Pair NGC 1512 / NGC 1510

ATNF News Issue No. 67, October 2009 ISSN 1323-6326 Questacon "astronaut" street performer and visitors at the Parkes Open Days 2009. Credit: Shaun Amy, CSIRO.

Cover page image Cover Figure: Multi-wavelength color-composite image of the galaxy pair NGC 1512/1510 obtained using the Digitised Sky Survey R-band image (red), the Telescope Compact Array HI distribution (green) and the Galaxy Evolution Explorer NUV -band image (blue). The Spitzer 24µm image was overlaid just in the center of the two . We note that in the outer disk the UV emission traces the regions of highest HI column density. See article (page 28) for more information.

2 ATNF News, Issue 67, October 2009 Contents

From the Director ...... 4 CSIRO Medal Winners ...... 5 CSIRO Astronomy and Space Science Unit Formed ...... 6 ATNF Distinguished Visitors Program ...... 6 ATNF Graduate Student Program ...... 7 Obituary — John Masterson ...... 8 Australian Pathfi nder (ASKAP) ...... 12 ASKAP Survey Science Projects enter Design Study Phase ...... 16 2009 CSIRO Astronomy School ...... 19 CSIRO Parkes Open Days ...... 20 CSIRO ATNF says Farewell to Pat Sykes ...... 22 The Nearest Powerful NGC612: First Science Results with the CABB C/X-band ...... 25 Gas Dynamics and Formation in the Galaxy Pair NGC 1512/1510 ...... 28 Exploring the Radio Bimodality of QSOs with CABB ...... 32 National Facility Operations ...... 36 Time Assignment Information ...... 37 Changes to the ATNF Time Assignment Committee ...... 38 ATNF Publications List ...... 39 Education and Outreach ...... 42

Editorial

Welcome to the October 2009 will reside, and we acknowledge Science Projects that have now edition of the ATNF News. ATNF’s own Warwick Wilson entered the Design Study Phase. who was recently awarded In this issue we feature a number Finally, we feature the obituary of the CSIRO Medal for Lifetime of articles, with several referencing John Masterson who died on 9 April Achievement for his inspirational CSIRO’s new Australia Telescope 2009. John was an esteemed and contributions to . Compact Array Broadband highly respected photographer within Backend upgrade (or CABB as it is We also provide a review of our the CSIRO Division of Radiophysics popularly known). This includes an extremely successful Parkes Open for over 40 years. He leaves article by Elizabeth Mahoney and Days which attracted record behind a magnifi cent photographic collaborators that employs CABB numbers, we report on the fi rst archive that records the events, to explore the radio bimodality of CSIRO Radio Astronomy School facilities and people that make up QSOs while Bjorn Emonts and team at the Parkes , the history of CSIRO Radiophysics examine our nearest powerful radio we chat with Pat Sykes who has and the ATNF since the earliest galaxy NGC612 and provide fi rst recently retired from the ATNF days. He will be greatly missed. science results with the CABB C/X- following 36 years of service and Please note that if you would like band. Our fi nal science article looks we provide an update on recent to contribute to later editions at gas dynamics and star formation changes relevant to the Time of the ATNF News, you can in the galaxy pair NGC 1512/1510, Assignment Committee (TAC). contact the newsletter team. contributed by Ángel López- In addition to this, we present our We hope you enjoy the issue. Sánchez and Baerbel Koribalski. regular ASKAP and SKA activity In other news, we report on the update. We also feature a special Tony Crawshaw, Joanne Houldsworth creation of the CSIRO Astronomy article by ASKAP Project Scientists The ATNF Newsletter Production Team and Space Science business unit Ilana Feain and Simon Johnston in which current ATNF activities that looks at the ASKAP Survey (newsletter@atnf..au)

3 From the Director Lewis Ball ATNF Acting Director

This newsletter comes at a In July the Australia Telescope the contract with CETC54 to time of signifi cant achievement Steering Committee (ATSC) met design and build the 36 antennas at Marsfi eld and provided timely required, marks the substantive and change for the ATNF. advice to the CSIRO Executive — shift from planning to construction represented by Alex Zelinsky, and and rollout. Spare a thought for In recent months the Australian to myself in my role as the ATNF the CETC54 and ATNF staff who Commonwealth Government has Acting Director. After a period of will work through Christmas and announced A$80M of new funding some uncertainty regarding the New Year at the Murchison Radio- for the Pawsey Centre for SKA status of the Steering Committee, astronomy Observatory to install supercomputing in Perth, A$88M in Minister Carr reaffi rmed the Antenna 1 as soon as possible after funding for Australia’s membership role of the ATSC in providing its delivery at the end of November. of the Giant Magellan Telescope strategic advice to CSIRO on its program, and in announcements The science highlights in this radio astronomy activities, and associated with the budget in newsletter include early results appointed fi ve new members. May it identifi ed Space Science from the Compact Array’s new While CSIRO had already and Astronomy as one of three Broadband Backend system, the determined its intention to bring Super Science areas which are brainchild of Warwick Wilson the ATNF and NASA Operations its highest priorities. All of these and a tribute to the very talented together and create the new CASS announcements are tremendous team from ATNF’s Engineering Division, the Steering Committee news for Australian astronomy, group that have worked tirelessly provided very valuable advice and continue to reinforce this over recent years on this major regarding the need to continue as a decade of unprecedented project. It is fi tting that on the day to focus on the key challenges of political visibility and support that I am writing this Warwick delivering ASKAP, restructuring for astronomy in Australia. will receive a CSIRO Medal for Operations to position the ATNF Lifetime Achievement, a token CSIRO has recently announced that for the future, and maximising of recognition for his outstanding it will create a new business unit, to Australia’s role in the SKA, contributions to radio astronomy. be known as CSIRO Astronomy and including promoting its candidate Space Science (CASS) incorporating SKA site in . the ATNF and its NASA Operations A personal highlight over recent activities, the most signifi cant months has been the selection of which is the Deep of the 10 ASKAP Survey Science Space Communications Centre Projects that has been so ably led (CDSCC or Tidbinbilla). At the by the ASKAP Project Scientists, end of February 2010 the CDSCC Ilana Feain and Simon Johnston. The activities will sit entirely within engagement and commitment of CSIRO, concluding a very successful such a large international community period during which Raytheon in ASKAP science provides Australia have operated Tidbinbilla tremendous incentive for ATNF staff for CSIRO under a subcontracting to maintain their over the arrangement. CSIRO Astronomy next three years as we deliver this and Space Science will come into innovative world-class instrument. being on 1 December 2009, and The successful factory acceptance the process to recruit the person of the fi rst ASKAP antenna, a bare who will be Chief of CASS and 10 months after CSIRO signed ATNF Director is underway.

4 ATNF News, Issue 67, October 2009 CSIRO Medal Winners Tony Crawshaw (ATNF)

ATNF’s Senior Principal Research Engineer Dr Warwick Wilson was recently awarded the CSIRO Medal for Lifetime Achievement for his inspirational contributions to radio astronomy at a special CSIRO event in Melbourne. The Lifetime Achievement Medal is awarded to an individual who has a record of sustained and meritorious achievement over a prolonged period of CSIRO service. Warwick, recognised internationally for his outstanding contributions to the fi eld of radio astronomy, especially for his work in correlator development and in receiver systems design and development has been part of CSIRO for 27 years. His efforts have not only kept CSIRO at the forefront of the world’s Graeme Carrad, Warwick Wilson and Lewis Ball at the CSIRO radio astronomy instruments Awards event in Melbourne. Credit: Meg Rive, CSIRO but have also enhanced the capabilities of other observatories around the world. increasing the instrument’s communication systems in over bandwidth and sensitivity. 800 million products worldwide. Of particular note is the pioneering work that he undertook The legacy of Warwick’s work is Interestingly, the A4 chip which in the design and construction an assembly of advanced radio formed a key enabling step in of the “AT Correlator” an telescopes that are, on a daily the development of the WLAN innovative wideband correlator basis, generating new research technology was closely aligned for the Australia Telescope results by a large international with the development of the AT Compact Array (ATCA) that community of radio astronomers. correlator chip. Radiophysics staff collaborated on both projects received its fi rst signal in 1988. Also recognised at the Melbourne with both chips going through Warwick has also played a major event were the Wireless LAN a similar design process. John role in the development of the (WLAN) team who were O’Sullivan who led the original ATCA Compact Array Broadband awarded the major CSIRO prize, WLAN research team played Backend (CABB) upgrade. Ably the Chairman’s Medal. The team an important early role in the leading the CABB project team, received this medal for delivering initial conception of the Australia the recently installed upgrade has major technical benefi ts to Australia Telescope receiving systems within maintained ATCA’s position at and the world via wireless local the Division of Radiophysics. the forefront of radioastronomy area networking technology instrumentation by vastly now underpinning wireless

5 CSIRO Astronomy and Space Science Unit Formed Tony Crawshaw (ATNF)

CSIRO has recently announced the management. It is consistent of Tidbinbilla as a separate creation of the CSIRO Astronomy with CSIRO’s strategy of entity from its radio astronomy and Space Science (CASS) business consolidating its structural units activities. Opportunities for unit which will reside within the to achieve appropriate scale synergies between space science Information Sciences Group. and also mirrors the increasing activities and astronomy will be alignment of astronomy and explored in the longer term. This new Business Unit brings space science within Australia. together CSIRO’s radio astronomy Currently, a process is taking place capabilities (the ATNF) and other The new business unit will — to recruit the person who will lead space science activities (notably the together with the ICT Centre the ATNF and CASS with the open operation of the Canberra Deep — provide the staff responsible advertisement of the role of Chief Space Communications Complex for commissioning the Australian of CSIRO Astronomy and Space or Tidbinbilla), as well as CSIRO SKA Pathfinder, and will Science - ATNF Director. The Chief Space Sciences and Technology facilitate relationships with major of CASS will be responsible for both (formerly known as COSSA). partners in the space domain, radio astronomy activities and space including space agencies and science, will report to the Group The enlarged business unit will members of the Australian and Executive for Information Sciences, encompass radio astronomy, space international space industry. and will work closely with the science coordination, advanced CSIRO SKA Director, Brian Boyle. aerospace business development For the meantime CSIRO’s intention and national/international facilities is to maintain the operation

ATNF Distinguished Visitors Program Robert Braun (ATNF)

Over the past months we have Center for Astrophysics , USA), Ravi The Distinguished Visitors program enjoyed working visits from Leo Blitz Subrahmanyan (Raman Research remains a very productive means (University of Berkeley, Institute, India), Marcella Massardi of enabling collaborative research USA), Phil Kronberg (Los Alamos (International School for Advanced projects with local staff, adding National Laboratory / University Studies, Italy) and Joel Weisberg substantially to the vitality of the of Toronto), Alberto Sesana (Carleton College, USA). Current ATNF research environment. (Pennsylvania State University, USA), visitors include DJ Saikia (Tata Visits can be organised for Rick Jenet (University of Texas Institute of Fundamental Research, periods ranging from only a few Brownsville, USA), Martin Cohen India). Upcoming visitors we expect weeks up to one year. For more (University of California Berkeley, include Paula Benaglia (Instituto information please see www.atnf. USA), Jayanne English (University of Argentino de Radioastronomía), csiro.au/people/distinguished_visitors. Manitoba, Canada), Lordes Verdes- Jean-Luc Starck (CEA Saclay, France) html. Prospective visitors should Montenegro (Instituto de Astrofísica and Daniel Pfenniger (University contact the local staff member de Andalucía, Spain), Daniel Espada of Geneva, Switzerland). with the most similar interests. Fernandez (Harvard-Smithsonian

6 ATNF News, Issue 67, October 2009 ATNF Graduate Student Program Baerbel Koribalski (ATNF)

We welcome the following • Kitty Lo (University of Sydney) Dr Aaron Chippendale continues students into the ATNF co- — Star formation and magnetic to work at ATNF, Dr Nadia Lo fi elds in nearby galaxies with is now a postdoctoral fellow at supervision program: supervisors Dr Bryan Gaensler Saclay, France, Dr Joris Verbiest (University of Bonn) and Dr is a postdoctoral fellow at the • Jay Blanchard (University of Baerbel Koribalski (ATNF); University of West Virginia, USA, Tasmania) — Linking the Radio and Dr Katherine Newton- and Gamma-ray properties of • Vicky Lowe (University of NSW) McGee now works in Canberra. Blazars with supervisors Dr Jim — The environments of massive Lovell, Prof John Dickey (both star formation with supervisors Dr The following students recently University of Tasmania) and Maria Cunningham, Prof Michael Dr Phil Edwards (ATNF); Burton (both University of NSW) submitted their PhD Thesis: and Dr James Urquhart (ATNF). • Justin Bray (University of • Leith Godfrey (Australian Adelaide) — Ultrahigh-energy Congratulations to: National University) — Multi- neutrinos and their detection with wavelength Studies of X-ray the lunar Cherenkov technique with • Aaron Chippendale on the Bright Extragalactic Jets; supervisors Prof Ray Protheroe successful submission of his • Attila Popping (University of (University of Adelaide) and University of Sydney PhD Groningen) — Diffuse Neutral Prof Ron Ekers (ATNF); thesis on Detecting Cosmological in the Local Universe; Reionisation on Large Scales • Stefan Oslowsky (University of through the 21 cm HI Line; • Rebecca McFadden (University Swinburne) — High-precision of Melbourne) — UHE timing and the formation • Nadia Lo on the successful Neutrino Detection using the and evolution of binary submission of her University Lunar Cherenkov Technique. with supervisors Prof Matthew of NSW PhD thesis on A Bailes, Dr Willem van Straten Multi-molecular Line Study of an Well done ! (both University of Swinburne), Entire Giant Molecular Cloud; and Dr George Hobbs (ATNF); • Katherine Newton-McGee on • Marion Wienen (University of the successful submission of her Bonn, Germany) — Understanding University of Sydney PhD thesis the earliest, cold phases of on Radio Polarimetry as a Probe high-mass star formation with of Interstellar Magnetism; and supervisors Prof Karl Menten, • Joris Verbiest on the successful Dr Friedrich Wyrowski submission of his University of (both Max-Planck-Institut Swinburne PhD thesis on Long- für Radioastronomie Bonn, Term Timing of Millisecond Pulsars Germany), Prof Pavel Kroupa and Detection. (University of Bonn, Germany) and Dr Baerbel Koribalski (ATNF);

7 Obituary — John Masterson Helen Sim (ATNF)

The photographic collection of perhaps most, were the work of its offshoots, the Division of the Radiophysics Laboratory photographer John Masterson, Cloud Physics, the ATNF and the contains more than 13,000 sets who died in April this year, aged precursors of the ICT Centre. of items. Although the names 73. Forty of those 73 years were And they were forty years of, of the photographers were spent working for the CSIRO not just work, but of service. not always recorded, many, Radiophysics Laboratory and

John joined the Laboratory in June 1957, at the age of 22. The Radiophysics Laboratory, created in 1940, was then still in its original home, the Madsen building at the University of Sydney. During the war, every piece of equipment the Laboratory produced had been photographed, says Phil Sharp, site coordinator for Property Services at Marsfi eld. The practice persisted into peacetime, and there was enough work for four photographers and an assistant. John started work as a Technical Assistant, level 1. He had completed the only photographic course available at the time, that of the School of Applied Photography in Sydney. One of the attractions of the Radiophysics position was that the Laboratory’s Senior Photographer, Ken Nash, offered a system of training similar to that for newspaper cadets: a mixture of technical reading, practical instruction, and on-the- job training. During 1960–1963 John was called up to do a wider range of tasks for Radiophysics and, increasingly, for other CSIRO Divisions. In this period he was awarded The Sun Trophy at the Sydney International Exhibition of John Masterson in 1982. Credit: CSIRO Photography, for the best entry by

8 ATNF News, Issue 67, October 2009 A DC3 used by the Division of Radiophysics for experiments on clouds. The photographer is not recorded, but John Masterson was responsible for photographing Radiophysics’ cloud seeding and cloud physics experiments. Notice how the photographer has captured the sun shining through two aligned windows of the plane.

an Australian. By 1963 John was end. Ken Nash — an “artsy” type, extremely diffi cult.” In the course second-in-charge of the department, according to former ATNF Assistant of his career John had to devise and had sole responsibility for the Director John Brooks — believed in photographic solutions to a diverse photographic coverage of the new making images that were beautiful range of problems, from counting observatory and radioheliograph as well as technically informative: and grading ice crystals to making near Narrabri, now the home John learned a lot from him, and high-speed studies of cutting tools of the Compact Array. was infl uenced by his style. He on experimental lathes, 24-hour always knew what was wanted, monitoring of weather radar results, When Radiophysics moved to what a photograph needed to show, and the printing of complex colour its Marsfi eld site in 1968, the according to Phil Sharp. “Some of outputs from spectrographs. An photolab was located in what is the stuff we had photographed was important part of his work in the now Wing G. Ken Nash’s health very tricky, with small components. 1980s was reduction photography of was deteriorating, and John took He’d spend hours working on that,” circuit layouts for solid-state devices. increasing responsibility for running said Mal Sinclair, a former head of the photolab, fi nally becoming its In its early days, Radiophysics had the ATNF Receiver Group. “The head in 1974 when Nash retired. operated a number of fi eld stations, work John did for the Division such as the one at Dapto, and John With respect to his craft, John was of Cloud Physics, photographing made frequent trips to those. He a professional from beginning to experiments in cloud chambers, was worked with Ken Nash to capture

9 the construction and early days of the Parkes telescope. Later, when the Compact Array was being built, he took essentially all of the still photographs recording its construction. For the Compact Array, he was called upon to record engineering techniques such as stretch forming, panel fabrication and feed horn construction in black and white, on colour slides, negatives, and video tape. The artwork for electronics had to be Dr Harry Minnett surveying the surface of the Parkes telescope in 1964. John photographically reproduced with Masterson and Ken Nash shared the work of photographing Parkes in its early great accuracy, to exact reduction days, and it’s not recorded which of them took this photo. The image is typical ratios. As well as all the technical of the beautifully composed black and white photographs of Parkes in the and recording photography he Radiophysics photo archives. needed to produce a constant stream of illustration for the some of the background using a single “John was not an empire builder,” media, displays and presentations. handheld electronic fl ash unit. With said Shaun Amy, Head of Computing “John would work 20 hours a day the camera lens open and set to an Infrastructure for the ATNF, and if he had to,” said Phil Sharp. appropriate aperture I was able to himself a keen photographer. “He John’s own description of traverse a carefully calculated path recognised he was in a service role, photographing at night antennas around the dishes and expose them and dedicated himself to that.” three, four and fi ve of the to many individual fl ashes to achieve John knew a lot, and was pleased Compact Array during their the result desired. This single exposure to share that knowledge, Shaun construction indicates the is made up of over 130 fl ashes. The says. Over the years John’s services amount of trouble he took: photograph was just what I had and advice were called upon not The aim was to isolate the antennas anticipated and has been in great only by Radiophysics but also by from the mass of cable drums, demand. (See back page image.) several other CSIRO Divisions, a range of departments at the compressors, containers and generally This care and attention to University of Sydney (Civil, Electrical confusing items at ground level, give detail were appreciated: a good view of the profi le and the and Aeronautical Engineering; Despite the fact that CSIRO and under-structure of , and Geography and Tropical Medicine), this Division have only recently paid produce a good stand-alone illustration Lewisham Hospital, and even the much heed to personal credits on of the progress on site. The site was NSW Forestry Department. In the published photographs quite a few in total darkness except for a single mid 1970s John was instrumental in people sought me out by name bulb mounted on a pole adjacent to forming the NSW Photographers and congratulated us on the quality antenna fi ve. Because of the large Group, and helped organise and obvious professionalism of the areas and long distances involved the fi rst national conference work coming from the Radiophysics’ I elected to wait until late evening for CSIRO photographers. Communication Group. and “paint” the two front dishes and

10 ATNF News, Issue 67, October 2009 his family: his wife Clare, whom he’d met when they both worked at the University of Sydney, and their children — Katherine, Michael, Peter, Sean, Paul, Bernadette and Matthew. Tragically, Sean was killed as a young man. It was after that that an incident occurred which was “the only time I ever knew John to lose his temper”, said Graham Moorey, another former head of the Receiver Group. At a railway station, someone had tried to steal John’s wallet: he put the bloke in a headlock and left him The photomontage of Dr Dick McGee referred to in the text. McGee had the worse for wear. That incident oversight of the Photolab. was an exception, however. John retired in September 1997. Photography was one vehicle McGee is said to have quipped For the Radiophysics Laboratory, for John’s sly sense of humour. “Ah, but that was when I had a full he had created a body of work John Brooks recalls the time he body of hair!” According to Brooks, recording four decades of its history: and colleague Bob Batchelor had John was able to photographically for himself, he had attained asked John to take head shots to turn an innocuous technical item [l]ong experience in micro/macro/ accompany a paper they were such as a feedhorn “into a UFO scientifi c/industrial/portrait/fi eld/ submitting for publication. When about to disgorge aliens”. aerial and illustrative photography, Brooks was supplied with his photo, John was a quiet man, but extremely cine and video techniques including something about it puzzled him: sociable: “he knew everyone, editing and audio mixing [,] and … “It was me alright, but he’d made could talk to everyone”, said Phil experience in what the Division needs me look really ugly”. When he Sharp. He liked a drink, liked his in the application of these techniques compared notes with Batchelor, the jazz — he used to frequent the penny dropped: Brooks’ photo had while still retaining Sydney Jazz Club, then housed in been subtly distorted by stretching the Ironworkers Building in Sydney’s an openness to and keen interest it vertically, while Batchelor’s had George Street — and was a fanatical in the need for constant reappraisal been stretched horizontally. “We support of the Rabbitohs (the South and change where necessary. went round to tell Masterson what Sydney Rugby League team). He was In his community, John worked for a bastard he was,” said Brooks. John dogged — for instance, as a union many, and made himself known and would just have grinned. A more representative in the mid 1970s loved: more than 200 people came overt joke was his photomontage — and he was generous, devoting to his funeral. His most important that put the face of Dick McGee, great time and energy to charitable legacy, however, is in the lives of who oversaw the Photolab, on causes associated with his church. his family: his wife, children, grand- the body of an orang-utan. When And, above all, he was devoted to children and great-grand-children. this appeared on the noticeboard,

11 Australian Square Kilometre Array Pathfi nder (ASKAP) Gabby Russell and Carole Jackson (ATNF)

Survey Science First Antenna on Track acceptance tests took place in late September to ensure timely delivery Projects Announced Manufacture of ASKAP’s fi rst of the antenna to the Murchison antenna has progressed well. Ten major science projects, Radio-astronomy Observatory in CSIRO and contractor CETC54 representing 363 unique authors late November. In preparation for have jointly fi nalised the full factory from 131 institutions, have been factory and site acceptance testing and site acceptance test plan that selected to use ASKAP during the the ASKAP antenna team has describes the procedures, tests fi rst fi ve years of the telescope’s been trained to use the VSTARS and pass conditions for every operation. A full report can be photogrammetry system, which will aspect of the antenna. The factory seen on page 16 of this newsletter. be used to measure the parabolic surface of the dish to ensure it meets the 10 GHz upper frequency specifi cation. A full outline of the ASKAP antenna performance specifi cations can be found at www.atnf.csiro.au/projects/askap.

Technology Update As the development of ASKAP progresses, the project has met several key technological milestones: The analog system has progressed from concept to design phase. The electrical and mechanical design of the phased array feed is well under way, as is the design of the conversion modules and rack that will be located in the pedestal of the antenna.

Refl ective dots have been applied to the 12-metre antenna at the Parkes Testbed Facility, which has been used by the ASKAP team for training in photogrammetry. Credit: Carole Jackson, CSIRO.

12 ATNF News, Issue 67, October 2009 Prototype hardware has been The next stage in the process been introduced to keep industry delivered for the entire ASKAP is for the ILUA to be formally and other interested stakeholders beamformer, which includes registered, a process which is informed on the progress of the digitiser, backplane, control and underway at the time of writing. ASKAP project. The fi rst two power boards (to be located at editions are available online at A tender for the design of support each antenna) and a digital signal www.atnf.csiro.au/projects/askap. infrastructure at the MRO was processing and rear transition published on the AusTender board (to be installed in the central website in June 2009 and, following Reaching Out in building as part of the beamformer). evaluation, Aurecon was selected Geraldton Software version 1.0 for as the successful tenderer. Two monitoring and controlling the further requests for tenders, for A recent visit to the MRO by a Parkes Testbed Facility’s 12-metre a telehandler (a specialised type group of Indigenous artists and antenna (used to test ASKAP’s of crane) to be used for antenna scientists (reported in ATNF News systems) has been released. assembly, testing, and maintenance, April 2009) has been the inspiration and transportable building (donga) for an art exhibition, Ilgarijiri — The fi rst simulated ASKAP 30- supply and installation, were things belonging to the sky. The square-degree image has been published on the AusTender group spent three days together made to the expected noise depth website at the end of August and made a special visit to the by using the SKA Design Studies’ 2009. Design of the Boolardy MRO, located on Wajarri Yamatji Simulated Skies model, which Homestead accommodation land, which produced a collection of demonstrates that the imaging improvements has started with a more than 90 artworks connecting and analysis software is working. Geraldton-based company, Eastman the land, culture and astronomy. Signifi cant progress has been made Poletti Sherwood Architects. Organised by the International with the development of several Centre for Radio Astronomy low-cost synthesiser units required Research and Yamaji Art Indigenous in each of ASKAP’s 36 antennas. Industry Engagement art cooperative, and sponsored News by CSIRO, the exhibition was Testing of ASKAP’s prototype offi cially launched at the Geraldton phased array feed has been On 10 July 2009, CSIRO hosted Regional Art Gallery on 12 June undertaken to characterise its second special ASKAP and 2009. More information on the its performance when SKA technical discussion session. artworks and exhibition can be equipped with improved Over two and a half hours, ASKAP found at http://ilgarijiri.wordpress.com. design low-noise amplifi ers. computing leaders Tim Cornwell and Ben Humphreys provided In August, Geraldton celebrated Murchison Radio- a thorough overview of ASKAP National Science Week with a computing challenges and the wide range of astronomy-themed astronomy Observatory development of SKA systems for the activities for school students (MRO) Plans Progress 12 industry participants. The third in and the wider local community. the discussion series is being planned Coordinated by CSIRO’s Priscilla In June 2009 CSIRO became the and will focus on the development Clayton, highlights included offi cial leaseholder of Boolardy of sensitive, ultra-wideband Geraldton amateur theatre club Pastoral Station and the MRO’s receivers for radio astronomy. Theatre Eight’s production The Indigenous Land Use Agreement Life of , exhibitions at the (ILUA) was executed after all the A new quarterly publication, Western Australian Museum — required signatures were obtained. ASKAP Technical Update, has

13 Geraldton, and public lectures by visit a small display including a Society of New Zealand, the Western Australian Government model of the focal plane array. International Astronomical Union Astronomer Dr James Biggs and General Assembly in Rio de ASKAP has also been represented at Australian National University’s Janeiro, the SKA Design Studies many astronomy events in Australia Dr Charley Lineweaver. The Training School in Paris, and at and internationally. In early June Murchison region also took part a Panoramic Radio Astronomy 2009, a small delegation attended with astronomy outreach activities meeting in The Netherlands. the 214th American Astronomical held at Yalgoo Primary School and Society meeting in Pasadena where Meekatharra School of the Air. the ASKAP exhibition stand was SKA-related News very successful in attracting interest Australia’s bid for the SKA was ASKAP on Display among the 1600 astronomers boosted in August 2009 by Visitors to the Parkes Open Days and other meeting participants. the signing of a collaborative on 18 and 19 July were able to Presentations on ASKAP have been arrangement with New Zealand. take the “ASKAP Walk” to the delivered at annual meetings of the The arrangement was signed 12-m testbed antenna, talk with Astronomical Society of Australia by New Zealand’s Minister an ASKAP team member and and the Royal Astronomical for Economic Development,

Ron Koenig at the ASKAP display during the Parkes Open Days. Credit: Tony Crawshaw, CSIRO.

14 ATNF News, Issue 67, October 2009 Signing of the Australia–New Zealand arrangement for a joint SKA bid by Senator Kim Carr and Minister Gerry Brownlee. CSIRO SKA Director Professor Brian Boyle (far left) and Scott McHardy from the New Zealand High Commission (far right) are also pictured. Credit: Photocall.

the Hon. Gerry Brownlee, major system integration company Selection) activity, CSIRO has and Australia’s Minister for to work on strategic SKA design continued working with Aurecon Innovation, Industry, Science and issues in Australia. A small team on geographic information system Research, Senator the Hon. Kim of engineers at BAE Systems analysis to help determine SKA Carr. Under the arrangement, will work alongside CSIRO staff array station placement and Australia and New Zealand will to analyse the performance standards for site characterisation. together offer the international of CSIRO’s phased array feed CSIRO staff have also continued to community the receivers within the proposed SKA actively participate in SKA design to develop the SKA across the antenna design. The fi rst phase of and development discussions, two countries, with a maximum this analysis will be completed in ranging from system engineering, baseline of around 5,000 km. time for a major PrepSKA Work antenna optics design, front-end Package 2 (SKA Design) workshop CSIRO has engaged BAE Systems receiver options, digital systems and to be held at the University of Australia to provide critical analyses SKA outreach activities, led by the Manchester, UK in October 2009. that will help guide the design SKA Project Development Offi ce. decisions for the SKA antennas. As part of PrepSKA Work Package This is the fi rst engagement of a 3 (Site Characterisation and

15 ASKAP Survey Science Projects enter Design Study Phase Ilana Feain and Simon Johnston (ATNF)

Since 2008, an open and group for which the ATNF will determine how the Design Studies international process to provide full support, an A- group should proceed over the next few for which the ATNF will make all years, in terms of management, determine the major Survey reasonable efforts to support and processes and working groups. a Strategic Priorities (SP) Group Science Projects (SSP) to be The ASKAP Survey Science for which the ATNF will work conducted by the Australian SKA Projects are listed in Table 1 and to ensure that capabilities are each is briefl y described below: Pathfi nder (ASKAP) telescope enabled to the extent possible. has been proceeding. The results A breakdown of the membership EMU: Evolutionary Map of of this process were announced of the 10 Survey Science Projects the Universe — PI Norris illustrates the international interest on Friday 4 September 2009. in the ASKAP program. There are EMU is a deep (10 µJy/beam rms) radio continuum survey of 75% This follows recommendations 363 unique team members from of the entire sky. EMU will probe provided by the ASKAP Survey 131 institutions. The breakdown typical star forming galaxies to Science Project Assignment of team members by region is 1, powerful starbursts Committee, a committee 33% Australia and New Zealand, to even greater , Active made up of a broad range of 30% North America, 28% Galactic Nuclei to the edge of the international experts. Projects Europe and 9% rest of world. Universe, as well as undoubtedly that were successful were chosen Successful Principal Investigators discovering new classes of rare according to their scientifi c merit (PIs) were invited to a one-day objects. The key science goals for and operational feasibility. SSP Design Study kick-off meeting EMU are to trace the evolution of Ten Survey Science Project held at the ATNF headquarters in star forming galaxies and massive proposals were successful. These Sydney on 21 October. The meeting black holes throughout the history projects were prioritised into brought PIs together with ASKAP of the Universe and to explore one of three categories: an A engineers and project scientists to large-scale structure. EMU will

Table 1: The Eight ASKAP Survey Science Projects and Two Strategic Priorities

A EMU Evolutionary Map of the Universe A WALLABY Widefi eld ASKAP L-Band Legacy All-Sky Blind Survey A- FLASH First Large Absorption Survey in HI A- VAST An ASKAP Survey for Variables and Fast Transients A- GASKAP The Galactic ASKAP Spectral Line Survey A- POSSUM Polarisation Sky Survey of the Universe’s Magnetism A- CRAFT The Commensal Real-Time ASKAP Fast Transients Survey A- DINGO Deep Investigations of Neutral Gas Origins The High Resolution Components of ASKAP: Meeting SP VLBI the Long Baseline Specifi cations for the SKA SP COAST Compact Objects with ASKAP: Surveys and Timing

16 ATNF News, Issue 67, October 2009 create the most sensitive wide- are focused on both the neutral gas and OH lines in the and fi eld atlas yet made, and provide content of galaxies and the cosmic Magellanic Systems. Compared with a long-lasting legacy survey. HI mass density in the redshift existing data, GASKAP will achieve range 0.5 < z < 1.0 where the HI about an order of magnitude WALLABY: Widefi eld emission line is too weak to be improvement in both brightness ASKAP L-Band Legacy All- detectable in individual galaxies. The sensitivity and in angular resolution. observations will increase the total Sky Blind Survey — PIs GASKAP will detect and map number of absorption line systems Koribalski & Staveley-Smith OH masers from evolved by an estimated two orders of and star formation regions, diffuse WALLABY is an extragalactic magnitude, representing a signifi cant emission from molecular and neutral hydrogen survey over 75% data set to study gas assembly and atomic clouds, HI absorption of the entire sky and will detect up galaxy formation during a time in toward background continuum to 500,000 galaxies to a redshift the history of the Universe that sources and the structures in of 0.26. The fundamental aims is largely unstudied thus far. the gas that trace the effects of WALLABY are to examine of stellar winds and the HI properties and large-scale An ASKAP Survey for Variables explosions. The Magellanic Clouds distribution of these galaxies in and Slow Transients (VAST) will show all these processes as order to study galaxy formation — PIs Murphy & Chatterjee they appear in two other, very and the missing satellite problem different environments. GASKAP in the Local Group, evolution VAST gives unprecedented will provide stunning images of and star formation of galaxies, opportunities to investigate the sky the interstellar medium that will the role of mergers and galaxy at radio wavelengths for transients be indispensible for astronomers interactions, the HI mass function with a timescale as short as fi ve working at other wavelengths. and its variation with galaxy seconds. ASKAP’s wide-fi eld survey density, the physical processes capabilities will enable the discovery governing the distribution and and investigation of variable and Polarisation Sky Survey of evolution of cool gas at low redshift, transient phenomena from the the Universe’s Magnetism cosmological parameters relating local to the cosmological including (POSSUM) — PIs Gaensler, to gas-rich galaxies and the nature fl are stars, intermittent pulsars, Taylor & Landecker of the cosmic web. WALLABY X-ray binaries, magnetars, extreme Understanding the Universe is will provide the largest, most scattering events, intra-day variables, impossible without understanding homogeneous HI sample of galaxies radio supernovae and the orphan magnetic fi elds. Magnetic fi elds are yet made, and will be an important afterglows of gamma-ray bursts. key to the non-thermal Universe, pathfi nder for key SKA science. VAST will probe unexplored regions yet it is unclear how large-scale of phase space where new classes of magnetic fi elds are generated and transient sources may be detected. First Large Absorption Survey maintained. POSSUM will use radio in HI (FLASH) — PI Sadler source polarisation, in particular GASKAP, the Galactic FLASH is a blind HI absorption-line the technique of rotation measure ASKAP Spectral Line survey that uses background radio (RM) synthesis, to perform a wide- continuum sources to identify and Survey — PI Dickey fi eld survey that will yield a grid characterise foreground neutral The GASKAP survey is a high of RMs over a substantial fraction hydrogen. FLASH science outcomes spectral resolution study of the HI of the sky. The science outcomes

17 of POSSUM will revolutionise our DINGO: Deep Investigation of Compact Objects with understanding of the ordered Neutral Gas Origins — PI Meyer ASKAP: Surveys and Timing components of the Milky Way’s DINGO will study the evolution (COAST) — PI Stairs magnetic fi eld, test dynamo and of neutral hydrogen (HI) from other models of magnetic fi eld COAST will undertake an the current epoch to redshift generation in galaxies and clusters, observational program of pulsar about 0.5, providing a legacy and carry out a comprehensive timing aimed at high profi le issues in dataset spanning cosmologically census of magnetic fi elds as a astrophysics. This includes limits on, representative volumes. function of redshift in galaxies, or the detection of, a background active galactic nuclei, galaxy clusters Measurements will be made of key of gravitational waves, stringent and the intergalactic medium. cosmological distributions, including tests of the predictions of General ΩHI, the HI mass function and Relativity and other theories of strong gravity and the studies of The Commensal Real-time the halo occupation distribution binary stellar evolution. In addition ASKAP Fast Transients function. ASKAP data will be combined with optical data to to pulsar timing, blind searches for Survey (CRAFT) — PIs pulsars will also be carried out which Dodson & Macquart enable a thorough study of the co- evolution of the stellar, baryonic and will lead to a better understanding CRAFT is a purely commensal dark matter content of galaxies. of the Galactic survey for transient sources with population, the pulsar emission mechanism and the structure and time-scales shorter than fi ve The High Resolution magnetic fi eld of the Galaxy. seconds. Short-timescale transients Components of ASKAP: Meeting are associated with the most the Long Baseline Specifi cations energetic and brightest single events for the SKA - PI Tingay in the Universe. They provide Nature’s ultimate laboratory; ASKAP, in combination with the their emission is generated by existing Australian Long Baseline matter under extreme conditions Array, high speed data recording whose properties probe physical equipment, innovative software regimes far transcending the range correlation facilities and high speed achievable in terrestrial experiments. data transport networks provides Fast timescale transients open a high resolution capability that new vistas on the physics of high is unmatched in terms of SKA brightness temperature objects, demonstrators around the world. extreme states of matter and Science outcomes include proper the physics of strong gravitational motion and parallax of pulsars, high fi elds. In addition, the detection of resolution imaging of Active Galactic extragalactic transients affords us Nuclei, follow-up of transient an entirely new and sensitive probe radio sources and distances and on the huge reservoir of baryons proper motions of OH masers. in the intergalactic medium.

18 ATNF News, Issue 67, October 2009 2009 CSIRO Radio Astronomy School Jimi Green and Mike Keith (ATNF)

The ATNF held a CSIRO Radio even allowing some students to thank the local staff at Parkes Astronomy School at the Parkes walk on the dish (although not to and the staff at the Dish Cafe for Radio Telescope for the fi rst time play cricket!). The school was well helping make the week a success. in the last week of September. attended by almost 30 students Copies of the presentations given The ATNF has for many years run from across Australia as well as at the School have been posted a Synthesis Imaging School at the further afi eld. The organising on the webpage at www.atnf.csiro. Australia Telescope Compact Array committee would like to heartily au/research/radio-school/2009/. in Narrabri, typically every other year. However, this year the ATNF took the step of moving towards an annual school, alternating between the synthesis imaging theme, held in Narrabri, and a primarily single- dish radio astronomy focussed school, held at Parkes. The program featured a range of topics, including: details of the illustrious history of Parkes; the core principles of radio astronomy; the range of single-dish radio astronomy observations; and placing radio astronomy in the wider context. It also contained one day dedicated to interferometric considerations. Three afternoon sessions were used for group tutorials, consisting of a site tour, an ATNF Spectral Analysis Package data reduction tutorial, and an observing session. Unfortunately, persistent strong winds resulted in the dish being wind-stowed for the fi rst two tutorial sessions and the “practical observing” tutorial becoming a theoretical exercise! For lighter entertainment the school had two evening talks, Making Beer in Space by Andrew Walsh and Aboriginal Astronomy by Ray Norris, both proving very popular, and included tours of “The Dish”, The 2009 CSIRO Radio Astronomy School. Credit: John Sarkissian, CSIRO

19 CSIRO Parkes Observatory Open Days Chris Hollingdake (ATNF)

The CSIRO Parkes Observatory celebrated the International Year of The open days, showcasing the Astronomy and the 40th anniversary of the achievements of the Observatory as a world-leading astronomical landing by giving members of the public a rare telescope as well as its roles in opportunity to tour the Parkes radio telescope. supporting some of the most signifi cant space missions in history, took place on the weekend of 18 – 19 July. A record crowd of more than 6,500 visitors visited the Observatory over the weekend with ATNF volunteers guiding 3000 visitors through the 64-m telescope on tours. This was 100% more than previous records achieved on Open Weekends. Takings were also well up at the Visitors Centre with each day’s takings about twice the previous record daily revenue. Notably, our most distant visitors travelled from London for the event, while the fi rst visitors in the queue on Saturday morning had driven especially from Townsville! As well as telescope tours of “The Dish”, the future of radio astronomy was highlighted through tours of the 12-m ASKAP testbed antenna, and through expert talks, brochures and interactions with staff. From a public relations perspective, the Open Days were also a resounding success with extensive media coverage generated on TV and radio, and in print and online mediums. In total around one hundred staff and volunteers were involved, and helped to make Parkes open days visitors. Credit: Tony Crawshaw, CSIRO the weekend run smoothly.

20 ATNF News, Issue 67, October 2009 More than 3,000 people toured the 64-m telescope during the CSIRO Parkes Radio Telescope Open Days 2009. Credit: Shaun Amy, CSIRO.

The ATNF collaborated with David Malin, Astrophotographer, generate is very important in CSIRO Education, Questacon – The who spoke on Galileo’s ensuring that the great work National Science and Technology astronomical legacy. conducted with our radio telescopes Centre, the Central West is recognised throughout Australia. Jill Tarter, Director of the Centre Astronomical Society, the Wireless These days would not be possible for SETI Research, whose talk was Institute of Australia, HeliWest, the without the support of the titled SETI: Science Fact, Not Fiction. NSW State Emergency Services and ATNF staff and their families. various other community groups. Wayne Lee and Erissa Hines, NASA Thank you, one and all! The diversity of groups present engineers, who spoke on NASA’s offered a variety of activities for plans to return to the moon. families to enjoy. Feedback from David Cooke and Neil Mason, these groups was very positive and former Parkes staff, who it is likely we will be able to build on spoke on their recollections these relationships for future events. of the Apollo missions. A world-class line up of speakers The public attention that Open also featured and included the Days at the ATNF Observatories following presentations:

21 CSIRO ATNF says Farewell to Pat Sykes Tony Crawshaw (ATNF)

ATNF News Editor Tony Crawshaw What do you remember the apprenticeship. In those days, spoke with Pat Sykes, ATNF’s about these early years? apprenticeships were Government leading cryogenics specialist and Well, I remember there was a fair funded and there was no guarantee Marsfi eld research team leader of amount of study involved going to that you’d get a full time job engineering, in the weeks before tech at night. I actually started a with the organisation that you’d his retirement. In the thirty-six mechanical engineering certifi cate at apprenticed at. From what I could years that Pat spent working for the same time that I was completing see within the Division it all looked CSIRO, he designed, developed and maintained a wide range of cryogenic cooling systems and ancillary technology, utilised by receiving systems on both ATNF and international antenna systems. This is an edited transcript of that conversation.

So Pat, you’ve been with the CSIRO for over 36 years. How did it all start? Well, it all goes back to my time at Kulnura (30 miles west of Gosford) where I was brought up on a citrus farm. It was pretty remote. The nearest neighbour was two miles away and it was all dirt roads. I’d start the day working on the farm. Then I’d make my way to school (a three mile bike ride to the bus stop, and then a bus into town). Then I’d have the journey in reverse, and work some more on the farm. Well, that was where I got my interest in machinery. I enjoyed working with the tractors and all of the farming implements so it seemed to make sense to apply for an apprenticeship. So, I did and was lucky enough to pick one up with CSIRO as a fi tter and machinist. It wasn’t the ATNF back then; it Pat Sykes with the Parkes 13-beam multibeam receiver ready for fi nal was the Division of Radio Physics. assembly in the Marsfi eld cryogenic lab.

22 ATNF News, Issue 67, October 2009 pretty interesting, so I thought I’d the digital electronics area. That left they needed a cryogenic person better pick up as many skills as me as responsible for Cryogenics so I applied for the job. This was possible. I fi nished my apprenticeship in the Division and I was fortunate in the early stages and there were and applied for my fi rst formal enough to be able to create the no antennas yet on site. CSIRO CSIRO role (as draftsman). That fi rst cryogenic lab in the basement gave me a technical transfer; I took was in 1977 and I worked on various here at Marsfi eld. It was a proper leave without pay and worked on projects at Marsfi eld before moving leap forward to have a proper lab. all things cryogenic. This was a real to Parkes several years later on. Initially the cryogenics work had eye opener for me. Everyone I been done with nothing more than worked with was a pure researcher. an ordinary bench top — I was I was the hands-on person with the What did you do at Parkes? rebuilding compressors on my desk! practical experience but I’d never I was working on the T.E.S.T (Two worked in a university before. To Element Synthesis Telescope) be surrounded by the students You’ve been involved in a number of project under Jon Ables which and the thinking and discussions exciting projects. What stands out? involved the refurbishing of the 18-m that would take place was amazing. Telescope, modifying a telescope Well the AT (Australia Telescope) At the antenna completion stage I service tower to be a telescope was a major project. The AT was was working on site at Hat Creek transporter and the construction of a bicentennial project and my job (Northern California). The summers two temperature controlled receiver was to fi t out all the antennas with were hot and the winters were packages. I also did the surveying all the cryogenics and to set up a blistering cold. I remember trying for the 400m of rail track and then world class lab in Narrabri. That to solder up connectors with supervised the laying as well. I did a was a busy time, looking after all three heater blowers on full blast, bit of everything at Parkes and have the plumbing on the antennas, just to get the solder to melt! really fond memories of my time designing equipment and running a there. Then that project fi nished and team of people installing all of the Then back to Sydney? I returned to Sydney to take up the machinery. I was based in Narrabri position of Cryogenic Technician. for two and a half years and to This was the start of designing and be in on the ground fl oor setting building a two-stage Helium scroll it all up was a once in a life time compressor to run the SIS mm So this was where you got opportunity and absolutely fantastic. receiver. It was a huge success and your cryogenic grounding? was the building block for our single Yes — that was the commitment stage compressors to follow, that And another project highlight? to building the K-band maser have been running trouble free since (which was about 60% complete Another was moving to the 1997. A result I am very proud of. at the time). The construction of University of California, Berkeley The next big project was working the 4K receiver cryogenic system in the early 1990s where I worked on the 13-beam multibeam receiver was done by John Griffi ths to on the design and construction of for Parkes. No one had ever built a whom I was assigned for a training the Berkeley-Illinois-Maryland Array receiver that big at that frequency. in Cryogenics. After fi nishing the particularly the 2.5-Kelvin receiver. I designed the cryogenic package maser, John moved on to work in Through Rick Forster I found out and all the mechanical components

23 that went into the receiver. The You’ve obviously had a number of whether it was to discuss your issues receiver was installed February 1997 highlights in your career. What’s the or to celebrate your successes. and is still operational. We actually one thing that really stands out? He was dedicated to his job and won the CSIRO medal for that. It a pretty inspiring bloke that you As airport traffi c co-ordinator at turned out to be a huge success didn’t want to let down. I’d also say Narrabri for the opening of the and I think, led directly, to ATNF Mal Sinclair who was in charge of Australia Telescope Compact Array getting the contract to create ALFA the receiver group. He was just a (ATCA) in 1988 I had to greet the — a 7-beam receiver in Arecibo wealth of knowledge and a great Prime Minister Bob Hawke at the [the Arecibo L-band Feed Array]. bloke as well. Both have played airport. He was there to open the a major role in my work life. Australia Telescope. He emerged from the plane surrounded by Can you tell me a bit minders, read my name tag and more about ALFA? Any fi nal thoughts? said “G’day Pat let’s go open this What I remember most about big thing”. To represent CSIRO and Just that CSIRO has been really ALFA was fl ying out to Arecibo in to be involved in something that good to me. I’d never have a bad Puerto Rico with Graeme Carrad, was worth the PM coming out to thing to say about the organisation. who was at that time the Project see was an incredible experience. I’ve always been proud to explain Manager. Graeme and myself went The whole opening went really my cryogenic work and people across there to do the installations well with the PM driving the have always been fascinated with and commissioning. It was very telescope up and down the track. the projects that I’ve worked on exciting and an ordeal at the time We’d put 1800 helium balloons over the years. I’ve been quite but something pretty special. We into the telescopes so that they chuffed about that. I’d have to say had to overcome a huge number could all be released at the same that looking back, it’s been a pretty of challenges — the heat, the time. It looked very spectacular steep learning curve. There’s been a climate, language diffi culties, living and then we had a huge party on- whole host of issues and challenges onsite and there was absolutely no site. That was a very special day. that have had to be overcome. escape from work. In one month These though, have been the we transported, then totally rebuilt ones that I’ve enjoyed the most. and installed the receiver, teaching You’ve obviously worked with a huge It’s the adventurous projects that the local technicians along the way. range of people during your time with have brought out my best work. I The receiver’s been a huge success CSIRO. Who would you say has been can honestly say that I’ve had the and has been virtually trouble the biggest infl uence on your career? best job in the world for me. free. It was a pretty satisfying Well it’s been more than one experience, due I think to the person. I’d have to say John Brooks huge effort that we all had to put Thanks for your time Pat who went on to be project manager in i.e. the whole receiver group for the ATCA and then assistant My pleasure and all the best for and workshop. It all worked out director at the ATNF. John always the ATNF in the upcoming years! really well though — an experience had the time to spend with you that I will always treasure.

24 ATNF News, Issue 67, October 2009 The Nearest Powerful Radio Galaxy NGC612: First Science Results with the CABB C/X-band Bjorn Emonts, Minnie Mao and Jamie Stevens

NGC 612 is the nearest in detail at other wavelengths. A rich galaxy mergers or collisions radio galaxy in the southern thorough study of powerful radio and that the radio source may be galaxies in the nearby Universe — fuelled by the cold gas associated hemisphere with a truly powerful although rare — will provide crucial with these events (e.g. Heckman and extended radio source. One information about the host galaxy et al. 1986, Baum et al, 1992; see properties and possible formation also Hardcastle et al. 2007). Our of its radio jets shows a clear history of these active systems. HI observations provide the fi rst hot-spot, typical for Fanaroff & direct evidence that NGC 612 The nearest powerful radio galaxy indeed contains a large reservoir Riley type-II radio sources. The with extended radio continuum of cold gas, possibly deposited by proximity of NGC 612 allows jets in the southern hemisphere is a past or collision. NGC 612 (z = 0.03; e.g. Ekers et al. us to study this radio source NGC 612 is one of only a handful of 1978). Although the host galaxies of powerful radio galaxies for which we and its host galaxy in great nearby radio sources are generally can study directly the properties of elliptical systems, NGC 612 has been detail. This gives us a unique the cold HI gas with the sensitivity identifi ed as an archetypal S0 galaxy of current-day telescopes. look into the physical processes with a disc of optical emission-line associated with powerful radio gas (Véron-Cetty & Véron 2001; galaxies, which are often too Goss et al. 1980). Star formation has First CABB results been detected along its optical disc on NGC 612 far away to be studied in detail. (Holt et al. 2007). In collaboration We observed the rich radio- with scientists at ASTRON and The complex and bright structure of the radio continuum source continuum source of NGC 612 the University of Sheffi eld, we recently discovered that NGC also makes NGC 612 an excellent as part of the commissioning 612 contains an enormous disc of target to image with the new of the 2 GHz Compact Array neutral hydrogen (HI) gas. Figure 2-GHz Compact Array Broadband 1 shows the HI observations that Backend (CABB). On 9 and 10 April Broadband Backend (CABB). we did with the Australia Telescope of this year, NGC612 was the fi rst Results obtained from these Compact Array. The HI disc around science target observed with the observations show the great NGC 612 has a diameter of 140 C/X-band system of the new CABB kpc and a total HI mass of 1.8 X system, using the hybrid H168 array potential of CABB, as well as 9 10 M (Emonts et al. 2008). A confi guration. Over the following the challenges faced in the medium-deep optical image of months, we repeated these data reduction over a full NGC 612 shows indications for observations at three additional faint shell-like structures within the epochs in the two most compact 2-GHz frequency range. extent of the HI disc. In addition, a hybrid array confi gurations (H168 and H75). CABB provides two Powerful radio galaxies are faint bridge-like structure of HI gas IFs, each with a 2-GHz bandwidth among the most active galaxies in stretched from NGC 612 along a with 2048 channels and full the Universe. Their bright radio total distance of 400 kpc towards stokes polarisation. In C/X-band, continuum can often be traced out the nearby gas-rich galaxy NGC 619 observations at 6 and 3 cm can be to very high redshifts and act as (see Figure 1). From optical studies, done simultaneously by tuning the beacons to trace the most massive it has been suggested that at least individual 2-GHz bands across a galaxies in the Early Universe, which a signifi cant fraction of powerful total frequency range of 8 GHz. are often too faint to be studied radio galaxies are triggered by gas-

25 Figure 1: Radio Galaxy NGC 612 (from Emonts et al. 2008). Top-left: contours of the 20-cm radio continuum of NGC 612 (also known as PKS 0131-36). Bottom-left: HI-rich environment of NGC 612 and its companion NGC 619 (contours represent the total intensity of the HI gas; levels: 0.2, 0.4, 0.7, 1.1, 1.7, 2.3, 3.4, 4.5, 5.7×1019 cm−2). Middle: High-resolution contour plot of the HI disc around NGC 612 overlaid on to an optical image of the S0 host galaxy (contour levels: 0.8, 1.1, 1.5, 1.9, 2.8, 4.0, 5.1, 6.5, 7.8 ×1019 cm−2). Left: Medium-deep VLT acquisition image of NGC 612 (10 sec integration time on an 8m VLT telescope).

Figure 2: Radio-continuum Spectral Index of NGC 612. Top-right: Preliminary radio continuum image of NGC 612 at 6 cm (greyscale) and 3 cm (contours) with CABB. Left: Spectral Index of the eastern hot-spot (dots) as well as the nucleus (triangles) of NGC 612 across the full 2 GHz range of the C- and X-band.

26 ATNF News, Issue 67, October 2009 Figure 2 shows preliminary results to clearly distinguish the resolved project for their hard work to make obtained from these CABB nucleus). These results appear to CABB a great success. Also thanks observations. A total intensity image be in agreement with continuum to Maxim Voronkov for his help of the radio continuum of NGC612 observations at 20 GHz by Burke- with the observations during the is displayed at 6 cm (grey-scale) and Spolaor et al. (2009) and at 843 commissioning period of CABB 3 cm (contours). The diagram in MHz by Jones & McAdam (1992). Figure 2 shows the spectral index The spectral index properties References: of both the hotspot as well as the of NGC 612 are typical for nucleus. Each individual data point powerful radio galaxies with an Ekers, R. D., Goss, W. M., was obtained by extracting a 128 unresolved nuclear continuum Kotanyi, C. G., Skellern, D. MHz part of the 2-GHz CABB- source and bright radio hot-spot. J. 1978, A&A, 69, L21 band (i.e. the same width as the We have also obtained polarisation Véron-Cetty, M.P. & Véron, old pre-CABB backend of the data for NGC612. Preliminary P. 2001, A&A, 375, 791 Compact Array). We performed analysis of this data shows that the Goss, W. M., Danziger, I. J., a full standard reduction on each hotspot is highly polarised (~25%) at Fosbury, R. A. E.;, Boksenberg, separate 128 MHz part of the 6 cm. This is the fi rst test of CABB’s A. 1980, MNRAS, 190, 23 data (bandpass, phase and fl ux polarisation capabilities, and it calibration) and derived the fl ux Holt, J., Tadhunter, C. N., indicates that calibration is possible from the cleaned image by fi tting González Delgado, R. M., Inskip, with the new wide-band system. a Gaussian to the hot-spot and K. J., Rodriguez, J., Emonts, B. nucleus. The same result is obtained However, our understanding of the H. C., Morganti, R., Wills, K. when performing a reduction over data reduction associated with the A. 2007, MNRAS, 381, 611 the full 2-GHz band and splitting up new CABB system is continuously Emonts, B. H. C., Morganti, the data only at the fi nal stage of progressing. Many new challenges R., Oosterloo, T. A., Holt, imaging, provided that the bandpass are faced regarding the reduction of J., Tadhunter, C. N., van der is derived from a calibrator with data over these large bandwidths, Hulst, J. M., Ojha, R., Sadler, E. known spectral index (such as PKS which will become standard M. 2008, MNRAS, 387, 197 1934-638). The preliminary image in the next generation radio of the radio continuum structure in telescopes. A full understanding Heckman, T. M., Smith, Eric P., Baum, Figure 2 is obtained by combining of the effects related to science Stefi A., van Breugel, W. J. M., Miley, the individual “128 MHz” images observations using large bandwidths G. K., Illingworth, G. D., Bothun, G. over the entire 2-GHz band at 6 is essential for assuring the data D., Balick, B. 1986, ApJ, 311, 526 quality obtained with these new and 3 cm (with only one observing Baum, S. A., Heckman, T. M. & van instruments. Nevertheless, our epoch in both the H168 and H75 Breugel, W. 1992, ApJ, 389, 208 array confi guration included so far). preliminary CABB results indicate However, in reality the continuum the excellent performance of the Hardcastle, M. J., Evans, D. structure changes signifi cantly new broadband system at the A. & Croston, J. H. 2007, over the full 2 GHz range. Compact Array and show the MNRAS, 376, 1849 great potential for broadband Figure 2 clearly shows the steep Burke-Spolaor, S., Ekers, R. technology in radio . spectral index of the radio hot- D., Massardi, M., Murphy, T., spot, while the nucleus shows a Acknowledgements: We would like Partridge, B., Ricci, R., Sadler, E. roughly fl at spectrum (note that at to thank Warwick Wilson and his M. 2009, MNRAS, 395, 504 6 cm the continuum of the inner team, the people in Narrabri and Jones, Paul A. & McAdam, radio lobes becomes too bright all others involved in the CABB W. B. 1992, ApJS, 80, 137

27 Gas Dynamics and Star Formation in the Galaxy Pair NGC 1512/1510 Ángel R. López-Sánchez and Baerbel Koribalski (CSIRO / ATNF)

Abstract As part of the Local Volume HI Survey (LVHIS) project, we obtained HI line and 20-cm radio continuum data of the nearby galaxy pair NGC 1512/1510 using the Australia Telescope Compact Array (ATCA). The results are stunning: we found a very large HI disk that is ~4 times the optical diameter of the barred galaxy NGC 1512, with two pronounced spiral/tidal arms. Both the HI morphology and the distribution of the star-forming regions are affected by gravitational interaction with the neighbouring blue compact NGC 1510. The two most distant HI clumps are likely tidal dwarf galaxies (TDGs). We complemented the study with GALEX UV-, SINGG Hα- and Spitzer MIR images, comparing the distribution and kinematics of the neutral atomic gas with the localisation, star-formation activity and ages of the stellar clusters in multiple regions of the system. This multi-wavelength analysis suggests that the galaxy pair NGC 1512/1510 is in the fi rst stages of a minor merger having started around 400 Myr ago.

Introduction HI morphology relatively recent (150 – 300 Myr) star formation activity in them. Hydrogen is the most abundant and kinematics Figure 2 displays the HI velocity fi eld element in the Universe, the Figure 1 shows that the NGC of the galaxy pair NGC 1512/1510 main fuel for star formation and 1512/1510 system possesses a huge which indicates a relatively regular a powerful tracer of galaxies in amount of neutral gas. Our deep rotating inner disk of NGC 1512 various stages of their evolution. ATCA HI mosaic reveals a very and a more disturbed outer disk. The Local Volume HI Survey (LVHIS; extended HI distribution, spanning The fi tting of the rotation curve Koribalski et al. 2008, www.atnf.csiro. a diameter of ~40’ (or 110 kpc). indicates important deviations au/research/LVHIS) will expand our Two prominent spiral arms, which near the position of NGC 1510 knowledge of the nearby Universe appear to wrap around ~1.5 times, and in the outer spiral/tidal arms. via HI line (21-cm) and radio are among the most remarkable continuum observations of all gas- HI features. Disturbances in the rich galaxies in the Local Volume (D outer disk of NGC 1512 are likely 20-cm radio < 10 Mpc). More than 70 southern caused by tidal interaction with and continuum emission galaxies previously detected in the accretion of the dwarf companion, The 20-cm radio continuum HI Parkes All-Sky Survey (HIPASS; NGC 1510. Individual HI clouds are emission towards the galaxy Koribalski et al. 2004) have been found out to projected radii of 30’ pair NGC 1512/1510 and its observed with the ATCA. (~83 kpc). The velocity gradient surroundings is shown in Figure 3. The galaxy pair NGC 1512/1510 detected within the extended Both galaxies are clearly detected. is located in the outskirts of the clumps agrees with that of the The fi eld contains a large number Local Volume, at around 9.5 Mpc. neighbouring spiral arms, suggesting of unresolved radio sources as well The barred, double-ring spiral that they are condensations within as a few head-tail and wide-angle galaxy NGC 1512 and the blue the outermost parts of the disk. tail radio galaxies. The barred spiral compact dwarf (BCD) galaxy NGC The two most distant HI clumps are galaxy NGC 1512 shows extended 1510 are an pair, likely tidal dwarf galaxies (TDGs), continuum emission (~5’×3’) and a separated by only ~5’ (13.8 kpc). as the GALEX UV images indicate

28 ATNF News, Issue 67, October 2009 Figure 1: ATCA HI distribution in the galaxy pair NGC 1512/1510. The ellipse (center) and the circle (~5’ towards the SW) mark the position of NGC 1512 and NGC 1510, respectively. The two TDG candidates are also labelled.

Figure 2: ATCA HI velocity fi eld of the galaxy pair NGC 1512/1510.

29 Figure 3: ATCA 20- cm radio continuum emission of the galaxy pair NGC 1512/1510 and its surroundings.

bright core while the much smaller an excellent way to highlight the that these spectacular XUV –disks BCD galaxy NGC 1510 appears locations of star formation within must be located within even larger unresolved at 30” resolution. The the gaseous disk (see cover fi gure). HI envelopes, here called 2X- “fi sh” shaped radio continuum NGC 1512’s HI envelope is four HI disks, which provide the fuel emission is due to enhanced star- times larger than its optical size and for continued star formation. formation in the region between about twice as large as the stellar the two galaxies which corresponds extent measured from Malin’s deep Star formation activity to the tail of the fi sh. Using the optical image and from the GALEX radio-continuum fl ux, we derive a UV images. Furthermore, the We derive the ages of the UV-rich star formation rate (SFR) of 0.11 correspondence between regions of star clusters using the GALEX FUV and 0.012 MO yr-1 for NGC 1512 high H I column density and bright and NUV images and fi nd a color and NGC 1510, respectively. UV emission is excellent throughout gradient along the spiral arms and the extended disk of NGC 1512 other regions of the NGC 1512/1510 Notice that both the HI and the (apart from the central area which system, indicating that younger continuum images are similar to must be rich in molecular gas). The clusters are usually located closer to those that will be provided by the large majority of the observed UV the inner regions. We investigated Widefi eld ASKAP L-band Legacy All- -complexes lie in regions where if the UV-rich clusters do obey the sky Blind surveY (WALLABY) project the HI column density is above 2 Schmidt-Kennicutt scaling laws of using the Australian SKA Pathfi nder × 1021 atoms cm−2. Deep GALEX star formation (Kennicutt 1998) (ASKAP). The Evolutionary Map images of nearby galaxies show and found that generally only the of the Universe (EMU) project that the UV profi les of many spiral youngest UV clusters are associated using the ASKAP will provide even galaxies extend beyond their Hα with high HI column densities, while higher resolution (10”) images. in older UV clusters only diffuse HI or B25 optical radius (Thilker et al. 2005; Gil de Paz et al. 2005, 2007) gas is detected. This might suggest UV – HI comparison and it seems that these XUV- that as the hydrogen gas depleted, star formation stopped in the The combination of the large- disks exist in ~30% of the local latter regions. As a consequence scale HI distribution with deep spiral galaxy population (Zaritsky we expect to detect Hα emission optical and UV emission maps is & Christlein, 2007). We contend

30 ATNF News, Issue 67, October 2009 Figure 4: Relation between FUV-based SFR density and the HI gas density for UV-rich clusters in the NGC 1512/1510 system (symbols) and the galaxy M51 (black dots, from Kennicutt et al. 2007). The solid line is the best fi t to the M51 data (Kennicutt et al. 2007); the dashed line is the relation for whole galaxies derived by Kennicutt (1998).

in all high density HI regions or from this relation, suggesting a large Gil de Paz, A. et al. 2007, equivalent in all young UV clusters. amount of molecular gas is present. ApJ, 661, 115 Figure 4 shows the FUV-based Kennicutt, R.C. 1998, SFR density versus the gas density Conclusions ARA&A, 36, 189 for UV-rich clusters in the NGC We analysed the distribution and Kennicutt, R.C. et al. 2007, 1512/1510 system and in the nearby kinematics of the HI gas as well as ApJ, 671, 333 Sbc galaxy M 51 (Kennicutt et al. the star formation activity in the Koribalski, B.S. et al. 2007; for r <_ 8 kpc). Because galaxy pair NGC 1512/1510 and its 2004, AJ, 83, 764 no molecular data are currently surroundings. Our study supports available for NGC 1512, only the HI a scenario in which the interaction Koribalski, B.S., et al. 2008, in gas density is shown. The solid line between the BCD galaxy NGC Galaxies in the Local Volume, is the best fi t to the data obtained 1510 and the large spiral galaxy Sydney, 8–13 July 2007, by Kennicutt et al. (2007) in the NGC 1512 has triggered star eds. B.S. Koribalski & H. analysis of the independent star- formation activity in the outskirts Jerjen, Springer, p. 41 forming regions within M 51 and of the disk and enhanced the tidal Koribalski, B.S. & López-Sánchez, includes the molecular data, that distortion in the HI arms. The are found to be essential for the Á.R. 2009, MNRAS, in press system is probably in the fi rst stages (astro-ph:0908.4128) observed correlation. As we see, of a minor merger which started UV-rich clusters within the NGC ~400 Myr ago. The results of our Thilker, D.A. et al. 2005, 1512/1510 system generally agree study will be published in MNRAS ApJ, 619, L79 with the relation followed by the (Koribalski & López-Sánchez, 2009). Zaritsky D. & Christlein, D. star-forming regions within M 51 2007, AJ, 134, 135 and not with the whole galaxies. Regions within the inner star- References: forming ring of NGC 1512 (located Gil de Paz, A. et al. 2005, at r = 90´´) are signifi cantly offset ApJ, 627, 29

31 Exploring the Radio Bimodality of QSOs with CABB Elizabeth Mahony (University of Sydney / ATNF), Elaine Sadler (University of Sydney), Scott Croom (University of Sydney), Ron Ekers (ATNF), Ilana Feain (ATNF) and Tara Murphy (University of Sydney).

Quasars (QSOs) are often classifi ed into two broad categories; radio-loud and radio-quiet, but the underlying distribution of radio luminosity has long been debated in the literature. Using the new Compact Array Broadband Backend (CABB) we are observing a large sample of X-ray selected QSOs at high radio frequencies as a new way of tackling this issue.

Although the fi rst QSOs were and a relatively narrow range in cores, which is signifi cantly different discovered by their radio emission, optical magnitude. This introduces from what is seen in low frequency it was soon realised that the a strong and spurious correlation surveys (Murphy et al. 2009). majority are radio-quiet (Sandage between redshift and luminosity, In our program we selected QSOs 1965). Since then, there have been which in combination with the from the ROSAT ALL Sky Survey numerous studies of the radio rapid cosmic evolution of the QSO (RASS) Bright Source Catalogue luminosity distribution of QSOs population introduces selection (Voges et al. 1999) that were or Type 1 active galactic nuclei effects which greatly complicate observed as part of the 6dF (AGN). There are two opposing any interpretation of the data. Galaxy Survey (6dFGS; Jones et views on this issue. The fi rst is Here we report on an on-going al. 2009). Details of this catalogue that the distribution of radio- observing program to investigate are presented in Mahony et al. loudness is bimodal, i.e. there are the high frequency radio luminosity 2009. Sources were selected if the distinct radio-loud and radio-quiet distribution of QSOs with the 6dFGS spectrum exhibited broad populations, with 10-20% of QSOs Australia Telescope Compact emission features indicative of a being radio-loud (Kellermann et Array (ATCA). Earlier attempts QSO or Type 1 AGN. We also set al. 1989). The second is that there to investigate the radio luminosity a redshift cutoff of z<1 to minimise is a broad, continuous distribution distribution of QSOs generally any evolutionary effects. We then with no clear dividing line between used 1.4 GHz radio observations searched the AT20G survey for any radio-loud and radio-quiet (e.g. Cirosuolo et al. 2003, Jiang known 20 GHz radio sources which QSOs (Cirasuolo et al. 2003). et al. 2007) due to the fact that were excluded from our target list. Clarifying this issue would shed most large area radio surveys This leaves a fi nal sample of 1138 light on some of the intrinsic are carried out at this frequency. sources spread across all Right properties of nearby QSOs. A There are also a few at 5 GHz ascensions (RAs) in the southern bimodal distribution in radio (Kellermann et al. 1989, Stocke et sky. Example 6dFGS spectra and luminosities suggests that there are al. 1992) and 8 GHz (Hooper et corresponding 20 GHz observations two intrinsically different classes al. 1995, Goldschmidt et al. 1999). are shown in Figure 1. Since this is of QSOs, only one of which is By observing at 20 GHz we pick a large, low-redshift QSO sample able to become a strong radio up the central core component of which spans a wide range in optical source. Alternatively a continuous the AGN and hence see the most luminosity and is not strongly distribution suggests that all QSOs recent activity. At lower frequencies affected by evolution within the have low-luminosity radio sources the observed emission includes the sample volume, we believe that which become stronger during radio lobes, which could be relics of it can provide a defi nitive test of episodes of unusually high activity. past activity integrated over large whether the z<1 QSO population One reason why different studies timescales. It has been shown in is bimodal in its high frequency have produced contradictory the recent release of the Australia radio properties. Selecting sources results is that previous radio Telescope 20 GHz (AT20G) survey that have 6dFGS spectroscopic studies have used QSO samples that the 20 GHz source population information not only provides a which span a wide range in redshift is dominated by fl at spectrum uniform sample, but will also give

32 ATNF News, Issue 67, October 2009 Figure 1: Example RASS selected QSOs. The left image shows the 6dFGS spectrum. The arrows denote where spectral features would occur at that redshift, but not all of these are necessarily observed. On the right are the corresponding optical (B-band) images with 20 GHz contours. The top source appears in the AT20G survey with a fl ux of 665 mJy while the others were observed as part of this program. The middle source was observed in October 2008 (15.0 mJy) and the bottom source in April 2009 (5.27 mJy). In each of these images the contours represent the 20% – 90% levels in steps of 10%. us a wealth of extra information. MHz correlator on the Compact rms of 0.6 mJy. This run resulted in Hence we can also study the optical Array with central frequencies 15 (11%) detections at the 5 sigma spectral line properties, black hole of 18752 and 21056 MHz. To threshold. We then had another masses, multiwavelength properties obtain good-quality images with run in April 2009 shortly after the (X-ray — optical — radio) and high sensitivity, we used the H168 commissioning of the new Compact how these vary with redshift. confi guration. We observed a Array Broadband Backend (CABB). total of 135 sources for 80s (2 x Using the same confi guration and Our fi rst observing run was in 40 second cuts) which gave a fi nal exposure times we were able to October 2008, using the old 2x256

33 Figure 2: 20 GHz fl ux density against redshift for the RASS QSOs observed as part of this program. The dots are the sources that had matches in AT20G, pluses were those sources detected in the October 2008 run with the old correlator and crosses those detected in April 2009 with CABB. The triangles denote upper limits from the sources that weren’t detected in each of the October and April runs.

Figure 3: “Radio-loudness” distribution for the targets observed in October 2008 (Left) and with CABB in April 2009 (Right). The dashed histogram denotes the upper limits for the non- detections in each run and the dotted lines are the dividing lines between radio-loud and radio-quiet. AT20G detections are also included in both plots. With CABB we are starting to push down to smaller R parameters and further into the radio-quiet regime.

34 ATNF News, Issue 67, October 2009 Figure 4: RASS-6dFGS source g1231372-475802. The greyscale is a SuperCOSMOS B-band image with the 20 GHz emission overlaid in black and 843 MHz SUMSS source overlaid in grey. There are two components at 20 GHz, each with a peak fl ux of ~1.2 mJy (contour levels are at 0.4, 0.6, 0.8 and 1 mJy). One of these peaks is centred on the 6dFGS position, corresponding to the core of the nearby (z=0.28) AGN, while the other component is at the position of the SUMSS source which has a peak fl ux of ~40 mJy (contours are at 4 – 36 mJy in steps of 4 mJy). observe another 417 sources. The (in terms of observing time) we spectra we are free from the central frequencies were chosen do not, at present, have enough kinds of systematic effects which to be 19000 and 21000 MHz to data to conclusively say whether limited earlier work. The increased be consistent with the previous the distribution is bimodal or not. bandwidth of CABB also allows observations. By observing at 20 However, this fi gure shows that us to push down to fainter fl ux GHz we are able to take advantage with CABB we can push down to limits. As such, we will be able to of the full 2-GHz bandwidth and smaller R parameters and detect conclusively say whether the 20 reach an rms of 0.15 mJy. Setting more radio-quiet objects. GHz radio distribution of X-ray a 5 sigma detection threshold selected QSOs at redshifts less An example RASS QSO detected of 0.75 mJy revealed that 103 than 1 is bimodal or not, providing at 20 GHz is shown in Figure sources (25%) are detected at 20 new insights into the physical 4. This particular source clearly GHz. Figure 2 shows the current properties of nearby active galaxies. shows two 20 GHz components, detections of these sources from one aligned with the core of a both of these observing runs as nearby (z=0.028) Type 1 AGN References well as the small number of RASS (characterised as such due to the QSOs that have known 20 GHz Cirasuolo M. et al. 2003, broad emission lines observed in counterparts in the AT20G survey. MNRAS 346, 447 the 6dFGS spectrum). The other The horizontal lines marked refer component corresponds to a 40 Goldschmidt P. et al. to the detection limit of each set mJy Sydney University Molonglo 1999, ApJ 511, 612 of observations. This highlights the Sky Survey (SUMSS) sources, Hooper E. et al. 1995, ApJ 445, 62 increased sensitivity between the perhaps implying the presence of October and April runs achieved Jiang L. et al. 2007, ApJ 656, 680 a steep spectrum jet (α=-0.85). by the increased bandwidth Jones D. H. et al. 2009, with the upgrade to CABB. We plan to complete observations MNRAS, in press for the full sample during the To investigate any possible upcoming observing semester Kellermann K. et al. 1989, AJ 98, 1195 bimodality, Figure 3 shows the (weather permitting). This involves distribution in the R parameter. Mahony E. et al. 2009, observing the rest of the sample This is the ratio of radio to optical MNRAS, in press (586 objects) down to the detection luminosity, fi rst proposed by threshold of 0.75 mJy. Sources that Murphy T. et al. 2009, Kellermann et al. 1989 as a measure have not been detected to this limit MNRAS, submitted of “radio-loudness”. The dividing will then be re-observed, this time line between the radio-loud and Sandage A. et al. 1965, ApJ 141, 1560 for a total of 10 mins (2 x 5min radio-quiet regimes is generally cuts) reaching an rms of 85 µJy. Stocke J. et al. 1992, ApJ 396, 487 taken to be between 1 and 10, Voges W. et al. 1999, A&A 349, 389 denoted by the dotted lines. As the By selecting a large and well defi ned project is less than 20% complete sample of QSOs with homogeneous

35 National Facility Operations Graeme Carrad (ATNF)

Changes to experience in operations and Operations Staff engineering on the Combined Array for Research in Millimetre-wave A recruitment process for Astronomy (CARMA) project will three senior positions has been be invaluable as a transition is made successfully completed. This was to accommodate ASKAP operations. prompted by the departure of It is anticipated he will begin on the Brett Dawson, Head of Engineering fi rst working day of 2010. In the Operations / Parkes Site Manager, meantime Graeme Carrad is the and the stepping down of David acting Operations Theme Leader. McConnell from the Assistant Erik Lensson. Credit: CSIRO Director of Operations. The role Operations undertaken by Brett Dawson was of a scale better served by two The installation of the Compact NASA Deep Space Station after people and, in July, we welcomed Array Broadband Backend (CABB) the commissioning of the 7-mm Erik Lensson to the position of hardware and its commissioning receiver system. A recertifi cation Head of Engineering Operations was certainly not the end of the process is required after major and Malcolm Smith to the position story for CABB. It is inconceivable changes to the facility and CABB of Site Manager, Parkes. Malcolm that such a complex piece of certainly qualifi es as a major had been acting Site Manager instrumentation could be expected change. To attain recertifi cation, since Brett’s departure and is to operate fl awlessly from “day the array is required to complete well known at Parkes. The Site one” and effort continues to bring four successive spacecraft tracks Manager role is to ensure the functionality to the system whilst to NASA specifi cations. These smooth day to day operation of ironing out little “bugs”. Provision of tests are now underway with the Parkes Observatory site. Erik zoom modes, specifi cally a 1 MHz tracking opportunities spaced (pictured) has a background in mode, is the current focus and is throughout the coming months. telecommunications and spectrum proving to be a signifi cant challenge. management. He comes to us from It is estimated that this capability Three Development Projects the Australian Communications will be available in a limited form by which support the automation and and Media Authority (ACMA) and the end of October with a more remote operation of Parkes, as well already has a great understanding comprehensive version in place as rationalising the Parkes receiver of the spectrum issues surrounding by year’s end. Experience gained suite, are currently undergoing our observations. Erik will be with the implementation of the signifi cant planning. Erik Lensson leading the 35 engineering and fi rst mode will lay the foundation takes the Project Leader role in technical staff responsible for for provision of further modes two of these and Tasso Tzioumis in engineering maintenance, operations with a consequent reduction in the other. The obvious similarities and upgrades for all ATNF radio development time. The system between the aims of these projects astronomy observatories. is being used to great effect in its and the aims of the Technologies current form and exciting results for Radio Astronomy theme Appointed but not yet “on deck” are being reported demonstrating based in Marsfi eld will lead to a is Douglas Bock who will take up the utility of the instrument. sharing of the resources between the role of Assistant Director of the themes. The determination Operations to lead the delivery The installation of CABB has of the timelines and priority of of the radio astronomy facilities direct implications for our NASA the projects will be the subject to astronomers from around tracking commitments. The of meetings through October. the world. Douglas’s previous ATCA gained certifi cation as a

36 ATNF News, Issue 67, October 2009 Time Assignment Information Phil Edwards and Jessica Chapman (ATNF)

The Time Assignment Committee Mopra observations will be correlated (TAC) met on 23 – 24 July to review at the software correlator Good progress is being made proposals for the 2009 October running on the Curtin University toward the implementation of semester. The July meeting was the of Technology supercomputer. a “fast mapping” mode with last with Andrew Hopkins (AAO) The software correlator is the Mopra telescope. Further serving as TAC chair. Andrew has capable of correlating the high testing will be made during been a thorough and dedicated TAC data rate observations at high October 2009: please consult chair and the ATNF thanks him for spectral resolution with arbitrary the Call for Proposals about the his efforts as Chair over the last two correlator integration times. expected availability of this mode years and his leadership and support for the 2010 April semester. Real-time e-VLBI observations for introducing changes to the TAC. are also offered, using the ATNF The next Call for Proposals will Parkes antennas connected together via be made on 16 November 2009 The Caltech Parkes Swinburne high-speed links and a version of with a deadline for the 2010 April Recorder Mark 2 (CPSR2), used the Swinburne software correlator semester on Tuesday, 15 December at the Parkes Observatory for running at Parkes, or on a new 2009. The semester will run from pulsar observations, is expected Curtin computer cluster installed at 1 April to 30 September 2010. to be phased out in 2010, once Narrabri. Data-rates on the e-VLBI the ATNF Parkes Swinburne system are limited to 512 Mbps Compact Array Recorder (APSR) baseband system from each antenna. Single baseline The Compact Array confi gurations is fully commissioned and has observations between Parkes and to be offered for this semester been run in parallel with CPSR2 ATCA are available at 1 Gbps. are 6A, 6C, 1.5D, 750C, EW352, for a six-month overlap period. Real-time eVLBI capabilities to the H214, H168 and H75. Array This new recorder uses the digital Hobart antenna are also available. confi gurations will only be scheduled fi lterbank, DFB3, as a front-end to Currently the data rates to Hobart if there is suffi cient demand. sample a single pair of inputs (two are limited to 128 Mbps or less polarisations, single frequency) of due to limited network speeds The recently installed Compact up to 1-GHz bandwidth and record to Tasmania. Users are invited to Array Broadband Backend (CABB) the baseband data at an aggregate propose shared-risk observations will ultimately offer several zoom rate of up to 8 Gbit/s. Proposers suitable for such real-time modes that provide high spectral are reminded that the standalone observations that include Hobart. resolution. The fi rst zoom mode will Wide Band Correlator and the be the CFB 1M–0.5k mode, available older fi lterbanks, DFB1 and DFB2, Tidbinbilla from approximately end-October are now effectively decommissioned A limited amount of time may be 2009. This has a bandwidth of 2 GHz — these may continue to be used available on the 70-m and 34-m with 2048 x 1-MHz channels, and an where their need is clearly justifi ed, antennas at Tidbinbilla for single- additional, optional zoom capability but maintenance and repair of dish use in the 2010 April semester, that provides for one to four spectra, these is now a low priority. as in previous semesters. As usual, each with 2048 spectral channels proposals may be submitted and across a bandwidth of 1 MHz. VLBI will remain in a pool for up to one For the latest information on The Long Baseline Array (LBA) uses year. Any available time will be available zoom modes for the a disk-based recording system for used in a service observing mode. 2010 April semester, please all recorded VLBI observations and see the web links provided very high data rates, up to 1 Gbps, with the Call for Proposals. can now be achieved. All recorded

37 Changes to the ATNF Time Assignment Committee Jessica Chapman (ATNF), Andrew Hopkins (AAO), Arkadi Kosmynin (ATNF) and Phil Edwards (ATNF)

Each semester the ATNF Time a small number of individuals, to automated algorithm is then used to Assignment Committee (TAC) have suffi cient expertise to cover solve a “combinatorial assignment reviews the proposals submitted all of the many areas of scientifi c problem”: in this case, to assign through OPAL for observing time research discussed in proposals. a set of proposals to a team of with the Australia Telescope Looking ahead, from late 2012 the reviewers. This algorithm belongs Compact Array (ATCA), the Parkes ATNF TAC will also review ASKAP to a class of algorithms known as radio telescope, the Mopra radio Guest Science Proposals and it was “greedy” that do not guarantee telescopes and the Long Baseline hard to see how this extra workload fi nding the optimal solution, but Array. Service proposals for the could be managed without some instead produce acceptable, Tidbinbilla 70-m antenna are also changes to the TAC processes. though possibly less-than-optimal assessed. Time is allocated on the solutions, in reasonable time. To address these issues, and basis of scientifi c merit. Typically after consulting with the user Each proposal is assigned to at least 140 proposals are received for community, several changes have one TAC member and two TAC the summer semester, while 200 recently been introduced to the readers. Prior to a TAC meeting, proposals are received for the ATNF TAC processes. A summary each member and reader provides winter semester when observations of TAC operations is as follows: pre-grades and comments for a at millimetre wavelengths are subset of the proposals. The TAC optimal. The TAC has eight The eight TAC members meetings are held twice a year and members, appointed by the ATNF are supported by a group of include a discussion on the scientifi c Steering Committee, who meet in approximately 16 TAC “readers” merits of each proposal as well Sydney each semester to review the who are appointed by the ATNF as any technical issues that may proposals. The meetings are also Director, usually for a term of three arise. The TAC member assigned attended by the Head of Science years, drawing in astronomers from to a proposal is responsible for Operations (Phil Edwards) and Australian and overseas institutions. compiling the fi nal comment that is the Operations Research Program The readers do not attend meetings sent back to the proposers, based Leader (Jessica Chapman). Technical but send their grades and comments on the information provided prior assessments are provided by ATNF on a subset of the proposals as to the meeting, together with any staff including Phil Edwards. input to the meetings. Unlike the additional information discussed at TAC members, who have full access The TAC processes have evolved the meeting. Shortly after the TAC to all proposals, the TAC readers since National Facility operations meeting is held, an email with the have access only to the subset began in 1990 and have generally TAC comment and grade is sent of proposals that they review. worked well. However, the to the principal investigator and number of proposals received has The TAC members and readers are all co-authors for each proposal. signifi cantly increased over the last assigned on a proposal-by-proposal To support the changes to the TAC, fi ve years and the work load on basis. Proposals are assigned using in particular to coordinate the input individual TAC members became a scheme that makes use of science received prior to and during TAC very high, with each TAC member keywords. The cover sheets of meetings, and to control access asked to provide proposal grades for ATNF proposals now ask proposers permissions for different groups, around 80 proposals per cycle, and to select one or more options several software tools have been detailed comments on a subset of from a list of 14 science keywords added into the ATNF proposal these. A further concern has been that best describe their proposals. applications system, OPAL. that, although the TAC members The TAC members and readers are selected to cover a broad range identify their areas of expertise The changes to the TAC were of expertise, it can be diffi cult for from the same set of keywords. An introduced in July 2009 for the

38 ATNF News, Issue 67, October 2009 ATNF Publications List

2009 OCT semester. The proposal Publication lists for papers which *BAINS, I., BREEN, S.L., BURTON, M.G. et al. “Recent science from Australian reviewing and the TAC meeting ran include ATNF data or ATNF large-scale millimetre mapping projects: smoothly. It was much appreciated authors are available on the proceedings from a Swinburne University at the ATNF that all reviewers Web at www.atnf.csiro.au/rsearch/ workshop”. PASA, 26, 110-120 (2009). submitted their reports (almost) on publications. Please email any *BAINS, I., COHEN, M., CHAPMAN, J.M., DEACON, R.M. & REDMAN, M.P. time! The TAC members responded updates or corrections to this list “Revealing the transition from post-AGB very positively to the changes and, to [email protected]. stars to planetary nebulae: non-thermal not surprisingly, prefer having a and thermal radio continuum observations”. MNRAS, 397, 1386-1401 (2009). smaller number of proposals to This list includes published refereed papers compiled since the April BLISS, A.F., WORRALL, D.M., review. Following the experience BIRKINSHAW, M., MURRAY, S.S. & gained at this meeting some further 2009 newsletter. Papers which TANANBAUM, H. “Unmasking the active software improvements have include one or more ATNF staff galactic nucleus in PKS J2310-437”. ApJ, 698, 1061-1067 [2009]. been implemented in OPAL, in are indicated by an asterisk. *BOUCHARD, A., DA COSTA, G.S. & particular to improve the proposal JERJEN, H. “The environmental infl uence on *ABDO, A.A. ,..., EDWARDS, P.G. et al. the evolution of local galaxies”. AJ, 137 3038 assignments tool. These are being “Fermi/Large Area Telescope discovery of (2009). tested now for use with the next gamma-ray emission from the fl at-spectrum proposal cycle. The TAC greatly radio PKS 1454-354”. ApJ, 697, 934- *BRAUN, R., THILKER, D.A., WALTERBOS, 941 (2009) R. & CORBELLI, E. “A wide-fi eld high- appreciates the ability to manage resolution H I mosaic of Messier 31. I. *ABDO, A.A., .... HOBBS, G., .... Opaque atomic gas and star formation rate the whole process on-line, from JOHNSTON, S., .... KEITH, M., .... density”. ApJ, 695, 937-953 (2009) initial grades and comments, MANCHESTER, R.N., .... WELTEVREDE, P. et al. “Discovery of pulsations from the BRYANT, J.J., BRODERICK, J.W., through revisions during the pulsar J0205+6449 in SNR 3C 58 with the JOHNSTON, H.M., HUNSTEAD, R.W., TAC meeting, to the generation Fermi Gamma-Ray Space Telescope”. ApJ, GAENSLER, B.M & DE BREUCK, C. “A of the fi nal comments, as well 699, L102-L107 (2009). new search for distant radio galaxies in the Southern hemisphere. II. 2.2 um imaging”, *ABDO, A.A. ..., HOBBS, G. ..., as on-line access to electronic MNRAS, 394, 2197-2222 (2009). JOHNSTON, S. ...., MANCHESTER, R.N. ...., versions of the proposals. Theise WELTEVREDE, P. et al. “Fermi Large Area *BUDDING, E., ERDEM, A., INNIS, features streamlines and simplifyies Telescope observations of the Vela pulsar’”. J.L., OLAH, K. & SLEE, O.B. “Recent the process of proposal review ApJ, 696, 1084-1093 (2009) observations of AB Dor and interpretation”. Astron. Nachr., 330, 358-365 (2009). immensely. With continued *ABDO, A.A. ..., HOBBS, G. ..., JOHNSTON, S. ...., MANCHESTER, R.N. *BURKE-SPOLAOR, S., EKERS, R.D., improvements and innovations, ...., WELTEVREDE, P. et al. “A population of MASSARDI, M., MURPHY, T., PARTRIDGE, the ATNF TAC, through OPAL, gamma-ray millisecond pulsars seen with the B., RICCI, R. & SADLER, E.M. “Wide-fi eld can effi ciently manage the growing Fermi Large Area Telescope”. Science, 325, imaging and polarimetry for the biggest 848-852 (2009) and brightest in the 20-GHz southern sky”. number of proposals for existing MNRAS, 395, 504-517 (2009) *ABDO, A.A. ,..., JOHNSTON, S., ..., facilities as well as incorporating HOBBS, G., KEITH, M., MANCHESTER, *CAMILO, F., NG, C.Y., GAENSLER, ASKAP proposals in the future. R.N. & WELTEVREDE, P. “Discovery of B.M., RANSOM, S.M., CHATTERJEE, S., pulsed g-rays from the young radio pulsar REYNOLDS, J. & SARKISSIAN, J. “Out of the J1028-5819 with the Fermi Large Area frying pan: a young pulsar with a long radio Telescope”. ApJ, 695, L72-L77 (2009) trail emerging from SNR G315.9-0.0”. ApJ, 703, L55-L58 (2009). *ABDO, A.A. ,..., JOHNSTON, S., ..., MANCHESTER, R.N., ..., WELTEVREDE, *CASWELL, J.L , KRAMER, B. H. & P. et al. “Pulsed gamma-rays from PSR REYNOLDS, J.E. “Maser maps and magnetic J2021+3651 with the Fermi Large Area fi eld of OH 300.969+1.147”. MNRAS, 398, Telescope”. ApJ, 700, 1059-1066 (2009) 528-534 (2009). *ARCHIBALD, A.M., STAIRS, I.H., ... , *CERSOSIMO, J.C., MADER, S., FIGUEROA, CHAMPION, D.J. et al. “A radio pulsar/X-ray N. S. et al. “Warped ionized hydrogen in the binary link”. Science, 324, 1411-1414 (2009). Galaxy”. ApJ, 699, 469-477 (2009).

39 *CHEN, M.T., .... , KESTEVEN, M.J., ... , *FURUKAWA, N., DAWSON, J.R. et al. *JACOBY, B.A., BAILES, M., ORD, S.M., WILSON, W. et al. “AMiBA: broadband “Molecular clouds towards RCW49 and EDWARDS, R.T. & KULKARNI, S.R. “A heterodyne cosmic microwave background Westerlund 2: evidence for cluster formation large-area survey for radio pulsars at high interferometry”. ApJ, 694, 1664-1669 (2009) triggered by cloud-cloud collision”. ApJ, 696, Galactic latitudes”. ApJ, 699, 2009-2016 L115-L119 (2009) (2009). *CORNWELL, T.J. “Hogbom’s CLEAN algorithm. Impact on astronomy and beyond. *GODFREY, L.E.H., BICKNELL, G.V., *JAMES, C.W., EKERS, R.D., ALVAREZ- Commentary on: Hogbom, J.A., 1974, A&AS, LOVELL, J.E.J., JAUNCEY, D.L. et al. “A MUNIZ, J., PROTHEROE, R.J., McFADDEN, 15, 417”. A&A, 500, 65-66 (2009). multiwavelength study of the high surface R.A., PHILLIPS, C.J. & ROBERTS, P. “Status brightness hot spot in PKS 1421-490”. 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40 ATNF News, Issue 67, October 2009 LYUBCHENKO, S. Yu. et al. “Search for PEN, U.-L., STAVELEY-SMITH, L., southern sample”. A&A, 502, 529-540 main-line OH emission toward high-latitude PETERSON, J. & CHANG, T.-C. “First (2009). IRAS sources in the southern hemisphere”. detection of cosmic structure in the 21-cm TULLY, R.B. et al. “The Extragalactic Astron. Reports, 53, 528-540 (2009). intensity fi eld”. MNRAS, 394 L6 (2009). Distance Database”. AJ, 138, 323-331 (2009). *MAO, M.Y., NORRIS, R.P., SHARP, R. & *PETROV, L., PHILLIPS, C. et al. “Use of the *UMETSU, K., .... , KESTEVEN, M.J., ... & LOVELL, J.E.J. “Cosmic evolution of radio Long Baseline Array in Australia for precise WILSON, W. “Mass and hot baryons in sources in ATLAS”. In: Starburst-AGN geodesy and absolute astrometry”. PASA, massive galaxy clusters from Subaru weak- Connection Conference, Shanghai, China, 26, 75-84 (2009) lensing and AMiBA Sunyaev-Zel’dovich effect 27-31 October , 2008, ASP Conf. 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41 Education and Outreach Rob Hollow (ATNF)

2009 has been a busy year for Conference for Australia Science Observatory in May. Featuring ATNF Education and Outreach. Teachers, at the NSW Science input from ATNF staff and PhD Teachers’ Association Annual students, Rob Hollow worked The International Year of Conference and in Geraldton with the writing team from the Astronomy has led to increased during National Science Week. Science Teachers’ Association of In addition, several ATNF staff NSW in developing the resource. demand for ATNF staff as have been active as part of the A copy of the book was provided speakers and involvement in Scientists in Schools program that free to every school in Australia many other events and programs. has included giving talks to students and every science teacher who is a and supporting viewing nights. member of their state association. Teacher Workshops ATNF staff also contributed to the National Science Week concept and development of the and School Events ATNF staff at Narrabri conducted Big Aussie Star Hunt, the National ATNF’s Education Offi cer, Rob a series of well-attended public Project for this year organised by the Hollow, has run teacher workshops events in town, including public ABC. The sky survey component across much of Australia over recent viewing nights with optical of the project saw over 1,200 months. This year’s Astronomy telescopes. Professor Ray Norris observations on sky brightness from the Ground Up, an annual was involved in many events in logged from people across Australia. three-day event at Parkes was Darwin as part of the Tope End a great success in May. Over 25 Science Festival. Rob Hollow was Window to the teachers, some from as far afi eld active in the Mid West region of Universe as Exeter in Tasmania, Townsville Western Australia with talks to and Geraldton participated. Many students at Nagle Catholic College This is a new teaching resource ATNF staff gave up their weekend and Meekatharra School of the Air, providing over 20 lessons to give talks and to help run the teacher professional development on astronomy, optics, the sessions. Collaborations with other for Geraldton teachers, a viewing electromagnetic spectrum and organisations also continue to grow, night for students from Yalgoo Australian science for students in allowing more teachers across Primary School, Pia Wadjarri Years 9 and 10 within the context Australia to undertake professional Remote Community School and of the SKA. It was developed as development in astronomy Sandstone Public School at Yalgoo part of the Questacon-Scitech education. Workshops were held and a pre-performance talk about SKA Education project by an at Scienceworks in Melbourne in the life and science of Galileo experienced team of science collaboration with the Victorian at Theatre Eight’s production teachers from the Science Space Science Education Centre, of Brecht’s The Life of Galileo. Teachers Association of NSW and in Perth as part of Astronomy coordinated by Rob Hollow from WA’s Space Camp and in Brisbane This year’s resource book; CSIRO Australia Telescope National and Townsville. Shorter sessions Astronomy: Science Without Limits Facility. Copies are available free were also held in Launceston for National Science Week was to all high schools in Australia. at CONASTA, the National launched at Mount Stromlo

42 ATNF News, Issue 67, October 2009 Staff from CSIRO work with students at Strathmore Secondary College who are remotely operating the Parkes Telescope. CSIRO’s Robert Hollow and students Katie Pearce and Elizabeth Pollard pictured. Credit: David Crosling

PULSE@Parkes This innovative ATNF program has observations were made using had monthly observing sessions twitter (@PULSEatParkes). This with students from many high experiment was a great success schools across NSW. The fi rst and will now be incorporated into run in Victoria was held at the all future observing runs, allowing Victorian Space Science Education people around the world to read Centre in August with students live updates and pose questions. The from four schools taking part. fi rst science paper from the project Another session with students from has been accepted for publication fi ve schools was held at SPICE in in PASA and an education Perth in September. As part of the paper is nearing completion. Melbourne session, broadcasting

43 For further information:

CSIRO Australia Telescope National Facility 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

One of the most often requested photos of the Compact Array, taken by John Masterson.