area the Vela Sun X.H., Reich W.,Waelkens A., and a better understanding of Nebula is also clearly visible. Enßlin T.A., 2008, A&A, 477, 573 the large scale Galactic field. The At high Galactic latitudes the data analysis has now begun and Testori J.C., Reich P., Reich emission is smooth and weak. The the next time we write on these W., 2008, A&A, 484, 733 large scale emission closely follows pages we hope to report on the that of Wilkinson Microwave Van Eck C.L., Brown J.C., Stil new findings that this project will Anisotropy Probe (WMAP) J.M., Rae K., Mao, S.A., have carried out. Stay tuned. maps, even though with much Gaensler B.M., Shukurov higher S/N. The S-PASS emission A., Taylor A.R, Haverkorn is thus mostly free from Faraday References M., Kronberg P.P., McClure- Griffiths N.M., 2010, submitted Rotation effects and its analysis will Boyle L.A., Steinhardt P.J., to ApJ, arXiv:1012.2938 give a sounding basis to estimate & Turok N., 2006, Phys. and clean the Galactic emission Rev. Lett. 96, 111301 Wolleben M., Landecker T.L., contamination in CMB data. Reich W., Wielebinski R., Carretti E., Staveley-Smith L., Moreover, the lowest emission 2006, A&A, 448, 411 Haverkorn M., Bernardi G., regions that will be identified in Cortiglioni S., Gaensler B., S-PASS can be ideal targets for CMB Kesteven M., Poppi S., 2007, ground based experiments, which seek for the cosmic signal in small

25 CABB Zoom Modes Produce New Science Maxim Voronkov, James Caswell and James Green (CASS)

The eagerly anticipated “zoom” mid 2010 and have begun to high spectral resolution (Voronkov et al., MNRAS, in press; http://dx.doi. modes of the new Australia yield new scientific results. o r g /10 .1111/ j .1365 -296 6 . 2011.18297. x ) Telescope Compact Array Recently put into press is a including a new type of methanol spectrometer (also known as maser study which demonstrates maser at 23.4 GHz. These results the capability of simultaneously are shown in Figure 1. The top CABB) became operational observing eight spectral lines at very full spectral lines are a related

Figure 1: Background map is the 8.0 micron IInfrared Array Camera (IRAC) Spitzer Space Telescope image of 357.97-0.16 on which we have marked the radio measurements of various maser species (circle and squares show class I and class II methanol masers, respectively; crosses show water masers). Alongside the map we show the eight spectra of the class I masers taken simultaneously in CABB high resolution multiple zoom mode.

26 Issue No. 70, April 2011 series of methanol transitions well can be seen to be the strongest of h t t p : / / d x . d o i . o r g /10 .1111/ j .1365 - known as masers, and clearly reveal all the lines. The new modes also 2966.2010.17856.x). This project the slowly changing properties allowed a study of an enigmatic OH demonstrates the new capability (amplitude and structure) as we maser showing both strong circular of recording full polarization at pass down the series. The bottom and linear polarisation, now recently a spectral resolution eight times line is a transition of methanol not published (Figure 2, and Caswell & better than was possible before. previously known as a maser, and it Green, 2011, MNRAS, 411, 2059; Furthermore, the full zoom mode capabilities are being exploited in a survey of the magnetic fields in high-mass star formation regions (entitled “MAGMO”), which aims to determine the magnetic fields across the Galaxy through the measurement of Zeeman splitting of OH masers. This survey will observe four transitions of OH masers simultaneously, with a large frequency coverage at each transition (equivalent to ~300 km/s), in all four Stokes parameters. The new zoom modes are currently being used in a wide variety of projects ranging from the studies of periodic maser flares to the mapping of HI in nearby galaxies.

Figure 2: Detailed spectra of the 1667-MHz OH transition towards OH24.329+0.145 (2010 July). The upper panel shows RHC(solid) and LHC(dashed) polarisations. The lower panel shows the Stokes parameters Q(solid) and U (dashed) revealing significant linear polarisation.

27 ATCA Discovers an Ionised Jet Associated With a Young High-mass Star G345.5+01.5 Andres Guzman (PhD student, University of Chile/CASS)

We have discovered, using So far there are about a dozen ionised protostellar jet towards ATCA, a very good example of reported detections of ionised jets the source G345.4938+01.4677 towards young high-mass stars. If (hereafter G345.5+01.5). an ionised jet associated with these ionised jets are analogues to G345.5+01.5 is associated with their low-mass counterparts then a very young high-mass star. the Infrared Astronomical Satellite these jets are intimately linked The presence of this jet forms (IRAS) source 16562−3959, and is to the accretion-disk formation believed to be a high-mass star in important observational evidence process and power the observed formation at a distance of 1.6 kpc. massive molecular bipolar outflows. that constrains the theory of The principal source is detected high-mass star formation. An ionised jet towards a high-mass by several infrared surveys (e.g. young stellar object (HMYSO) Midcourse Space Experiment An intriguing datum about the can be observed through its radio (MSX), Spitzer-GLIMPSE [Galactic process of forming high-mass stars continuum emission at centimeter Legacy Infrared Mid-Plane Survey (greater than 8 solar masses) is wavelengths. This thermal free- Extraordinaire]) from which we the common presence of massive free continuum emission is more deduce it has ~ 60,000 times the and fast-moving molecular bipolar commonly associated with the solar luminosity, and the central outflows, typically of several solar ionised gas that surrounds more object corresponds to a star of masses and velocities in excess of developed, but still young, high- 15 times the mass of the Sun. The tens km/s. Are these more powerful mass stars (referred to as ultra- object is also associated with a versions of the outflows that are compact HII regions). We are able massive (~ 1000 solar masses) 4 5 -3 readily observed toward very young to distinguish this type of emission and dense (10 -10 cm ) low-mass stars and consequently from jets using a combination of core of cold gas and dust. spectral and detailed morphological do they imply one generic disk- Figure 1 shows an image of the information. The wide spectral mediated accretion formation ATCA 8.6-GHz continuum emission. coverage (1 to 100 GHz) and process for all stars across the stellar The image shows five sources the high-angular resolution of the mass spectrum? Confirmation of roughly aligned and symmetrically Australia Telescope Compact this would be via direct observation offset with respect to the central Array (ATCA) make it well-suited of an accretion disk surrounding a source, which we identify as the to getting this information. In fact high-mass star. Unfortunately the ionised jet. We interpret the outer the ATCA has already discovered sites of high-mass star formation four sources as lobes where the one of the best examples of an hamper such observations high-velocity gas ejected from the ionised protostellar jet (IRAS because they are located far from jet has impacted the surroundings, 16547-4247, Brooks et al. 2003). Earth, embedded in dense, dusty generating shock-ionised gas molecular clouds, and evolve on We are nearing to completion a (Guzmán et al. 2010). They are fast time-scales. Observation of systematic search using the ATCA the radio equivalent of optical ionised jets offer an alternative, to look for more detections of Herbig-Haro objects. All of the five albeit indirect, means to confirm a ionised jets toward HMYSOs. Here emission sources were observed disk-accretion formation process. we report on the discovery of an at four different frequencies.

28 Issue No. 70, April 2011 Figure 1: ATCA 8.6-GHz continuum emission image of the newly discovered thermal ionised jet system in the high-mass star- forming site G345.5+01.5. Data were taken on June 2008, October 2008 and February 2009. The synthesised beamsize is 1.62’’ x 1.01’’ and indicated in the bottom left corner.

This allows us to obtain spectra east, coincident with the eastern References towards each of the lobes and radio lobe (Guzmán et al. 2011) Brooks, K. J., Garay, G., the jet, the latter being a power Of the small list of HMYSOs known Mardones, D. & Bronfman, law with a spectral index equal to to harbor a thermal ionised jet, L., ApJ 2003, 594, L131 +0.85 and consistent with free- G345.5+01.5 has taken the lead as free emission from a thermal jet. Guzmán A., Garay, G. & Brooks, the most luminous. In second place K. J., ApJ 2010, 725, 734 Using the Atacama Pathfinder is IRAS 16547-4247. Both of these EXperiment (APEX) telescope jets were discovered with ATCA Guzmán A., Garay, G., Brooks, K. in Chile we have also discovered and we look forward to their follow- J., Rathborne, J. M. & Güsten, a CO molecular outflow that up studies at higher frequencies R., ApJ 2011, submitted extends in the jet direction and has using the Atacama Large Millimeter/ its blue-shifted part towards the (ALMA).

29 SZ and X-ray Peaks Don’t Correspond Helen Sim, CASS

Two independent studies have been made with the Compact Array of the Sunyaev-Zel’dovich (SZ) effect in galaxy clusters. They show that the relationship between the SZ effect and X-ray brightness is complex, suggesting that we have much more to learn about the processes involved in cluster mergers.

When Cosmic Microwave mergers. They have then compared An Active Galactic Nuclei (AGN) Background (CMB) photons these to X-ray emission maps. could have locally heated the gas encounter a cloud of electrons, in the region of the SZ effect In one study, Marcella Massardi, they undergo inverse Compton minimum. But there is no sign of an Ron Ekers, Simon Ellis and Ben scattering. For frequencies above X-ray or radio AGN in the region, Maughan targeted the cluster CL 218 GHz, the CMB brightness and the cluster galaxies present in J0152-1357. This is one of the most increases, while for frequencies this region are subluminous, so such massive clusters known (with a total below that value, it decreases. heating seems unlikely. The team has mass of 1015 solar masses), and This spectral distortion is known also ruled out astrometric errors lies at a of 0.83. Previous as the Sunyaev-Zel’dovich effect. as an explanation for the offset. studies have shown that clusters The amplitude of the distortion with z ≥ 5 are more structurally In the second study, Siddharth depends only on the properties of complex, and less virialized, than Malu, Ravi Subrahmanyan, the electron cloud: in the case of clusters at low ; and that Mark Weiringa and Delampady thermal electrons, it is proportional clusters of z > 0.8 tend to be Narasimha examined the well- to both the electron density and clumpy, suggesting they are closer known Bullet Cluster, a cluster the electron temperature. The hot, to the epoch of cluster formation. collision (or merger) with a redshift dense, ionised gas found in galaxy 0.296. The strongest SZ feature clusters is a source of such electrons. The team had observed this cluster was again significantly offset from in 2005, before the advent of Hot cluster gas is commonly the X-ray emission peak; indeed CABB, with the Australia Telescope studied through its thermal X-ray other SZ features in this cluster Compact Array (ATCA) in its most emission: this, however, is more were all offset from the lesser compact configuration (H75, with dependent on electron density, but peaks in X-ray emission. This baselines from 30 m to 75 m). less dependent on temperature, implies that, in this cluster, the peak They detected a (negative) peak than the SZ effect. As a result, the in intracluster gas temperature is in the SZ effect in the cluster’s SZ effect will tend to trace the offset from the peak in gas density. northeast subclump, displaced hot, low-density gas in a cluster about 35 arcsec to the northwest Through the higher-resolution (which may be a better indicator of of the X-ray peak. The offset was SZ observations made possible the cluster’s large-scale structure), unexpected and, as the detection by CABB, these two studies have while the X-ray luminosity will was at a level of just 3.5 s, it was shown, for the first time, that the be a better tracer of clumpiness not convincing. In 2009, after the SZ effect does not correspond well (and thus perhaps highlight short- upgrade to CABB, they repeated to X-ray brightness in non-virialised term activity in the cluster). the observation of the X-ray peak clusters. The finding implies that Two teams have used the in the northeast subclump. Again, the physics of cluster mergers is capabilities offered by the Compact they saw the peak in the SZ effect more complicated than our current Array Broadbank Backend (CABB) offset from the X-ray peak—by models provide for, and throws to make the first subarcminute- about 45 arcsec to the north; into question the combined use resolution observations of the SZ and this time, the detection was of X-ray and SZ observations to effect in galaxy clusters undergoing at a very convincing 10 s level. derive cosmological parameters.

30 Issue No. 70, April 2011 Figure 1: A false-colour X-ray image from the Chandra X-Ray observatory of the Bullet Cluster, with superimposed contours of the pressure/temperature distribution in the gas, determined from SZ observations with the Australia Telescope Compact Array. The hottest gas, seen by the SZ observations (contours), is displaced from the densest gas regions, which are traced by the X-ray emission (grey-scale tones). Only two other clusters are known to show such a displacement, which may indicate an energetic cluster merger. Interferometers are best suited for such SZ observations and the Compact Array is the only one capable of these measurements for southern clusters such as the Bullet Cluster. Credits: ATCA data: S. Malu et al. Chandra data courtesy of the Chandra X-ray Observatory Center, operated by the Smithsonian Astrophysical Observatory on behalf of NASA. NB: For reference, please see the colour image published on the inside back page of this newsletter.

Publications Effect in the Massive z ≈ 0.83 Compact Sunvaev-Zeldovich “Hole” Cluster CL J0152 – 1357. ApJ in the Bullet Cluster. Submitted M. Massardi, R.D. Ekers, S.C. Letters, 718: L1-L5 (2010) to The Astrophysical Journal. Ellis, and B. Maughan. High Angular Resolution Observation S.S. Malu, R. Subrahmanyan, M.H. of the Sunyaev-Zel’dovich Weiringa, and D. Narasimha.

31 Education and Outreach Rob Hollow (CASS)

PULSE@Parkes working on PULSE@Parkes modules students with developments in and science. He has developed a radio astronomy including the A milestone marked the start of new module that allows students Australian Square Kilometre Array the fourth year of CSIRO’s PULSE@ to determine the period of a Pathfinder (ASKAP) and the Parkes project, with the first ever pulsar. It is currently being tested Square Kilometre Array (SKA). session held from a school taking by an external group of teachers place in February 2011. Hosted by and should go live soon. Penrith Anglican College, students Other Education and from Glenmore Park High School, Outreach Activity Caroline Chisholm College and CASS Summer The annual one-day Astrophysics Penrith Anglican College took Vacation Program for Physics Teachers workshop was direct control of the Parkes radio held at Marsfield in late March 2011. telescope from a control desk set up Ten scholars from across Australia Participating teachers from across in the school’s music performance spent their summer based either NSW learnt about new ways and space. CASS staff members, Dr at Marsfield or Parkes, working activities to engage and challenge George Hobbs and Rob Hollow on a diverse range of projects students. Speakers included Dr were assisted by PhD student under the supervision of CASS Jimi Green, Dr George Hobbs and Stefan Ozlowski from Swinburne staff. The students also had the Rob Hollow from CASS, Dr Fred University. The session was a great opportunity to use the Australia Watson from the AAO and Geoff success and provided a wonderful Telescope Compact Array in January Wyatt from Sydney Observatory. opportunity for students and for short observing proposals Rob also presented sessions to teachers from the three local of their own choosing during an teachers at the Sydney Observatory schools to meet and interact. observing trip to Narrabri. as well as at the Science Teachers’ Every student gave a presentation In March, the first PULSE@ Association of Victoria Physics of their work at a joint symposium Parkes Teacher Scholar, Stephen Teacher Conference in February. Broderick from St Ursula’s College with summer vacation students The students and staff from Pia in Toowoomba, spent a successful from the Australian Astronomical Wadjarri Remote Community week at CASS headquarters Observatory and the Australian School toured the Murchison at Marsfield. He worked with Gemini Scholars based in Chile. Radio Observatory to inspect the project team in developing The CASS students then finished the first six dishes of ASKAP in new outreach related resources. their program by participating December. This was the first Stephen’s article about his time in the Big Day In at Macquarie site visit by the students. Work with CASS can also be seen in University with other summer is continuing on an Indigenous this issue of the ATNF News. students from across the CSIRO Education resource for the Wadjarri Information Sciences Group. In a further update, Alex Mathews Yamatji community in conjunction CASS Director Dr Phil Diamond from University of Western with the building of ASKAP. Australia spent ten weeks as a gave the keynote address at CASS Summer Vacation Scholar this two-day event, inspiring the

32 Issue No. 70, April 2011 CASS Teacher Scholarship Stephen Broderick

Teacher Stephen Broderick was the recipient of the first CASS I have been teaching mathematics Teacher Scholarship. The scholarship provided Stephen with the and science at St Ursula’s College in Toowoomba for 25 years, so I saw opportunity to work alongside the PULSE@Parkes team in a the CSIRO Teacher Scholarship as a research environment. He spent a week at the CASS Marsfield unique opportunity to combine my love of astronomy and mathematics. site, meeting with scientists and outreach staff, and learning about After arriving at the CSIRO main the program and the ATNF more generally. Stephen will also gate in Marsfield, (reminiscent of a develop astronomy related educational resources in the coming scene out of Mission Impossible), I proceeded to turn a combination lock months and will have the opportunity to remain involved in future (successfully I might add) in various PULSE@Parkes activity. An account of his enjoyable week follows: directions using the secret number until my key and instructions on how to reach the lodge were revealed. The lodge was my on site accommodation for the week. Two overseas post graduate students and a visiting professor from Melbourne were also staying at the lodge. The lodge would rival any three or four star motel. Everything you could possibly imagine was available in the lodge, including toothpicks, bicycles, and combination locks, puncture kits, etc. The Marsfield site is very picturesque and is nestled amongst lots of gum trees which consequently attract many varieties of parrots, native birds and exotic insects. The spectacular sunsets from my window in the lodge were framed by the two iconic 12-metre radio telescopes. On Monday Rob Hollow gave me a tour of the CSIRO facilities which included the Astronomy and Space Science division, library, canteen and Robert Hollow, Jonathan Khoo, Stephen Broderick and Dr George various workshops which included Hobbs. Credit: Helen Sim, CSIRO

33 full scale models of various sections illuminating, providing alternative CSIRO canteen provided a huge of the 12 metre radio telescopes solutions and more questions than range of culinary delights and currently being constructed in answers. The robustness of some lunch time was always enjoyable Western Australia as part of the well known standard theories was listening to various scientists Australian Square Kilometre Array also questioned. It was breathtaking and computer programmers Pathfinder (ASKAP) telescope. witnessing the level of thinking speaking about their triumphs.) The hallways are decorated with and reasoning within the room. Friday was my last day and I felt eye catching educational posters It was science in the making. contented that I had learnt a lot which show a progression in On Wednesday afternoon, electrical in such a short time; however, my technology and precision depending engineer Mark Bowen gave me journey with pulsars has only just on which direction you travel in. a guided tour of the engineering begun. I am very grateful to all of Later in the day we met with section. He explained what the staff at the CSIRO Marsfield George Hobbs and Jonathon happened to the radio signal after site especially Rob Hollow, George Khoo to discuss my role which was it arrived at the focus cabin and Hobbs and Jonathon Khoo for mainly working on the web based entered the multibeam receiver. For allowing me to work with them. PULSE@Parkes student modules. example the multibeam receiver All of the staff at CSIRO appeared My knowledge of pulsars was at Parkes (which was built in the focused on a common goal — greatly enriched hour by hour and CSIRO workshop) can look at 13 the advancement of scientific one of my favourite astronomical points in the sky simultaneously. knowledge. I feel confident that objects is now the pulsar PSR Each receiver uses vacuum and I can give my students accurate J0437-4715 (my students also liquid helium to amplify the signal. career advice about what a scientist know about PSR J0437-4715 and Eventually the integrity of the at CSIRO does and I have also are familiar with its sound file). vacuum breaks down and the registered St Ursula’s College in the receivers need to be resealed. Scientist in Schools project as I see On Wednesday I was privileged to the connection between schools be involved in a meeting chaired On Thursday I attended a lecture and scientists as an enterprising by Robert Braun who was the at the Australian Astronomical and positive step in Australian head of the Astrophysics section. Observatory on the distribution Education. My week at CSIRO has The meeting showcased various of dark matter. The lecture was certainly been the highlight of my developments on site, including very interesting and generated teaching career to date and I look the progress of several projects lots of discussion. Once again forward to reading about future and the research findings by there were more questions than achievements in CSIRO newsletters. post graduates was also shared. answers and plenty of food for Discussions were encouraging and thought. (Speaking of food, the

34 Issue No. 70, April 2011 Operations Douglas Bock (CASS)

Several upgrades are coming signal chain reconfiguration) will csiro.au/dap/. For more details, see to their conclusion this year. enable remote observing with the the report in the April 2010 News. Parkes Telescope. Also supporting Upgraded “16 cm” receivers remote observing are significant replacing the 20 cm and 13 cm April 2011 Time upgrades to the Parkes power receivers are now available on Assignment supply and distribution systems, all Australia Telescope Compact which are underway and will The Time Assignment Committee Array (ATCA) antennas (see continue for the next few years. (TAC) met at Marsfield on 2 – 4 report elsewhere in this issue). February to consider proposals for The new receivers have increased In February, CSIRO and the the 2011 April semester (2011APRS). sensitivity and bandwidth to Auckland University of Technology A total of 212 proposals were complement CABB, the Compact (AUT) formally agreed to reviewed; 132 for the Compact Array Broadband Backend. collaborate on , 38 for Mopra, 29 for Parkes, Meanwhile, the 64-MHz mode Interferometry (VLBI) observations. 12 for the Long Baseline Array for CABB is now being released. As a result, the AUT 12-m (LBA) and one for Tidbinbilla. This will substantially improve Warkworth radio telescope is the capability for extragalactic now commonly available for VLBI With ongoing enhancements to millimetre-wave observations this sessions at 20, 13, and 3 cm. A single OPAL (ATNF Online Proposal winter. Together the upgrades are a ASKAP antenna is also sometimes Applications & Links), the Time major enhancement to the ATCA. available at 20cm. These antennas Assignment Committee now has Installation of the University of are requested explicitly in proposals. better access to proposals and TAC New South Wales water vapour comments from previous semesters, The Australian National Data radiometers has also recently be and is paying closer attention to Service (ANDS)/ATNF Data completed. These will be charactised ensure resubmitted proposals have Management Project has recently during the coming winter. addressed the comments made on been successfully completed. previous submissions. A resubmission During March, Parkes was shut This project produced a public that does not consider any of the down for four weeks to enable the archive of several important Parkes feedback provided by the TAC is MCP (Manual Control Panel) to pulsar datasets and established unlikely to be reviewed favourably! be replaced. While the front panel the framework for including all still looks largely the same, the Parkes data in the future. This will In the past, proposal teams have internal workings of the MCP have complement the ATCA and Mopra been notified individually on the been completely overhauled. This, data already available in the Australia outcome of their proposal review together with the “switch matrix” Telescope On-line Archive. The data by the TAC, and again once the installed last year (that automates may be accessed at http://datanet. schedules have been released. From

35 April 2011, a single message is between the two 64-MHz channels June, primarily for refurbishment being sent to all proposers. The possible. It is expected that the 64- of the focus cabin translator rails. first, soon after the TAC has met, MHz mode will be expanded with It is expected that all receivers will advises all proposers that the TAC the full thirty-two 64-MHz channels be removed from the focus cabin grades and comments are available available per IF early in the semester. for this work to be undertaken. in OPAL. The second notifies all Work has commenced on the proposers that the schedules have 6/3 cm (“C/X”) upgrade, which will Notes on Mopra been released and provides links to provide coverage over the range the detailed information available Owing to the relocation of Balt 4.0 –12.0 GHz and thus fill the gap from the schedule webpages. Indermuele to Sydney, most between the existing 6 cm and 3 cm Mopra support will now be Abstracts of all accepted proposals bands. The first prototype receiver delivered from Marsfield. In the are now available in ADS. may be ready for installation 2011APRS, “on-site” observing toward the end of the 2011APRS. will be supported from Marsfield Notes on the Two weeks during the semester (where a dedicated observing room Compact Array have been allocated for C2479 will be set up) or at Narrabri. ATCA Characterisation of the first Recent changes to the Mopra The 2011APRS will commence BETA fields, in order to characterise Spectrometer (MOPS) have enabled with the “standard” CABB 1 MHz the two 30 square degree fields “fast mapping” observations to continuum mode available, and that will become the first science be made, with a correlator cycle with up to 16 zoom bands per IF fields observed on BETA (the time of 256 milliseconds rather (intermediate frequency) available first six antennas of ASKAP). than the standard 2 seconds, in the 1M-0.5k mode. The 64-MHz The fields are centred on the for a reduced number of MOPS CABB mode will, for the first few Circinus galaxy and the Fornax zoom bands (no more than four is weeks, have a single 64-MHz band cluster (and including Fornax A). in each IF, which will have 2048 recommended). In order to allow channels across it. (Thus, if the The “Science Operations Centre” a seamless transition between fast- 64-MHz mode is selected for an pilot observing mode trialled last mapping observations and regular IF, the total bandwidth in that IF year for Mopra (see October 2010 observations, it is intended from will be 64 MHz and not 2 GHz). ATNF News) will be extended to early 2011APRS to change the cycle For continuum plus spectral line selected ATCA projects this year. time for all Mopra observations studies, having one IF set with the from the current 2.0 seconds to 64-MHz mode and the other with Notes on Parkes 2.048 seconds. We will ensure that the standard 2048 1-MHz-wide all Mopra users are made aware The 2011APRS schedule for Parkes channel is possible. For spectral line when this change is made, and that has a three-week shutdown period, studies, 64 MHz is available in both old scripts (assuming a 2.0 sec cycle from Monday 23 May to Friday 10 IFs — with separations up to 7 GHz time) will be handled gracefully.

36 Issue No. 70, April 2011 Publications List

Publication lists for papers which Körding, E. “X-ray and radio variability selected cluster of galaxies”. ApJ, 727, include ATNF data or CASS authors are in the low-luminosity active galactic L25 (2011). available on the Web at www.atnf.csiro. nucleus NGC 7213”. MNRAS, 411, 402 * Brown, S.; Duesterhoeft, J.; Rudnick, au/research/publications. Please email ( 2011) . L. “Multiple Shock Structures in a Radio- any updates or corrections to this list to *Benaglia, P.; Ribó, M.; Combi, J. A.; selected Cluster of Galaxies”. ApJ, 727, [email protected] Romero, G. E.; Chaty, S.; Koribalski, B.; L25-L25 (2011). This list includes published refereed Mirabel, I. F.; Rodríguez, L. F.; Bosch, *Brown, S.; Farnsworth, D.; Rudnick, papers compiled since the October G. “Radio and IR study of the massive L. “Cross-correlation of diffuse 2010 issue of ATNF News. Papers which star-forming region IRAS 16353-4636”. synchrotron and large-scale structures”. include CASS authors are indicated by A&A, 523, A62 (2010). MNRAS, 402, 2-6 (2010). an asterisk. *Bietenholz, M.F.; Soderberg, A.M.; *Buitink, S.; Scholten, O.; Bacelar, J.; *Abdo, A. A.; Ajello, M.; Antolini, Bartel, N.; Ellingsen, S.P.; Horiuchi, S.; Braun, R.; de Bruyn, A.G.; Falcke, H.; E.; Baldini, L.; Ballet, J.; Barbiellini, Phillips, C.J.; Tzioumis, A.K.; Wieringa, Singh, K.; Stappers, B.; Strom, R.G.; G.; Baring, M. G.; Bastieri, D.; M.H.; Chugai, N.N. “VLBI Observations Yahyaoui, R. “Constraints on the flux Bechtol, K.; Bellazzini, R.; and 144 of the Type I b/c SN 2009bb”. ApJ, 725 of ultra-high energy neutrinos from coauthors. “Fermi large area telescope 4 (2010). Westerbork Synthesis Radio Telescope observations of gamma-ray pulsars *Blake, C.; Brough, S.; Colless, observations”. A&A, 521, A47-A47 PSR J1057-5226, J1709-4429, and M.; Couch, W.; Croom, S.; Davis, (2010). J1952+3252”. ApJ, 720, 26-40 (2010). T.; Drinkwater, M.J.; Forster, K.; *Burke-Spolaor, S.; Bailes, M.; Ekers, R.; *Ackermann, M.; Ajello, M.; Baldini, Glazebrook, K.; Jelliffe, B.; and 11 Macquart, J.-P.; Crawford, F., III. “Radio L.; Ballet, J.; Barbiellini, G.; Bastieri, coauthors. “The WiggleZ Dark Energy bursts with extragalactic spectral D.; Bechtol, K.; Bellazzini, R.; Berenji, Survey: the selection function and z = characteristics show terrestrial origins”. B.; Bloom, E. D.; and 161 coauthors. 0.6 galaxy power spectrum”. MNRAS, ApJ, 727, 18 (2011). “Fermi-lat search for pulsar wind 406 803 (2010). nebulae around gamma-ray pulsars”. *Calvelo, D.E.; Fender, R.P.; Russell, Bozzetto, L.M.; Filipovic, M.D.; ApJ, 726, 35-35 (2011). D.M.; Gallo, E.; Corbel, S.; Tzioumis, Crawford, E.J.; Bojicic, I.S.; Payne, J.L.; A.K.; Bell, M.E.; Lewis, F.; Maccarone, Aversa, Alan G.; Johnson, Kelsey E.; Medik, A.; Wardlaw, B.; de Horta, A.Y. T.J. “Limits on the quiescent radio Brogan, Crystal L.; Goss, W. M.; Pisano, “Multifrequency radio observations of emission from the black hole binaries D. J. “ and ATCA a SNR in the LMC. The case of SNR GRO J1655-40 and XTE J1550-564”. Search for Natal Star Clusters in Nearby J0527-6549 (DEM 1204).” SerAJ, 181, MNRAS, 409, 839-845 (2010). Star-forming Galaxies”. AJ, 141, 125 43-49 (2010). ( 2011) . *Caswell, J.L.; Breen, S.L. “An unbiased *Braine, J.; Gratier, P.; Kramer, C.; pilot survey for Galactic water masers”. Bailes, M. “Curious properties of the Xilouris, E. M.; Rosolowsky, E.; MNRAS, 407, 2599-2610 (2010). recycled pulsars and the potential of Buchbender, C.; Boquien, M.; Calzetti, high precision timing”. NewAR, 54, 86- D.; Quintana-Lacaci, G.; Tabatabaei, F.; *Caswell, J.L.; Breen, S.L.; Ellingsen, S. 86 (2010). and 16 coauthors. “Cool gas and dust P. “A water maser survey towards the in M 33: Results from the HERschel M galactic centre”. MNRAS, 410, 1283- *Bates, S.; Johnston, S.; Lorimer, D.R.; 33 Extended Survey (HERM33ES)”. 1294 (2011). Kramer, M.; Possenti, A.; Burgay, J.; A&A, 518, L69 (2010). Stappers, B.; Keith, M.J.; Lyne, A.; Bailes, *Caswell, J.L.; Green, J.A. “Blueshifted M.; McLaughlin, M.A.; O’Brien, J.T.; *Braun, R.; Heald, G.; Beck, R. “The outflow from 24.329+0.145”. MNRAS, Hobbs, G. “A 6.5-GHz Multibeam Westerbork SINGS survey. III. Global 411, 2059-2066 (2011). Pulsar Survey”. MNRAS, 411, 1575-1584 magnetic field topology”. A&A, 514, ( 2011) . A42 (2010). Cernuda, I. “Cosmic-ray electron anisotropies as a tool to discriminate *Bell, M. E.; Tzioumis, T.; Uttley, P.; *Brown, S.; Duesterhoeft, J.; Rudnick, between exotic and astrophysical Fender, R. P.; Arévalo, P.; Breedt, E.; L. “Multiple shock structures in a radio sources”. Astroparticle Physics, 34, 59- McHardy, I.; Calvelo, D.E.; Jamil, O.; 69 (2010).

37 *Champion, D.J.; Hobbs, G.B.; Davies, L.J. M.; Bremer, M.N.; Stanway, * Ferdman, R.D.; Stairs, I.H.; Kramer, Manchester, R.N.; Edwards, R.T.; Backer, E.R.; Birkinshaw, M.; Lehnert, M.D. M.; McLaughlin, M.A.; Lorimer, D.R.; D.C.; Bailes, M.; Bhat, N.D.R.; Burke- “Limits on the molecular gas content Nice, D.J.; Manchester, R.N.; Hobbs, G.; Spolaor, S.; Coles, W.; Demorest, P.B.; of z ~ 5 LBGs”. MNRAS, 408, L31-L35 Lyne, A.G.; Camilo, F.; and 7 coauthors. and 12 coauthors. “Measuring the mass (2010). Erratum: “A precise mass measurement of solar system planets using pulsar of the intermediate-mass binary pulsar *Dawson, J.; McClure-Griffiths, timing”. ApJ, 720, L201-L205 (2010). PSR J1802-2124”. ApJ, 713, 710 (2010). N.; Kawamura A.; Mizuno, N.; *Chandola, Yogesh; Saikia, D.J.; Gupta, Onishi, T.; Fukui, Y. “Supershells as Filipovic, M.D.; Crawford, E.J.; Jones, N. “HI gas in the rejuvenated radio molecular cloud factories: Parsec-scale P.A.; White, G.L. “Radio-continuum jets galaxy 4C29.30”. MNRAS, 403, 269- observations of HI and 12CO(J=1- around the peculiar galaxy pair ESO 273 (2010). 0) in GSH 287+04-17 and GSH 295-IG022”. SerAJ, 181, 31-37 (2010). 277+00+36”. ApJ, 728, 127 (2011). *Clay, R.W.; Whelan, B.J.; Edwards, P.G. *Ford, H.A.; Lockman, F.J.; McClure- “Centaurus A at ultra-high energies”. Dedes, C.; Leurini, S.; Wyrowski, F.; Griffiths, N.M. “Milky Way Disk-Halo PASA, 27, 439-448 (2010). Schilke, P.; Menten, K.M.; Thorwirth, S.; Transition in H I: Properties of the Ott, J. “A study of three southern high- Cloud Population”. ApJ, 722, 367-379 *Cluver, M.E.; Jarrett, T.H.; Kraan- mass star-forming regions”. A&A, 526, (2010). Korteweg, R.C.; Koribalski, B.S.; A 59 ( 2011) . Appleton, P.N.; Melbourne, J.; Emonts, *Ford, H.A.; McClure-Griffiths, N.M.; B.; Woudt, P.A. “Active disk building *Defraigne, P.; Manchester, R.; Matsakis, Lockman, F.J.; Bailin, J.; Calabretta, M.R.; in a local HI-Massive LIRG: the synergy D.; Petit, G.; Hosokawa, M.; Leschiutta, Kalberla, P.M.W.; Murphy, T.; Pisano, D.J. between gas, dust, and star formation”. S.; Zhai, Z.-C. “Commission 31: Time”. “Erratum: “HI clouds in the lower halo. ApJ, 725, 1550-1562 (2010). IAUTB 6, 140-141 (2010). I. The galactic A survey pilot region”. AJ, 710, 1868 (2010). Crawford, E.J.; Filipovic’, M.D.; Haberl, *Dickel, J.R.; Gruendl, R.A.; McIntyre, F.; Pietsch, W.; Payne, J. L.; de Horta, V.J.; Amy, S.W. “A 4.8 and 8.6 GHz *Freudling, W.; Staveley-Smith, L.; A.Y. “Multi-frequency study of Local survey of the small magellanic cloud: the Catinella, B.; Minchin, R.; Calabretta, Group supernova remnants. The images”. AJ, 140, 1511-1518 (2010). M.; Momjian, E.; Zwaan, M.; Meyer, curious case of the Large Magellanic M.; O’Neil, K. “Deep 21 cm H I *Dickel, J.R.; McIntyre, V.J.; Gruendl, Cloud SNR J0528-6714”. A&A, 518, Observations at z ˜ 0.1: The Precursor R.A.; Milne, D.K. ERRATUM: “A (2010). to the Arecibo Ultra Deep Survey”. 4.8 and 8.6 GHz survey of the large ApJ, 727, 40 (2011). *Croft, Steve; Bower, Geoffrey C.; Magellanic Cloud. I. The Images”. (2005, Ackermann, Rob; Atkinson, Shannon; AJ, 129, 790) AJ, 140, 1567 (2010). Ghirlanda, G.; Ghisellini, G.; Tavecchio, Backer, Don; Backus, Peter; Barott, F.; Foschini, L. “Correlation of Fermi *Eatough, R.P.; Molkenthin, N.; Kramer, William C.; Bauermeister, Amber; Blitz, Large Area Telescope sources with the M.; Noutsos, A.; Keith, M.J.; Stappers, Leo; Bock, Douglas; and 41 coauthors. 20-GHz Australia Telescope Compact B.W.; Lyne, A.G. “Selection of radio Erratum: “The Array radio survey”. MNRAS, 407, 791- pulsar candidates using artificial neural twenty-centimeter survey - a 690 deg 803 (2010). networks”. MNRAS, 407, 2443-2450 (2), 12 epoch radio data set. I. catalog (2010). *Gliozzi, M.; Panessa, F.; La Franca, and long-duration transient statistics”. F.; Saviane, I.; Monaco, L.; Foschini, L.; ApJ, 724, 827-827 (2010). Elson, E.C.; de Blok, W.J.G.; Kraan- Kedziora-Chudczer, L.; Satyapal, S.; Korteweg, R.C. “A search for non- Cui, L., Liu, X., Liu, J., Song, H.G. & Sambruna, R.M. “Q2122-444: A naked circular flows in the extended HI disc Ding, Z. “The follow-up European VLBI active galactic nucleus fully dressed”. of NGC 2915”. MNRAS, 411, 200-210 Network observations of twelve GPS ApJ, 725, 2071-2077 (2010). ( 2011) . radio sources at 5 GHz”. A&A, 518, A23 (2010).

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42 Issue No. 70, April 2011 Figure 1: A false-colour X-ray image from the Chandra X-Ray observatory of the Bullet Cluster, with superimposed contours of the pressure/temperature distribution in the gas, determined from SZ observations with the Australia Telescope Compact Array. See page 31 for further details.

43 For further information:

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Ross Forsyth stands in the receiver cage of one of the Australian Square Kilometre Array Pathfinder antennas at the Murchison Radio-astronomy Observatory. Credit: CSIRO