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ATNF News Issue No

ATNF News Issue No

ATNF News Issue No. 69, October 2010 ISSN 1323-6326

CSIRO Astronomy and Space Science – undertaking world leading astronomical research and operator of the Telescope National Facility. Two of CSIRO’s new Australian Pathfinder (ASKAP) antennas, close to the centre of the array, during assembly at the Murchison Radio- astronomy Observatory in September 2010. Credit: Carole Jackson

A reflector dish is placed on its pedestal as one of CSIRO’s new ASKAP anennas is assembled at the Murchison Radio- astronomy Observatory. Credit: Ross Forsyth

Cover page image

Three newly constructed CSIRO ASKAP antennas pictured at the Murchison Radio-astronomy Observatory in Western Australia.

2 ATNF News, Issue 69, October 2010 Editorial Contents

Welcome to the October issue From the Chief of CSIRO Astronomy and Space Science...... 4 of ATNF News for 2010. CASS Organisational Change...... 5 In this issue we report on a number ASKAP and SKA News...... 6 of staff changes including the arrival Super Science Fellowships Awarded to CASS...... 9 of Dr Phil Diamond, on 1 June Distinguished Visitors...... 9 as new CASS Chief and ATNF Education and Outreach...... 10 Director, as well as the recent Graduate Student Program...... 11 departures of Lewis Ball to the Australia Telescope Compact Array Open Day...... 12 Atacama Large Millimeter Array CASS Telescopes Track IKAROS...... 14 (ALMA) and Dave DeBoer to the 2010 Grote Reber Medal Awarded to Alan Rogers...... 16 University of , Berkeley. 2010 CASS School...... 18 We wish both Lewis and Dave well In France at the International Space University’s Space Studies Program...... 20 in their new endeavours. You can The Southern Cross Astrophysics Conference Series...... 21 read more about Phil Diamond’s Supernovae and their Host Galaxies...... 21 first impressions of CASS and the The MALT 90 GHz Survey and the SOC Pilot Project...... 22 ATNF in his column on page four. Discovery of a Radio–loud X-ray–quiescent Magnetar in the High Time Resolution In other news, we report on CASS Universe Survey...... 26 success at being awarded three of First Science from the ASKAP and Warkworth Antennas...... 30 the Australian Research Council’s Bonsai-ed Gives Clue to Jet Energies...... 33 new Super Science Fellowships. National Facility Operations...... 34 The Fellowships, worth a total of Publications List...... 36 $835,000 over three years, will help develop technology for the future international Square Kilometre Array (SKA) . In other newsletter highlights, we to be installed at the Murchison International Space University’s feature a number of science articles, Radio-astronomy Observatory, along Space Studies Program in France. with a new 12-m antenna installed all based on the fantastic research As always, we provide our regular at Warkworth in New Zealand. that is being undertaken at our in-depth update on CSIRO’s observatories. In the first, Roberto We also feature a report on the Australian Square Kilometre Array Soria reports on a new Compact MALT-90GHz survey, and examine Pathfinder (ASKAP) and SKA Array study of a microquasar in how this activity has been used related activity. As we go to print, the galaxy NGC 7793. His research as a demonstration project in the ASKAP project remains well suggests that the true power of the development of a Science on track with staff currently busy black hole jets is a thousand times Operations Centre in Sydney. at the MRO site, constructing larger than the power estimated ASKAP antennas numbers 2-6. In other news, Phil Edwards looks from observed radio emissions. We at the Japanese mission To conclude, we finish with our also feature an article by Michael IKAROS — successfully tracked by regular Operations report. Keith and collaborators, who report the Mopra telescope; we report on on the intriguing discovery of a If you would like to contribute to this year’s CASS Radio Astronomy magnetar, by its radio emission alone. future editions of the ATNF News, School held recently at the Narrabri please contact the newsletter team. Also on a science front, Professor Observatory; Chris Hollingdrake Steven Tingay reports on successful details a successful public open Tony Crawshaw and Joanne Houldsworth VLBI observations undertaken using day at the Compact Array; and The ATNF Newsletter Production Team the first of the ASKAP antennas Kjetil Wormnes undertakes the (newsletter@atnf..au)

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

In years past I would receive, originally by post and then more recently via a URL, a copy of the ATNF Newsletter. I was always admiring of the Newsletter: a professional looking document with a range of articles of interest to the users of the ATNF and the wider community. I now find myself in the role of the Chief of CSIRO Astronomy and Space Science (CASS) and the Director of the ATNF and so it is a pleasure to write the “Chief’s Column” for the first time.

To begin, I’d like to take the Newsletter) and the huge potential will become clearer and then, of to give my views on the opportunity of the SKA and the course, we need to know where current status of the Division and local precursor project, ASKAP. the SKA will be located. All of these the ATNF as well as to elaborate, issues will have implications for Opportunities however also bring to some extent, on future strategic radio astronomy across the planet. challenges. A big issue facing CASS direction. Since starting this role and the Australian astronomy To conclude the column, I’d like to on the 1 June 2010 I’ve discovered community is the rapidly changing share with you one of the principal that there is no getting away from strategic landscape. CSIRO is building attractions of coming to lead the fact that CASS and the ATNF ASKAP and aims to be delivering CASS — and that’s the chance to are embedded within CSIRO, science to the user community in work with such an excellent team. a large organisation of 6,500 2013. One immediate challenge Australia and CSIRO in particular, people. This brings with it various is ensuring that we have the full have always had a world-class challenges and opportunities. One operating funds for ASKAP and the reputation in radio astronomy. This personal challenge is that I’ve had existing ATNF facilities, an issue that is still the case. People express to learn CSIRO-speak at which I is being vigorously pursued right now. concern when essential senior staff am told, to my dismay, that I am approach retirement. I worry less, already alarmingly proficient. More In the slightly longer term we especially when I see the quality of seriously, I have been impressed need to understand what might the young engineering team here at at the huge support that CSIRO be the impact of the SKA on radio CASS. This is a talented team that and the astronomy in Australia. As I write, I is oriented towards the future. provide for radio astronomy, a sum am preparing to attend a series of exceeding $300M over the last high-level SKA meetings in Oxford, I hope you enjoy reading this few years. This support is driven which will be taking decisions vital issue of the ATNF Newsletter. both by the excellent science for the future of the project. As we These are exciting times for undertaken with the current facilities see the outcomes of these meetings radio astronomy Down Under. (see articles elsewhere in this the future structure of the SKA

4 ATNF News, Issue 69, October 2010 CASS Organisational Change Tony Crawshaw (CASS)

Since the previous issue of ATNF News (April edition), CSIRO Astronomy and Space Science has seen a number of organisational and personnel changes.

June 1st saw Dr Phil Diamond on board as CASS Chief, arriving from his previous role as Director at the Jodrell Bank Centre for Astrophysics at the . Lewis Ball announced his departure as Deputy Chief of CASS to take up a new role as the Deputy Director for ALMA, the ~US$1B Atacama Large Millimeter Array. Graeme Carrad has taken on the role of Acting Deputy Chief of CASS (effective 17 September) with a search to recruit a new Lewis Ball - “best wishes” for the future Deputy Chief currently underway. Credit: Flo Conway-Derley, CSIRO. Dave DeBoer, ASKAP Project Leader will be leaving CSIRO in early October and is moving back to UC Berkeley to take up a post as ASKAP Leader in a substantive the Department of Innovation, working on the Allen Telescope appointment on 1 September. Industry, Science and Research. Array and other projects. The post In other role changes, CSIRO’s SKA We wish everyone well in their became available as a result of Director Brian Boyle has become new appointments and thank the untimely death of Don Backer. the Project Director for the Australia Lewis and Dave for their many As a result of this move, Ant – NZ SKA site bid, spending 80% years of service within CSIRO. Schinckel replaced Dave DeBoer of his time on secondment to

5 ASKAP and SKA News

Florence Conway-Derley (CASS)

Antenna construction site has been achieved with of Intent to cooperate on the underway at the MRO a preliminary connection (in development and testing of phased the lab) of the analog pedestal array feed technology for the SKA. As this article goes to print, system to the digital system. The partnership is an example of construction of CSIRO’s next • Design of civil works, building the cooperation needed to bring five Australian Square Kilometre and power and data distribution a monumental undertaking such Array (ASKAP) antennas is well at the MRO is now complete; a as the SKA project to fruition. underway at the Murchison Radio- prototype ground-coupled cooling The collaboration pools world- astronomy Observatory (MRO). system has been trialled at the site leading expertise from ASTRON The initial manufacture of ASKAP of the first antenna and preliminary and CSIRO to develop phased antennas 2 – 6 was completed design work has commenced for array feeds for future radio on schedule earlier in the year, a solar/diesel hybrid power plant. telescopes. The wide field of view with the antennas passing factory • The long-haul fibre link from capability that phased arrays acceptance testing in July. Antenna Geraldton to the MRO is offer would fully exploit the build on site, site acceptance testing progressing well with AARNET; science potential of the SKA. and commissioning then took place civil works have commenced during September and October. with the route surveyed and pegged for direct burial fibre CSIRO delivers new Technology Update along the 390 km route. SKAMP Digital System A major milestone has been The ASKAP project continues • A process to validate the reached for the Square Kilometre to reach key milestones, electromagnetic compatibility Array Molonglo Prototype progressing towards successful (EMC) of all equipment destined (SKAMP) project with the delivery delivery of the project. for the MRO is in place, with an EMC test facility operational of its new digital correlator. • Two prototype ASKAP prime at CSIRO’s Marsfield site. CSIRO officially handed-over the focus receivers are being • Monitoring of radio frequency completed digital system to the designed and assembled, and interference (RFI) at the SKAMP team in September. are destined for testing at the Australasian core site for Over the last few years, the Molonglo Parkes Testbed Facility (PTF) and the SKA has concluded. Observatory Synthesis Telescope at one of the ASKAP antennas. (MOST) has been transforming • Data networks have taken on General News from the narrowband MOST a three tier development; with (4-MHz centred at the operating networks specific to the testbed frequency of 843-MHz) into SKAMP CSIRO-ASTRON to Collaborate at CSIRO’s Marsfield site, at — a significant SKA prototype. Parkes, and at the ASKAP site, on the Development of the Murchison Radio-astronomy Phased Array Feeds SKAMP increases the bandwidth, Observatory (MRO). sensitivity, field of view and adds During the International SKA Forum spectral line capabilities of MOST by • Prototype assemblies for test (ISKAF2010), held in Assen in June the installation of a correlator. Greatly and engineering software have 2010, CSIRO and the improved calibration of astronomical been developed, and initial Institute for Radio Astronomy data and significantly improved integration of an ASKAP testbed (ASTRON) signed a Statement image quality can be achieved. system at CSIRO’s Marsfield

6 ATNF News, Issue 69, October 2010 Representatives from CSIRO, ASTRON and SPDO celebrate the signing of the Collaborative Agreement at ISKAF 2010. From left: Richard Schilizzi (SPDO), Dr Brian Boyle (CSIRO), Dr David DeBoer (CSIRO), Wim van Cappellen (ASTRON), Dr Carole Jackson (CSIRO), Dr Mark Verheijen (ASTRON), Dr Tom Oosterloo (ASTRON), and Professor Mike Garrett (ASTRON). Credit: Hans Hordijk

CSIRO SKA Director Dr Brian Boyle hands over a correlator board to SKAMP Project Leader Prof Anne Green. Credit: Tony Crawshaw, CSIRO

7 In SKAMP, the data is received by an new electronically-steered wide-band As both the MRO and the Pawsey analog system and digitised before feed system capable of observing Centre will have high electricity being sent to the correlator. The over an expanded frequency demands, a combination of on- correlator processes this data into a range (700 MHz – 1100 MHz). site geothermal and renewable form that is then used to generate systems will deliver clean, green radio images and spectral cubes; Renewable Energy Solutions energy and provide a reduced this is the astronomer’s “result”. to Support the SKA carbon footprint with ongoing demand-side management. The development of the digital With funding from the correlator has been a joint Round of the Working with Melbourne-based collaboration between CSIRO Australian Government’s Education company Direct Energy, CSIRO and the , Investment Fund (EIF), CSIRO has already installed a prototype with the ASKAP Digital Systems will utilise full-scale, clean energy geoexchange system at the site team providing a major part of technology to support the Australia of ASKAP’s first antenna. This the technical and implementation – New Zealand bid to host the technology has the potential for expertise. CSIRO is also building international SKA project. long term sustainability, using the the digital correlator for the ground as a heat sink to reduce The Sustainable Energy for the SKA Murchison Widefield Array the telescope’s overall energy use. project will develop renewable (MWA) SKA Precursor project. energy technologies to help power ASKAP is building on the digital the MRO. This includes CSIRO systems design developed for both working to develop a collaborative the SKAMP digital systems and partnership with Western Australia’s the Compact Array Broadband Horizon Power to develop a solar/ Backend installed at the Australia diesel power generation system Telescope Compact Array for ASKAP and other telescopes (ATCA, Narrabri NSW). under construction at the MRO. SKAMP was also recently The funding also allows a variety designated an official SKA Pathfinder of demand-side management project by the SKA Science and technologies to be implemented. Engineering Committee (SSEC). Additionally, the nation’s It was determined that SKAMP’s largest direct heat geothermal contribution satisfied the Pathfinder demonstrator will be developed criteria within the areas of to help cool ASKAP’s support technology, science and operations. computing facility, the Pawsey High The next (final) stage of the SKAMP Performance Computing Centre project will see the installation of a for SKA Science based in Perth.

8 ATNF News, Issue 69, October 2010 Super Science Fellowships Distinguished Visitors Awarded to CASS Robert Braun (CASS) Tony Crawshaw (CASS)

CSIRO has been awarded three ASKAP; the WALLABY survey of Over the past months we have of the Australian Research neutral hydrogen emission of the enjoyed working visits from Jianping nearby universe and the EMU survey Yuan (Urumqi Obs,ervatory China), Council’s new Super Science of the continuum sky. ASKAP is Ding Chen (Chinese Acadamy Fellowships, worth a total of currently being built at the Murchison of Sciences, China), Marchella Radio-astronomy Observatory in Massardi (Instituto Nazionale di $835,000 over three years, to the mid west of Western Australia. Astrofisica, Italy), James Jackson help develop technology for the (Boston University, USA), Martin Robert Braun, Head of Astrophysics Cohen ( international Square Kilometre at CASS commented, “The Super Berkeley, USA), Bill Coles (University Array (SKA) radio telescope. Science Fellowships provide a of California, San Diego, USA), vital contribution to enabling Marianne Lemoine (Bordeaux, The announcement was made world-class science in Australia. France), Thierry Reposeur (Bordeaux, in April 2010, by Senator Kim The three CSIRO fellows will France) and Marie-Helene Carr, Minister for Innovation, play a key role in facilitating that Grondin (Bordeaux, France). Industry, Science and Research. science with ASKAP and further refining our cutting edge, wide-field Upcoming visitors we expect The aim of the awards is to give technology so that it is SKA-ready.” include Dale Frail (National Radio early career researchers the Astronomy Observatory, USA) opportunity to work in areas Support for SKA related science and Patricia Henning (University of national significance. Space was evident in the Minister’s of New Mexico, USA). science and astronomy is one of announcement, with twenty-one of the three areas targeted by the the one-hundred new Fellowships The Distinguished Visitors program Super Science Fellowships — the announced, going towards research remains a very productive means other two are marine and climate related to the development of SKA of enabling collaborative research science, and future industries pathfinder instruments in Australia projects with local staff, adding (biotechnology and nanotechnology). or the use of those instruments to substantially to the vitality of the undertake ground-breaking research. research environment. Visits can be The three CSIRO Fellows are likely organised for periods ranging from to be in place by the end of the ASKAP and SKA related Fellowships only a few weeks up to one year. year. One will be working on refining went to of the innovative radio camera (or Technology, The University of For more information please see Western Australia, the Anglo- phased array feed) of the Australian www.atnf.csiro.au/people/ Australian Observatory, the Square Kilometre Array Pathfinder distinguished_visitors.html (ASKAP) telescope. The other two University of Sydney, the University will be solving some of the technical of , Swinburne University Prospective visitors should challenges of the highest priority all- of Technology, the University of contact the local staff member sky surveys being carried out with Melbourne and . with the most similar interests.

9 Education and Outreach Rob Hollow (CASS)

PULSE@Parkes interest in the session and were CASS Education Officer Rob Hollow the first group to see one of the also ran a one-day workshop Teaching With the recent PULSE@Parkes project’s nulling pulsars actually Astronomy and Astrophysics for the observing session held at the turn on whilst being observed. VCE in collaboration with VSSEC Victorian Space Science Education at Scienceworks in Melbourne in Centre (VSSEC) in September 2010, April. CSIRO SKA Director Dr Brian over 500 students from 47 schools Teacher Workshops Boyle gave the prestigious Stanhope have now observed remotely with and School Events Oration at CONASTA 59, the annual the 64-m CSIRO Parkes radio The highly popular Astronomy from national conference for Australian telescope. Regular sessions have the Ground Up teacher workshop Science Teachers. His talk The Square been held at the CASS Marsfield site, held at the in Kilometre Array: Inspiring the Next with another recently held at SPICE May saw a record number of 30 Generation and beyond was extremely in the University of Western Australia teachers participate in the three- well received and prompted lengthy as part of National Science Week day event. A diverse range of discussion and questions. Rob Hollow activities in August. The interstate talks, workshop sessions, practical also ran workshop sessions at the sessions involve students from a activities, a viewing night and a conference. He also presented a number of schools coming together telescope tour kept the teachers session on careers in science at the for an intense day of background engaged and stimulated. Some second Mid West Youth Science Forum talks, observing and data analysis. of the participating teachers also in Geraldton in July as well manning Interest in the program continues presented sessions, sharing with the astronomy desk with Professor to grow and it was featured as other participants, the activities that Steven Tingay from ICRAR for a part of an article in the Sydney they and their students undertake. Q&A session with Year 10 students. Morning Herald about the search for gravitational waves at Parkes. The program continues its international expansion with students from Emelwerda College in the Netherlands controlling the Dish in May during the second international PULSE@Parkes event hosted and supported by ASTRON. Project Coordinator Rob Hollow and team member Dr David Champion from Bonn were assisted by several ASTRON staff including regular Parkes observer Dr Marijke Haverkorn. The students showed great

CSIRO’s Rob Hollow linking Dutch students to the Parkes telescope. Credit: CSIRO

10 ATNF News, Issue 69, October 2010 Graduate Student Program Baerbel Koribalski (CASS)

We would like to officially welcome the following students into the ATNF co- supervision program.

• Vanessa Moss (University of • Emma Kirby (Australian Sydney): Low and intermediate National University): Sharing velocity HI clouds in the Milky the Baryons: Stars and Gas Way with supervisors Dr in Local VolumeGalaxies. Tara Murphy and Dr Naomi • Alyson Ford (University of McClure-Griffiths (CASS). Swinburne): The HI Cloud Population • Yanett Contreras (Universidad in the Lower Halo of the Milk Way. de Chile): Study of filamentary • Shari Breen (University of structures in the southern galactic Tasmania): Masers as evolutionary plane with supervisors Dr Guido tracers of high-mass star formation. Garay (Universidad de Chile) and Dr Jill Rathborne (CASS). Dr Shari Breen is now a Bolton Fellow at ATNF, CSIRO • Kathrin Wolfinger (University Astronomy & Space Science. of Swinburne):The effect of environment on the evolution Dr Urvashi Rao Venkata is of gas-rich spiral galaxies with now working at the National supervisors Dr Virginia Kilborn, Radio Astronomy Observatory Dr Emma Ryan-Weber (both Science Operations Center. University of Swinburne), and Dr Alyson Ford is now a postdoc DrBaerbel Koribalski (CASS). at the University of Michigan, USA. Congratulations to the Dr Paul Hancock is now a postdoc following graduating students. at the University of Sydney. Well done ! • Urvashi Rao Venkata (Department of Physics, New Mexico Institude A summary of the ATNF Graduate of Mining and Technology, Student Program, current and Socorro, NM, USA): Parameterized past students, as well as new Deconvolution for Wide-Band application forms can be found at Radio Synthesis Imaging. • Paul Hancock (University of http://www.atnf.csiro.au/research/ Sydney): The Australia Telescope graduate/scholars.html 20 GHzSurvey and the Search for Young Radio Galaxies. Images clockwise from top left: Urvashi Rao Venkata, Paul Hancock., Alyson Ford, Emma Kirby, and Shari Breen, Images courtesy Baerbel Korabilski.

11 Australia Telescope Compact Array Open Day Chris Hollingdrake (CASS)

More than 700 people took combination of both. Around fifty and astronomy and space science advantage of the rare opportunity volunteers donated their time to talks. Antenna tours ran continuously help showcase the great work throughout the day, with the to get a closer look at the of our division, and Narrabri put compact configuration of the array Australia Telescope Compact on perfectly clear blue skies. Our allowing us access to four antennas. volunteers came from around the These guided tours took visitors Array (ATCA) during the recent state including staff from Narrabri, up and inside the antennas and Open Day on the 17 July. The Marsfield, Parkes and Tidbinbilla. allowed our Compact Array experts to share their enthusiasm and test Open Day aims to give the public Attendance was up twenty percent their knowledge with the many an increased understanding on the previous Open Day. Early tricky questions thrown their way. planning and demographic surveying of radio astronomy and the of the previous Open Day allowed us Four talks were held across the research that we undertake. to target our promotional activities day with each being well attended. in the region. Family groups were by Dr Jamie Stevens presented Under Two things generally help to ensure far the most common attendees. the hood of the Compact Array, a successful Open Day — lots of Dr Phil Edwards presented From enthusiastic volunteers and beautiful The most popular activities were the the Universe to Culgoora, Glen weather. This year we had the perfect antenna tours, control building tours

Caption: Visitors make their way around the Observatory. Credit: Cornelia Kellenberg

12 ATNF News, Issue 69, October 2010 Nagle from Tidbinbilla presented Bootleg postcards: Participatory exploration of distant worlds and Professor Jim Jackson presented Star birth and snaky dark clouds. CSIRO Education supported the Open Day with their fantastic hands-on physics displays. CSIRO Education officer, Mitch Serena, did a great job entertaining many of Shane O’Sullivan and Angela Hein, two of the many volunteers that the families, dazzling them with fun helped out on the day. Credit: Tony Crawshaw, CSIRO and educational demonstrations. A visit by the local scout group tested the durability of both Mitch and his equipment. The laughter and excitement of the group indicated the activity was a good match for this age group. Other activities offered included solar telescope viewing, a science and astronomy education shop, face painting and a jumping castle. The assortment of quality activities saw visitors staying longer at the Open Day. Some families spent the entire day at the observatory. One of the major benefits of holding open days is the opportunity for CASS staff to socialise away from our usual places of work. The Saturday night barbeque was a great success. Thank you to the Narrabri staff for putting on such wonderful hospitality. The evening topped off a great weekend. Thank you also to all the volunteers who made the Open Day such a great success and I look forward to our next Open Day in Parkes in 2011.

Visitors wait for their antenna tour. Credit: Cornelia Kellenberg

13 CASS Telescopes Track IKAROS Phil Edwards

CASS’s Mopra radio-telescope Accelerated by Radiation Of the year was to send the and CDSCC’s Tidbinbilla antennas Sun (IKAROS) is an experimental on its way to . were used in August as part of spacecraft of the Japan Aerospace The opportunity was also used to a program to track the Japanese Exploration Agency (JAXA). The launch four other small spacecraft, solar sail mission, IKAROS. main purpose of a Japanese H-IIA one of which was the 300kg The Interplanetary Kite-craft rocket launch on 21 May this IKAROS craft.

This figure shows the successful search for interferometric fringes on the baseline between the Mopra 22-m telescope and the Usuda 64-m telescope in Japan. The data used to produce this figure are from an 81 second integration at 8.4- GHz on PKS 1354-17, which was used as a phase reference calibrator for IKAROS spacecraft from the observation on 1 July, 2010. The x-axis shows the delay residual, and the y-axis shows the residual rate. The fringes can be seen at a delay of 62 nanoseconds, and a rate close to zero.

14 ATNF News, Issue 69, October 2010 IKAROS is the first spacecraft to with a widely-spaced array of radio IKAROS observations and who use solar sailing as the main means telescopes (using the technique of were able to be compensated with of propulsion. Unfurling of the Very Long Baseline ), additional time on other days. sail, which is made of a polyimide the spacecraft’s position in the Radio telescopes in Japan, China, membrane 7.5 micrometres thick plane of the sky can be accurately and Australia are collaborating in — thinner than a human hair! — determined, perfectly complementing this venture. In Australia, besides was completed on 10 June. The sail the method of timing signals to and Mopra and Tidbinbilla, the Hobart is square in shape and measures from the spacecraft, which constrain dish operated by the University of 14 metres on each side. Thin- the position along the line of sight. Tasmania, and the European Space film solar cells are integrated into The JAXA coordinator of these Agency’s antenna at New Norcia in the sail to power the spacecraft observations, Dr Hiroshi Takeuchi, Western Australia have been used. payload, and eight LCD panels are notes “Long north-south baselines embedded in the sail to control The orbit of IKAROS will take it are vital, because the conventional the orientation of the spacecraft past Venus in December this year, range and range-rate based orbit by electronically adjusting the and then on a three year journey determination has less sensitivity reflectance of each panel. to the far side of the Sun as seen to the Declination component of from the Earth. However there is On 9 July, JAXA announced that the spacecraft position when the only a limited opportunity for radio they had detected the very slight declination of the spacecraft is low. astronomers to contribute: as the acceleration of the spacecraft due The long Australian – Japanese orientation of the spacecraft changes, to the pressure of sunlight on the baselines are ideal for evaluating the antenna transmitting the series solar sail. The main spacecraft payload the performance of the VLBI-based of tones will end up pointing further includes the on-board computer and orbit determination for IKAROS.” and further away from the Earth. The antennas to receive commands from Dr Chris Phillips, who arranged the next chance to use this technique Earth and transmit signals back. By Mopra observations, commented may come in March 2011, but as measuring the time taken for signals “These observations demonstrate the nominal lifetime for IKAROS is to be transmitted from Earth to the strides made recently with only 8 months, it may not live long IKAROS and returned, the distance international compatibility. We enough to “talk” to us again next year. to the spacecraft and the speed with were able to easily observe the which it is receding can be calculated. The initial successes of IKAROS spacecraft with standard LBA However this technique does not are likely to pave the way for other setups then transfer all the data allow the position of the spacecraft solar-sail spacecraft, with both the electronically to Japan for processing.” on the sky to be determined, and USA and Japan developing plans that’s where a network of radio The Mopra observations were for future missions based on this telescopes is coming to the rescue. conducted with the kind cooperation “energy efficient” approach. of the MALT-90 survey team, IKAROS includes a transmitter who were willing to give up the that sends a series of tones in the 1~2 hour blocks required for the 8-GHz band, and by detecting these

15 2010 Grote Reber Medal Awarded to Alan Rogers Helen Sim (CASS)

The 2010 Grote Reber Gold Medal for outstanding and innovative contributions to radio astronomy has been awarded to Dr Alan Rogers, a Research Affiliate at the Massachusetts Institute of Technology . Rogers is being honoured for his many pioneering developments in radio and radar interferometry, radio spectroscopy, and for his application of radio astronomy techniques to society.

The Medal was presented on 7 July 2010 in Hobart, Tasmania, at the annual meeting of the Astronomical Society of Australia. The Reber Medal was established by the Trustees of the Grote Reber Foundation to honour the achievements of Grote Reber and is administered by the Queen Victoria Museum in Launceston, Tasmania. The previous winners of the Grote Reber Medal have been Professor Bill Erickson (University of Maryland, 2005), Professor Bernard Mills (University of Sydney, 2006), Professor (Tata Institute of Fundamental Research, Dr Alan Rogers, MIT Haystack Observatory, receiving the Grote Reber Medal 2007), Dr Sander Weinreb (Caltech– for 2010. Credit Martin George

16 ATNF News, Issue 69, October 2010 Jet Propulsion Laboratory, 2008) radio spectrometer, is to detect the • in 1937, building the world’s first and Dr Barry Clark (National Radio cosmological epoch of reionization purpose-built radio telescope Astronomy Observatory, 2009). (EoR), a significant but poorly (a 9.75-m diameter dish); understood period in the history Alan Rogers received his B.Sc. • in the late ‘30s and early ‘40s, of the Universe. The experiment degree in mathematics and physics making the world’s first detailed measures the all-sky radio spectrum from the University College of radio map of the sky (published between 100 and 200 MHz in Rhodesia in 1962, and his S.M. in 1944). This was done at 160 order to probe the global evolution and Ph.D degrees in Electrical MHz, and showed for the first of 21-cm emission from neutral Engineering from Massachusetts time the Galactic Centre in hydrogen gas at high . In this Institute of Technology in 1964 and Sagittarius, the radio source type of measurement, reionization 1967 respectively. Following a year Cassiopeia A, and the first should produce a faint, step-like as a Lecturer at the University of observational evidence for spiral contribution to the spectrum that is Zimbabwe in 1968, he has since arms in our Milky Way Galaxy; superimposed on the much brighter been at the Haystack Observatory • in the early 1940’s, being the first Galactic synchrotron foreground. where he was the Associate Director to publish the detection of radio The observed frequency of the until his retirement in 2006. emission from the “quiet” sun “step” and its sharpness encode and the intense radio emission Rogers is best known for his both the redshift and duration of associated with solar activity. contributions over many decades to the reionization epoch. The EDGES the techniques of Very Long Baseline antenna and receiver were deployed • in the early 1950s, becoming Interferometry. More recently, he in August 2009 at the Murchison the first astronomer to build developed an innovative radio array Radio-astronomy Observatory in a high-altitude observatory in which he successfully used to detect Western Australia (Australia and Hawai’i (on Mt Haleakala); and the 327 MHz line of interstellar New Zealand’s candidate site for • from the mid 1950s, building the deuterium, capping a 40-year quest the SKA core). The first three- first “Square Kilometre Array” — for this important astrophysical month deployment of EDGES was an array of dipoles covering an atomic gas. He was also the leader of successful, and yielded constraints on area of one square kilometre in a program to apply radio astronomy reionization that have implications central Tasmania. This operated techniques to locate emergency for future EoR experiments. at a frequency of 2.13 MHz. In calls from mobile telephones. the 1960s Reber mapped the Who was Grote Reber? For almost southern sky with this telescope. Rogers is now working with a decade—1937 to 1946—he was Judd Bowman of Caltech on an the world’s sole radio astronomer. Next year, 2011, is the 100th Epoch-of-Reoinisation project, the Born in Wheaton, Illinois, in 1911, anniversary of Grote Reber’s birth. Experiment to Detect the Global he moved to Tasmania in 1954 For more information please see EoR Signature (EDGES). The aim of and spent more than half of his the Grote Reber Medal homepage this NSF-funded experiment, which long life there. (He died in 2002.) uses a single low-frequency dipole Reber’s achievements include: http://www.qvmag.tas.gov. antenna and a high dynamic-range au/?articleID=539

17 2010 CASS Radio Astronomy School Phil Edwards (CASS)

The 2010 CASS Radio radio astronomy with indigenous introduced calibration and editing, Astronomy School was held culture in Western Australia, which and Emil Lenc walked the students described a successful introduction through imaging and deconvolution, at the Narrabri Observatory to the Murchison Radio Astronomy before Naomi McClure-Griffiths from Monday 27 September Observatory and cultural exchange described various approaches of astronomical stories, which to data analysis. This placed the to Friday 1 October. A total of inspired indigenous artists to participants in good stead for the 45 participants attended, with capture the experience on canvas, Wednesday and Thursday tutorial a number of students travelling leading to a series of national sessions, which were divided into and international exhibitions. scheduling an ATCA observation, from China, South Korea, and hands-on ATCA observing, and data Tuesday talks focussed more on New Zealand for the School. reduction. Thanks to the Sydney the specifics of using the Compact University Stellar Interferometer Array, with Alex Dunning and Dick team, who were visiting that week, Ferris giving an overview of the The program of talks included participants were also able to have a front-end receiver design and back- introductions to radio astronomy guided tour to SUSI. Fortunately the end processing electronics. Maxim fundamentals by Jay Lockman skies cleared in time for participants Voronkov described observing (NRAO Green Bank) and John to enjoy optical views of the night strategies and Kate Brooks gave Reynolds, and to the principles sky before and after wood-fired particular attention to aspects of of interferometry by Rick Perley pizzas on site at the Observatory. mm-wavelength observing. The (NRAO Socorro). CASS Chief After dinner, Jay Lockman gave an tutorial session on Tuesday took Phil Diamond gave a talk on next entertaining pictorial history of full advantage of the availability generation radio telescopes. Tara the . of Mopra on the day, with all Murphy described the astronomers four tutorial groups having the Thursday’s program started with IT toolkit, with information on the chance to see Mopra put through Steven Tingay describing error software packages and computing its paces. Other sessions on the recognition, which was followed by skills that are becoming increasingly Tuesday were “Q&A with Rick an introduction to polarisation by important in all fields of astronomical & Jay”, an introduction to ATCA Dave McConnell (and his Poincare research. John Storey rounded out observing, and an antenna tour. spheres!). Galvanised by another Monday’s program by taking his cup of coffee, students returned audience on a tour of telescopes of Robert Braun kicked off Wednesday for Rick Perley to further stoke the world, replete with tales of their with an introduction to Fourier the polarisation furnace and distill germination, growth, and harvesting! Transforms, which had the an improved understanding, sullied unintended consequence of a The School Dinner was held in only by some remaining D-terms. couple of cats and one Radio School Narrabri on Monday evening, Mark Wieringa concluded the student being Fourier Transformed with Steven Tingay giving an after- morning with a review of observing in subsequent days! Jamie Stevens dinner talk entitled Connecting

18 ATNF News, Issue 69, October 2010 Participants of the 2010 CASS Radio Astronomy. School Credit: Emil Lenc

sensitivity and the approaches a opportunity to join a tour to All speakers, and additional tutors to attempting to improve it. Sawn Rocks in the afternoon. John Bateman, Shari Breen, Jimi Green, Balt Indermuehle, James The school concluded on Friday The efforts of all Narrabri staff in Urquhart, Robin Wark, and the SUSI with an overview of VLBI by Jamie setting up the Visitors Centre for the team, ensured the week was a great Stevens, an introduction to wide- school and in keeping participants success. Finally, the contribution of field imaging by Maxim Voronkov, well-fed, caffeinated, transported, financial support from the Donovan and a description of OPAL and and educated are applauded, Trust is gratefully acknowledged. ATOA by Jessica Chapman. The particularly the unstinting efforts of school wrapped up with a BBQ Jo Houldsworth and Marg McFee in lunch with Narrabri staff, and keeping everything running smoothly!

19 In France at the International Space University’s Space Studies Program Kjetil Wormnes (CASS)

In July and August of 2010, with the fantastic support of CASS, My group (of about 45) investigated I was fortunate enough to attend the International Space University’s the future feasibility of mining Near Earth Asteroids (NEA). NEAs have (ISU) Space Studies Program (SSP). The annual program is held at attracted some interest in recent international facilities — last year at NASA AMES and this year at the years as many of them fall into the category of being potentially main campus of the ISU in Strasbourg, France. All aspects of space- hazardous to us here on Earth. related activity are covered over the intensive nine week program. NASA has undertaken an effort to detect and characterise 90% of NEAs And what a time it was. There around the world. With visits often larger than 140 meters in diameter were 36 countries represented lasting a few weeks, it gave us time over the next 10 years; a huge task by 122 participants and various to get to know them “off-line”. and one in which we can expect a lot of interest to build as more attending lecturers, as well as those The first four weeks covered lectures information (and funding) becomes running workshops and other from the seven departments of the available over the coming years. activities. Backgrounds as diverse ISU; Engineering, Law, Space and as journalism, law and business to Society, Business, Space Life Sciences, There were two other Australians of course engineering and science Physical Sciences and Satellite participating in this year’s program, were represented by the group. Applications. The second half of the one from the Defence Space Staff and faculty were usually program allowed us to focus on Coordination Office and the other well-known names within NASA, a department of choice and was who used to be in the mining ESA or one of many other space- finished off by a large team project. industry. Among the lecturers and related organisations or businesses

Kjetil’s final project team. Credit: K.Wormnes

20 ATNF News, Issue 69, October 2010 The Southern Cross Astrophysics Conference Series* Fourth annual conference Sydney Powerhouse Museum, 20-24 June 2011 teaching staff there were actually Supernovae and their Host Galaxies quite a few Australians, mainly in the Policy and Law areas. between supernovae and I also had the pleasure to talk to Motivation their host galaxies. David Southwood, the director of The current generation Science and Robotic Exploration at of wide field transient Some topics to be ESA. We spoke about his involvement with Australia in establishing the surveys will revolutionise covered include first of ESA’s deep space antennas, our understanding of why located at New Norcia outside Perth. stars become supernovae. • the many different paths to a supernova explosion Other attendees included people Designed to revisit large from Brazil who were involved areas of sky at multiple • the progenitors of with the launch vehicle to be wavelengths, these surveys supernovae used by SHEFEX-2, a project by are now discovering the German Aerospace Centre • supernova remnants (DLR) which will be launched from hundreds of supernovae • supernova rates Woomera later this year, as well as each year. During the those involved with the landing of coming year, the number of • the relationships at Woomera in June. supernova discoveries will between the properties From 2010 onwards, a Southern increase even further as of supernovae and Hemisphere version of the SSP is new transient surveys come the properties of planned, with a format mostly similar online. As well as finding rare to the SSP, but a bit shorter and their host galaxies and possibly new types of with more focus on applications. • supernovae as tracers This year it will be based in , supernovae, these surveys of star formation but it will eventually move around will generate new insights the Southern Hemisphere just as into both core-collapse and • unusual supernovae the ISU SSP does in the north. I thermonuclear supernovae. expect it will attract the same calibre • unexplained transients It is therefore timely to have of lecturers and staff, and being • current and future closer to home, and held during our a conference that explores summer, will be a program that more the current (observational transient surveys Australians will be able to attend. and theoretical) supernova * Jointly organised by I hope we will be able to work landscape and the connection CASS and the AAO. with them to share some of the tremendous expertise available within CASS. It is an opportunity for us to build a relationship with the ISU and through that promote both astronomy and space science not only in Australia but around the rest of the Southern Hemisphere as well.

21 The MALT 90 GHz Survey and the SOC Pilot Project Jill Rathborne, Jessica Chapman, Kate Brooks (CASS) and Jim Jackson (Boston University) On behalf of the MALT90 science team and the Mopra Large Surveys Working Group

Abstract: Underway this year is a new, large, molecular line survey of dense cores at 90 GHz, the Millimetre Astronomy Legacy Team 90 GHz (MALT90) survey. The MALT90 survey will exploit the fast- mapping capability of the Mopra radio telescope, combined with the broadband MOPS correlator which allows the simultaneous imaging of 16 molecular lines near 90 GHz. These molecular lines will probe the physical conditions, chemical state, and evolutionary state of ~3,000 dense molecular cores. The target cores are selected as likely sites for the early stages of high-mass star formation and to span the complete range of their evolutionary states. Each core will be mapped simultaneously in 16 molecular lines at excellent angular (40 arcsec) and spectral (0.1 km/s) resolution. MALT90 will be especially useful to identify important targets for future ALMA observations.

A major goal for CASS is to develop molecular cores, high-mass stars the main-sequence and ionizes a Science Operations Centre may instead acquire most of their its surrounding material to form (SOC) in Sydney. Ultimately the mass by “competitive accretion,” a hyper- and ultra-compact H II SOC will provide the full range of process by which high-mass cores regions. Observationally, however, activities carried out for the science agglomerate material well outside of the very earliest stages of high- operations of ATNF facilities. As their gravitationally-bound parental mass protostellar evolution have well as a major science project, the cores (e.g., Bonnell et al. 1997). In remained elusive. Only a handful MALT90 project has been used this theory, material falls through the of candidate high-mass pre-stellar for a trial of SOC-mode observing. potential well of a large molecular cores have been tentatively identified, In the first part of this article we cloud, and is funnelled down to and it has been difficult to confirm describe the science goals of the molecular cores near the centre. The their pre-stellar . The earliest MALT90 survey. The second part cores near the cloud centre thus well-characterised phase is the “hot describes the SOC Pilot study. receive a fresh supply of material, molecular core” phase, well after and continue to accrete additional accretion has begun. Recently, earlier The MALT90 mass. Secondly, while low-mass stars phases have been identified as cold, Science Project reach the main-sequence after the compact cores within Infrared Dark accretion process has essentially Clouds (IRDCs; e.g., Carey et al.2000; Although the basic sequence for finished, young O stars first reach Rathborne et al. 2005, 2006). high-mass protostellar evolution is the main-sequence as B stars The community has now identified a generally thought to be the same as that are still significantly accreting large number of high-mass protostars. for low-mass stars, modern theories (e.g., Behrand & Maeder 2001). These span the range from cold (e.g., see reviews by Zinnecker & All theories agree that a high-mass pre-stellar cores found in IRDCs, to Yorke 2007 and McKee & Ostriker star begins its life as a “pre-stellar” or hot cores, and compact H II regions. 2007) suggest the possibility of “starless” core, which collapses to Important new samples have been two important differences. Firstly, form a deeply embedded, accreting found using the Spitzer GLIMPSE (3-8 although low-mass stars are thought protostar or “hot molecular core.” um) and MIPSGAL (24 um) surveys, to acquire their mass by accreting When fusion begins, the star enters the HOPS Survey (1.3 cm), and material solely from their parental

22 ATNF News, Issue 69, October 2010 various mm and submm continuum surveys. With these new surveys, we can begin to study the evolutionary sequence of high-mass protostellar evolution by finding large numbers of objects in each of these stages. The major goal of the MALT 90 GHz Survey is to characterise high-mass star-forming cores and to study their physical and chemical evolution. The Spitzer Galactic surveys GLIMPSE and MIPSGAL have shown that IRDCs host the massive dense cores, which are making the transition from cold, quiescent pre-stellar cores to active hot cores and H II regions. Moreover, submm Galactic surveys such as the Apex Telescope Large Area Survey of the Galaxy (ATLASGAL) are now identifying huge numbers (~10,000) of dense molecular cores associated with star formation. We aim to capitalise on these advances in high-mass star formation by conducting a large, new molecular line survey of dense cores with the Mopra radio telescope.

Figure 1: Spitzer GLIMPSE and MIPSGAL images toward three examples of high- mass star forming cores (contours are of the 1.2 millimetre continuum dust emission): Pre-stellar (top), Protostellar (middle), and a HII region (right). The primary goal of the MALT 90 GHz Survey is to characterise star-forming cores and to study their physical and chemical evolution.

23 The 90 GHz molecular lines undertaken. MALT90 will be is done remotely by astronomers are especially interesting probes valuable not only in its own right, from other locations. In the future, because they require high-densities but also as an important finding this “user-operator” mode will for excitation. Because the cores chart to identify key ALMA targets. continue to be used for the Compact are much denser than typical CO- Array, and the Parkes and Mopra MALT90 has just completed its first emitting molecular clouds, 90 GHz telescopes. However, an increasing observing season, spanning more emission will arise only from the amount of observing will be carried than 860 hours since mid-July. The dense, star-forming cores. Moreover, out from the SOC, particularly season was extremely successful; since these lines span a large range for observing teams that require we obtained maps toward ~ 520 of excitation energies and critical expert support. The user-operator cores, which spanned the complete densities, they indicate distinct mode will not be used for ASKAP. range in the proposed evolutionary physical conditions and distinct Instead, ASKAP observations will be sequence. We are in the process of stages of chemical evolution. Mopra’s taken remotely from the SOC in a completing the final data reduction unique broad-band capability queue-based model. Astronomers before the data are released allows us to image 16 of these will access their data and data to the team. We expect a data molecular lines simultaneously. Finally, products through archive facilities. release to the wider community because many chemical species early next year. Already the team The full SOC will be developed are observable, for the first time has identified over 12 key science using a staged approach. As a first a large systematic survey of core projects, which aim to characterise step, in the 2010 April semester, chemistry can be conducted. the high-mass star-forming cores. we have carried out a pilot study Due to the small solid angle The MALT90 team consists of to try out “SOC-mode” observing occupied by star-forming cores over 50 astronomers worldwide. where the observers and the emitting strongly at 90 GHz, a blind, astronomers who provide observing fully sampled survey of a significant MALT90 and the support are based in Sydney. The portion of the Galactic plane is SOC Pilot project MALT90 project has been used as a impractical. Thus, to survey significant demonstration project for this study. numbers of star-forming cores An important part of the planning The goals of this pilot study are to: efficiently, we must choose selected for future ATNF Operations, that targets. Because submm emission will include the operations of ASKAP, • Trial SOC-mode observing traces cores in all evolutionary now under construction in Western from Marsfield, initially for stages, we are using the ATLASGAL Australia, is the establishment observations of Mopra Large point source catalogue as our basic of a Science Operations Surveys from Sydney. target list, supplemented by core Centre (SOC) in Sydney. • Establish and implement the categorisation based on GLIMPSE At present, most observations technical and user requirements and MIPSGAL images. We aim to needed to do this. image roughly 1,000 cores each in are carried out in a mode where the pre-stellar, protostellar, and H astronomers are present for and • Gain experience of Sydney-based II region phases. MALT90 will be control their own observations, observing, and working with the largest systematic molecular at either the Parkes or Narrabri science teams on Large Projects. line survey of dense cores ever site. Additionally, some observing

24 ATNF News, Issue 69, October 2010 • Extend the ATNF data archives line data processing of the feedback shows that the science (ATOA) to provide a search Mopra Large Survey data. team found it straightforward facility and access to the to observe from Sydney, and • A high-quality point-point video processed data cubes that will appreciated the high level of expert link has been installed at Narrabri result from the MALT90 survey. support they received. The observing and Marsfield to facilitate the systems were robust, with very few To establish and implement the interactions between staff and technical problems and the video technical and support requirements observers located at the two sites. connection helped facilitate working for this pilot study, in May 2010 a • Improvements have been made between the two sites. The level of “Mopra Large Surveys Working to the Marsfield Lodge services to comfort provided by the Visitors Group” was established. This group provide darker bedrooms and hot Services Group, and the hot meals worked in consultation with the meals after hours and at weekends. were also appreciated. There has MALT90 project team leader (Jim Access to a small kitchen near the been some impact on local staff Jackson) and other members of observing areas was also provided. who worked long hours, some staff the science team. Suggestions and visitors raised concerns over received from Australia Telescope • Some improvements have been the use of the video system. These Users Committee (ATUC) and made to the on-line observing matters will be carefully considered input from focus groups were software tools, including the use over the next few months as we also included in this planning. of an on-line observing log. Other improvements that will include learn from the recent experience. The MALT90 project was allocated batch processing of schedule files Over the next year, CASS will ~860 hours of observing time and automated telescope pointing continue to provide support for between mid July and late September. are planned but not yet completed. SOC-mode observing, with a focus The science team initially spent three on Mopra Large Surveys. Further weeks at Narrabri to ensure that A critical element of SOC observing information on SOC observing their observing and data reduction is to provide local support to for the 2011 April semester will strategies were working effectively. the observers in Marsfield. For be provided to the community Almost all of the observing from the MALT90 project, support with the next Announcement of early August was then carried astronomers were available on the Opportunity in mid-November 2010. out from Sydney. To support this, site at all times during the scheduled a number of new facilities were observations. The support roster was introduced. These included: set up with a default of two 3.5 day blocks per week. Accommodation • Dedicated access to remote and travel costs were provided observing computing facilities in for support astronomers who Marsfield. This area is used for travelled to the site and gave remote observations with the at least seven days support. Compact Array and/or Mopra. In the next few weeks a review will • A powerful new server and be held to consider the “lessons dedicated disk space was learnt” from this pilot study. Initial provided to allow for fast off-

25 Discovery of a Radio–loud X-ray–quiescent Magnetar in the High Time Resolution Universe Survey M J Keith, L Levin, M Bailes, S Johnston, M Kramer, A Possenti, A Jameson, W van Straten, S D Bates, N D R Bhat, M Burgay, S Burke- Spolaor, N D’Amico, S Milia, B W Stappers

Magnetars are neutron stars hardware available. Of particular events. This is because as pulses travel with some of the strongest merit is the “20-cm Multibeam” to the Earth, the low frequencies receiver, which packs 13 feeds are delayed with respect to the magnetic fields in the known into the focus of the antenna. This high frequencies by interstellar universe, typically above 1014 enables 13 patches of sky to be dispersion. The result is that the surveyed in a single observation, pulse is smeared out over the finite Gauss. These stars are usually allowing for deep surveys of large bandwidth of our instrument. This observed through highly energetic areas of sky, such as the Parkes effect can be negated by recording X-ray and gamma-ray outbursts, Multibeam Pulsar Survey (PMPS; the observation in sufficiently Manchester et al. 2001). This survey narrow frequency channels that can thought to be powered by the ran for six years beginning in 1997 then be corrected for the delay. and discovered over 700 pulsars, release of energy trapped in the In order to detect faster objects more than doubling the known structure of the magnetic field located deeper in the disk of the population of pulsars at the time. itself. In recent years we have Galaxy, we have designed and built Even though the survey was highly a new an all-digital multi-beam detected radio pulses, similar to successful, the finite width of the filterbank system known as BPSR. those from pulsars, associated analogue filters in the recording This system provides ten times the system limited the ability to detect frequency resolution of the old with these energetic outbursts the fastest pulsars and transient system, and in the typical observing in two magnetars. Now, for the first time, we have discovered a magnetar by its radio emission alone. This is most intriguing, especially as the standard pulsar emission theories do not allow for radio emission in the presence of such extreme magnetic fields.

The High Time Resolution Universe survey The Parkes radio telescope has a long and impressive record of pulsar discoveries, having discovered almost half of all known radio pulsars. This success can be put down to a combination of the location of the antenna (the Galactic Centre passes directly overhead) and the Figure 1: Contours of constant smearing time for the analogue excellent receivers and backend (dotted) and BPSR digital (solid) filterbank systems. Contours are 0.5, 1,5 and 10 ms. The Galactic centre is marked “GC”

26 ATNF News, Issue 69, October 2010 Figure 2: Light curve and profile variations for PSR J1622−4950. The top plot shows the temporal variation of flux density at 1.4 GHz. Archival timing data collected within the framework of the Parkes Multibeam Survey ends just before MJD = 54000, and the discovery of PSR J1622−4950 by the HTRU pulsar survey was made on MJD = 54939. The asterisks show the detections (with errors smaller than the size of the points), and the circles indicate observations during which PSR J1622−4950 was not detected (down to a limiting flux density of 1.2 mJy). The purple error bar indicates the observation centered at 6.3 GHz from the Methanol Multibeam survey that detected PSR J1622−4950. When converted into a 1.4 GHz flux density, the large error is dominated by the uncertainty in the spectral index; the top value of the bar corresponds to a flat radio spectrum, and the bottom value is derived from our best estimate of the spectral index. The bottom plots show three different pulse profiles from three consecutive observations, taken on 30 June 2009, 16 July 2009, and 23 July 2009. mode records samples every 64 remainder of the sky. The survey was detected with a signal-to-noise microseconds. With this new digital is expected to run for four more ratio of 250, by far the brightest pulsar system we can see through much years, and full details of the survey discovered in the HTRU survey. Follow more of the interstellar medium. are given in Keith et al. (2010). up observations indicated that the Figure 1 shows contours of constant pulsar was highly variable, both in the In addition to discovering many smearing timescale for the analogue shape of and the intensity of the pulse. millisecond pulsars, the survey is hardware (dotted lines) and the turning up many longer period The area of sky containing PSR BPSR system (solid lines). This makes pulsars. Some are found because J1622−4950 was previously covered it clear that for the fastest pulsars, they fell in regions of low sensitivity by the PMPS but, somewhat the BPSR system can see more than of earlier surveys, for example, surprisingly given its large apparent twice as far into the Galactic plane. between adjacent observations. flux density and DM, the pulsar was To take advantage of these new In the case of PSR J1622−4950, not detected in these data. However, advances we have embarked on however it was clear that something that survey did find two other radio the High Time Resolution Universe very different was happening. pulsars in close proximity to PSR survey for pulsars and fast transients. J1622−4950 and monitored them This survey covers the entire The radio magnetar for a number of years, namely PSRs sky, with northern declinations J1623−4949 and J1622–4944 at being covered by a twin survey at PSR J1622–4950 an angular separation of 11′ and 7′, Effelsberg. For the Parkes portion PSR J1622−4950 was discovered in respectively. These archival data were of the survey the mean sensitivity April of 2009, with a spin period of reprocessed using the period and DM is ~0.10 mJy for Galactic latitudes 4.3 s, and a dispersion measure of of PSR J1622−4950. As can be seen in between ±3.5°, ~0.25 mJy for those 830 cm-3 pc (Levin et al. 2010). In Figure 2, the pulsar was not detected between ±15° and 0.32 mJy for the the survey observation the pulsar until data from June 1999. It was

27 Figure 3: Top panel shows a 5.5 GHz image made with the ATCA. Bottom panel shows Chandra X-ray image of the same region of sky. Detailed analysis indicates that PSR J1622-4950 is the bright point source visible in both images.

28 ATNF News, Issue 69, October 2010 again detected in 11 observations and therefore any remnant from impossible) for pulsars but rather taken between October of 2000 the supernova event that formed low for expanding SNRs. Therefore and July of 2002, after which the it would likely still be visible. To we feel that this association, pulsar was detected only in the search for such a remnant we though possible, is unlikely. 14 subsequent observations. In performed 12-hour tracks of the This discovery of a highly polarised, April of 2007 the area of sky was source with the Australia Telescope radio-luminous magnetar is the covered by the 6.7 GHz pulsar Compact Array, in each of the first major result from the HTRU survey at Parkes, where it was again EW352 and 750B configurations. survey. The pulsar shares many of detectable (though it was missed The observations utilised the the properties of the two known in the original analysis as it was simultaneous 2-GHz bands centred radio magnetars, however PSR confused with interference signals). at 5.5 and 9 GHz made available J1622−4950 indicates that bright by the Compact Array Broadband Figure 2 demonstrates this flux radio emission can be present even Backend. The image showed a variability, and indicates that there when a magnetar displays an X-ray highly-polarised flat-spectrum point have been at least two quiescent luminosity typical of a quiescent state. source co-incident with both an periods in the radio emission. Also We finally note that the extreme X-ray source. Additional Compact shown are samples of pulse profiles variability in the flux density of PSR Array observations confirmed that taken in adjacent observations, J1622−4950 also demonstrates the this source matched the magnetar’s indicating the considerable change advantages of surveying the radio sky flux density at 1.4 GHz and was in the integrated pulse profile at regular intervals with even modest therefore the only suitable candidate. on fairly short time-scales. sensitivity. This highlights the potential The image also shows a tantalising of the upcoming radio facilities like The radio polarisation of the ring of nebulous emission. This ring the LOFAR, ASKAP, or SKA which magnetar is also variable, however lacks an infrared counterpart and promise to characterise the dynamic it is often almost completely linearly appears to be non-thermal, whereas radio sky at an unprecedented level. polarised. The polarisation fraction the slightly extended radio source is typically greater at 3.1 GHz than in the south of the ring is clearly at 1.4 GHz, similar to young radio References thermal in nature. If we assume a pulsars. It also occasionaly displays distance of ∼9 kpc to the magnetar Keith M. J. et al., 2010, MNRAS, significant circular polarisation, and further assume it was born in in press (arXive:1006.5744) particularly at the leading edge the centre of the ring, the magnetar of the pulse. Faraday rotation has Levin L. et al., 2010, ApJ would need a velocity of ∼1300 been detected with a rotation Letters, 721 L33 -2 km/s to reach its current location measure of −1484 ± 1 rad m . Manchester R. N. et al., 2001, whereas the ring itself would have MNRAS, 328, 17 The characteristic spin-down age a lower expansion velocity. Such of the magnetar is only 4000 years, a velocity is high (though not

29 First Science from the ASKAP and Warkworth Antennas: on the Path to “Maximum Discovery” Professor Steven Tingay, International Centre for Radio Astronomy Research – Curtin University On behalf of the Australian and New Zealand VLBI teams

One of the ten ASKAP Survey Science Projects is aimed at high consequence of success with goal 1 angular resolution observations using CSIRO’s Australian Square and preparatory work toward goal 2. Kilometre Array Pathfinder (ASKAP) telescope as part of Australian Over the course of a three week period in late April and early May and international very long baseline interferometry (VLBI) arrays. This 2010, successful VLBI observations Survey Science Project (SSP) pursues activities in two main areas: were performed using the first of 1) achieving early science results from ASKAP as an element of the the ASKAP antennas to be installed at the Murchison Radio-astronomy Australian VLBI array, from the point at which a single ASKAP antenna Observatory (MRO), along with is available, through the use of custom RF and digital systems; a new 12-m antenna installed at Warkworth on New Zealand’s 2) produce an operational VLBI system for the mature ASKAP that is fully North Island. Figure 1 shows integrated with the final versions of the ASKAP RF and digital systems. the distribution of the antennas used in these observations. Goal 1 is a near term goal and will proceed at the pace at which The observations used a custom RF one that has been primarily the the various ASKAP sub-systems system built by engineers at CSIRO focus of work over the year since mature into their final forms. Astronomy and Space Science and the SSP was approved. Work for We report here on the first science a custom digital backend built at goal 2 has a longer-term focus and results to emerge from ASKAP, a the International Centre for Radio

Figure 1: Geographic distribution of antennas used for VLBI observations in April/May 2010. ASKAP, ATCA, Mopra and Parkes are operated by CASS. Hobart is operated by The .

30 ATNF News, Issue 69, October 2010 Astronomy Research (ICRAR), Curtin University, by PhD candidate Mr Bruce Stansby. Identical systems were installed at ASKAP and Warkworth. Regular systems were used at the rest of the LBA stations. The data recorded at each telescope were transferred to ICRAR and correlated using the DiFX software correlator. High quality data were obtained for a range of astronomical objects: 3C 273; PKS 1934-638; Centaurus A; and a selection of geodetic calibration sources. The data yielded images with a resolution of approximately 5 mas at 1.4 GHz (dual-polarisation 64 MHz bandwidth). Shown below in Figure 2 is the image of Centaurus A that accompanied a press release announcing the success of the experiment — Aussies and Kiwis forge a cosmic link: http://www.csiro.au/news/Aussies-and- Kiwis-forge-a-cosmic-connection.html.

Figure 2: The structure of Centaurus A, from the largest scales observed with the ATCA, to the smallest scales probed by new VLBI observations with a maximum baseline of 5500 km, from Western Australia to New Zealand. Image credit – Whole galaxy: I Feain, T Cornwell & R Ekers (CSIRO/ATNF); ATCA northern middle lobe pointing courtesy R Morganti (ASTRON); Parkes data courtesy N Junkes (MPIfR). Inner radio lobes: NRAO / AUI / NSF. Core: S Tingay (ICRAR) / ICRAR, CSIRO and AUT NB: For reference, please see the colour image published on the back page of this newsletter.

31 Figure 3: Image of the double component structure of PKS 1934-638 at 1.4 GHz, part of a paper submitted for publication to The Astronomical Journal.

The Centaurus A data were self-absorption. Previously this range of observations during the featured at the 2010 International frequency dependant structure remaining ASKAP development and SKA Forum, held recently in Assen, has been incorrectly identified as will transition to the full system as The Netherlands. In his address structural evolution over a 40 year ASKAP matures. Both ASKAP and to the forum, Professor Brian period. The new observations show Warkworth are now included in the Boyle presented the results as a the way to the correct conclusion Australian Long Baseline Array call step toward the demonstration that the structure is frequency for proposals and are thus available of the “Maximum Discovery” dependant due to absorption effects to proposers who require high possible for an SKA located in and very stable with time. Figure 3 angular resolution at 1.4 GHz. Australia – New Zealand. shows the image of PKS 1934-638 The SSP team is also working with obtained from the observations. Another significant result arose Indian colleagues to establish the from observations of PKS 1934- The PKS 1934-638 results have been Giant Metrewave Radio Telescope 638, an archetypal GHz-Peaked submitted for publication in The (GMRT) for VLBI observations, spectrum radio galaxy. Because Astronomical Journal (Tzioumis et al. aiming to extend the reach of VLBI of the high angular resolution 2010, submitted) and document the in the region, adding to regular obtained at low frequency, these first science to be obtained from the VLBI partners in South Africa, observations have revealed for the ASKAP and Warkworth antennas. Japan, China and the USA. first time a frequency-dependant The VLBI capability established angular separation between the two in the first year of this SSP will compact components in this radio be retained and deployed for a galaxy, likely due to synchrotron

32 ATNF News, Issue 69, October 2010 Bonsai-ed Radio Galaxy Gives Clue to Jet Energies Robert Soria (University of Sydney)

A new Australia Telescope Compact Array (ATCA) study of a microquasar in the galaxy NGC 7793 strongly suggests that the true power of black hole jets is a thousand times larger than the power estimated only from their observed radio emission.

The ATCA observations of this object, S26, complement optical and X-ray observations carried out with Chandra and European Southern Observatory’s Very Large Telescope, published in Nature earlier this year. The radio observations have made it clear that S26 is a near-perfect analogue for a radio galaxy. The new data show that S26 has exactly the structure of a radio galaxy, in a way never seen before in microquasars derived from stellar-mass black holes. Measuring the power of black hole jets, and therefore their heating effect, is usually very difficult. Figure 1: The ATCA 3-cm map with the position of the X-ray core (black hole) and Powerful jets are characterised by hot spots highlighted. strong radio emission from their lobes: large, expanding blobs of end of the pair of jets, plus a energetic electrons, moving at close is given to relativistic electrons supersonically-expanding bubble of to the speed of light, at the end (emitting in the radio bands). heated gas. We can directly measure of the jet. But such radio-emitting the energy in both the lobes and We find that about a thousandth (or, electrons contain only a small bubble: because we have good at most, a few parts in a thousand) of fraction of the total jet energy. The observations in three wavebands, the jet power is given to the radio- rest of the energy is generally not we can determine what fraction emitting electrons in the lobes, while detected: only in rare cases can of the initial jet power (kinetic the rest is used to blow the large it be indirectly estimated from its energy of the particles in the jet) is bubble of heated gas, 300 pc across. effect on the surrounding gas. converted to thermal energy of the This result confirms models positing S26 helps shed light on the warm gas (T ~ 10,000 K, emitting that the true power of black hole energetics of these systems. The optical lines); what fraction is given jets is a thousand times larger than radio, optical and X-ray observations to the hot gas (T > 106 K, emitting the power estimated only from its reveal bright radio lobes at the in the X-rays); and what fraction observed radio emission. It suggests

33 National Facility Operations Douglas Bock, Jessica Chapman, Phil Edwards, Erik Lensson, Mark Bowen (CASS)

that black hole jets can be both more Remote Operations (CSIRO) and Michael Burton powerful and more efficient than (University of New South Wales). Several efforts are underway to previously thought, and therefore prepare for remote operation of that their cosmic heating effect can all the telescopes. A pilot Science Managing be stronger. And it gives us a way Operations Centre project was to estimate the true jet power in Radiofrequency conducted over the winter, with other black holes (including those in Interference (RFI) most observations of the MALT- quasars and radio galaxies) where 90 Mopra survey taken from at National Facility only the radio lobes may be directly Marsfield. The results will be used Observatories observable, not the bubble of hot gas. to inform the design of the Science The increasing demand for The significantly improved continuum Operations Centre that will commercial wireless communications sensitivity of the Compact Array eventually serve users of all ATNF and government services represents Broadband Backend (CABB) let instruments including ASKAP. an ongoing challenge for the us trace the radio morphology at At Parkes, projects to improve national facility observatories sensitivity levels of less than 10 the reliability of power and drive and radioastronomy facilities microJanskys/beam, in three days control, and to automate frontend worldwide. About forty CSIRO of observations. Before CABB this and backend re-configurations are Astronomy and Space Science staff would have taken 15 days. As this at the installation phase. The impact met at Marsfield on 1 September is much longer than the typical of this work on observing time this 2010, to share experiences and ATCA time allocation, it’s likely semester is described below. In practical approaches to dealing with that, without being able to use addition, a new UPS for the Marsfield increasingly complex radiofrequency CABB, we would not have been PABX and UPS batteries for Parkes interference (RFI) and spectrum use allocated the time to do this work and for the ATCA antennas will matters relevant to running national and hence would not have been be installed over the summer. facility observatories. Workshop able to map the fine structure of participants included staff from ATNF the radio lobes and cocoon. Water Vapor Engineering and Science Operations, Astrophysics, Technologies for Radio References Radiometers Astronomy and ASKAP, as well as a Pakull, Manfred W.; Soria, Roberto; Water Vapour Radiometers for all number of staff from the Motch, Christian. A 300- Compact Array antennas have been Deep Space Communications parsec-long jet-inflated bubble delivered by Melbourne company Complex at Tidbinbilla. The in- around a powerful microquasar ASTROWAVE. They have been house event concentrated on in the galaxy NGC 7793. installed on the antennas and are practical operational objectives: Nature, 466, 209 (2010) undergoing calibration. Pleasingly, 1. Increasing staff awareness a comparison with the 12 mm Soria, Roberto; Pakull, Manfred as to the different kinds of “science” data shows that they are W; Broderick, Jess W; Corbel, RFI related expert skills and tracking phase changes as required. Stephane; Motch, Christian. experience that already exists Development of algorithms to Radio lobes and X-ray hot across the observatories correct astronomical data for spots in the microquasar S26. and CSIRO Astronomy and phase effects continues through MNRAS, in press (2010) Space Science generally; the efforts of Balt Indermuehle

34 ATNF News, Issue 69, October 2010 2. sharing knowledge about hardware • new and improved RFI Projects are now required to and software tools useful for related databases and analysis provide web pages on their projects. operational RFI management; software tools to support Please include information on the staff and observers at existing spectral coverage, spatial coverage, 3. improving cross-site and new observatories; and sensitivity of the survey collaboration on RFI detection, observations. For ongoing surveys, identification and tracking; • the creation of a new online regular updates should be provided “RFI Report”, as an adjunct to to indicate the current survey 4. considering strategies for the existing generic observatory transitioning the National Facility status, including the areas of the “Fault Report”, for streamlining survey that have been completed. Operations to ASKAP and beyond. the reporting and tracking of For further information see Many topical issues were outlined RFI events, including data mining and discussed, including relevant of related ATNF archives; www.atnf.csiro.au/observers/ international RFI threshold standards apply/large_projects.html • options for improved observatory in Recommendation ITU-R RA.769 RFI monitoring, independent of In a number of cases, proposers (Tasso Tzioumis), international the actual observing instruments, re-submitted previous proposals vs national regulation (Carol including facilities for time-series but used a new proposal code: Wilson), approaches to site related analysis, automated source if a proposal is resubmitted electromagnetic compatibility (Mal identification and reporting. (regardless of whether or not it Smith), RFI identification, & tracking has been allocated time in previous (John Reynolds), tools for RFI semesters) then please use the hunting & tracking (Peter Mirtschin), October 2010 Time same proposal identification mitigation (Mike Kesteven), dealing Assignment code as allocated previously. with other spectrum users and current & future challenges from The Time Assignment Committee geostationary and non-geostationary met at Marsfield on 22 – 23 July Notes on the satellite RFI sources, airborne and to consider proposals for the 2010 Compact Array space radars (Erik Lensson). Staff October semester (2010OCTS) The 2010OCTS will commence also heard about the development A total of 163 proposals were with the “standard” CABB 1 MHz of the Murchison Radio Quiet Zone reviewed, 103 for the Compact continuum mode available, and (Michelle Storey) and related RFI Array, 26 for Parkes, 14 for with up to four zoom bands per IF level measurements (Ron Beresford). Mopra, seven for Tidbinbilla and 13 for the Long Baseline Array. available in the 1M – 0.5k mode. It The day concluded with an open is hoped that a problem affecting “Q&A” Panel Session (Phil Edwards), The Time Assignment Committee one of the four zoom bands with further discussions about the was pleased to see that the (specifically all baselines to CA04 in key issues identified during the revised guidelines for Large one polarisation) will be resolved Projects (requiring more than 400 course of the day. These issues early in the October semester. will be further considered as part hours for the expected lifetime The 64-MHz CABB mode was of future planning for national of the program) were observed first used in late September. Initially, facility operations, including: by proposers. Please note that Proposers allocated time for Large the 64-MHz mode has a single 64-

35 Publications List

Publication lists for papers which include ATNF data or CASS authors are available on the Web at www.atnf. csiro.au/research/publications. Please email any updates or corrections to MHz band in each IF, with 2048 new receiver. CA01 will be without this list to channels across the band. (Thus, an LS receiver until December. [email protected] or Julie. if the 64-MHz mode is selected [email protected]. for an IF, the total bandwidth in Notes on Parkes This list includes published that IF will be 64 MHz, not 2 GHz.) refereed papers compiled since For continuum plus spectral line The 2010OCTS schedule for the April 2010 Newsletter. studies, having one IF set with the Parkes has two shutdown periods. Papers which include CASS staff 64-MHz mode and the other with The first, from 5 – 19 October, is are indicated by an asterisk. the standard 2048 1-MHz-wide primarily for commissioning of the channels is possible. For spectral new RF switching matrix. This will *ABBOTT, B. P., ... HOBBS, G.B., ... line studies, 64-MHz is available in enable “recabling” between standard observing set-ups to be carried out MANCHESTER, R.N. et al.”Searches for both IFs — with separations up to gravitational waves from known pulsars with 7 GHz between the two 64 MHz quickly and automatically. The second, science run 5 LIGO data “. ApJ,713,671- channels possible. As only two 64 from 28 February – 24 March, is 685(2010). MHz zoom bands will be available primarily for a major overhaul of the *ABDO, A.A., ... , HOBBS, G., ... , JOHNSTON, at the beginning of the semester, telescope Manual Control Panel. The S., ... , MANCHESTER, R.N. et al.”Discovery several highly ranked proposals H-OH receiver has recently been of pulsed g-rays from PSR J0034-0534 with the Fermi Large Area Telescope: a case for for observations of multiple upgraded and fitted with a new feed, which will increase the bandwidth co-located radio and g-ray emission regions”. lines with 64 MHz zoom bands ApJ,712,957-963(2010). available. Testing of this receiver on have not been scheduled: these *ABDO, A.A., ... HOBBS, G., ... JOHNSTON, S., should be resubmitted at the 15 the telescope is also planned for ... MANCHESTER, R.N. et al.”Detection of the December deadline (using the same this second shutdown period. energetic pulsar PSR B1509Ð58 and its pulsar proposal code) for consideration Parkes observers have at times this wind nebula MSH 15Ð52 using the Fermi- Large Area Telescope”. ApJ,714,927-936(2010). in the 2011 April Semester. year been adversely affected by *ABDO, A.A., ... HOBBS, G., ... MANCHESTER, During the 2010OCTS it is expected strong Radio-Frequency Interference R.N. et al.”The Vela pulsar: results from the first that progress will be made toward (RFI). To help with efforts to mitigate year of Fermi LAT observations”. ApJ,713,154- expanding the number of zoom against RFI and to characterise 165(2010). bands per IF in the 1-MHz CABB the various sources, observers are *ABDO, A.A., ... JOHNSTON, S. et al.”Fermi mode, and that pulsar binning asked to record as accurately as Large Area Telescope observations of the Vela-X pulsar wind nebula “. ApJ,713,146- and higher time resolution modes possible the onset, duration, and 153(2010). will become available. It is also spectral characteristics of any RFI experienced during observing. *ABDO, A.A. ..., JOHNSTON, S. ..., hoped that the 64-MHz mode MANCHESTER, R.N., ..., WELTEVREDE, P. will be expanded to provide et al.”The first Fermi Large Area Telescope more 64-MHz bands per IF. catalog of gamma-ray pulsars”. ApJS,187,460- 494(2010). The weeks starting on 18 October *ABDO, A.A. ..., WELTEVREDE, P. et and 6 December will be used for al.”Observations of the Large Magellanic Cloud maintenance towards the next stages with Fermi “. A&A,512,A7(2010). of the 20cm/13cm (L/S) receiver *ALVES, M.I.R., DAVIES, R.D., , upgrade. By the start of the semester, C., DAVIS, R.J., AULD, R.R., CALABRETTA, antennas CA02, CA03, CA04, and M. & STAVELEY-SMITH, L.”Diffuse radio CA06 had been outfitted with the recombination line emission on the Galactic plane between 1=36o and 440”. new 1.1 – 3.0 GHz receivers. By MNRAS,405,1654-1669(2010). the time you receive this newsletter, *BOQUIEN, M. ..., KORIBALSKI, B. et al.”100 CA05 should be outfitted with the mm and 160 mm emission as resolved

36 ATNF News, Issue 69, October 2010 star-formation rate estimators in M 33 *DESAI, K.M., CHU, Y.H., GRUENDL, R.A., *HENNING, P.A., SPRINGOB, C.M., (HERM33ES)”. A&A,518,L70(2010). DLUGER, W., KATZ, M., WONG, T., CHEN, MINCHIN, R.F., MOMJIAN, E., CATINELLA, *BREEN, S.L., CASWELL, J.L., ELLINGSEN, S.P. C.H.R., LOONEY, L.W., HUGHES, A. et B., McINTYRE, T., DAY, F., MULLER, E., & PHILLIPS, C.J.”Water masers accompanying al.”Supernova remnants and star formation KORIBALSKI, B. et al.”The Arecibo L-band OH and methanol masers in star formation in the Large Magellanic Cloud”. AJ,140,584- Feed Array Zone of Avoidance survey. I. regions”. MNRAS,406,1487-1532(2010). 594(2010). Precursor observations through the inner and outer Galaxy”. AJ,139,2130-2147(2010). *CARRETTI, E., HAVERKORN, M., *DOUGHERTY, S.M., CLARK, J.S., McCONNELL, D., BERNARDI, G., McCLURE- NEGUERUELA, I., JOHNSTON, T. & *HILL, D.T., DRIVER, S.P., CAMERON, E., GRIFFITHS, N.M, CORTIGLIONI, S. & CHAPMAN, J.M.”Radio emission from the CROSS, N., LISKE, J. & ROBOTHAM, A.”The POPPI, S.”The Parkes Galactic Meridian massive stars in the galactic super star cluster ugrizYJHK luminosity distributions and Survey: observations and CMB Westerlund 1”. A&A,511,A58(2010). densities from the combined MGC, SDSS and foreground analysis”. MNRAS,405,1670- *ELLINGSEN, S.P., BREEN, S.L., CASWELL, J.L., UKIDSS LAS data sets”. MNRAS,404,1215- 1689(2010). QUINN, L.J. & FULLER, G.A.”Masers associated 1230(2010). *CASWELL, J.L., FULLER, G.A., GREEN, with high-mass star formation regions in the HILL, T., LONGMORE, S.N., PINTE, C., J.A., AVISON, A., BREEN, S.L., BROOKS, K.J., Large Magellanic Cloud”. MNRAS,404,779- CUNNINGHAM, M.R., BURTON, M.G. 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38 ATNF News, Issue 69, October 2010 Right: One of CSIRO’s new ASKAP antennas being assembled at the Murchison Radio-astronomy Observatory, October 2010. Credit: Ross Forsyth

Below: An elevated view of three of CSIRO’s new ASKAP antennas at the Murchison Radio-astronomy Observatory, October 2010. Credit: Ross Forsyth

39 For further information:

CSIRO Astronomy & Space Science Email enquiries: [email protected], Email newsletter: [email protected] Web central: www.atnf.csiro.au Web newsletter: www.atnf.csiro.au/news/ newsletter, Web outreach: outreach.atnf.csiro.au

The structure of Centaurus A, from the largest scales observed with the ATCA, to the smallest scales probed by new VLBI observations with a maximum baseline of 5500 km, from Western Australia to New Zealand. See page 31

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