sign in sign up
<<
Home , CSIRO, Imai (star), Parkes Observatory

’s National Science Agency

Australia Telescope National Facility Annual Report 2019–20

Contents

Chair’s report 2 Director’s report 3 Management team 4 About us 5 Performance indicators 9 Science highlights 13 reports 19 29 Technology development 33 People and community 37 Appendices 45

A: Financial summary 46

B: Staff list 47

C: Demographic data 50

D: Committee membership 51

E: Postgraduate students 52

F: PhD theses 53

G: Observing programs 54

H: Publications 60

I: Abbreviations 72

CSIRO Australia Telescope National Facility

Annual Report 2019–20

ISSN 1038-9554

This is the report of the CSIRO Australia Telescope National Facility for the period 1 July 2019 to 30 June 2020 and is approved by its Steering Committee.

Editor: Nic Svenson

Science highlights: Helen Sim

Cover: The Parkes telescope with the and the surface of the Moon. Images: Alex Cherney and NASA.

Inside cover: steps onto the lunar surface, as received by the Parkes . Image: NASA. Chair’s report

The Australia Telescope National The mid-term review and the ATSC Facility Steering Committee (ATSC) also both made recommendations met twice this . By our May 2020 highlighting the importance of Prof David Skellern, Chair, ATNF Steering meeting, COVID-19 constraints were instrumentation development. We Committee. Photo: John Sarkissian. in full force and we met virtually, hold that the ATNF’s not in Perth as had been planned. engineering and computing group investment in ASKAP and potentially is of long-term value to CSIRO. Its provide the global astronomy While we didn’t get to see the work sustains and advances the community with cost effective remarkable Australian Square nation’s science in astronomy, and commercial solutions for radio Kilometre Array Pathfinder (ASKAP), it demonstrably adds value to other interference mitigation. we were impressed mightily by the telescopes around the world. But it also results coming from it. The images adds value to Australia’s growing space Another commercial activity endorsed from the Rapid ASKAP Continuum sector (where ATNF know-how is being this year is that of a small team Survey (RACS) are beautiful, while the applied) and it could be better utilised undertaking a feasibility study of latest news from the in support of advanced manufacturing, potential near horizon business (FRB) team is truly extraordinary (see computing, big data, and models that leverage the telescopes Science highlights) and the critically telecommunications, the latter notably and other infrastructure of the ATNF. important ASKAP pilot survey in software defined radio engineering. While opportunistic commercial use program has provided more than Ensuring an appropriately skilled has occurred in the past, the team is just hints of how impressive full-scale workforce is vital to Australia’s future taking a more structured approach to surveys will be. A fully functioning industries. While the ATNF is playing its the sale of telescope time, scoping in ASKAP and transition to the era of part in ensuring that Australia’s future areas such as future Lunar missions, the Square Kilometre Array (SKA) engineering, computing and data deep space missions, space situational are clearly, and rightly, the ATNF’s analytics professionals acquire high awareness (including asteroid top priorities. level occupational skills, we believe tracking), education and tourism. We were this year presented with there is untapped potential here. We continue our strong endorsement a science case for the Australia After a year of rigorous market of the ATNF’s plans to increase Telescope Compact Array (ATCA). analysis and thorough consultation gender diversity, particularly in The ATNF, and facilities around the with industry, the ATSC was this the engineering disciplines. The world, are being asked to keep aging year presented with a plan that appointment this year of the instruments operational longer would see technology developed first , CSIRO than expected. That is, until the SKA for ASKAP applied to the looming Astronomy and Space Science Women is online. We found the case for bottleneck in satellite communications. in Engineering Scholarship holder is ATCA operation until this time to be Development of the plan was led a welcome step. compelling, a position mirrored by by commercialisation specialist, On the operational front, the ATSC the Australian Academy of Science Dr Ilana Feain, whose position we National Committee for Astronomy’s appoints the ATNF Users’ Committee recommended be created, so it is (ATUC) and the Time Assignment mid-term review of its Decadal tremendously satisfying to see a solid Plan for Australian Astronomy. The Committee (TAC). We are grateful commercial that leverages for the connection to the community ATNF’s partners in the university ATNF technology laid out in detail. sector clearly feel the same way and provided by ATUC and of the diligence We wish Dr Feain every success in her of the TAC. were this year successful in securing efforts to get the plan funded. Apart Australian Research Council funding from solving a pressing problem for The ATSC is an advisory committee for an urgent and essential upgrade the satellite communication industry to the CSIRO Board. As such, of ATCA’s digital system that should and end users, the realisation of we commend this Annual see it through until at least 2025. this opportunity would provide a Report to the Board and to the clear demonstration of return on astronomy community.

2 Australia Telescope National Facility | Annual Report 2019–20 Director’s report

This year our newest telescope, Our innovative low frequency ASKAP, achieved a major milestone by ultra-wideband receiver has been completing a program of pilot surveys operating on Parkes for a year and Dr Douglas Bock, Director, ATNF. with the full 36-antenna array. Each is now requested by almost all Photo: Wheeler Studios. of the survey teams received around users. Parkes continued to support 100 hours of observing time to test the program These include using our high-speed and optimise their survey strategies. searching for ‘technosignatures’ digital processing expertise on The strong engagement of the wider (evidence of technology) beyond our small satellites, our antennas for ASKAP community throughout Solar System and to follow up space situational awareness and the pilot surveys was particularly discoveries made by China’s Five- our cutting-edge receivers for space important. hundred metre Aperture Spherical communications. Telescope (where our 19-beam The scientific highlight of the year receiver has been in operation for This year has been a challenging one. was again ASKAP fast radio burst some two ). The next major The summer was one of the hottest (FRB) detections. These flashes of receiver development for Parkes is a on record and catastrophic bushfires high intensity radio waves have now cryogenically cooled, next-generation, raged in the eastern states. While our been used to discover the missing phased array feed receiver, supported telescopes were largely unscathed, ‘ordinary’ matter of the Universe. by our university partners and the some staff lost property, and many Sadly, celebrations were cut short Australian Research Council (ARC). spent their holidays volunteering with with the death of one of the principal emergency services or community investigators: Jean-Pierre Macquart. Also with the support of the ARC and groups supporting them and the university partners, we commenced affected communities. Then came The Square Kilometre Array (SKA) a project to replace the Australia the COVID-19 pandemic. We took project made a major advance by Telescope Compact Array’s aging special precautions around our passing its Critical Design Reviews. digital signal processing ‘back end’ operations staff and telescope sites. We continued to prepare for with cutting-edge digital technology As a consequence, and because construction and commenced work as developed in our Technologies for the virus did not spread in regional the Site Entity, delivering Australia’s Radio Astronomy program. Along Australia, we were able to maintain obligations under the SKA Convention with increased bandwidth and greater operations. The stresses of these (treaty). South Africa became the first observing flexibility, this technology strange times have been felt by all of SKA host nation to ratify the treaty: will allow active mitigation of radio us and I particularly wish to thank the it was also examined by Australia’s frequency interference, which is staff of the ATNF for their tolerance, parliamentary Joint Standing an important area of research as perseverance and for the support that Committee on Treaties, which interference continues to increase. they have provided one another. supported ratification in Australia. The planned partnership between Alongside growth in Australia’s space My thanks to the ATSC, ATUC, TAC, and CSIRO and the SKA Observatory to industry, we started to explore new my management team, for their advice operate SKA in Australia is reflected applications for our technologies. and guidance over the year. in a memorandum of understanding negotiated during the year.

2019 marked the 50th anniversary of the Moon landing and we include here a feature on the role our Parkes radio telescope, and Australia’s space tracking facilities, played in the legendary broadcast. The anniversary was the occasion for a massive communications campaign, which captured 55.5 million views in Australia through mainstream media alone. We hope it will lead to a new wave of Australians taking up careers in science, Douglas Bock (second from left) with fellow Australians at the opening of the SKA technology, engineering and maths. Headquarters in Manchester. The ceremonial key is made from the original dish surface of the nearby . Image: SKAO.

3 Management team

ATNF Director and Director CSIRO Deputy Director ATNF Chief Scientist Astronomy and Space Science Sarah Pearce Elaine Sadler Douglas Bock

Program Director, SKA Program Director, Technologies Program Director, ATNF Science for Radio Astronomy Antony Schinckel Phil Edwards Tasso Tzioumis

Program Director, ATNF Chief Operating Officer Operations Kate Callaghan John Reynolds

4 Australia Telescope National Facility | Annual Report 2019–20 About us

The Australian Square Kilometre Array Pathfinder.

5 We operate world-class radio astronomy facilities for users from across Australia and around the world. We are global leaders in technology and research, exploiting the world’s premier radio quiet site. We attract and retain the best staff.

The Australia Telescope National Facility (ATNF) is operated by Australia’s national science agency, CSIRO (the Commonwealth Scientific and Industrial Research Organisation).

The ATNF comprises the: • Parkes radio telescope Murchison • Australia Telescope Compact Array Radio-astronomy (ATCA) Observatory • Australian Square Kilometre Array Geraldton Pathfinder (ASKAP) New Norcia Narrabri • combination of instruments forming Perth Parkes the Long Baseline Array (LBA) Sydney Tidbinbilla • associated research and development program1.

The ATNF is the major part of CSIRO Our major sites. Astronomy and Space Science (CASS), a Business Unit within CSIRO. NUMBER CASS also includes:  • NASA’s Deep Space Communication Complex (CDSCC)  at Tidbinbilla. We also manage Australian astronomers’ access  to CDSCC antennas. • The (ESA)  tracking station at New Norcia north of Perth.  • The CSIRO Centre for Earth Observation, which includes managing Australian researchers’ access to the              NovaSAR Earth observation satellite. Sta Papers • CSIRO’s Space Technology Future Science Platform. Figure 1: Total publications by staff over time.

ASKAP ATCA Parkes Radio Telescope Collecting area 36 x 12 m Collecting area 6 x 22 m Diameter 64 m Frequency range 0.7-1.8 GHz Frequency range 1-105 GHz Frequency range 0.7-26 GHz Bandwidth 288 MHz Bandwidth 4 GHz Bandwidths up to 1 GHz Field of view 30 deg2 Configurable antenna location

1 Our 22-m Mopra telescope near Coonabarabran is not offered as part of the ATNF.

6 Australia Telescope National Facility | Annual Report 2019–20

1 Our 22-m Mopra telescope near Coonabarabran is not offered as part of the ATNF. The Canberra Deep Space Communication Complex, operated by CSIRO Astronomy and Space Science. Image: CDSCC.

Operations In 2019, 132 papers using data from Mission ATNF telescopes were published The ATNF affords astronomers all To develop and operate world‑class in refereed journals. Overall, our over the world the opportunity to National Facilities in radio staff published 173 refereed papers, use its telescopes free of charge. astronomy. including those using data from other Access is based on the scientific merit facilities (Fig. 1). • Operate the ATNF as a financially of the proposed observing project. viable and user‑focused Australian astronomers have access to research facility for the many overseas facilities on the same Governance principle. benefit of the Australian and The Director of CASS is also the ATNF international communities. Telescope access can also be Director and is ultimately responsible • Play a key role in the purchased outside the merit allocation to the Minister for Industry, Science international Square Kilometre framework. We have such agreements and Technology via the CSIRO Array (SKA) project, covering with, for example, the Breakthrough Executive and the CSIRO Board. in-country operations, Prize Foundation and the National The CSIRO Board appoints the science leadership and Astronomical of China. technology development. ATNF Steering Committee (ATSC) which provides high-level advice • Deliver world-class science Twice a year a call for observing to the Director, and CSIRO, on the through exploitation of proposals is made to the international ongoing delivery of radio astronomy our southern location and astronomical community. In recent capabilities for the nation. technological advantages. years about 100 observing proposals have been received each semester, • Develop, apply and The ATSC appoints the ATNF Users representing over 500 astronomers. commercialise our innovative Committee (ATUC), which represents The largest number of proposers are technologies and big data the interests of astronomers who affiliated with Australian institutions. processing techniques. use ATNF telescopes, and the Time Beyond Australia, the countries with Assignment Committee (TAC), • Foster a diverse and the largest numbers of proposers are which reviews observing proposals. creative workforce. the USA, UK, Germany and Italy. Committee membership is at Appendix D.

7 Staff and funding $ MILLION  The ATNF received $35.7m in funding from CSIRO: $1.8m for  capital expenditure and $33.9m for operations (including overheads but  not depreciation of assets). This is  supplemented with $16.6m from external sources, such as sale of  receivers and telescope time and funding for our SKA work (Fig. 2).  Also included is $1.5m for ASKAP operations from the National  Collaborative Research Infrastructure –– –  – –– – Strategy, administered by Astronomy CSIRO External Australia Limited. A financial summary Figure 2: Funding by source over time. appears in Appendix A.

As at 30 June 2020, CSIRO employed NUMBER 191 people on activities related to  radio astronomy around Australia  (Fig. 3). The list of staff is at Appendix B.   Traditional owners  We acknowledge the Traditional  Owners of the land of all our sites and  pay our respects to their Elders past, present and future:                

• Marsfield, Sydney, Wallamuttagil Sydney Narrabri Parkes Perth Geraldton/MRO people of the Gurringai nation Figure 3: ATNF staff by site over time. • Paul Wild Observatory, Narrabri, Gomeroi • , Wiradjuri • Mopra, Coonabarabran, Gamilaroi • CDSCC, Ngunnawal and Ngambri • Kensington, Perth, Whadjuk people of the Noongar nation • Geraldton, Nhanhangardi, Amangu, Wilunyu and Naaguja • Murchison Radio-astronomy Observatory and Boolardy Station, Wajarri Yamatji

This year CSIRO had plaques acknowledging the traditional owners installed in a prominent position at all our sites.

WA Senators Slade Brockman and Matt O’Sullivan visit the MRO. Image: Jesse Wotton.

8 Australia Telescope National Facility | Annual Report 2019–20 Performance indicators

The Australia Telescope Compact Array.

9 Telescope usage

Over the two observing semesters covered by this Report 213 observing proposals were received: 113 for the April to September 2019 semester and 100 for October 2019 to March 2020.

The oversubscription rate (the factor Massive dust storms by which proposals exceed available swept the central telescope time) was 1.2 for the Parkes west of New South radio telescope and 1.7 for ATCA (after Wales in January 2020. Wind gusts peaked at excluding allocations for ATCA Legacy 84 kilometres per hour Projects) and 1.4 for the Long Baseline on edge. Array (LBA). Image: Parkes Observatory webcam. In this reporting period, observing proposals were received from As ASKAP commenced astronomy In addition, the ATNF handles 762 individual researchers from operations, the ATSC agreed that the proposals requesting service 34 countries. ATNF staff led 17% of fraction of time successfully used for observations with the 70-m and these proposals, 27% were led by staff observing be 30% in 2019/20, rising 34-m antennas of the CDSCC, which of other Australian institutions and 10% per year to be 70% in 2023/24. are available under the Host Country 57% by overseas researchers. The fraction of scheduled observing agreement. In this reporting period, time lost due to equipment failure is to 113 hours were used for observing On both ATCA and Parkes, up to be no more than 5% across all years. under this agreement: 95 hours were 10% of time is made available as as part of the LBA. CDSCC antennas Director’s Time. This is time that is In this reporting period, time are increasingly used in partnership initially not allocated in the published successfully used for observing at with ATCA (and sometimes Parkes) version of the schedule, but which Parkes rose to 79%, while ATCA fell to to track near-Earth objects. Being can be made available later for 75% (Fig. 4). ATCA scheduled observing a communications station, CDSCC approved observing projects. In this time lost through equipment failure antennas transmit as well as receive. reporting period, Director’s Time has was stable, but Parkes saw a slight A signal is beamed at a passing been used for triggered NAPA (Non increase to 3%. Idle time at ATCA asteroid and the reflection is detected A Priori Assignable) and Target of rose slightly while Parkes, once by an ATNF telescope. This enables Opportunity proposals, makeup time again, bore the brunt of bad weather. physical properties of the asteroid to where proposals have lost time for ASKAP exceeded its first performance be inferred and for details of its orbit various reasons, extensions of existing targets, achieving 35% of time used for to be refined. projects, and small pilot studies or successful observing and only losing test observations. 2.6% of scheduled observing time due to equipment failure. The key performance goals for ATCA and Parkes are: PERCENTAGE % • at least 70% of telescope time be  successfully used for observing • no more than 5% of scheduled Idle time  observing time lost due Time lost to weather to equipment failure.  Time lost to ASKAP is now operating with all equipment failure 36 antennas and the first surveys are  complete. These Pilot Surveys were Maintenance/test time undertaken for each ASKAP Survey Science Project and were designed  Successful astronomy observations to incrementally test more aspects of telescope functionality and robustness  and build towards commencement of ATCA Parkes full-scale survey programs. Figure 4: Use of ATCA and Parkes in this reporting period.

10 Australia Telescope National Facility | Annual Report 2019–20 Time allocation

From 1 April 2019 to 31 March 2020, However, we are now starting to see has been for a greater proportion 91 proposals were allocated time on more ASKAP follow-up proposals of ATCA time to go to investigators ATCA or the Parkes radio telescope for time on ATCA. In this period, from Australian universities, at the (counting each proposal only once 14 proposals were allocated time on expense of overseas investigators, each even though a number were the LBA and 2 on CDSCC antennas. and for there to be a slight increase submitted in both semesters): Successful proposals are listed in in the proportion of Parkes time 43 proposals were given time on Appendix G. going to CSIRO investigators, at ATCA and 48 on Parkes. This number the expense of `other Australian’ has again decreased for ATCA most Time allocated to observing teams researchers. LBA experiments involved likely due to some large projects in using ATCA and Parkes (broken 17 unique principal investigators recent years, such as the four on-going down in different ways) is shown in (PIs), 6 of whom were affiliated with Figures 5-8 (where each year captures Legacy Projects (which take up ~35% an Australian institution. Australian of available observing time). To some the observing semesters that end collaborators were involved in 10 of extent, members of the Legacy Teams in that year, except for 2017 which the 12 experiments that were led by are tied up in those big projects, so captures October 2016 to March international PIs. are not submitting smaller proposals. 2018). The trend over the last six years

PERCENTAGE % PERCENTAGE %  

 

 

 

 

             

CASS/ATNF Other Australian Overseas CASS/ATNF Other Australian Overseas

Figure 5: ATCA time allocation by PI. Figure 6: Parkes time allocation by PI.

PERCENTAGE % PERCENTAGE %  

 

 

 

 

             

CASS/ATNF Other Australian Overseas CASS/ATNF Other Australian Overseas

Figure 7: ATCA time allocation by all investigators. Time Figure 8: Parkes time allocation by all investigators. Time allocated to each proposal has been divided evenly between allocated to each proposal has been divided evenly between all authors on the proposal. all authors on the proposal.

11 Publications

In 2019, 132 papers using data from ATNF PERCENTAGE % telescopes were published in refereed  journals. Of these, 65% included a CSIRO author or authors.  In 2019 there were 173 refereed publications by ATNF staff, including scientific papers with data from other facilities. In total, 219 refereed  journal papers and 18 conference papers – both those using National Facility data and other papers by our staff – were published  during the year. They are listed in Appendix H.

As anticipated, ASKAP publications have risen significantly in the last year with the results  of Early Science and the first Pilot Survey       observations now flowing through. ATCA First author CASS First author non-CASS Australian publications have dropped a little, which was First author overseas expected given the significant fraction of time devoted to the Legacy Projects in recent years. Figure 9: Publications that use data from ATNF telescopes by calendar year.

NUMBER OF PUBLICATIONS 







LBAMopraParkesCompact ArrayASKAP-related

     

Figure 10: Publications in refereed journals that include data from ATNF telescopes grouped by telescope. A few papers with data from more than one instrument are counted more than once.

NUMBER OF PUBLICATIONS 







      

LBA Mopra Parkes Compact Array ASKAP-related

Figure 11: Publications in refereed journals that include data from ATNF telescopes grouped by year. A few papers with data from more than one instrument are counted more than once.

12 Australia Telescope National Facility | Annual Report 2019–20 Science highlights

The centre of our Galaxy as seen with ASAKP in a single pointing using 28 antennas during early commissioning. It was processed using the ASKAPsoft automated pipeline. Image: Wasim Raja.

13 ATCA helps capture details of mysterious ‘cow’

Anna Ho Institute of Technology

ATCA and other telescopes have (at 5-34 GHz), the Smithsonian From their own observations, observed the first nearby example of Millimeter Array (215-351 GHz) and and those of others, Ho and her a new class of cosmic object: fast blue the Atacama Large Millimeter/ collaborators pieced together a optical transients, which first appeared (336‑671 GHz). picture of what had unfolded in in optical surveys. Their observations spanned 76 days. AT2018cow. Fast-moving ejecta from an explosion sped out into a dense In the last decade astronomers AT2018cow proved to be a remarkable shell of gas, giving rise to the radio started doing surveys that visited each radio source. Peaking at nearly emission. Slower ejecta, heated by a 41 target patch of sky once a night. This 10 ergs, it was far stronger at radio central source, expanded and emitted revealed transient sources previously wavelengths than even the most ultraviolet, optical and infrared missed, including highly luminous radio‑luminous supernovae. radiation. And within the dense ones that rose and fell in just a radio‑emitting shell, a black hole few days. Their wide range of observing frequencies let Ho and her or magnetar drove the generation These rapid transients appeared collaborators gauge the source’s of X-rays. in -forming galaxies, which spectral distribution (SED): So, what was AT2018cow? The most hinted that they might be unusual how the signal strength varies likely options are a , or a star supernovae (exploding ). But most with frequency. The distribution’s being ripped apart by a black hole (a examples were too far away (z > 0.1) shape implied that the millimetre/ tidal disruption event). The millimetre to observe in detail. And most were submillimetre emission was coming and radio observations point to the found in recorded data well after they from a shell of dense gas impacted by presence of high-density gas, which had faded, so they were not followed a shock wave from an explosion. favours a supernova. AT2018cow up with other observations. Because the observations stretched stood out from other fast transients In 2018 the ATLAS telescope in Hawaii over several weeks, the researchers because of its strong millimetre and spotted a source brightening rapidly at could look at how the SED changed submillimetre emission; however, other optical wavelengths. Officially named with time and measure or estimate its supernovae might appear just as bright AT2018cow (and quickly dubbed peak on different dates. The emission at millimetre wavelengths if observed ‘the cow’), it was clearly something peaked at relatively high frequencies, early in their development, Ho and her unusual: it reached peak brightness implying that the initial explosion was collaborators suggest. three to six times faster than very energetic and had taken place Ho, A.Y.Q.; Phinney, E.S.; Ravi, V.; et al. ordinary supernovae and it became inside dense gas. “AT2018cow: A Luminous Millimeter Transient.” ApJ, 871:73 (2019). 10‑100 times brighter. Its spectrum was not typical of a supernova. And no The spectrum of gamma-rays were seen, suggesting it AT2018cow at was not a gamma-ray burst either. three epochs (from Ho et al. 2019). AT2018cow lay in the galaxy CGCG The ATCA data at frequencies 137‑068, 196 million light-years below 40 GHz are (60 Mpc) away – close enough to study consistent with in detail. Soon at least two dozen an optically thick, or self-absorbed, major telescopes were trained on it. spectrum whereas at higher Most transient sources are hard to frequencies the detect at millimetre (short radio) spectrum becomes optically thin. wavelengths, being either too dim or fading within a day. But AT2018cow was still bright days after its discovery. Anna Ho (Caltech) and her collaborators were able to observe it at wavelengths from radio to submillimetre, using ATCA

14 Australia Telescope National Facility | Annual Report 2019–20 ASKAP finds the Universe’s missing matter

Jean-Pierre Macquart International Centre for Radio Astronomy Research,

By pinpointing the origins of fast radio the burst’s frequency dispersion, but estimates for the contributions bursts (FRBs), ASKAP has fulfilled a only the matter in intergalactic space associated with both our Galaxy and 20-year quest to locate most of the will contribute a distance-related the host galaxies. This gave them ‘ordinary’ matter (that is, not dark component. The further an FRB travels – the contribution from intergalactic matter) in the Universe. that is, the greater its – the baryons, DMcosmic. Then for each burst

more frequency dispersion it shows. they plotted DMcosmic against the host Stars and planets, gas and dust, trees galaxy’s redshift, z . and people – all are made of particles ASKAP began hunting for fast radio FRB called baryons, collectively known as bursts in 2017 as part of the CRAFT The points matched the relation baryonic matter. But the Universe is (Commensal Real-time ASKAP Fast predicted by theory. Macquart and his also home to the exotic dark matter Transients) survey, a project started by collaborators had found the missing and dark energy. And the dark stuff Jean-Pierre Macquart (ICRAR/Curtin baryons. The DMcosmic–zFRB relation dominates. In the 1990s cosmologists University) and then jointly led by has now been named the Macquart calculated that baryonic matter makes him, Keith Bannister (CSIRO), and Ryan relation. The Macquart relation has up less than 5% of the Universe’s mass. Shannon (Swinburne University of more to give. When they have many Technology). In 2018 the CRAFT team FRBs to work with, astronomers will be Astronomers then set out to look used ASKAP to both detect a single able to use it to constrain the density for all the baryonic matter. Yet, after FRB pulse and identify the galaxy it of baryons around both our Galaxy two decades, they’d found only half came from – the first time this had and the FRB host galaxies. of what was expected. The problem? been done. Less than a quarter of the Universe’s Jean-Pierre Macquart died baryons are in galaxies and galaxy By July 2019 the team had a number unexpectedly on 9 June 2020, 11 days clusters – places where they could of FRBs that had been traced to their after this work was published in be readily observed. The rest were host galaxies. Five were considered . He was one of Australia’s thought to lurk, chiefly in the form outstandingly good examples. leading theoretical astrophysicists of charged particles, in the space and his work on FRBs is a major part between galaxies. Macquart led an analysis of these of his legacy. bursts and others that had been Here they were hard to detect: all the localised to within an arcsecond. He Macquart, J.; Prochaska, J.X.; McQuinn, M; et al. “A census of baryons in the Universe existing techniques for finding them and collaborators took the bursts’ from localized fast radio bursts.” Nature 581, had limitations. What astronomers measured frequency dispersion 391‑395 (2020) needed was a new, comprehensive (abbreviated as DM) and subtracted tool. They got one, in the form of FRBs.

Discovered in Parkes data in 2007, FRBs are short, sharp spikes of radio energy. Most come from galaxies beyond ours, often at great distances. Bursts interact with all the charged particles they meet on their journey to Earth, which slows them down. The longer radio wavelengths in a burst are delayed most and arrive on Earth a little later than the shorter ones. This tell-tale sign is called frequency dispersion.

A burst can meet matter anywhere along on its path: in and around its galaxy of origin, in intergalactic space, and then in and around our The DMcosmic–redshift relation (Macquart relation) for localised FRBs. The solid

Galaxy. All this matter will increase line is the predicted relationship. The shaded region covers 90% of the DMcosmic values allowed by a model of galactic halos (from Macquart et al. 2020).

15 Parkes proves a spinning drags space-time

Vivek Venkatraman Krishnan Max Planck Institute for Radio Astronomy

Eighteen years of observations with Venkatraman Krishnan and his ‘spun up’ by mass transfer from the Parkes radio telescope have collaborators sought to establish its original companion. established that a fast-spinning white the sizes of these two effects. They dwarf star is dragging space-time measured the rate at which the With that evidence in hand, the in its vicinity around with it. It’s the pulsar’s orbital plane is tilting. But researchers ran simulations of how first time this effect has been seen there were key unknowns: two angles the system had evolved. These let in a system. in the geometry of the system and the them constrain the white dwarf’s white dwarf’s spin period. spin period even further, to less than PSR J1141–6545 is a radio pulsar with 200 seconds. a spin period of ~394 milliseconds. The researchers used Markov chain It orbits its companion star, a white Monte Carlo computations to obtain By measuring the relativistic effects dwarf, in just under five hours. The likelihood distributions for both in the PSR J1141–6545 system, system is one of only two pulsar‑white effects. For all allowed values of the Venkatraman Krishnan and his dwarf partnerships where the white two unknown angles, there was always collaborators have determined the dwarf is known to have formed a contribution from frame-dragging. masses of both the white dwarf and before the pulsar. This implies that Frame-dragging has been seen the pulsar; measured the inclination the system evolved in an unusual way, before – satellites have confirmed that of the pulsar’s orbit and its rate of with the white dwarf being ‘spun the spinning Earth creates it – but this change; put a upper limit on the white up’ by material transferred from is the first time it has been shown to dwarf’s spin period; and confirmed the its companion star before that star occur in a binary pulsar system. history of this remarkable system. exploded and created the pulsar. Bhat, N.D.R; Bailes, M.; and Verbiest, J.P.W. Using Bayesian statistics, the “Gravitational-radiation losses from the pulsar‑white-dwarf binary PSR J1141‑6545”. PSR J1141–6545 was discovered with researchers also inferred that the Phys. Rev. D 77, 124017 (2008) the Parkes telescope in 1999. An white dwarf takes no more than Venkatraman Krishnan, V.; Bailes, M.; van Straten, international team led by Swinburne 900 seconds (15 minutes) to spin W.; et al. “Lense-Thirring frame‑dragging induced by a fast-rotating white dwarf in a binary University of Technology has spent around. This is extraordinarily fast pulsar system”, Science, vol. 367, issue 6477, two decades recording the times its and confirms that this star was indeed pp. 577-580 (2020) pulses arrive on Earth, using both Parkes and, since 2015, the University The rapid rotation of the of Sydney’s UTMOST telescope. white dwarf companion This pulsar timing has been used to to PSR J1141–6545 induces relativistic (LT) measure the system’s characteristics and non-relativistic with exquisite accuracy. (QPM) spin-orbit interactions that cause In 2008 the researchers showed the pulsar’s orbit to precess (Ẋ). Panel B the pulsar’s orbit is shrinking (Bhat shows the constraints et al. 2008). Now a member of this on the white dwarf’s spin period and the research group, Vivek Venkatraman absolute ratio of the Krishnan (MPIfR), has led work two contributions. The which demonstrates that the plane contours define 68%, 95% and 99% likelihood of the orbit is also tilting (known as confidence intervals: the precessing). grey, dotted contours arise only from pulsar The changing tilt is being driven timing, while the red, solid ones also include mainly by the spin of the white constraints from binary dwarf through two effects. One is a evolution simulations. Newtonian (non-relativistic) effect, Panels A and C show the corresponding derived quadrupole spin-orbit coupling. The probability densities with other is a prediction of the general their 68% confidence theory of relativity: frame-dragging, intervals shaded (adapted from Venkatraman in which a spinning body drags nearby Krishnan et al. 2020). space-time around with it.

16 Australia Telescope National Facility | Annual Report 2019–20 ATCA sees star-making potential of little galaxy

Katherine Jameson Australian National University

A tiny galaxy that orbits ours has emission that combined Parkes and researchers calculated the fraction of turned out to be surprisingly rich in ATCA data. The ratio of absorption cold HI in the SMC to be ~20%, which cold atomic hydrogen, a phase gas to emission gives the average ‘spin is similar to that of the Milky Way goes through on its way to forming temperature’ (which tracks the gas’s (~15‑20%). stars. For a galaxy to make stars, it average physical temperature) of the must first cool and condense some of mixture of cold and warm gas along This work builds on an ATCA study its reservoir of atomic hydrogen gas the line of sight. of the SMC carried out in the 1990s (HI) into clouds of molecular hydrogen (Dickey et al. 2000). Upgrades done Each feature in the absorption spectra since then have given ATCA greater (H2). If these clouds collapse and compress the gas further, stars form. represents an individual cold HI cloud. sensitivity and velocity resolution. Taking them one by one, Jameson and As a result, Jameson and her In our galaxy, the Milky Way, the HI her collaborators plotted absorption collaborators detected absorption in is cooled mostly by elements such as as a function of emission and used three times as many sources, including oxygen and carbon in the interstellar the resulting plots to estimate the seven in which Dickey et al. had not medium, the gas between the clouds’ temperatures. The average seen absorption. stars. But what happens in galaxies temperature was ~30 K (-243 C), about where the interstellar medium is 10 degrees lower than that of cold Despite its very different chemical very different? A test case, the Small clouds in the Milky Way. composition, the SMC is as rich in Magellanic Cloud (SMC), orbits the cold HI clouds as the Milky Way. How Milky Way. The SMC is an irregular Strikingly, the temperatures of these the SMC has cooled this gas is still an dwarf galaxy and its interstellar clouds seem unrelated to their opacity, open question. their location in the SMC, or the medium is far less rich in oxygen and Dickey, J.M.; Mebold, U.; Stanimirovic, S.; and carbon than the Milky Way’s. To see amount of HI along the line of sight. Staveley-Smith, L. “Cold Atomic Gas in the Small The cold clouds seem to be peppered Magellanic Cloud”. ApJ, 536:756–772 (2000) how well the SMC cools HI, we need Jameson, K.E.; McClure-Griffiths, N.M; Liu, randomly throughout the warm gas. to determine what fraction of its gas is B.; et al. “An ATCA Survey of HI Absorption in The average spin temperature of the the Magellanic Clouds. I. HI Gas Temperature cold. The key tool for doing this is the Measurements in the Small Magellanic Cloud”. characteristic radio emission of HI, a SMC gas was 150 K. From this the ApJ Supplement Series, 244:7 (2019) spectral line with a wavelength 21 cm.

HI both emits this radiation and absorbs it: hot gas tends to emit while cool gas tends to absorb. To trace cold HI in a galaxy, astronomers look for regions absorbing 21‑cm emission from background radio sources (that is, galaxies behind the one being studied).

Katherine Jameson, an ANU postdoc at the time and now an ATNF Bolton Fellow, and her collaborators used ATCA to look for HI absorption across the SMC, detecting it against 37 of their 55 background sources. ATCA, with its high angular resolving power, is ideal for looking for the absorption signal because it’s not sensitive to the Spin temperatures measured with ATCA across the Small Magellanic Cloud. large-scale emission from the warm HI. The greyscale background shows HI density. Coloured circles represent average spin temperature along the line of sight (colour scale, bottom left): these temperatures are The researchers then compared generally low, suggesting a significant fraction of cold gas. The size of each circle shows their absorption measurements with the measurement’s signal-to-noise ratio. (From Jameson et al. 2019) previous measurements of SMC HI

17 LBA tracks a travelling trigger for masers

Ross Burns National Astronomical Observatory of Japan

The Long Baseline Array (LBA) has They observed twice, 26 days apart. as conditions favourable for making seen an expanding ring of radio The first round of observations used them propagated out from G358‑MM1. emission that may signal a young star Australian antennas (ATCA, Mopra and The travelling trigger for maser ‘feeding’. Stars grow in fits and starts. antennas at Ceduna and Hobart), plus formation was probably a ‘heatwave’ – A protostar is born in a disk of gas and others at Warkworth, New Zealand, a higher level of far-infrared radiation dust. Every so often the disk sheds and Hartebeesthoek, South Africa; that poured out of G358-MM1 after a clumps of gas that fall onto the infant the second round used the same clump of gas fell onto the young star. object, fattening it up. line-up but with Parkes instead of Hartebeesthoek. Two other high-mass protostars, Astronomers have known for decades S255IR-NIRS3 and NGC6334I-MM1, that some types of low-mass stars The maser emission lay roughly in have been seen to brighten rapidly, grow in this episodic way. But in the a ring, centred on a core detected apparently as the result of accretion. last few years they’ve realised high- at millimetre wavelengths. This But G358-MM1’s outburst differed from mass stars must too. Now they’re ring is probably the edge of a those events: it rose and fell faster looking for signs of the process – three‑dimensional shell surrounding and didn’t brighten at millimetre or known as variable accretion – at work. G358‑MM1. near‑infrared wavelengths.

Accretion is hard to spot directly but The ring swelled rapidly between High-resolution maser observations can be detected through its effect on the two observations, its radius of similar events will help show bright radio sources called masers. growing from 40 milliarcseconds to how diverse accretion bursts can These develop around a star in 77 in 26 days – that is, between 1 and be in high-mass stars. And studying regions of gas where the temperature 2 milliarcseconds per day. Given the examples of episodic accretion in our and density are just right and are source’s distance, this growth rate Galaxy will help us understand it in powered by the star’s radiation. Young corresponds to 4-8% of the speed of the early universe, where, modelling high‑mass stars are often signposted light. But methanol clouds can’t travel suggests, it was ubiquitous. by a particular kind of maser, one that fast. The researchers concluded Burns, R.A.; Sugiyama, K.; Hirota, T.; et al. created by methanol molecules and they were seeing masers being kindled “A heatwave of accretion energy traced by masers in the G358-MM1 high-mass maser emitting radio waves at 6.7 GHz. then quenched in an expanding shell, protostar.” Nature Astronomy, 4, 506-510 (2020).

In 2006 the Parkes radio telescope found a source of this 6.7-GHz emission, G358.93-0.03, lying 22 000 light-years (6.75 kpc) away in our Galaxy. In 2019 NOAJ’s Hitachi 32-m telescope north of Tokyo saw this source flaring: its 6.7-GHz emission jumping ninefold in less than two weeks.

Follow-up observations were made at several wavelengths. In the submillimetre, G358.93-0.03 was resolved into a cluster of several objects: the strongest, G358-MM1, was seen to brighten almost threefold. G358-MM1 looked to be a high-mass protostar undergoing accretion.

Ross Burns (NAOJ) and his collaborators used the LBA to study the 6.7 GHz maser emission around G358–MM1 at high resolution. Schematic illustration of the methanol masers observed in G358-MM1. (From Burns et al.)

18 Australia Telescope National Facility | Annual Report 2019–20 Observatory reports

The Parkes radio telescope tracks the Moon in rehearsal for the Apollo 11 landing. Image: ATNF Image Archive.

19 Australia Telescope Compact Array

Science highlights lightweight but strong material able to withstand harsh climatic conditions, • Following a rapid response trigger bird droppings, bird strike, and yet from a maser flare toward the be invisible to radio waves. After system G 358.931-0.030, ATCA much bench testing and prototyping, examined how several different the antennas now bear brand new species of maser emissions varied. Dyneema covers and sensors have Observations revealed three new been installed to detect if the covers Australia’s High Commissioner to torsionally-excited class II methanol South Africa, Ms Gita Kumath, visits come off. in September. Image Phil Edwards. maser transitions, which will enable significant improvements to models An exceptional feature of ATCA is of this class of masers and illustrates that five of its six antennas move Early in 2020 we and our university the importance of rapid response along railway tracks. Once in the partners were awarded an Australian (Breen et al. 2019 ApJ 876, L25). right position, the antenna is plugged Research Council grant to replace the Compact Array Broadband Backend, • Long-term ATCA observations of into the nearest station post, which the digital signal processing system the binary neutron-star merger GW provides power and data connectivity. that converts raw data from ATCA’s 170817, famous as the first observed After 30 years the electrics were in antennas into information astronomers electromagnetic counterpart to a need of attention and water ingress can use. CABB was one of the earliest gravitational-wave detection, led was noted in several stations. We broadband digital systems and a to the conclusion that the collision have overhauled stations on the world-leader when it was built 15 years produced a relativistic jet (Troja north‑south track and are now ago, but technology has moved on et al. 2019 MNRAS 489, 1919). working on the east-west track. and we can no longer source spare • ATCA was used to confirm the The buildings on site also got some parts. CSIRO will receive $530 000 discovery of a new gamma-ray attention this year. The control as part of the overall $2.6m project binary system 4FGL J1405.1-6119, building switchboard was replaced led by Western Sydney University which is likely to be an O-star and and a second uninterruptible power to develop a state-of-the-art system rapidly rotating pair. supply installed, lessening the chance based on modern signal processing (Corbet et al. 2019 ApJ 884, 93). of power failure to the screened room techniques and cutting‑edge software (housing such important systems as (see Technology development). This the correlator and timing equipment). will double the telescope’s bandwidth, GLASS, the GAMA Legacy ATCA The visitors centre was closed in March preparing ATCA for its next career: Southern Survey, is now complete in response to COVID-19, giving us the particularly in following up ASKAP after 3051 hours observing. It began in opportunity to renovate its interior. detections. October 2016. Of the three remaining Legacy Projects (which together are allocated roughly one-third of observing time), Imaging Galaxies Intergalactic and Nearby Environments (IMAGINE) will finish next.

Early in 2020, the Narrabri region welcomed the return of widespread rainfall, but the rain also revealed the sorry state of the weatherproof covers over the vertex rooms in each dish (these rooms sit directly under the dish surface and house the receivers). Covers were coming loose and were no longer watertight. With no spares, and the original material no longer available, the hunt was on to find a Repairing station posts. Image: Tim Wilson.

20 Australia Telescope National Facility | Annual Report 2019–20 Parkes radio telescope

Science highlights Observing projects have this year operational. But some days were transitioned to the new web-based simply too hot, and the telescope had • Publication of the 2.3 GHz (S-Band) control system, DHAGU (the Wiradjuri to be stowed. The region was also hit all sky polarisation survey with word for ‘where to?’), designed for by severe dust storms. Parkes, revealing magnetised the UWB-L, and new UWB-L modes structure across the southern sky, of operation have continued to There were no large maintenance including prominent depolarisation expand: for example, simultaneously shutdowns this year, but the telescope towards the inner Galaxy (Carretti observing in high spectral- and high jacks (which lift the moveable et al. 2019 MNRAS 489, 2330). time-resolution modes. We ran telescope structure much like a car • Discovery of five millisecond three training sessions for UWB-L jack) were extensively refurbished. in the Omega Centauri globular and DHAGU in March attracting This work is crucial to upcoming maintenance of the azimuth gearboxes cluster through a combination ~50 participants. These were to be of Parkes’ ultra-wideband in person but transitioned to online and other systems. receiver and ATCA observations in light of COVID-19. The transformation of the Parkes (Dai et al. 2020 ApJ 888:L18). With remote observing being the receiver fleet continues with • 40 new pulsars from the High norm, Parkes continued observing development of a cryogenically Time Resolution Universe through the months impacted cooled next-generation phased Pulsar Survey (Cameron et al. by COVID-19. Our education and array feed receiving funding from 2020 MNRAS 493 1063). outreach program, PULSE@Parkes also the Australian Research Council in continued, albeit online (see People early 2020. The full-size prototype is and community). COVID-19 presented under construction (see Technology 2019 was, of course, the Apollo 11 the opportunity of characterising the development). 50th Anniversary (see overleaf). This radio frequency interference (RFI) was further commemorated by the environment (because the visitors’ IEEE honouring Parkes with the centre was closed and there were first of its prestigious Milestones fewer aircraft). Led by George Hobbs, to be recognised in Australia. the team characterised signals within We are in the midst of a program to the UWB-L band and how they varied update the receiver suite of our 64-m with time and direction. These data steerable dish. The low frequency are being folded into our work on ultra-wideband receiver (UWB-L), active RFI mitigation (see Technology installed in 2018 (Hobbs et al. 2020 development). PASA 37, E012), is now enabling While Parkes weathered COVID-19, impactful science. Indeed, in the the hot, dry summer that preceded October 2019 semester, the astronomy the pandemic was a real challenge. community almost universally Days over 38oC required observing requested the UWB-L in its observing only in directions where the breeze proposals. could cool the dish and Site Leader, The Breakthrough Listen project Mal Smith, was driven to hose down maintained its regular observing the compressors to keep the telescope (~1700 hours across the year), completing its Galactic plane survey and targeted searches of nearby stars (e.g. Price et al. 2020 AJ 159, 86). This project has now largely transitioned to observing with the UWB-L and commenced a deep search of the Parkes is honoured with the first IEEE Galactic centre. Milestone to be made in Australia, for achievement of reception of the Apollo 11 TV and telemetry signals. On 11 October 2019, IEEE President Elect, Prof Toshio The jacks (blue) that lift the movable Fukuda, and IEEE History Committee part of the telescope structure were representative, Mr David Burger, unveiled overhauled this year. Image: Brett Preisig. the plaque. Image: John Sarkissian.

21 Parkes’ giant leap

At 12.56 pm on Monday, 21 July 1969, 600 million people Australia’s Postmaster General’s department established watched the first human step on the Moon through links and voice communication television signals received courtesy of Australian channels for Parkes. NASA provided radio astronomy and space tracking facilities. data recorders, equipment to convert incoming signals from the Moon into CSIRO’s Parkes radio telescope is In the original mission plan, the a television picture and the receiving designed to track galaxies and pulsars astronauts would land during the equipment. CSIRO designed and built and other astronomical objects across coverage period of NASA’s Goldstone the feed horns for the Parkes receivers the sky and its large collecting area tracking station in California, USA, to NASA specifications (see box). (the dish has a diameter of 64 m) gives at 6.17 am (AEST) with the moonwalk Some two months before launch NASA it great sensitivity. These capabilities occurring soon after landing. The changed the plan: the astronauts were also make Parkes ideal for tracking moon would not rise at Parkes until now required to rest for ten hours spacecraft. 1.02 pm (AEST), so Parkes would after landing. This meant the Moon be a backup in case of a delayed would have set for Goldstone before In late 1968, NASA requested the moonwalk. NASA’s tracking station the moonwalk began, but it would be involvement of Parkes in the upcoming at Honeysuckle Creek, near Canberra, high overhead at Parkes. Consequently, Apollo 11 mission to receive the faint Australia, would track the command Parkes’ role was upgraded from signals from the lunar module while module and co‑ordinate the other backup to prime receiving station it was on the surface of the Moon. Australian stations, during the for the historic moonwalk. moonwalk (see graphic).

Australia’s roles in the Apollo 11 Moon landing.

NASA facility at Carnarvon, WA Communicated with the Apollo spacecraft and received signals from scienti c experiments deployed during the moonwalk.

INTELSAT III ton Hous n to Pacic satellite en o ite th atell Apollo „„ TV i c s I Pac AT II broadcast sent TELS he IN Signal received from to t OTC Paddington and to the USA and ent sent toPaci c INTELSAT satellite III als s Sign then the world.

Overseas Telecommunications Commission Moree Earth Station

CSIRO radioheliograph at Culgoora, NSW Observed the Sun to warn of impending solar ‚ares, which could have killed the Parkes and Honeysuckle Creek sent their TV signals to the astronauts during the moonwalk. OTC Paddington Terminal

CSIRO Parkes radio telescope, NSW Overseas Telecommunications Tracked the lunar module, Eagle, on Commission (OTC) Paddington the Moon. Relayed TV broadcast. Terminal A NASA employee selected the best NASA facility at Tidbinbilla, ACT quality TV picture from the Parkes Tracked the command module, and Honeysuckle Creek signals. It Columbia, in lunar orbit. was then split with one feed sent via satellite to the rest of the world, while ABC distributed another feed NASA facility at Honeysuckle Creek, ACT to Australian networks. Australian Tracked the lunar module, Eagle, on the TV viewers saw the moonwalk rst, Moon. Received TV broadcast. by a fraction of a second.

22 Australia Telescope National Facility | Annual Report 2019–20 L to R: Neil ‘Fox’ Mason and Dennis Gill at the control desk. Fox drove the dish throughout the moonwalk but was not allowed to leave his post so did not see the famous event until the TV replay that evening. Image: ATNF Image Archive. The team watches the moonwalk on the small monitor in the Parkes control room. Image: ATNF Image Archive. Astronaut Michael Collins took this photo from the command module orbiting the Moon the day before the landing. Australia is in the top left of the globe and the storm gathering over the eastern seaboard is clearly visible. Image: NASA.

The television signals were to be sent had been brewing all morning and improvement in contrast as Armstrong from Parkes via the microwave links, chose that moment to hit, buffeting walks on the Moon. NASA stayed to the Overseas Telecommunications the dish with wind gusts of 110 km per with Parkes for the remainder of the Commission (OTC) terminal in Sydney. hour. The telescope tower shook, the 2.5-hour broadcast. The weather at From there the television signal would structure of the dish groaned, and the Parkes did not improve (there was be split: one split would go to the wind alarms sounded, but the team even a hailstorm) so the telescope was Australian Broadcasting Commission held its collective nerve – a scene operating well outside its safety limits. studios for Australian television made famous in the iconic Australian networks, the other went to the OTC movie, The Dish. The wind abated a While the visuals alternated between Earth Station at Moree for satellite little and, just as Buzz Aldrin switched Goldstone, Honeysuckle Creek, and transmission to NASA Mission Control on the TV camera mounted on the side Parkes (and it was Honeysuckle that in Houston, Texas, for international of the lunar module, Parkes picked caught Armstrong’s step onto the broadcast. up the signal using its less sensitive Moon), the audio signal, with those off‑axis feed. famous words ‘…one giant leap…’, In the weeks leading up to the launch, came through Goldstone. the team at Parkes installed and tested The Moon had not yet set at all of the receiving equipment, the Goldstone, so it too was able to pick microwave relays, and the tracking up the TV signal. The smaller 26-m Stalwart support procedures. They even practised antenna at Honeysuckle Creek could tip Based on the success of the Apollo hand-cranking the dish to follow the lower to the horizon than Parkes and 11 mission, Parkes was contracted spacecraft in case of a power failure. was also able to take the signal. For to support all subsequent Apollo the first few minutes NASA alternated manned lunar landing missions. We between the TV signals being received again stand ready, this time to support Tranquillity base… at Goldstone and Honeysuckle, NASA’s Artemis mission, named after Right on schedule (6.17 am AEST) on searching for the best TV picture to the twin sister of Apollo, which aims 21 July, astronauts and broadcast. Eight minutes in, the Moon to land the first woman, and the next Edwin (Buzz) Aldrin landed the lunar finally rose into the field of view of man, on the Moon. module, Eagle, on the surface of the Parkes’ main receiver. The signal was Moon at the Sea of Tranquillity with so much stronger that NASA switched John Sarkissian OAM Goldstone tracking. to Parkes – this can be seen on the Operations Scientist, Parkes Radio footage as a marked brightening and Observatory The schedule required the astronauts to rest before attempting the moonwalk, but Armstrong opted to Feed horn head out straight away – who could have slept at a moment like that! Two identical receivers were installed for the Apollo 11 Fortunately for the Australian team, it mission: one at the focus of the telescope (on-axis), the took the astronauts some time to don other offset a small distance (off-axis). The receivers were their spacesuits and depressurise the commercial units, but CSIRO’s Bruce Thomas designed lunar module, so the Moon was on the feed horns, which funnel the signals to the receiver the verge of rising over Parkes as they electronics. The horn for the on-axis receiver was a one opened the hatch. wavelength, two hybrid-mode corrugated horn – the first of its kind. The horn for the off-axis receiver had a Down on Earth, the massive Parkes smooth circular cross-section with a flared tapered aperture and a corrugation dish was tipped right over – almost surrounding the aperture. The corrugations increased the sensitivity and touching the ground – to receive the bandwidth of the receivers and was one reason Parkes performed so well. signals as soon as the Moon rose high The corrugated feed horns of the Lunar receivers visible on the underside of Parkes’ enough above the horizon. But a storm focus cabin. Image: ATNF Image Archive.

23 Australian Square Kilometre Array Pathfinder

Science highlights ASKAP, our newest telescope The ASKAP community has rallied of 36 12-m dishes, concluded its around the pilot surveys as a source of • The growing number of fast radio first pilot surveys on 14 May 2020 scientific discovery and an example of bursts localised with ASKAP has seen after 304 days. Observing of the telescope’s workflow – full-scale them used as cosmological probes ~100 hours was done for each of science quality data flowed through (see Science highlights), including to EMU, WALLABY, POSSUM, DINGO, to the archive for the first time. investigate the properties of galaxies CRAFT, VAST, GASKAP, FLASH and Communication with our diverse and they pass through (Prochaska LIGO. The goal was to verify that distributed community remains key et al.2019 Science 366, 231). ASKAP can meet the science data to achieving mutual goals. Channels • ASKAP is now a crucial follow‑up quality requirements of each team. such as the monthly science forum instrument to detections Translating these requirements into and newsletter complement events from the Interferometer observing modes was a joint effort organised by the survey science Gravitational‑wave Observatory between the observatory and the teams. Weekly workshops bring (LIGO). Repeated observations teams, with iteration over the survey together groups with similar interests were made of the field surrounding strategies, telescope configuration and large-scale workshops are held LIGO event S190814bv and one and processing parameters. The to plan major activities, such as the candidate radio counterpart was Pawsey Supercomputing Centre second phase of pilot surveys. Project found, but further observations provided additional data storage, scientists nominated by each survey ruled out any association with which proved instrumental in science team take an active role in all the event completing the pilot surveys. Data these events, providing a common (Dobie et al. 2019 ApJL 887:L13). processing is proceeding well point of contact with observatory • ASKAP’s polarisation capabilities (see Data archives) and roughly a staff. were used to detect periodic dozen papers are in preparation. transient emission from active dwarf star UV Ceti (Zic et al. 2019 MNRAS 488, 559), confirming that auroral activity can occur in M-dwarf stars. • A new pulsar (PSR J1431-6328) was serendipitously discovered in ASKAP data (Kaplan et al. 2019 ApJ 884:96). Detected as a highly polarised, steep-spectrum continuum source during test observations, follow-up with Parkes found pulses of 2.77 milliseconds. This rapid spin rate makes the pulsar difficult to detect in traditional pulsar searches and indicates

ASKAP’s potential in this field. A typical RACS image (middle, σ = 235 µJy) compared to the previous best surveys: Sydney University Molonglo Sky Survey (SUMSS, left. σ = 1.5mJy) and the NRAO VLA Sky Survey (NVSS, right. σ = 530 µJy). Each box is one degree wide. RACS clearly has superior sensitivity and resolution, meeting our goal of making it the new benchmark in radio continuum surveys around 1 GHz. Image: Dave McConnell.

24 Australia Telescope National Facility | Annual Report 2019–20 ASKAP observing during a pilot survey. Image: Brett Hiscock.

We are now planning a second phase are released, they will provide the pipeline scripts continue to be tuned of pilot surveys that will merge several world’s best sensitivity and resolution as we, and the survey science teams, observing strategies, allowing them all-sky catalogue at centimetre gain experience with full-scale pilot to run concurrently and improve the wavelengths (~1 GHz). survey data. overall efficiency of survey operations. Engineering development continues The CSIRO ASKAP Science Data Archive Processing of ASKAP’s first all-sky alongside telescope operations (CSADA) is now receiving regular survey, the Rapid ASKAP Continuum with establishment of a routine test, deposits of data, providing the first Survey (RACS), is proceeding well. release and test again process that opportunity to test quality reporting, Our staff and collaborators from dedicates time each week to rolling cut-out services and other features (see the performed out software and firmware updates. Data archives). ASKAP is unique among extensive cross‑checks to verify This will ensure that the efficiency of ATNF telescopes in that CASDA is the data quality. This led to improved the telescope continues to improve, primary point of interaction for external understanding of ASKAP’s phased while minimising disruption to astronomers as all observations are array feed primary beams, which will science observations. ASKAP’s image run by our staff – this is the model that now be incorporated into the image processing software and associated will be used by the SKA. processing software. When the data

Murchison Radio‑astronomy Observatory

The Murchison Radio-astronomy Observatory (MRO) in The MRO also hosts the: is 300 km from the coastal town of • Murchison Widefield Array (MWA), a low-frequency Geraldton on a former pastoral property, Boolardy Station. instrument of 4096 dipole antennas operated by Curtin CSIRO acknowledges the Wajarri Yamatji as the traditional University on behalf of an international consortium owners of the observatory site. of some 21 organisations, including CSIRO.

The Murchison region has a low population density so there • Experiment to Detect the Global -of‑Reionisation is less radio frequency interference (RFI) that can drown out Signature (EDGES), a radio spectrometer operated or mimic the weak signals radio telescopes are trying to by Arizona State University and the Massachusetts detect. This radio quiet environment is protected by a series Institute of Technology’s . of concentric zones; within 70 km of the centre of the MRO, • SKA test arrays, the Aperture Array Verification System, radio astronomy is the primary user of spectrum. CSIRO which tests prototype SKA1-Low antennas, and the Early also has strict standards to keep interference made on site Development Array, which uses MWA antennas in the to a minimum and an RFI monitoring system is in place (see configuration of an SKA1‑Low station. Both are operated Radio environment). by an international consortium, led by Curtin University.

The MRO is powered by a hybrid power station with a 1.85 MW solar component. It is designed to run for a large part of the day without recourse to diesel.

25 Long Baseline Array

Science highlights The Long Baseline Array (LBA) is a of observations. This system has been network of telescopes across Australia running reasonably smoothly, with • The radio afterglow from and the southern hemisphere a median time of 111 days between gravitational wave event GW170817 used together for simultaneous observation and release of data. The (a binary ) may observations, a technique called processing time is dominated by the have been produced by a narrow very long baseline time taken to transfer data (median relativistic jet or an isotropic (VLBI). There were 20 LBA 93 days), largely due to a problem outflow. A global telescope experiments in the two observing with the disk array in Hobart which array, including elements of the semesters covered by this Report, took some time to repair. A total LBA, was used to constrain the totalling 425 hours observing. of 258 000 hours of CPU time was apparent source size, indicating used on Magnus. All correlator that GW170817 produced a The bulk of LBA observations occurred output was uploaded to the Australia structured relativistic jet. (Ghirlanda during four dedicated VLBI sessions, Telescope Online Archive once verified et al. 2019 Science 363, 968). however an increasing number of (see Data archives). • Final results from the LBA experiments happen outside these Calibrator Survey: a catalogue of sessions, such as target of opportunity accurate positions and correlated and non a-priori assignable Antennas used at least once in flux densities for 1100 compact observations (of which there were the LBA in 2019/20 and where extragalactic radio sources. five), and joint observations with data was correlated at the Pawsey This work increased by six times other international VLBI arrays which Supercomputing Centre. the number of compact radio have specific timing requirements. • Parkes radio telescope sources south of One experiment in this period, for • ATCA -40° with positions known to example, was a joint observation with milliarcsecond accuracy. (Petrov the European VLBI Network to improve • Mopra sky coverage along the jet axis of a et al. 2019 MNRAS 485, 88). • CDSCC, three 34-m and 70-m giant . • Measurement of the • University of Tasmanaia, 20-m of two black hole X-ray binaries LBA experiments (other than global and 12-m in Hobart and the 32-m which, combined with other data, ones) were correlated by CSIRO in Ceduna, plus their AuScope showed that three quarters of staff using the Distributed FX (DiFX) 12-m in Yarragadee and Katherine such systems receive potential software correlator running on • South African Radio kick velocities in excess of 70 km the Magnus supercomputer at the Astronomy Observatory, per second on formation (Atri Pawsey Supercomputing Centre in 26-m in Hartebeesthoek et al. 2019 MNRAS 489, 3116). Perth. A total of 23 user projects were • Auckland University of correlated representing 297 hours ~ Technology, 12-m and 30-m in Warkworth • Shangai Astronomical Observatory, 65-m Tianma • Yunnan Astronomical Observatory, 40-m dish in Kunming • National Institute of Information and Communications Technology, 34-m in Kashima • National Astronomical Observatory of Japan 32-m Hitachi and Yamaguchi

Results of the LBA Calibrator Survey of compact radio sources in the Southern hemisphere at 8.3 GHz. Blue dots are sources known before the survey. Image: Petrov et al. 2019 MNRAS 485, 1.

26 Australia Telescope National Facility | Annual Report 2019–20 Data archives

Science highlights Our data archives include the Developments to the pulsar DAP Australia Telescope Online Archive include revamped web pages and • Discovery of 21 confirmed and (ATOA), the Parkes Pulsar Archive – improved search functionality 2 candidate supernova remnants the primary component of CSIRO’s (https://data.csiro.au/), enhancements (SNRs) from a multiwavelength Data Access Portal (DAP) – and the to the data verification and ingest study of the Small Magellanic CSIRO ASKAP Science Data Archive pipelines and improved access to data Cloud (SMC) using ATCA archival (CASDA). At least 7 papers used ATOA by high-performance computing users. data (Maggi et al. 2019 A&A 631, archival data this year and another 127). SMC SNRs were found to be 5 used the Parkes Pulsar Archive. Much of the data from ASKAP’s first larger and less elongated than pilot surveys are already processed and counterparts in the neighbouring The ATOA this year expanded in scope deposited into CASDA. This includes all Large Magellanic Cloud (LMC), to store files produced by the Parkes of EMU and VAST, the first field from suggesting that the LMC has radio telescope’s ultra-wideband WALLABY and some data from POSSUM a denser interstellar medium. receiver in its new Single Dish and GASKAP (see image). CASDA now • A multifrequency study of the Hierarchical Data Format (SDHDF). contains ~192 TB of data and handles mode-switching phenomena of PSR The ATOA dataset is now ~308 TB and more than 7000 queries per month. J0614+222. Using Parkes archival growing at ~60 TB/year – half of that growth being SDHDF data. In 2019/20, Developments include a new CASDA data at 686, 1369 and 3100 MHz, webpage (casda..au), which and data at other frequencies more than 4 TB of ATOA files were downloaded per month. now hosts data validation reports from the literature, the pulse and highlights primary images width, brightness and phase offset The DAP is the primary access point and data cubes in search results. of PSR J0614+222 were studied for Parkes pulsar data. The DAP We have implemented a common as a function of frequency. The contains 2.5 PB, over 90% of which is authentication between CASDA mode occurring earlier in the pulsar data, and the DAP is growing and the Australian Astronomical pulse phase (Mode A) has a flatter at ~700 TB annually. Over 1.5 PB Observatory’s Data Central. We have spectrum than the second mode are now publicly available. During integrated catalog and image/cube (Mode B), and the two modes this reporting period, ~70 pulsar upload for user‑uploaded value-added show a different dependence collections (each up to 1.5 TB) were data (Level 7) and developed a CASDA of pulse width with frequency accessed per month, one quarter module for the Astroquery package of (Zhang et al. 2020 ApJ 890, 31). of which were downloaded to high Astropy (an ecosystem of interoperable performance computing facilities astronomy software packages). This run by the two main pulsar groups in allows astronomers to search for and Australia, at Swinburne University of download ASKAP data as part of their Technology and CSIRO. Python workflows.

Sky coverage of ASKAP pilot survey data in CASDA in equatorial coordinates as of late June 2020. Dots mark the centre of each ~30 deg2 pointing. Image: Minh Huynh.

27 Radio environment

Radio telescopes study the Universe The Australian Communications Radio astronomers routinely observe using receivers so sensitive they could and Media Authority (ACMA) is the outside the allocated bands as detect a mobile phone on the far side national regulator and in 2006 we signals from space span the entire of the Solar System, so small portions worked together to establish Radio electromagnetic spectrum and so of the radio spectrum are set aside for Notification Zones around several modern telescope receivers have radio astronomy to avoid interference radio telescopes, including ATCA and increasingly wide bandwidths. But the from other users of the spectrum, such Parkes. Under these measures CSIRO increasing number of communications as the telecommunications sector. must be notified of applications for applications is making observing radio licences within frequency and more difficult because of the radio Our staff work hard to retain as distance limits specific to each site. frequency interference (RFI) they much spectrum as possible for cause. This is a particular issue radio astronomy and play pivotal For the MRO, we worked with for instruments studying the early roles in the regulatory bodies that ACMA to establish the Australian Universe, which ‘look back’ billions manage use of the radio spectrum. Radio Quiet Zone WA (ARQZWA): of years, because signals that would At the international level it is the a series of concentric rings centred have fallen in a protected radio Radio Sector of the International on the MRO with different levels astronomy band have been shifted Telecommunication Union (ITU-R) of protection as the distance from by the expansion of the Universe to whose activities culminate every four the telescopes increases. Within frequencies below 200 MHz – most of years in the World Radio Conference 70 km of the centre of the MRO, which are allocated to communication (WRC). The most recent WRC was held for example, radio astronomy is services. This is where the ARQZWA in November 2019 and consensus was the primary user of the spectrum, comes into play: the 2018 detection sought between radio spectrum users while the outer ring (protecting low made by EDGES of the first stars on frequency use, allocations, and frequencies) extends 260 km from forming could not have been made at protections, resulting in variations to the observatory. Applicants for radio any other observatory and bodes well the treaty-level document, the Radio licences within the various rings of for the SKA’s low frequency telescope. Regulations. Competition for radio the ARQZWA are directed by ACMA to spectrum is fierce, with commercial work with us to develop a workable, We are also taking a more hands- entities often at odds with the compliant solution – and we have on approach to managing RFI by research community. found one each time we have been monitoring the radio environment formally asked. at our observatories. This gives us visibility of long-term trends and allows us to detect all users of the spectrum. This guides development of mitigation techniques to overcome interference that cannot be addressed through regulatory action alone (see Technology development). In the case of active mitigation, interference is automatically filtered out – which risks accidentally removing real signals that look like interference. FRBs, for instance, might have never been found if short duration signals had been filtered out – as might be done to remove digital TV transmissions, for example.

The RFI tower at the MRO monitors mobile phone signals and other interference occurring within and far outside the ARQZWA.

28 Australia Telescope National Facility | Annual Report 2019–20 Square Kilometre Array

Dr Maria Grazia Labate, SKA-Low Telescope Engineer at the MRO. Image: ICRAR/Curtin University.

29 Square Kilometre Array

SKA in Australia legal drafting is largely complete, but registration of the ILUA and both are the planned community meetings, contingent on the SKA Council voting CSIRO’s Murchison Radio-astronomy where hundreds of traditional owners to build SKA1-Low in Australia. Observatory (MRO) will be home to gather to approve the agreement the low frequency telescope of the that has been struck by their A crucial component of our MRO Square Kilometre Array (SKA) project: representatives, could not be held Site Entity work is surveying the land SKA1-Low. It will comprise up to because of the pandemic. for artefacts or sites of significance 132 000 dipole antennas grouped into to the traditional owners. Over 70% 512 stations along spiral arms running The terms of the new lease with the of the land to be occupied by SKA the length and breadth of Boolardy Western Australian State Government infrastructure has now been surveyed. Station, as well as a large central were also agreed this year. Land This work has revealed sensitivities processing facility, a power station beyond the current MRO is deemed over a portion of Boolardy Station and an accommodation facility. to be for pastoral use, not radio and several options for how to avoid astronomy, so a new lease is required the area without compromising Staff with key roles in the SKA include: to transition the rest of Boolardy science outcomes were proposed • Douglas Bock, Australia’s Science Station to radio astronomy. However, and evaluated. Director on the SKA Board. granting of the lease is contingent on • Sarah Pearce, member of the Council Preparatory Task Force As part of host overseeing transition of the SKA country operations planning, SKA Organisation (a UK company) into South Africa’s an intergovernmental organisation. Karoo Site Manager, Dawie • Phil Edwards, Chair of Australia’s Fourie, and systems SKA Science Advisory Committee. engineer Clifford Gumede, toured • Antony Schinckel, seconded to the the MRO with Kevin SKA Organisation as its Head of SKA Ferguson, Head of Construction Planning in Australia. ATNF Observatory Operations • Rebecca Wheadon, our newly in the west. appointed MRO Site Entity lead. Image: Shaun Amy.

Site entity This year we commenced work as the MRO Site Entity, delivering on Australia’s obligations under the SKA Treaty on behalf of the . Together with colleagues of the Australian SKA Office in the Department of Industry, Science, Energy and Resources, we worked on activities necessary to allow SKA1-Low to be built and operated here.

The most important of these is the Indigenous Land Use Agreement (ILUA) with the Wajarri Yamatji traditional owners. The MRO already has an ILUA, but, as SKA1-Low will go beyond the boundaries of the current MRO to span virtually all Boolardy Station, a new ILUA is required. Antony Schinckel is CSIRO’s negotiator of this new ILUA. Major items are agreed, and technical Heritage surveying on Boolardy Station. Image: Kerry Ardern.

30 Australia Telescope National Facility | Annual Report 2019–20 Auxiliary facilities Essential to operation of the SKA in Australia, but not included in the SKA’s construction project, are several facilities that have seen much development over the past year.

Engineering Operations Centre. Initial concept designs have been developed and funding is being sought for this facility that is similar in purpose to our current Murchison Support Facility in Geraldton, but will be almost three times the size.

Boolardy Accommodation Facility. Concept designs have been developed and funding is being sought for a permanent accommodation facility of some 80 beds for staff and visitors of all the telescopes at the MRO.

Australian SKA Regional Centre. Dame , co-discoverer of the first radio pulsars, gives the keynote lecture at the opening of the new SKA Headquarters in Manchester, UK. Image: SKAO. The first staff for the AusSRC were appointed this year and projects commenced taking the most complex be ratified by the three host nations, sets out high level principles around computing challenges from ASKAP plus two members. governance, employment and health and the MWA and working with the and safety. With more than 100 people Together with colleagues in DISER, science teams on the best way to solve to be working in Australia under the we have this year worked with the them. The SKA project includes ingest partnership, this will see a substantial SKA Organisation on the terms of the of data from the telescopes and initial growth in radio astronomy staff in Hosting Agreement: a legal instrument data reduction (in Australia’s case, Perth and Geraldton. between Australia and the SKA at CSIRO’s Pawsey Supercomputing Observatory, essential to allow the Centre in Perth), but does not provide operation of SKA1-Low here. for astronomers’ access to the data. Construction The AusSRC, a consortium of CSIRO, A key role for the SKA Council ICRAR and Astronomy Australia Operations partnership Preparatory Task Force is allocating Limited, will provide the crucial link construction roles for member A partnership model will be used for between telescope data and the nations. Detailed national and operation of the SKA telescopes in astronomy community. international negotiations this year Australia and South Africa, to best saw Australia confirm its priorities draw on the expertise of the host for SKA construction and win the International sphere countries but ensure functional control allocation of these. CSIRO will take remains with the SKA Observatory. South Africa became the first SKA a leading part in Australian site Principles for this partnership were host country to ratify the SKA infrastructure, assembly integration developed this year and described in a Convention on 2 June 2020. The and verification of SKA1-Low, and memorandum of understanding (MoU) Convention is the first formal step in construction of its correlator and negotiated between CSIRO and the transitioning the SKA Organisation beamformer. We will also partner SKA Organisation. The MoU sets out a into an intergovernmental body, the in developing software for the model that will see staff from the SKA SKA Observatory. For this treaty-level SKA and in managing manufacture Observatory and CSIRO working as a document to come into force, it must and deployment of the antenna team in support of SKA construction, stations on site at the MRO. commissioning and operations, and

31 Design development

After six years’ designing the We made significant advances although its primary purpose is to components of the SKA telescopes, in firmware and software for the de-risk the system design and major the entire system design passed Perentie system and its interface with procurements. review by an independent panel in other parts of the telescope. We are December 2019. There was, however, also developing integrated models We have this year produced the more work required to get the design and emulators for testing interfaces technical specifications for the documentation to the point where and overall system performance Integration Test Facility and developed contracts for construction could be throughout SKA construction. the model for how it will be used put out to tender: a phase known in testing sub-systems of SKA1-Low as Bridging. Our laboratory in Sydney, formerly before they are deployed to the used to test ASKAP digital systems, MRO. This facility will be part of has been transformed into a Prototype the Engineering Operations Centre Correlator and System Integration facility for in Geraldton. beamformer SKA1‑Low. As for ASKAP, this facility mimics the computing set-up in the The correlator/beamformer system central processing facility at the Science data processor for SKA1-Low, named Perentie after MRO and is where relevant SKA1-Low Our work this year focused on an Australian lizard, has at its heart systems will be brought together and further development of our software our Gemini high performance signal tested before deployment to the MRO. prototype for the SKA’s Science Data processing boards which will handle We installed the first tile processing Processor (SDP). Based on ASKAP’s some 1.5 Pb per second from the module, built for the prototype low YANDAsoft, and named yanda after telescope. frequency aperture array, and the first the Wajarri Yamatji word for image, pulsar timing beam server and have the SDP will process data from the Together with partners ASTRON, in the interfaced them with Perentie. correlator (received at rates of around Netherlands, and Auckland University 5 Tb per second) and produce up to of Technology, in New Zealand, we 300 PB per year, per telescope of achieved a major milestone in April Assembly integration images and other science-ready data when the first Gemini boards came products. These data products will off the production line. ASTRON and verification then be distributed to SKA Regional equipped Gemini’s high bandwidth We worked closely with the SKA Centres for access by the astronomy memory‑enabled boards with an Organisation to develop the community. We also continued optimised liquid cooled monolithic concept for and then plan a critical development of the monitoring, heatsink, to dissipate the considerable early SKA1-Low deliverable: Array control and calibration system amount of heat generated by the Assembly 0.5. AA0.5 will comprise software prototype for SKA-Low. electronics, and a backplane which six stations of 256 antennas each supports synchronisation of all (plus supporting systems) and will the boards. be capable of producing images, Site infrastructure This year was spent implementing A Gemini board has 1000 parts, the design changes arising from the biggest challenge system critical design review, impact being the 50 mm assessment of subsequent engineering square FPGA with its 2892 connections. change proposals and implementation Image: ASTRON. of those that were approved. Work on changes to the layout of the telescope prompted by these activities is on hold pending completion of the heritage surveys, which have been delayed by the impacts of COVID-19. We also undertook a thorough cost review and contributed to an options analysis for reducing costs. Our work on power for SKA-Low, while still in its early days, has grown in scope to include defining technical requirements.

32 Australia Telescope National Facility | Annual Report 2019–20 Technology development

The distinctive rocket-shaped receiver elements integral to the design of the cryogenically cooled phased array feed. Image: Shaun Amy.

33 Technology development

Parkes CryoPAF Design and construction of a cryogenically cooled phased array feed (CryoPAF) receiver for the Parkes radio telescope (which promises an up to 30-fold increase in survey speed compared with the multibeam receiver) has gained momentum following a $1.15m Australian Research Council (ARC) grant, supporting the broader $3m project.

The design of the CryoPAF is modular, comprising 26 eight-channel low noise amplifier (LNA) modules in the cooled part of the receiver (the The CryoPAF structural thermal model. The grid of circular pockets in the foam will cryostat) and corresponding ‘warm’ accommodate the rocket elements. Image: Nick Carter. electronic modules outside to provide additional amplification, filtering design based on discrete transistors is ATCA digital upgrade and digitisation using state-of-the- also being investigated as a means of art Radio Frequency System on a mitigating the schedule risk associated System level design and detailed Chip (RFSoC) devices. Commercially with fabrication of the MMIC LNAs. planning for the upgrade of ATCA’s available programmable network A scheme to allow the injection of digital system is underway, with switches and Field Programmable Gate noise calibration signals directly at news of $530 000 in ARC funding, Array (FPGA) processing boards are the LNA input is being prototyped supporting a broader $2.6m project: being investigated for the CryoPAF in preparation for integration into a the Broadband Integrated-GPU beamformer, which will feed a cluster prototype eight-channel LNA module. Correlator for the Australia Telescope of Graphics Processing Unit (GPU) (BIGCAT). This project will replace A mechanical prototype of the servers for correlation and scientific the aging Compact Array Broadband integrated warm electronics module data processing. Backend (CABB) signal processing incorporating the radio frequency electronics and double the processed The full-size cryostat passed leak (RF) signal chain (which conditions bandwidth from 4 GHz to 8 GHz testing with a vacuum load equivalent the signals before digitisation) (which will also require replacement to 10 T. The first cooldown achieved and the RFSoC-based digitiser is of the RF signal chain and the timing temperatures of 28 K across the complete. The prototype module is distribution system). ground plane, exceeding the design being used to verify the mechanical target of <35 K. The cryostat will attributes, thermal performance and BIGCAT replaces the existing contain 88 distinctive ‘rocket’ radio frequency interference (RFI) CABB Analog to Digital Converters elements forming 196 active channels. shielding effectiveness of the design. (ADCs) with state-of-the-art RFSoC The rocket elements have been A prototype of the RF electronics, technology, also being developed manufactured and are being silver providing amplification and band as part of the CryoPAF project. The plated to improve their emissivity and selection, has been evaluated. old correlator will be replaced by minimise the thermal load. Assembly and testing of the prototype one based on GPUs. This will greatly digitiser was delayed due to supply increase the flexibility of ATCA, Prototype LNAs have been fabricated chain issues; although firmware to enabling implementation of innovative in a European foundry for Microwave control the digitiser and provide the signal processing techniques and Monolithic Integrated Circuits (MMICs) first stage filterbank, located in the active RFI mitigation. and cryogenically tested in our Sydney RFSoC device, is complete. Work on laboratory. A number of improvements the firmware for the beamformer has were identified and incorporated also commenced. into the design. An alternative LNA

34 Australia Telescope National Facility | Annual Report 2019–20 Radio Frequency evaluation is underway. Jimble targets RFI mitigation applications such as the CryoPAF, System on a Chip BIGCAT and future ultra-wideband In partnership with institutions in Australia and internationally, We have continued to investigate systems. we have been investigating RFI RFSoC technology as a potential Bluering is based around a mitigation algorithms and their next‑generation digitisation and digital 16-channel, 2GSps device and includes implementation, particularly signal processing platform relevant to a 16 customisable daughterboards, which regarding PAFs, the low frequency range of radio astronomy applications. contain the input RF signal conditioning ultra-wideband receiver and in The RFSoC devices incorporate electronics. The first prototype signal pulsar science. multiple high-speed ADCs, an Arm® processing board completed initial microprocessor and programmable testing of key components. Two of the We took advantage of the pandemic logic in a single package, enabling 16 customisable RF modules have been shutdown and quantified the much greater integration of the signal produced and their RF performance radio environment at the Parkes processing chain. This technology is undergoing comprehensive testing. radio telescope. This provides a has been developed for the software Bluering is also liquid cooled and baseline for exploring mitigation defined radio market and has the shielded, to ensure operation in remote strategies and for ensuring that potential to be a common platform and RFI-challenged environments. the CryoPAF will work in Parkes’ for future systems. Bluering targets array-based astronomy RFI environment. We have also deployed a frequency interpolation Work is divided into two streams instruments, such as low frequency technique on ASKAP to stop PAF (Jimble and Bluering) targeting aperture arrays. beams being corrupted by RFI different applications. Jimble and Bluering use a common that occurs during measurements Jimble uses an 8-channel device time and frequency distribution system, taken to calculate the beamformer running at 4 giga samples per second currently under development. The weights. (GSps) that simultaneously digitise timing system allows synchronisation We are also working on new time/ 8 channels, each 2 GHz wide. The of multiple boards, necessary for frequency domain RFI mitigation on-board programmable logic and array-based applications. The firmware algorithms and prototyping their Arm® processor enable incorporation and software required for control implementation on the latest RFSoC of the first stage filterbank, ethernet and monitor of the RFSoC device, devices, targeting both single pixel interfaces and the control and monitor ethernet communication and support receivers and PAF systems. functionality within the RFSoC chip. other functions is well advanced A prototype Jimble board has been and is available to support detailed built and detailed performance performance evaluation.

A prototype Jimble board using cutting edge RFSoC technology. Image: Puzzle Precision.

35 The FAST radio telescope in the FAST impact mountains of Guizhou province. When the National Astronomical Image: NAOC. Observatories of China (NAOC) was considering options for design and during commissioning. The We developed highly specialised manufacture of the flagship receiver collaboration has also led to six components and techniques for the for its Five hundred metre Aperture papers jointly authored by NAOC 19-beam receiver. For example, the key Spherical Telescope (FAST), at the time and CSIRO staff. component of the receiver’s low noise under construction in the mountains performance, the LNAs, were designed of Guizhou province, they came to us The research benefits of more precise and built in-house and are among the because of our track record in building observations include: world’s best. We have since applied similar receivers: for our 64-m Parkes • a reduction in the amount of the LNA bias circuits, LNAs, and the telescope (13 beams) and for the 305‑m individual resources necessary to advanced FPGA-based monitor and in Puerto Rico participate in research, with more control system, to the ultra‑wideband (7 beams). For FAST we built a 19‑beam time available for data analysis as receiver, currently installed on Parkes wideband receiver: the largest and opposed to observing and attracting international interest, most complex we’ve ever made. leading to potential increased • improved ability of astronomers to scientific and research exports. A recent independent analysis2 of distinguish common events from this four-year project revealed a total anomalies and hence build out FAST will produce an estimated impact value of $19.4m associated a more comprehensive image of 18.8 PB of data per annum, requiring with: contract revenue for follow‑up our skies a throughput data rate capability of observations with the Parkes radio • higher probability of successful 150 TB per day. The ATNF is no stranger telescope, scientific discovery (counted discoveries. to handling big data and we were in publications and citations), soft We have hosted five international contracted by NAOC to advise on the diplomacy, formation of human capital PhD students analysing FAST requirements for archiving of pulsar (through students, for example) and data and/or making follow-up and spectral line data from FAST, increased scientific and research observations with Parkes. Overall, specifically because of our experience exports. an estimated 50 students are with the Parkes Pulsar Archive and CASDA (see Data archives). FAST is the largest single reflector involved in FAST projects across telescope in the world. It has double 133 Principal Investigator programs Our international reputation for the sensitivity, 5-10 times the survey from 21 institutions. The skills gained outstanding radio astronomy receivers speed and has up to three times the by these students through designing is built on our unique combination of sky coverage of the next largest radio software to store, use and analyse data engineering capability (cryogenics, telescope (Arecibo). Most of FAST’s from FAST and/or Parkes, is just one electronic, electro-magnetic, digital science goals rely on surveys, and example of the human capital being and software), telescope operations our multibeam receiver multiplies the generated by this collaboration. experience and astronomy expertise. speed, or equivalently the depth, of Astronomy plays an important role in We understand every aspect of how a these surveys by 19 times. FAST expects the broader Australia-China bilateral receiver should work and that’s what to discover ~10 000 new galaxies and relationship as it provides apolitical sets us apart. ~4000 pulsars and has purchased avenues for engagement and shows around 2000 hours observing time on how Australia and China can be global the Parkes radio telescope to confirm partners. This project is one part of a its potential pulsar sightings. radio astronomy relationship between The receiver was installed in 2018 so it the two countries that spans some is still early days for scientific output 40 years. Our FAST collaboration is however, working with our Chinese aligned to the Foreign Policy White colleagues, Parkes confirmed 24% of Paper and the Global Innovation the new pulsars observed by FAST Strategy, both part of the Australian The focus cabin of FAST, with the from 2017‑2019, including the first Government’s National Innovation and 19‑beam receiver on board, is hoisted pulsar discovered by FAST – found Science Agenda. into position. Image: Xinhua.

4 Centre for International Economics (April 2020). Costs and benefits calculated from an Australian perspective.

36 Australia Telescope National Facility | Annual Report 2019–20

2 Centre for International Economics (April 2020). Costs and benefits calculated from an Australian perspective. People and community

An astronaut actor entertains the crowd at Parkes’ Apollo 11 anniversary weekend.

37 Staff

There are currently 191 people working Overall the survey results were Awards on radio astronomy in CSIRO: that is, positive: the majority of respondents in the ATNF and our SKA activities had good relationships with Our award winners include: (Appendix B). There were 2 joint colleagues, felt valued at work, believe • Karren Lee-Waddell – CSIRO John appointments and 1 secondment. people are treated respectfully and Philip Award for Promotion of We exceeded CSIRO’s target of fairly and that culture and diversity Excellence in Young Scientists. 3% indigenous employment with is supported by their colleagues. • Robin Wark – CSIRO Lifetime 8 staff identifying as indigenous. Younger staff, staff with caring Achievement Award. The gender breakdown of CASS staff responsibilities and those identifying • Sarah Pearce – New South is at Appendix C. as LGBTQI+, while reporting better Wales (NSW) Telstra Business relationships with colleagues, Woman of the Year. CSIRO’s Science in Australia Gender also reported experiencing more • Sarah Pearce – selected into Equity (SAGE) program undertook a discomfort with how they felt their Science and Technology Australia’s benchmarking exercise which assessed lives were perceived. the gender breakdown of CASS Superstars of STEM program. staff weighted against the gender As a result of these bodies of work, • Charlotte Sobey – selected into diversity in matched disciplines and the Diversity Champion’s role was the science communication organisations and set targets based clarified, terms of reference agreed program, Fresh Science. on this benchmark plus 10%. This for the Committee and a process • Jane Kaczmarek and Karen found that: the percentage of CASS’ commenced to refresh its membership. Lee‑Waddell – among five young female research staff exceeded the The Diversity Champion is to be the leaders selected to represent target, but the percentage of female link between CASS and wider CSIRO CSIRO at the prestigious Science technical staff fell below the target. activities, including the SAGE initiative. and Technology in Society Forum Improving our gender balance relies They lead the D&I Committee and in Kyoto from 4-7 October. on there being qualified women: we now attend all meetings of the CASS • Douglas Bock – elected a Fellow have established an undergraduate Executive. The D&I Committee is of the Australian Academy of scholarship program for women in formed of volunteers passionate about Technology and Engineering engineering with Macquarie University creating a culture of inclusivity and in Sydney and have appointed our first respect throughout CASS. • Rob Hollow – made Life Member scholar. Further work on this front, of the Science Teachers’ as well as the technical trades, will The Committee will provide a forum Association of NSW. be considered by CASS’ Diversity and for staff, students and visitors and Inclusion Committee. facilitate the exchange of information and ideas and assist in developing a common understanding of issues Diversity and inclusion facing CASS. It will also identify areas in which we have scope to improve Our commitment to ensuring a safe, diversity and inclusion, understand respectful, inclusive and diverse potential barriers to that happening environment for staff and visitors and recommend and support the continued this year as we welcomed implementation of targeted actions to new Diversity Champion, Kevin help remove these barriers. Ferguson, following Jane Kaczmarek’s departure to take up a new job The expression of interest process in Canada. Jane’s stepping down for new Committee members closed provided the opportunity for a review on 1 July 2020. The first task for of the position and of the Diversity the refreshed Committee will be to and Inclusion (D&I) Committee. develop and implement an annual The review also considered the results D&I Action Plan. Meanwhile, ongoing of the Culture Survey conducted in activities such as a buddy system for June 2019. Education and Outreach Officer, Rob new staff and mentoring of staff at any Hollow, is made a life member of the career stage continued. Science Teachers Association of NSW. Image: STANSW.

38 Australia Telescope National Facility | Annual Report 2019–20 Indigenous engagement Recognising that it is important to not just attract, but to retain and to develop, Indigenous staff, we have developed an Indigenous Talent Management Plan to grow the options available. One of our co-supervised students, Karlie Noon, became the first Indigenous student to obtain a Masters of Astronomy Robin Wark wins the CSIRO Medal for Lifetime Achievement and Karen Lee‑Waddell wins the John Philip Young Scientist of the Year award. and Astrophysics (Advanced) from the Australian National University. CSIRO also co-hosted the virtual ceremony for the 2019 Aboriginal and Torres Strait Islander STEM Student Achievement Award, which was made to year 12 student Alana Dooley in Perth. We look forward to supporting Alana as she pursues her dream of studying astrophysics.

We continued our significant engagement with the Wajarri Yamatji, traditional owners of the MRO, Sarah Pearce: NSW Telstra Business principally through the Indigenous Woman of the Year and Superstar Land Use Agreement in areas such as: of STEM.

• educational support, such as mentoring and visits to the MRO Charlotte Sobey takes the pub test at • contracting, employment and Fresh Science. Image: Ross Swanborough. training opportunities • acknowledgement of traditional owners in science publications Health, safety and environment using data from the MRO ATNF staff again reported no medical treatment injuries, that is, no injuries • an Indigenous heritage that required medical treatment beyond first aid, and one lost time injury (LTI), induction for all who work that is, where one or more day was lost from work after an injury. The LTI was on or visit the MRO. due to a musculoskeletal injury incurred doing a routine task.

Health, safety and environment incidents over time.

PERIOD E INCIDENTS H&S INCIDENTS LTI MTI

Jan–Dec 2014 1 14 1 0

Jan–Dec 2015 2 4 3 2

Jan–Dec 2016 0 12 0 2

Jan 2017 – Jun 2018 1 23 1 0

Jul 2018 – Jun 2019 0 8 1 0

Jul 2019 – Jun 2020 0 8 1 0

E = environmental, H&S = health and safety, LTI = lost time injury, MTI = medical treatment injury

39 Education

Postgraduate students NUMBER OF STUDENTS  This reporting period saw ATNF staff co-supervise 33 PhD students and  1 Masters student (Fig. 12). While the number of students remains stable,  they were drawn from a larger range  of institutions (Fig. 13). Our staff also co‑supervised two honours students for the industrial placement component             of their degrees. In this reporting Figure 12: Postgraduate students co-supervised by ATNF staff over time. period, 7 students were awarded PhDs and three earned their Masters. Student affiliations and thesis titles are University of Sydney listed in Appendix E and Appendix F. Curtin University Swinburne University of Technology Undergraduate University of University of New South Wales vacation scholars CAS, National Astronomical Observatory The 2019-20 Undergraduate Vacation Western Sydney University Scholarship program had 14 students: Univeristy of Technology, Sydney 10 in Sydney, 3 in Perth and one at the Macquarie University CDSCC. Several of this year’s projects Univeristy of Melbourne involved examining new ASKAP data, while others focused on space, CAS, Xinjiang Astronomical Observatory satellites and communications, along CAS, Purple Mountain Observatory with the usual mix of astrophysics CAS, Shanghai Astronomical Observatory and engineering. All the students Kumamoto University visited ATCA in January and got University of Iowa the opportunity to gain observing Tata Institute of Fundamental Research experience with a major facility. The  program concluded with the annual NUMBER OF STUDENTS Student Symposium in February where each student presented their research. Figure 13: Affiliation of co-supervised postgraduate students.

Summer vacation scholars on an ATCA dish. Image: Jamie Stevens.

40 Australia Telescope National Facility | Annual Report 2019–20 Radio school Students and staff from Pia Wadjarri We again held a session in Remote Community School made their collaboration with the Pawsey The annual Radio Astronomy annual visit to the MRO in October. Supercomputing Centre for students School was held at ATCA from This was followed by astronomy from four Perth schools visiting 30 September to 4 October 2019. activities back at school the next day. the facility. After this, COVID-19 Aimed at postgraduate students, restrictions saw us develop ways of the school involved a mix of lectures Education specialist, Rob Hollow, delivering PULSE@Parkes remotely, and hands-on workshops presented ran specialist workshops for supported by CSIRO Education and by astronomers and engineers from science teachers at science teacher Outreach. This approach has proved Australia and overseas. While single- conferences in , Darwin so successful, we intend offering dish telescopes were part of the and Melbourne. the program remotely even after curriculum, the emphasis this year restrictions ease. It has also opened was on interferometry and managing PULSE@Parkes the program to schools in regional very large data sets, which followed areas, interstate and overseas. We on from last year’s school at ASKAP. Our educational program, ran a remote session for 35 Year 9 The 35 students and 24 lecturers and PULSE@Parkes, designed to give girls across northern Queensland visiting staff were joined on the last school students the opportunity who are in CSIRO’s Young Indigenous day by 25 undergraduate students to observe with the Parkes radio Women’s STEM Academy and we from the University of Sydney’s telescope, this year saw more than were part of CSIRO’s trial of a Virtual Talented Student Program in Physics. 160 students and 25 teachers from Work Experience Program, which saw 19 schools take part. As part of the five students from three states work Apollo 11 open days at Parkes in July School visits together over a week observing with 2019, about 500 people participated Parkes and analysing their data. We Several staff were active in the STEM and the program also ran at Perth also ran a remote session for school Professionals in Schools program, Astrofest in February 2020. students in a radio astronomy summer working with partner schools over the school at the We held a special session at the year. National Science Week in August in Italy. Here we reconnected with Robotic Telescopes, Student Research saw several staff head to Geraldton to Marta Burgay of the Italian National and Education conference in give talks and run hands-on activities Institute for Astrophysics who had Melbourne in December, which gave at Geraldton Primary School, Champion been involved in early PULSE@Parkes international participants the chance Bay Senior High School, Meekatharra sessions in 2008. to observe and learn more about School of the Air, Central Regional the program. institute for Technical and Further Education and the Geraldton Museum.

Jane Kaczmarek and students from the Pia Wadjarri Remote Chenoa Tremblay at a school in Perth. Community School on their annual excursion to the MRO – here with ASKAP digital equipment in the control building. Image: Rob Hollow.

41 Outreach and media

Our approach in recent years of attending for science shows, talks and year’s results due to closure of both working with our partners to promote exhibits, such as ours for CASS and facilities in March due to COVID-19 joint research outcomes continued this the SKA. CSIRO is a sponsor of Perth (see table). Parkes would have had a year to great effect. For example, we Astrofest and were proud to see it record-breaking year were it not for worked with the International Centre named joint winner of the Chevron the virus: 13 248 people came through for Radio Astronomy Research to Science Engagement Initiative of the the visitors centre on the Apollo promote the Science paper describing Year in the Premier’s Science Awards. anniversary weekend. the missing matter of the Universe Sydney Astrofest didn’t go ahead due discovery that started with ASKAP to COVID-19. Apollo 11 anniversary finding and localising FRBs. We celebration provided images, broadcast-quality For the Moon to the Murchison event, part of National Science Week in footage and other content as well as CSIRO’s campaign to mark the August, we worked with our partners comprehensive background material 50th anniversary of the Apollo 11 to deliver six science outreach events for journalists and supported the Moon landing and Australia’s role in Geraldton, reaching 600 people university’s press release via our social in supporting the historic mission with the wonder of astronomy and media channels. was one of the largest integrated space science, and the role CSIRO is marketing and communications To celebrate the centenary of the playing in the region. campaigns we have ever undertaken. International Astronomical Union, We started three months before the we joined with partners around the For the past couple of years we have anniversary, staggering events to nation to create Australia’s video been actively managing the ATNF maximise coverage and avoid news contribution highlighting astronomical Twitter account (@CSIRO_ATNF) which fatigue. The lynchpin of the campaign discoveries made ‘down under’. One now has around 3700 followers and was its website (www.csiro.au/apollo11) of our principal international partners that number is climbing steadily. We featuring historical information, is, of course, the SKA Organisation. are finding social media, Twitter in a national event calendar and We provided staff for interview and particular, to be a to highly successful supplied other content for its annual mechanism for amplifying the reach of promotion of Women in Engineering our stories. Day and regularly contribute stories to Another important aspect of our its magazine Contact. outreach work is our visitors’ centres Perth Astrofest in February was again at the Parkes radio telescope and a success with thousands of people ATCA. Numbers were down on last

Number of visitors to ATCA and the Parkes Radio Telescope.

2014-15 2015-16 2016-17 2017-18 2018-19 2019-20 CSIRO’s Dave Williams speaks at the Parkes 68 427 95 212 83 851 105 085 112 224 100 013 opening of the Apollo 11 exhibition ATCA 10 971 11 511 10 965 12 081 10 363 7434 at the Powerhouse Museum in Sydney. Image: Gabby Russell.

Open days at the Parkes radio telescope attracted 19 500 visitors. Image: Stephen Holland.

42 Australia Telescope National Facility | Annual Report 2019–20 CSIRO staff and volunteers were easy to spot guiding some 2226 CSIRO’s Moon landing footage is donated to the National people on the telescope and around the site. Image: Chris Khoury. Film and Sound Archive. From left: Dave Williams (CSIRO), Badri Younes (NASA) The Hon Karen Andrews MP, The Hon Paul Fletcher MP, Jan Müller (NFSA). resources for students, teachers and We joined with the Australian All free to air television networks media. The site’s 147 pages were Space Agency to create a brief covered the open days, with eight viewed over 34 000 times. about Australia’s involvement for programs doing at least 46 live crosses the Department of Foreign Affairs to the telescope. ABC Local Radio We were principal sponsor of an and Trade. Australia’s embassies broadcast several programs live from Apollo 11 exhibition at the Powerhouse and consulates around the world the event. Overall, media coverage Museum in Sydney, which included used social media and local events around the weekend reached at least artefacts such as the feed horn from to promote Australia’s role and our 7.8 million Australians Parkes that captured the signals from ongoing excellence in STEM. the Moon. The year-long exhibition The open days had a positive impact attracted 181 935 visitors in its first We also donated the only copy of for the local community as well. The six months. the restored television footage of Parkes’ Visitor Information Centre the Apollo 11 Moon landing to reside had a 300% increase in custom and For CSIRO’s Discovery Centre in outside the United States, which accommodation was booked out in Canberra we developed a virtual had been presented to CSIRO, to the towns across the central west region. reality experience, Earthlight: Lunar National Film and Sound Archive. Hub, taking visitors on an immersive Over the weekend, 110 staff and their tour through a fictional Moon base families volunteered their time to before a walk on the lunar surface. The anniversary weekend make the weekend a success. We also supported exhibitions at Open days at the Parkes radio telescope Questacon, the National Museum of on 20 and 21 July attracted 19 500 That’s a wrap Australia and Geoscience Australia. visitors (almost double the population of Parkes) including the US Ambassador The campaign resulted in We worked with leading metropolitan to Australia, a former astronaut, overwhelmingly positive feedback for and regional media groups on exclusive Australia’s Deputy Prime Minister and CSIRO, raised awareness of Australia’s Apollo 11 content, a commemorative the Minister for Industry, Science and contribution to the Apollo 11 poster and lift-outs. In total, more Technology. With The Dish as backdrop, mission, CSIRO and our partners. Its than 3300 news stories were produced we rebroadcast the Moon landing ‘as it success shows the pride Australians across Australian TV, radio, print and happened’, and more than a thousand have in the nation’s technological websites, reaching an audience of people gathered ‘on location’ on the achievements and their fascination 55.5 million. Our posts on social media (very cold) Saturday night to watch the with what our future in space holds. were viewed over 4.1 million times by iconic Australian movie The Dish. more than 2.7 million people.

43 Astronomy community

The ATNF User Committee (ATUC) ICRARcon. A number of staff were represents astronomers who use invited to this biennial internal ATNF instruments. ATUC meets twice workshop of Curtin University and the a year and is a forum for users to University of Western Australia, held raise problems with operation of the 24-26 September at Margaret River in facility and to discuss and recommend Western Australia. priorities for its future development. The April 2020 meeting was, for the International VLBI Technology. th first time, held entirely online. ATUC’s We hosted the 8 workshop in this reports, and the ATNF Director’s annual series at our Sydney site, replies, are available on the web. 18‑20 November. New Zealand SKA Forum. This event Meetings, workshops, brought together the Science for SKA and Computing for SKA Colloquia conferences and in Auckland, New Zealand from colloquia 12‑15 February. CSIRO staff gave talks including experience with ASKAP’s With the advent of COVID-19, many Senior digital engineer, Grant Hampson, ingest pipeline and the digital signal speaks at the SKA Engineering conference meetings in 2020 were postponed processing system for SKA1-Low. in Shanghai. Image: SKAO. or cancelled. The scientific meetings we did host, or in which we had OzSKA. The annual Australian SKA and developing software and firmware significant participation, include: meeting was held at Mt Stromlo prototypes for the SKA and included a Observatory, near Canberra, AusSRC Community Workshop. visit to the MRO. 6-7 November. Opened by SKA Our staff co-organised this event, Director General, Phil Diamond, the SKA Engineering. The final SKA held at Mt Stromlo near Canberra two-day program featured many talks engineering meeting was held in on 8 November, to further develop from CSIRO staff. Shanghai, China, 25-28 November. It the vision for a global network of focused on system design, operations SKA Regional Centres, focussing on PAF Workshop. This annual workshop plans and, for the first time, presented data processing for ASKAP and MWA was hosted by the Max Planck the full design of both SKA telescopes. surveys. Institute for Radio Astronomy in Bonn, Germany, 16-18 September. CSIRO SKA VLBI. Two staff were on the Australia-ESO Joint Conference. CSIRO staff spoke on topics including using scientific organising committee and sponsored the 2nd such conference, PAFs in noisy radio environments and several spoke at this workshop in which was held in Perth, 17-21 development of the CryoPAF. Manchester, UK, 14-17 October, which February, and looked at coordination introduced VLBI capabilities of the of next-generation galaxy evolution th RFI 2019. The 5 in this series of SKA and discussed potential SKA-VLBI surveys. Elaine Sadler chaired the first workshops focussed on coexisting observing programmes. day and she and other staff gave talks. with RFI and was held in Toulouse, France, 23-26 September. Balthasar SPARCS. Several staff spoke at the Bolton Symposium. This forum, to Indermühle was the Technical Program 9th SKA Pathfinder Radio Continuum promote collaboration between early Chair, Carol Wilson was on the Survey meeting ‘Pathfinders get to career researchers and those with Scientific Organising Committee and work’ in Lisbon, Portugal, 6-10 May. more seniority, was held in Perth on these and other staff chaired sessions 10 March. and/or presented talks. World Radiocommunication Conference. This major event of the IAU Astronomy for Equity, Diversity SAFe6. The 6th SKA Scaled Agile International Telecommunications and Inclusion. We were gold sponsors Framework (SAFe) Program Increment Union was held in Sharm el‑Sheikh, of the inaugural IAU symposium (S358) planning meeting was hosted by Egypt, 28 October to 5 November. on this important topic, which was CSIRO and ICRAR and sponsored by Balthasar Indermühle and Tasso held in Tokyo, Japan 12-15 November. DISER and held 24-28 February in Tzioumis were among Australia’s Jimi Green chaired the session on Perth. This quarterly event in the SKA negotiators and Carol Wilson chaired inclusion, diversity, equity, and calendar gathered together engineers the working group forming the empathy in communicating astronomy. and researchers involved in designing agenda for the next WRC.

44 Australia Telescope National Facility | Annual Report 2019–20 Appendices

Parkes Elvis Festival contestants DeanZ and Shania Sarsfield. Image: John Sarkissian.

45 A: Financial summary

The table below summarises revenue and expenditure applied to CSIRO’s radio astronomy activities ($’000s).

The notable factors affecting the financial results for this year include an increase to external funding, primarily due to SKA site entity funding, and a decrease in CSIRO indirect appropriation, due to a revaluation of the useful life of assets and changes in depreciation. Travel spend was reduced both due to a budget realignment and COVID-19. ATNF funding supported 169 FTE in FY 19/20, an increase of three on the previous year.

YEAR TO YEAR TO YEAR TO YEAR TO YEAR TO YEAR TO OPERATING 30 JUNE 2015 30 JUNE 2016 30 JUNE 2017 30 JUNE 2018 30 JUNE 2019 30 JUNE 2020

Revenue

External 13 209 14 377 15 418 14 889 13 806 16 648

CSIRO direct appropriation 18 454 18 282 19 532 20 632 20 612 20 550

CSIRO indirect appropriation1 22 019 23 812 25 099 25 637 25 261 18 754

Total revenue 53 682 56 471 60 049 61 158 59 679 55 952

Expenditure

Salaries 19 545 21 179 22 784 20 959 22 289 24 096

Travel 1 429 1 981 1 866 1 713 1 879 1 269

Other operating 9334 8837 11 708 13 250 10 562 11 977

Overheads2 14 506 13 711 13 492 13 316 14 947 13 394

Depreciation & amortisation 7 513 10 101 11 607 12 321 10 314 5360

Total expenses 52 327 55 809 61 457 61 559 59 991 56 096

Operating result 1 355 662 -1 408 -401 -312 -144

1. CSIRO indirect appropriation is funding for: overheads, depreciation and amortisation. 2. Overheads include support services such as human resources, health and safety, finance and property services.

The table below shows CSIRO capital investment, including from the Science and Industry Endowment Fund.

YEAR TO YEAR TO YEAR TO YEAR TO YEAR TO YEAR TO CAPITAL INVESTMENT 30 JUNE 2015 30 JUNE 2016 30 JUNE 2017 30 JUNE 2018 30 JUNE 2019 30 JUNE 2020

ATNF 855 1 310 547 2 360 1 445 1 823

ASKAP 15 179 9 728 3 121 1 235

46 Australia Telescope National Facility | Annual Report 2019–20 B: Staff list

People contributing to radio astronomy: ATNF and the SKA as at 30 June 2020. Includes casual staff, joint appointments, honorary fellows and those employed under contractor or labour-hire arrangements, but not students. Note: many people working on SKA projects are based in another Program, such as Technologies.

SYDNEY (NSW) Death Michael Technologies

Ahmed Azeem SKA Deng Xinping Technologies

Allen Graham SKA Doherty Paul Technologies

Amy Shaun Operations Drazenovic Vicki Operations

Ardern Kerry SKA Dunning Alex Technologies

Bannister Keith Technologies Edwards Leanne Operations

Baquiran Mia Technologies Edwards Phil Science

Barker Steve Technologies Ekers Ron Science

Bekiaris Georgios Science Feain Ilana Technologies

Bengston Keith Technologies Fedeli Jordan Technologies

Beresford Ron Technologies George Daniel Technologies

Bhandari Shivani Science Gough Russell Technologies

Bhandari Yukti Operations Gray Amanda Science

Biswas Raj Technologies Hampson Grant Technologies

Bock Douglas Management Hartmann Carmel SKA

Bolin Andrew Technologies Hayman Douglas Technologies

Bourne Michael Technologies Hobbs George Science

Bowen Mark Technologies Hollow Robert Science

Brothers Michael Technologies Howard Eric Operations

Bunton John Technologies Humphrey David Technologies

Callaghan Kate Management Huynh Minh Technologies

Cameron Andrew Science Indermuehle Balthasar Science

Carter Nick Technologies Ingold Brett Technologies

Castillo Santiago Technologies Jeganathan Kanapathippillai Technologies

Chapman Jessica Science Johnston Simon Science

Chekkala Raji Technologies Kesteven Michael Technologies

Chen Yuqing Technologies Koribalski Baerbel Science

Cheng Wan Technologies Kosmynin Arkadi Operations

Chippendale Aaron Technologies Lee-Waddell Karen Science

Chow Kate SKA Lenc Emil Science

Chung Yoon Technologies Lennon Brett Operations

Cooper Adam Technologies Lim Boon Technologies

Cooper Paul Technologies Luo Rui Science

Craig Daniel Operations Mackay Simon Technologies

Dai Shi Science Macleod Adam SKA

D'Costa Howard SKA Madden Cathy Management

47 SYDNEY (NSW) (CONTINUED) Tearall Liz Management

Mahony Elizabeth Science Tesoriero Julie Technologies

Manchester Dick Science Toomey Lawrence Science

Marquarding Malte Operations Troup Euan Operations

McConnell David Science Tuthill John Technologies

McIntyre Vincent Operations Tzioumis Tasso Technologies

Mitchell Daniel Operations Voronkov Max Operations

Moss Vanessa Science Whiting Matthew Science

Norris Ray Science Wiedemann Markus Technologies

Nosrati Hamed Technologies Wieringa Mark Operations

Ord Stephen Operations Wilson Carol Technologies

Pearce Sarah Management Wu Xinyu Operations

Perry Grant Technologies NARRABRI (NSW)

Petranovic Aeva Operations Cole James Operations

Phillips Chris Science Forbes Kylee Operations

Pilawa Mike Technologies George Mike Operations

Pope Nathan Operations Hill Mike Operations

Raja Wasim Operations Kelly Pam Operations

Reilly Les Technologies Lee Kun Operations

Reynolds John Operations Mirtschin Peter Operations

Rispler Adrian SKA Rex Jordan Operations

Roberts Paul Technologies Stevens Jamie Operations

Roush Peter Technologies Sunderland Graeme Operations

Sadler Elaine Science Trindall Jane Operations

Schinckel Antony SKA Wilson Chris Operations

Severs Sean Technologies Wilson John Operations

Shaw Robert Technologies Wilson Tim Operations

Smart Ken Technologies PARKES (NSW)

Smith Stephanie Technologies Abbey Alex Operations

Storey Michelle SKA Clark David Operations

Svenson Nic Management Hoyle Simon Operations

48 Australia Telescope National Facility | Annual Report 2019–20 Kaletsch Robert Operations Huynh Minh Science

Lees Tom Operations Jameson Katie Science

Lensson Erik Operations Reynolds Cormac Science

Mader Stacy Operations Roja Maria Science

Milgate Lynette Operations Sobey Charlotte Science

Palmer Kyasha Operations Taylor Zoe Operations

Preisig Brett Operations Thomson Alec Science

Reeves Ken Operations Tremblay Chenoa Science

Ruckley Tim Operations Vernstrom Tessa Science

Sarkissian John Operations Wheadon Rebecca SKA

Sarkissian Annie Operations Wong Ivy Science

Sharwood Warren Operations Yu Yun Science

Smith Mal Operations Zhang Xiang Science

Trim Tricia Operations GERALDTON & MRO (WA)

Unger Karin Operations Boddington Leonie Operations

PERTH (WA) Cox Tom Operations

Austin Matt Operations Danischewsky Shaina Operations

Bastholm Eric Operations Desmond Rochelle Operations

Bignall Hayley Science Hannah James Operations

Broderick Jess Science Harding Alex Operations

Chhetri Rajan Science Hathway Steve Operations

Cloake Beth Operations Hiscock Brett Operations

Elagali Ahmed Science McConigley Ryan Operations

Ferguson Kevin Operations McCormack Bernadette Operations

Galvin Tim Science Merry Clarence Operations

Green Jimi Science Morris John Operations

Guzman Juan Operations Pena Will Operations

Hale Catherine Science Puls Lou Operations

Haskins Craig Operations Reay Michael Operations

Heald George Science Rowan Haydn Operations

Hotan Aidan Science Warhurst Kurt Operations

49 C: Demographic data

These figures show people contributing to radio astronomy: ATNF and the SKA. Includes casual staff, joint appointments and, from 2020, those employed under contractor or labour hire arrangements. Does not include honourary fellows or students.

NUMBER OF PEOPLE 









           

Male Female

Figure 14: Gender breakdown over time.

NUMBER OF PEOPLE 















ATNF Operations ATNF ScienceTechnologiesSKA Other

Male Female

Figure 15: Gender breakdown across Programs as at 30 June 2020. Note: many staff working on SKA projects are based in other Programs, such as Technologies.

50 Australia Telescope National Facility | Annual Report 2019–20 D: Committee membership

Years in brackets indicate when a member stood down.

ATNF Steering ATNF User ATNF Time Assignment Committee Committee Committee Chair Chair Chair

Dr David Skellern AO, RoZetta Institute Dr James Miller-Jones, ICRAR/ Dr Martin Meyer, ICRAR/University Curtin University (2019) of Western Australia Australian astronomy community Dr Ramesh Bhat, ICRAR/ Voting members Prof Matthew Bailes, Swinburne Curtin University University of Technology (2019) Prof Geoff Bicknell, Australian National Members University A/Prof Cathryn Trott, Curtin University (2019) Dr Shari Breen, University of Sydney Dr Barbara Catinella, ICRAR/University (2019) of Western Australia Prof David Davidson, Curtin University Dr Michelle Cluver, Swinburne Dr Adam Deller, Swinburne University Prof Sarah Brough, University of NSW University of Technology of Technology Prof Naomi McClure-Griffiths, Dr Jo Dawson, Macquarie University/ Dr Katie Jameson, CSIRO Australian National University CSIRO Dr Christene Lynch, ICRAR/Curtin Prof Tara Murphy, University of Sydney Prof Miroslav Filipovic, University Western Sydney University International astronomy community Dr Elizabeth Mahony, CSIRO Dr Catherine Hale, CSIRO Prof John Carlstrom, University Dr Chris Power ICRAR/University of Chicago (2019) Dr Bi-Qing For, ICRAR/University of Western Australia (2019) of Western Australia Prof Scott Ransom, National Radio Dr Nick Seymour, ICRAR/Curtin Astronomy Observatory, USA Dr Stefan Oslowski, Swinburne University University of Technology (2019) Prof Michael Wise, Netherlands Dr Stas Shabala, Institute of Space Research Dr Maria Rioja, University of (2019) Western Australia/CSIRO Prof Xiang-Ping Wu, National Dr Charlotte Sobey, CSIRO Astronomical Observatories of China Student members Ex-officio Australian stakeholder communities Mr Dougal Dobie, University of Sydney Dr Douglas Bock Ms Catherine Livingstone AO (2019) Dr Jimi Green Dr David Skellern AO, RoZetta Institute Ms Lei Zhang, National Astronomical Observatories of China (2019) Dr Jamie Stevens Ex-officio Mr Chikaedu Ogbodo, Secretariat Mr Brendan Dalton, Chief Information Macquarie University Officer, CSIRO Dr Hayley Bignall, Executive Officer Ms Cherie Day, Swinburne University (2019) Dr David Williams, Executive Director, of Technology Digital, National Facilities and Dr Jimi Green, Executive Officer Collections, CSIRO Secretariat Amanda Gray, Administration

Secretariat Dr Cormac Reynolds, CSIRO

Nic Svenson

51 E: Postgraduate students

Postgraduate students co-supervised by ATNF staff as of 30 June 2020 (PhD, unless marked otherwise).

NAME UNIVERSITY PROJECT TITLE

Wayne Arcus Curtin University Fast radio bursts as cosmic probes

Aman Chokshi Low frequency beam simulations

Daniele d’Antonio University of Technology Sydney Radio afterglow of gravitational waves

Cherie Day Swinburne University of Technology Pinpointing the origin of fast radio bursts

Dougal Dobie University of Sydney Radio transient detection using the Australian Square Kilometre Array Pathfinder

Yi Feng Chinese Academy of Science (CAS) Jitter noise and gravitational waves National Astronomical Observatory

Sarah Hegarty Swinburne University of Technology Accelerating and enhancing knowledge discovery for the petascale astronomy era

Lucas Hyland University of Tasmania Structure of the Milky Way

Dilpreet Kaur Curtin University Probing the interstellar medium towards timing array pulsars with the MWA

James Leung University of Sydney An ASKAP search for gamma ray burst afterglows

John Lopez University of New South Wales Molecular clouds in the Milky Way: peering into the galactic centre and unravelling the origins of Planck cold clumps

Marcus Lower Swinburne University of Technology Application of astrophysical inference to next generational pulsar timing datasets

Peter MacGregor (MRes) Western Sydney University An Investigation of the diffuse radio emission in the galaxy cluster Abell S1136

Perica Manojlovic Western Sydney University Origin of the diffuse emission of galaxy clusters in the SPT field

Noor Md Said University of Tasmania Intraday variability of active galaxies

Shannon Melrose University of New South Wales Characterising the star formation properties of the interstellar medium

Chikaedu Ogbodo Macquarie University MAGMO: mapping the galactic magnetic field with masers

Dylan Pare University of Iowa Radio polarimetric observations of non-thermal filaments in the Galactic Centre: probing the magnetic field structure

Aditya Parthasarathy Madapusi Swinburne University of Technology High precision pulsar timing in the SKA era

Steve Prabu Curtin University detection using the Murchison Widefield Array

Harry Qiu University of Sydney Exploring the dynamic radio sky with ASKAP

Tristan Reynolds University of Western Australia The effect of the environment on the neutral hydrogen content of Galaxies

Jonathan Rogers University of Tasmania Unravelling the physics of galaxies and active galactic nuclei in the Square Kilometre Array era

Gary Segal University of Queensland Machine learning algorithms for detecting the interesting and the unexpected

Renzhi Su CAS, Shanghai Astronomical Tracing fuelling and feedback in powerful radio galaxies with Observatory 21-cm HI absorption

Abhimanyu Susobhanan Tata Institute of Fundamental Search for gravitational waves from eccentric super-massive Research black hole binaries in the Parkes data sets

Jishnu Thekkeppattu Curtin University Towards detection of the redshifted 21-cm signal from cosmic dawn and epoch of reionisation

52 Australia Telescope National Facility | Annual Report 2019–20 NAME UNIVERSITY PROJECT TITLE

Shuangqiang Wang CAS, Xinjiang Astronomical Radio observations of the two intermittent pulsars: J1841- Observatory. 0500 and J1832+0029

Yuanming Wang University of Sydney Searching for extreme transients with ASKAP

Ziteng Wang University of Sydney Radio follow-up of gravitational wave events

Naoyuki Yonemaru Kumamoto University Simulation of gravitational wave signals from cosmic strings and the effects of the interstellar medium

Chao Zhang CAS, National Astronomical Pulsar search with interpretable machine learning Observatory.

Songbo Zhang CAS, Purple Mountain Observatory Searching for radio bursts in archival Parkes data

Andrew Zic University of Sydney Characterising the low frequency radio emission of dwarf stars and planets

F: PhD theses

Theses awarded to co-supervised postgraduate students (PhD, unless marked otherwise).

NAME UNIVERSITY MONTH AWARDED THESIS TITLE

Ahmed Elagali University of Western March 2020 Studies of interacting galaxies and the environmental Australia effects on their evolution

Hiroki Kumamoto Kumamoto University March 2020 The observational studies of pulsars for detecting gravitational waves by radio telescopes

Ali Lalbakhsh Macquarie University March 2020 All-dielectric near-field transforming structures to dielectric-less metasurfaces for high-gain antenna systems

Kieran Luken (MSc) Western Sydney University September 2019 An investigation of machine learning algorithms for the estimation of galaxy redshift

Lachlan Marnoch (MSc) Macquarie University April 2020 The host galaxies and possible progenitors of fast radio bursts

Tommy Marshman (MSc) Macquarie University June 2020 Finding pulsars in a new SETI survey with a GPU based pipeline

Tiege McCarthy University of Tasmania June 2020 Class I methanol masers toward external galaxies

Bradley Meyers Curtin University September 2019 Investigating the links between radio pulsar populations that display intermittent emission phenomena at low frequencies

Karlie Noon (MSc) Australian National November 2019 Distances and motions of high velocity clouds University

Stuart Weston Auckland University of October 2019 Astronomical catalogue cross identification for data Technology mining and statistical analysis of the infrared and faint radio sky

Lei Zhang National Astronomical May 2020 Pulsar observation and study with FAST and Parkes Observatory, CAS radio telescope

53 G: Observing programs

Proposals allocated time on ATNF telescopes over the April 2019 – September 2019 and October 2019 – March 2020 semesters. A small number of target of opportunity observations are not listed.

ATCA

OBSERVERS PROGRAM NO

Stevens, Edwards, Wieringa, Moss ATCA Calibrators C007

Lundqvist, Perez Torres, Ryder, Bjornsson, Fransson, Filipovic, Kundu Probing type Ia supernova progenitors with ATCA C1303

Ryder, Kundu, Filipovic, Anderson, Stockdale, Renaud, Kotak NAPA observations of core-collapse supernovae C1473

Edwards, Stevens, Ojha, Kadler, Wilms ATCA monitoring of Fermi gamma-ray sources C1730

Luken, Filipovic, Wong, Maxted, Alsaberi, de Horta, Brose Evolution study of the youngest Galactic SNR G1.9+0.3 C1952

Possenti, Wieringa, Esposito, Israel, Rea, Burgay Continuum radio emission from magnetars in C2456 outburst

Atri, Miller-Jones, Jonker, Maccarone, Nelemans, Sivakoff, Tzioumis Constraining black hole formation with LBA C2538

Russell, Miller-Jones, Sivakoff, Altamirano, Soria, Krimm, Tetarenko Jet-disc coupling in black hole X-ray binary outbursts C2601

Massardi, Lopez-Caniego, de Zotti, Bonato, Galluzzi The ultimate definition of blazar candidates in the C2673 H-ATLAS fields

Coti Zelati, Russell, Papitto, de Martino Deep radio observations of the transitional pulsar C3007 candidate CXOU J110926.4-650224

Russell, Altamirano, Ceccobello, Markoff, Miller-Jones, Russell, The evolving jet properties of transient black hole C3057 Sivakoff, Soria, Tetarenko X-ray binaries

Huynh, Seymour, Shabala, Davies, Robotham, Sadler, Wong, GAMA Legacy ATCA Southern Survey (GLASS): A legacy C3132 Meyer, Prandoni, Riseley, Murphy, Smolcic, Butler, Turner, Drouart, 4 cm survey of the GAMA G23 field Gurkanuygun, Swan, Rogers, Galvin, Kapinska, Delhaize, Chow, O'Brien, Hopkins, Norris, White, Marvil, Collier, Franzen

Breen, Walsh, Rowell, Ellingsen, Cunningham, Jones, Burton, Dense gas across the Milky Way – The ‘full-strength’ C3145 Contreras, Schneider, Voronkov, Ott, De wilt, Green, Barnes, MALT45 Longmore, Indermuehle, Fuller, Avison, Smith, Bronfman, Novak, Toth, Jordan, Hyland, McCarthy, Phillips, Federrath, Jackson, Fissel, Kainulainen, Dawson

van Velzen, Miller-Jones, Anderson, Shappee, Jonker, Arcavi, Holoien, Radio emission from stellar tidal disruption flares C3148 Gezari

Jackson, Barnes, Rathborne, Longmore, Contreras, Sanhueza, Hogge, A comprehensive ATCA census of high-mass cores C3152 Stephens, Whitaker, Walker, Smith, Krumholz, Kruijssen, Walsh, Caselli, Cunningham, Ott, Allingham, Killerby-Smith, Breen, Jordan

Popping, de Blok, Gannon, Heald, Koribalski, Lee-Waddell, Lopez- Imaging galaxies intergalactic and nearby C3157 Sanchez, Spitler, Madrid, Moss, Meyer, Obreschkow, Pisano, Power, environment Rhee, Staveley-Smith, Wang, Westmeier, Wolf, Kaczmarek, Sardone, Vinsen, Elagali, Wong, Kleiner

Dannerbauer, Emonts, Huynh, Smail, Jin, Thomson, Altieri, Allison, COALAS: CO ATCA Legacy Archive of Star-forming C3181 Aretxaga, Brandt, Chapman, Casey, de Breuck, Drouart, Hodge, galaxies Indermuehle, Kimball, Kodama, Koyama, Lagos, Lehnert, Miley, Narayanan, Norris, Rottgering, Schinnerer, Seymour, Swinbank, Valtchanov, Julie Wardlow, Simpson

Anderson, Bell, Hancock, Lynch, Miller-Jones, Bahramian, Bannister, ATCA rapid-response triggering on X-ray and gamma- C3200 Kaplan, Murphy, Ryder, Macquart, Plotkin ray superflares from the smallest stars

Anderson, Bell, Hancock, Miller-Jones, Bahramian, Rowlinson, Aksulu, ATCA rapid-response triggering on Swift detected C3204 Bannister, van der Horst, Macquart, Ryder, Plotkin, Wijers short gamma-ray bursts: Exploring the link with gravitational wave events

Shannon, Bannister, Macquart, Bhandari, Mahony, Deller, Dodson, Radio continuum emission from ASKAP-localised fast C3211 Flynn, James, Oslowski, Prochaska, Sadler, Tejos, Day radio bursts

54 Australia Telescope National Facility | Annual Report 2019–20 OBSERVERS PROGRAM NO

Bannister, Bignall, Stevens, Walker, Reynolds, Tuntsov, Md Said TAILS: Testing the Association of Intra-hour variability C3214 with Local Stars

Plotkin, Miller-Jones, Gallo, Jonker, Russell, Homan, Tomsick, Kaaret The disk/jet connection for hard state black holes C3219

Heald, Alexander, Anderson, Basu, Brown, Callingham, Carretti, The QUOCKA Survey C3244 Crawford, Farnes, Filipovic, Gaensler, Galvin, Harvey-Smith, Johnston- Hollitt, Kaczmarek, Landecker, Leahy, Lenc, Mao, McClure-Griffiths, Miyashita, O'Sullivan, Pasetto, Purcell, Riseley, Rudnick, Schnitzeler, Sobey, Sun, Thomson, Zhang

Dobie, Murphy, Kaplan, Lenc, Brown, Stewart, Bannister Long term radio follow-up of GW170817 C3251

Kuznetsov, Doyle, Metodieva, Nakariakov, Li, Banerjee, Kupriyanova Searching for superflares on nearby active solar-like C3260 stars

Pineda, Lynch, Moss, Zic, Lenc Uncovering the population of radio ultracool dwarfs C3261

Callingham, Pope, Tuthill, Marcote Sampling the orbit of the newly discovered and C3267 brightest non-thermal radio-emitting colliding wind binary

Bojicic, Filipovic, Crawford, Galvin, Wong High frequency observations of ASKAP detected SMC C3275 PNe

Dobie, Murphy, Kaplan, Stewart, Bell, Lenc, Bannister, Hotokezaka, Radio follow-up of LIGO gravitational wave events C3278 Brown, Qiu, Zic

Chomiuk, Ryder, Sokolovsky, Filipovic, Alsaberi, Manojlovic, Aydi, E-nova project monitoring of Nova Muscae 2018 and C3279 Linford Nova Carinae 2018

Plotkin, Miller-Jones, Bahramian, Reynolds, Gandhi An ATCA-Gaia search for the weakest black hole Jets C3280

Schulze, Bauer, de Ugarte Postigo, Hunt, Jonker, Klose, Malesani, The properties of compact-object mergers detected C3281 Michalowski, Nicastro, Palazzi, Pellizzoni, Possenti, Tanvir, van der by LIGO and VIRGO Horst, Wieringa, Brocato, Kann, Lamb, Lekshmi, Lyman, Misra, Pian, Kim, Stanway

Moin, Ilyasi Circinus X-1 high time resolution survey C3284

Tothill, Stark, Chapman, Aravena, Marrone, Spilker, Vieira SPT0348-62: Molecular content of a high-redshift C3287 massive protocluster

Lee-Waddell, Mahony, Koribalski, Bhandari HI mapping of ESO 601-G036 and its neighbouring C3288 stellar plume

Laskar, Alexander, Berger, Bhandari, Chornock, Coppejans, Drout, van GRB physics with ATCA: Direct implications for the C3289 Eerten, Fong, Guidorzi, Margutti, Mundell, Schady explosions and progenitors

Ghaavam, Filipovic, Tothill, Kaczmarek, Maxted, Bozzetto, Maggi, ATCA radio continuum study of the LMC supernova C3292 Alsaberi, Gurovich remnant N 49: `bullet ejecta' or `bow-shock bullet ejecta' or `bow-shock' PWN

Alsaberi, Filipovic, Maitra, Maggi, Gurovich, Bozzetto, Sano, Ghaavam New bow-shocked pulsar wind in Small C3293 Magellanic Cloud

Brown, Parkash, Dzudzar, Murugeshan, Kilborn, Cluver HI galaxies with little or no star formation C3294

Filipovic, Alsaberi, Maitra, Oliveira, Ghaavam, Galvin, Grieve, A 5.5 GHz ATCA large survey of the Small Magellanic C3295 Bozzetto, Maggi, For, Crawford, O'Brien, Norris, Sano, Sasaki, Cloud (SMC) Staveley-Smith, Joseph, Wong, Tothill, Haberl, Rowell, van Loon, Bojicic, Gurovich, Gaensler, Chu, Yew, Pennock, Urosevic

Vardoulaki, Filipovic, Norris, Britzen, Rudnick, Alsaberi Revealing the putative binary nature of an X-shaped C3296 radio source behind the Small Magellanic Cloud

Dempsey, McClure-Griffiths, Buckland-Willis, Jameson Follow-up observations of HI absorption near the SMC C3297 detected by ASKAP van Den Eijnden, Degenaar, Russell, Miller-Jones, Wijnands, Sivakoff, Be/X-ray binary jets 1: jet monitoring at periastron C3298 Hernandez Santisteban, Rouco Escorial passage

55 ATCA continued

OBSERVERS PROGRAM NO

van Den Eijnden, Degenaar, Russell, Miller-Jones, Wijnands, Sivakoff, Be/X-ray binary jets 2: evolving jets during a giant C3299 Hernandez Santisteban, Rouco Escorial outburst

Troja, Piro, Ricci, Wieringa, Cenko, Lien, Sakamoto Electromagnetic counterparts to gravitational wave C3300 events

Bonato, Trombetti, Galluzzi, de Zotti, Massardi, Burigana, Negrello, A systematic search for ultra-bright high-z strongly C3301 Herranz lensed galaxies in Planck catalogues

Benaglia, De Becker, Marcote, Blanco Determining near-periastron properties of the hottest C3302 and most luminous colliding-wind binary with ATCA

Pineda, Villadsen, Moss Searching for auroral star-planet interactions C3303

Gusinskaia, Hessels, Russell, Miller-Jones, Deller, Jaodand Mapping accretion states in transitional millisecond C3307 pulsars using (quasi-)simultaneous radio and X-ray observations

Lucas, Forbrich, Thompson, Dale, Krause, Minniti, Smith, Cross, Observation of a candidate protostellar collision C3309 Dekany, Ivanov, Kurtev, Saito, Catelan

Wong, Elagali, Koss, Privon, Ricci, Smith, Trakhtenbrot Pilot SHIBS: a pilot study for the Southern HI BASS C3311 survey

Horesh, Murphy, Dobie, Qiu A study of an unexplored population of fast radio C3312 supernovae

Zhao, Dodson, Jung, Rioja, Stevens, de Vicente, Cho, Kino, Sohn, Probing the vicinity of SMBHs with high-precision C3313 Hada, Johnson, Koyama, Nakamura, Krichbaum, Zensus, Savolainen, astrometry Lu, Giroletti, Gomez, Akiyama, Rygl, Hodgson, Fraga-Encinas, Moran, Algaba, Mizuno, Ros, Pötzl, Kim

Alexander, Leahy, Heald, Riseley, Callingham, Anderson A polarised look at extended DRAGNs in Ophiuchus C3315

Fenech, Prinja, Andrews, Clark, Oskinova, Rickard Robust mass-loss measurements of massive stars: C3318 Constraining the clumping gradients in the outer winds

Horiuchi, Benner, Benson, Edwards, Stevens, Phillips, Stacy, Kruzins, Southern hemisphere radar observations of near- C3319 Giorgini, Molyneux Earth asteroids (NEAs)

Wenger, Anderson, Armentrout, Balser, Bania, Dawson, Dickey, Resolving the distance ambiguity for SHRDS HII C3320 Jordan, McClure-Griffiths regions

Orosz, Breen, Ellingsen, Voronkov, Burns, McCarthy, Hyland ATCA follow-ups of maser flares C3321

Laskar, Alexander, Berger, Bhandari, Blanchard, Chornock, ATCA follow-up of NS mergers from LIGO/Virgo in O3 C3322 Coppejans, Cowperthwaite, Duffell, Eftekhari, Fong, Gomez, Hajela, Hosseinzadeh, MacFadyen, Margutti, Metzger, Mundell, Nicholl, Paterson, Schady, Schroeder, Terreran, van Eerten, Villar, Williams, Xie

Bietenholz, Bartel, Bauer, Ellingsen, Dwarkadas, Horiuchi, Mtshweni, The spectral energy distribution of SN 1996cr two C3323 Tzioumis decades after the explosion

Cala, Gomez, Miranda Searching for SiO masers in extremely young C3324 planetary nebulae

Alexander, Wieringa, Berger, Blanchard, Chornock, Coppejans, Exploring mass ejection in SMBHs via radio C3325 Cowperthwaite, Eftekhari, Hosseinzadeh, Laskar, Margutti, Nicholl observations of TDEs

Jones, Avison, Fuller, Breen, Voronkov, Green Marking the end of evolution: The association of class C3327 II methanol masers with high-mass star formation

Kundu, Ryder Investigating the progenitors of core-collapse C3328 supernova

Huynh, Seymour, Galvin Probing the physics of high redshift AGN with water C3331 masers

Ross, Hurley-Walker, Callingham, Seymour Unexpected low-frequency spectral variability of C3333 peaked-spectrum sources

Anderson, Miller-Jones, Rau, Wilms ATCA follow-up of eROSITA-detected tidal disruption C3334 Events

Quici, Seymour Constraining the broad-band radio SED between 0.1-9 C3335 GHz for dying radio galaxies

56 Australia Telescope National Facility | Annual Report 2019–20 Parkes radio telescope

OBSERVERS PROGRAM NO

Burgay, Kramer, Manchester, Stairs, Lorimer, Possenti, McLaughlin, Timing & geodetic precession in the double pulsar P455 Wex, Ferdman, Hu

Hobbs, Coles, Manchester, Sarkissian, Wen, Zhang, Keith, Wang, A millisecond pulsar timing array P456 Kerr, Dai, van Straten, Dempsey, Russell, Spiewak, Parthasarathy, Bailes, Bhat, Levin, Oslowski, Reardon, Shannon, Zhang, Zhu, Kaczmarek

Sobey, Johnston, Dai, Kerr, Weltevrede, Shannon, Manchester, Young pulsar timing: probing the physics of pulsars and P574 Hobbs, Possenti, Kumamoto neutron stars

Hobbs, Hollow, Dai, Green, Kaczmarek, Zhang, Cameron PULSE@Parkes (Pulsar Student Exploration online at P595 Parkes)

Hobbs, Manchester, Bailes, Reynolds, Johnston, Sarkissian, Dai, Instrumental calibration for pulsar observing at Parkes P737 Green, Kaczmarek, van Straten, Jameson, Sobey, Mader, Oslowski, Shannon

Spiewak, Bailes, Barr, Burgay, Cameron, Camilo, Champion, Timing of binary & millisecond pulsars discovered at P789 Cromartie, Eatough, Ferdman, Freire, Jankowski, Johnston, Keith, Parkes Kerr, Kramer, Levin, Lorimer, Morello, Ng, Possenti, Ransom, Stappers, Ray, Stairs, van Straten, Wex

Mader, Green, Dawson, Tremblay, Bracco A search for methylidyne and hydroxyl in the Musca Dark P798 Cloud

Balakrishnan, Cameron, Champion, Kramer, Bailes, Johnston, Initial follow-up of pulsar discoveries from the HTRU P860 Possenti, Stappers, Burgay, van Straten, Bhat, Petroff, Ng, Barr, Galactic Plane survey Flynn, Jameson, Bhandari, Wongphecauxson

Camilo, Lower, Scholz, Reynolds, Sarkissian, Johnston Understanding the remarkable behaviour of radio P885 magnetars

Keane, Bailes, Barr, Bhandari, Bhat, Burgay, Caleb, Eatough, Farah, SUPERBx – The SUrvey for Pulsars & Extragalactic Radio P892 Flynn, Green, Jankowski, Jameson, Johnston, Kramer, Levin, Bursts Extension Morello, Ng, Petroff, Possenti, Primak, Spiewak, Stappers, van Straten, Tiburzi, Venkatraman Krishnan

Hobbs, Coles, Keith, Manchester, Sarkissian, Kerr, Wen, Dempsey, Where are the gravitational waves? P895 You, Rosado, Lasky, Toomey, Zhang, Ravi, Wang, Russell, Spiewak, Bailes, Bhat, Burke, Oslowski, van Straten, Zhu, Dai, Reardon, Parthasarathy, Shannon

Green, Robishaw, Mader, Tremblay, Dawson, Breen, Ogbodo Dark magnetic fields P935

Possenti, Ducci, Mereghetti, Burgay Catching the first transitional pulsar in an early-type P945 binary system

Shannon, Oslowski, Bannister, Macquart, Bhandari, Deller, Studying the southern repeating fast radio burst P958 Dodson, Flynn, Kerr, James, Qiu, Farah, Phillips, Zhang, Kumar population with Parkes

Mader, Green, Kaczmarek, Robishaw Receiver characterisation P960

Venkatraman Krishnan, Reardon, Bailes, van Straten, Keane, Orbital dynamics and the intra-binary medium of PSR P971 Oslowski, Bhat, Flynn J1141‑6545

Dawson, Bracco, Green, Joncas, Grenier, Hill, Lee, Mader, Wardle, Simultaneous UWL observations of OH and CH in a P974 Robishaw, Dame, Nguyen, Petzler, Miville-Deschenes, Krishnarao, pristine high-latitude cloud: benchmarking dark gas Marchal tracers

Zhang, Hobbs, Li, Kaczmarek, Dai, Cameron Characterising the broadband intermittency time scale, P985 mode changing, periodicities and polarization variations of PSR J1926-0652

Kumamoto, Dai, Takahashi, Hobbs, Sobey Targeted search of steep spectrum sources with the ultra- P986 wideband receiver

Hollow, Hobbs, Green, Kaczmarek, Zhang, Dai, Toomey, Cameron, Maximising the science and education output from P988 Oslowski, Sobey PULSE@Parkes and OPTIMUS in the era of the wide- bandwidth receiver

Li, Hobbs, Green, Krco, Stanimirovic, McClure-Griffiths, Dai, A follow-up study of stimulated emission toward PSR P990 Cameron, Kaczmarek, Weisberg, Zhang B1641-45

Dai, Zhang, Johnston, Hobbs A pulsar survey towards the Galactic Centre with the P991 ultra‑wideband low receiver

57 Parkes radio telescope continued

OBSERVERS PROGRAM NO

Han, Manchester, van Straten, Hobbs, Zhou Magnetic field reversals in distant spiral arms P996

Xie, Hobbs, Li, Wang, Zhang, Dai Wideband receiver observations of bright pulsars: Flux P1004 density measurements Cameron, Champion, Kramer, Bailes, Johnston, Possenti, Stappers, Mapping the orbits of two nulling, long spin-period P1005 Balakrishnan pulsars Zhang, Hobbs, Li, Dai, Toomey, Cameron, Zhu The first ultra-high time resolution coherently P1006 de‑dispersed search for new pulsars in globular clusters Main, Antoniadis, Mahajan, Lin, Wucknitz An ultra-wideband study of plasma lensing in eclipsing P1007 binaries Tiburzi, Shaifullah, Verbiest, Janssen, Oslowski, Zucca, Moochickal Tracking the solar wind with pulsars P1008 Ambalappat, Fallows Tiburzi, Verbiest, Shaifullah, Zucca, Janssen, Oslowski, Fallows, Tracking the solar wind with pulsars P1008 Sarkissian, Donner, Moochickal Ambalappat Posselt, Dai, Manchester, Weltevrede, Pavlov Probing for radio – X-ray correlations in the pulse profile P1010 of PSRB1055-52 Jankowski, Keane, Stappers A wideband survey of pulsars with spectral features P1011 Wang, Li, Lorimer, Cordes, Chatterjee, Pan, Zhu, Hobbs, Lynch, Confirming a certain dispersion measures range of pulsar P1012 Wang, Cameron, Qian candidates Meyers, Hobbs, Johnston, Dai, Wang, Shannon, Tremblay, Bhat An ultra-wideband study of the intermittent pulsar J1107- P1013 5907 Liu, Krco, Li, Hobbs, Dawson, Stanimirovic A search for small-scale structures in the ISM (few to P1014 hundreds of AU scales) Li, Simard, Kirsten, Baker, Macquart, Main, Marthi, Pen Testing models of interstellar scintillation with the Vela P1015 pulsar Kaczmarek, Hobbs, Oslowski, Dai, Johnston Instant GRRATificiation P1016 Anderson, Kaczmarek, O'Sullivan, Carretti, Heald, Leahy, The CenA lobes in ultra-high definition: Precision radio P1017 McClure‑Griffiths, Sobey galaxy astrophysics with the Parkes UWL receiver and ASKAP Zic, Lynch, Murphy, Price, Kaplan, Lenc, Croft Wide-band radio monitoring of space weather on P1018 van Jaarsveld, Stappers, Camilo, McBride Searching for pulsations from a newly discovered pulsar P1019 bowshock nebula discovered with MeerKAT Cameron, Champion, Kramer, Balakrishnan, Bailes, Johnston, Mapping the orbit of an enigmatic 1.5-yr eclipsing binary P1021 Stappers, Possenti pulsar. Zhang, Hobbs, Li, Dai, Toomey, Kaczmarek, Wang The first well-calibrated, coherent de-dispersed search P1022 for pulsars in 47 Tucanae Horiuchi, Benner, Benson, Edwards, Stevens, Phillips, Stacy, Southern hemisphere radar observations of near-Earth P1024 Kruzins, Giorgini, Molyneux asteroids (NEAs) Corongiu, Belfiore, Burgay, Clark, Nieder, de Luca, Mignani, Monitoring the radio pulsations and eclipses of the RB P1025 Possenti, Ridolfi pulsar PSR J2039-5617. Dai, Cameron, Kaplan, Hobbs, Lenc, Murphy Follow-up of the ASKAP discovery of millisecond pulsar P1027 J1431-6328 Spitler, Wharton, Kramer, Johnston, Main, Eatough, Noutsos, Shao, Wideband characterization of Galactic center pulsars P1028 Desvignes, Torne, Liu Hobbs, Johnston, Li Catching a pulse in the act of nulling P1029 McSweeney, Bhat The frequency-dependent phase shifts of subpulses due P1030 to relativistic effects Primak, van Straten, Tiburzi, Parthasarathy A pilot study to demonstrate novel radio pulsar emission P1031 analysis techniques Venkatraman Krishnan, Freire, Kramer, Champion, Parthasarathy, Mass measurements of southern binary pulsar systems P1032 Buchner, Lower Venkatraman Krishnan, Freire Estimating the Shapiro delay in the binary pulsar system P1033 PSR J1748-2021B

58 Australia Telescope National Facility | Annual Report 2019–20 OBSERVERS PROGRAM NO

Dai, Johnston, Kumamoto Follow-up of the first millisecond pulsar discoveries in P1034 Omega Centauri and a new coherently de-dispersed survey Li, Cameron, Hobbs, Zhang, Dai, Toomey, Dempsey, Zhu, Pan, FAST: category 1 PX500 Green, Kaczmarek, Wang, Wang, Miao, Yuan Li, Cameron, Hobbs, Zhang, Dai, Toomey, Dempsey, Zhu, Pan, FAST: category 2 PX501 Green, Kaczmarek, Wang, Wang, Miao, Yuan Siemion, Price, McMahon, Lebofsky, Isaacson, Gajjar, and the Breakthrough Listen BL Berkeley SETI Institute

LBA

OBSERVERS PROGRAM NO

Kumar, Ellingsen, Reid, Brunthaler, Menten, Honma, Rioja, Dodson, Astrometric observation of methanol masers: V255 Chibueze, Green, Krishnan, Sakai, Breen, Chen, Dawson, Fujisawa, determining Galactic structure and investigating high- Phillips, Sanna, Shen, Xu, Voronkov, Zheng, Goedhart, Zhang, mass star formation Hyland, Orosz Atri, Miller-Jones, Jonker, Maccarone, Nelemans, Sivakoff, Tzioumis Constraining black hole formation with LBA astrometry V447 Burns, Rioja, , Honma, Handa, Sakai, Ellingsen, Dodson, Orosz, 6.7 GHz maser parallax of a particularly interesting high- V525 Sugiyama, Krishnan mass star forming region Orosz, Gomez, Tafoya, Imai, Suarez, Burns, Ellingsen, Hyland, Astrometric measurements of the first water fountain V544 Horiuchi planetary nebula Yang, Deller, Reynolds, Quick, Hobbs, Weston, Gurvits, Paragi, An, Toward a sub- accuracy for VLBI distance V558 Hong, Chen, Xia, Yan, Guo, Ding, Li, Chen, Xu, Hao measurement of PSR J0437-4715 Kirichenko, Shternin, Tanashkin, Shibanov, Voronkov, Zyuzin, Determining the distance to PSR B1727-47 by parallax V560 Danilenko measurements with VLBI Xu, Zhang Distance and rotation of R Dor via VLBI maser astrometry V576 Main, Baker, Deller, Kirsten, Reardon, Wucknitz Imaging the scattering screens of PSR J0437-4715 V580 Burns, Breen, Orosz, Ellingsen, Sugiyama, Hirota, Kim, MacLeod, VLBI follow-ups of maser flares V581 Brogan, Sobolev, Bayandina, Olech, van Den Heever Riseley, Reynolds, Radcliffe Resolving the core/jet system of the giant radio galaxy V582 ESO 422-G028 Titov, Shu, Zhang, Xu, He, Chen, Anderson, Phillips, Lunz, VLBI observations of radio stars using large radio V583 Heinkelmann, Lopez telescopes Golden, Reynolds Resolving stellar magnetospheres using the LBA V586 Ramakrishnan, Nagar, Bignall, Reynolds EHT+ sample: parsec-scale structure of nearby AGNs V587 Edwards, Stevens, Corbet, Marcote, Strader, Reynolds A first epoch LBA observation of a new gamma-ray binary V589 Marcote, Benaglia, De Becker, Blanco, Blanchard Determining near-periastron properties of the hottest V191 and most luminous colliding-wind binary with LBA Ojha, Kadler, Edwards, Ros, Wilms, Angioni, Beuchert, Dutka, Physics of gamma-ray emitting AGN V252 Eberl, Fey, Hase, Horiuchi, Jauncey, Johnston, Katz, Klockner, Krauß, Kreter, Langejahn, Lindeholz, Lister, McEnery, Nesci, Phillips, Plotz, Pursimo, Quick, Reynolds, Rosch, Schulz, Taylor, Thompson, Tingay, Tosti, Tzioumis, Weber, Zensus Bietenholz, Bartel, Bauer, Ellingsen, Dwarkadas, Horiuchi, Structure and size of SN 1996cr, the strongest V253 Mtshweni, Tzioumis optically‑identified radio supernova

CDSCC

OBSERVERS PROGRAM NO

Orosz, Gomez, Horiuchi, Imai Monitoring of H2O masers in all known water fountains T215 Horiuchi, Benner, Benson, Edwards, Stevens, Phillips, Stacy, Southern hemisphere radar observations of near-Earth C3319 Kruzins, Giorgini, Molyneux asteroids

59 H: Publications

Papers citing data from, or related to, ATNF telescopes, and other staff papers, from the calendar year 2019.

Journal publications *Anderson, C.S.; O’Sullivan, S.P.; *Barnes, A.T.; Longmore, S.N.; Heald, G.H.; Hodgson, T.; Pasetto, A.; Avison, A.; Contreras, Y.; Ginsburg, *Acciari, V.A.; Ansoldi, S.; Antonelli, Gaensler, B.M. “Blazar jet evolution A.; Henshaw, J.D.; Rathborne, J.M.; L.A.; Engels, A.A.; Baack, D.; Babić, A.; revealed by multi-epoch broad-band Walker, D.L.; Alves, J.; Bally, J.; and 12 Banerjee, B.; Barres de Almeida, U.; radio polarimetry”. MNRAS, 485, coauthors. “Young massive Barrio, J.A.; Becerra González, J. and 3600-3622 (C) formation in the Galactic Centre is 297 coauthors. “Observation of inverse driven by global gravitational collapse Compton emission from a long γ-ray Andrews, H.; Fenech, D.; Prinja, of high-mass molecular clouds”. burst”. Nature, 575, 459-463 (C) R.K.; Clark, J.S.; Hindson, L. “A radio MNRAS, 486, 283-303 (O) census of the massive stellar cluster *Agarwal, D.; Lorimer, D.R.; Fialkov, A.; Westerlund 1”. A&A, 632, 38 (C) *Barry, N.; Wilensky, M.; Trott, C.M.; Bannister, K.W.; Shannon, R.M.; Farah, Pindor, B.; Beardsley, A.P.; Hazelton, W.; Bhandari, S.; Macquart, J.-P.; Flynn, *Angioni, R.; Ros, E.; Kadler, M.; Ojha, B.J.; Sullivan, I.S.; Morales, M.F.; C.; Pignata, G.; and 12 coauthors. “A R.; Müller, C.; Edwards, P.G.; Burd, P.R.; Pober, J.C.; Line, J.; and 20 coauthors. fast radio burst in the direction of the Carpenter, B.; Dutka, M.S.; Gulyaev, “Improving the Epoch of Reionization Virgo Cluster”. MNRAS, 490, 1-8 (A) S.; and 15 coauthors. “Gamma-ray power spectrum results from emission in radio galaxies under Murchison Widefield Array season 1 Agliozzo, C.; Mehner, A.; Phillips, N.M.; the VLBI scope. I. Parsec-scale jet observations”. ApJ, 884, 1 (O) Leto, P.; Groh, J.H.; Noriega-Crespo, kinematics and high-energy properties A.; Buemi, C.; Cavallaro, F.; Cerrigone, of γ-ray-detected TANAMI radio *Bassi, T.; Del Santo, M.; D’Aì, A.; L.; Ingallinera, A.; and 4 coauthors. galaxies”. A&A, 627, 148 (V) Motta, S.E.; Malzac, J.; Segreto, A.; “A massive nebula around the Miller-Jones, J.C.A.; Atri, P.; Plotkin, luminous blue RMC 143 *Atri, P.; Miller-Jones, J.C.A.; R.M.; Belloni, T.M.; and 2 coauthors. revealed by ALMA”. A&A, 626, 126 (C) Bahramian, A.; Plotkin, R.M.; Jonker, “The long outburst of the black hole P.G.; Nelemans, G.; Maccarone, T.J.; transient GRS 1716-249 observed in the *Allison, J.R.; Mahony, E.K.; Moss, V.A.; Sivakoff, G.R.; Deller, A.T.; Chaty, X-ray and radio band”. MNRAS, 482, Sadler, E.M.; Whiting, M.T.; Allison, S.; and 7 coauthors. “Potential kick 1587-1601 (C,V) R.F.; Bland-Hawthorn, J.; Curran, S.J.; velocity distribution of black hole Emonts, B.H.C.; Lagos, C.D.P.; and 6 X-ray binaries and implications for *Beardsley, A.P.; Johnston-Hollitt, coauthors. “PKS B1740-517: an ALMA natal kicks”. MNRAS, 489, 3116-3134 (V) M.; Trott, C.M.; Pober, J.C.; Morgan, view of the cold gas feeding a distant J.; Oberoi, D.; Kaplan, D.L.; Lynch, interacting young radio galaxy”. *Banfield, J.; O’Sullivan, S.; Wieringa, C.R.; Anderson, G.E.; McCauley, P.I.; MNRAS, 482, 2934-2949 (A) M.H.; Emonts, B.H.C. “Faraday and 49 coauthors. “Science with the rotation study of NGC 612 (PKS Murchison Widefield Array: Phase I *Alsaberi, R.Z.E.; Barnes, L.A.; 0131-36): a hybrid radio source results and Phase II opportunities”. Filipović, M.D.; Maxted, N.I.; Sano, H.; and its magnetized circumgalactic PASA, 36, e050 (O) Rowell, G.; Bozzetto, L.M.; Gurovich, environment”. MNRAS, 482, 5250-5258 S.; Urošević, D.; Onić, D.; and 12 (C) *Bell, M.E.; Murphy, T.; Hancock, P.J.; coauthors. “Radio emission from Callingham, J.R.; Johnston, S.; Kaplan, interstellar shocks: Young type Ia *Bannister, K.W.; Deller, A.T.; Phillips, D.L.; Hunstead, R.W.; Sadler, E.M.; supernova remnants and the case of N C.; Macquart, J.-P.; Prochaska, J.X.; Croft, S.; White, S.V.; and 31 coauthors. 103B in the Large Magellanic Cloud”. Tejos, N.; Ryder, S. D.; Sadler, E.M.; “The Murchison Widefield Array Ap&SS, 364, 204 (C) Shannon, R.M.; Simha, S.; and 44 Transients Survey (MWATS). A search coauthors. “A single fast radio burst for low-frequency variability in a *Alsaberi, R.Z.E.; Maitra, C.; Filipović, localized to a massive galaxy at bright Southern hemisphere sample”. M.D.; Bozzetto, L.M.; Haberl, F.; Maggi, cosmological distance”. Science, 365, MNRAS, 482, 2484-2501 (O) P.; Sasaki, M.; Manjolovic, P.; Velovic, 565-570 (A,C) V.; Kavanagh, P.; and 25 coauthors. “Discovery of a pulsar-powered bow shock nebula in the Small Magellanic Cloud supernova remnant DEM S5”. MNRAS, 486, 2507-2524 (C)

60 Australia Telescope National Facility | Annual Report 2019–20 *Bernal, J.L.; Raccanelli, A.; Kovetz, *Brook, P.R.; Karastergiou, A.; *Chanapote, T.; Asanok, K.; E.D.; Parkinson, D.; Norris, R.P.; Johnston, S. “Linking long- and Dodson, R.; Rioja, M.; Green, J.A.; Danforth, G.; Schmitt, C. “Probing short‑term emission variability in Hutawarakorn Kramer, B. “Tracing the Lambda CDM cosmology with the pulsars”. MNRAS, 488, 5702-5712 (P) magnetic field and other properties of Evolutionary Map of the Universe G351.417+0.645 at subarcsecond scales survey”. JCAP, 2, 30 (A) *Burgay, M.; Stappers, B.; Bailes, with the Long Baseline Array”. MNRAS, M.; Barr, E.D.; Bates, S.; Bhat, N.D.R.; 482, 1670‑1689 (V) *Bhandari, S.; Bannister, K.W.; James, Burke-Spolaor, S.; Cameron, A.D.; C.W.; Shannon, R.M.; Flynn, C.M.; Champion, D.J.; Eatough, R.P.; *Chanapote, T.; Dodson, R.; Rioja, M.; Caleb, M.; Bunton, J.D. “A southern sky and 14 coauthors. “The High Time Asanok, K.; Stevens, J.; Martí-Vidal, search for repeating fast radio bursts Resolution Universe Pulsar Survey – I. “Demonstration of polarisation using the Australian SKA Pathfinder”. XV. Completion of the intermediate- calibration with the LBA on selected MNRAS, 486, 70-76 (A) latitude survey with the discovery and AGNs”. PASA, 36, e013 (V) timing of 25 further pulsars”. MNRAS, *Bignall, H.; Reynolds, C.; Stevens, 484, 5791-5801 (P) *Chatys, F.W.; Bedding, T.R.; Murphy, J.; Bannister, K.; Johnston, S.; S.J.; Kiss, L.L.; Dobie, D.; Grindlay, J.E. Tuntsov, A.V.; Walker, M.A.; Gulyaev, *Butler, A.; Huynh, M.; Kapińska, A.; “The period– relation of red S.; Natusch, T.; Weston, S.; and Delvecchio, I.; Smolčić, V.; Chiappetti, supergiants with Gaia DR2”. MNRAS, 2 coauthors. “Spica and the annual L.; Koulouridis, E.; Pierre, M. “The XXL 487, 4832-4846 (O) cycle of PKS B1322-110 scintillations”. Survey. XXXVI. Evolution and black MNRAS, 487, 4372-4381 (C) hole feedback of high-excitation and *Chauhan, J.; Miller-Jones, J.C.A.; low-excitation radio galaxies in XXL-S”. Anderson, G.E.; Raja, W.; Bahramian, Billington, S.J.; Urquhart, J.S.; Figura, A&A, 625, 111 (C) A.; Hotan, A.; Indermuehle, B.; C.; Eden, D.J.; Moore, T.J.T. “The RMS Whiting, M.; Allison, J.R.; Anderson, survey: mapping of the Caleb, M.; van Straten, W.; Keane, E.F.; C.; and 3 coauthors. “An H I absorption environment of young massive stellar Jameson, A.; Bailes, M.; Barr, E.D.; distance to the black hole candidate objects – II”. MNRAS, 483, 3146-3167 (C) Flynn, C.; Ilie, C. D.; Petroff, E.; Rogers, X-ray binary MAXI J1535-571”. MNRAS, A.; and 3 coauthors. “Polarization 488, L129-L133 (A) *Bolli, P.; Orfei, A.; Zanichelli, A.; studies of rotating radio transients”. Prestage, R.; Tingay, S.J.; Beltrán, M.; MNRAS, 487, 1191-1199 (P) *Clarke, A.O.; Scaife, A.M.M.; Burgay, M.; Contavalle, C.; Honma, Shimwell, T.; van Weeren, R.J.; M.; Kraus, A.; and 11 coauthors. Callingham, J.R.; Tuthill, P.G.; Pope, Bonafede, A.; Heald, G.; Brunetti, “An international survey of front-end B.J.S.; Williams, P.M.; Crowther, G.; Cantwell, T.M.; de Gasperin, receivers and observing performance P.A.; Edwards, M.; Norris, B.; F.; Brüggen, M.; and 6 coauthors. of telescopes for radio astronomy”. Kedziora‑Chudczer, L. “Anisotropic “Signatures from a merging galaxy PASP, 131, 85002 (P,M) winds in a Wolf-Rayet binary identify a cluster and its AGN population: LOFAR potential gamma-ray burst progenitor”. observations of Abell 1682”. A&A, *Breen, S.L.; Contreras, Y.; Dawson, Nature Astronomy, 3, 82-87 (C) 627, 176 (O) J.R.; Ellingsen, S.P.; Voronkov, M.A.; McCarthy, T.P. “84-GHz methanol Calzadilla, M.S.; McDonald, M.; Bayliss, Contreras, Y.; Rebolledo, D.; Breen, masers, their relationship to 36-GHz M.; Benson, B.A.; Bleem, L.E.; Brodwin, S.L.; Green, A.J.; Burton, M.G. methanol masers, and their molecular M.; Edge, A.C.; Floyd, B.; Gupta, N.; “Environmental conditions shaping environments”. MNRAS, 484, Hlavacek-Larrondo, J.; and 2 coauthors. star formation: the Carina Nebula”. 5072‑5093 (M) “Discovery of a Powerful >1061 erg AGN MNRAS, 483, 1437-1451 (M) Outburst in the Distant Galaxy Cluster *Breen, S.L.; Sobolev, A.M.; Kaczmarek, SPT-CLJ0528-5300”. ApJ, 887, L17 (C) J.F.; Ellingsen, S.P.; McCarthy, T.P.; Voronkov, M.A. “Discovery of six new *Carretti, E.; Haverkorn, M.; Staveley- class II methanol maser transitions, Smith, L.; Bernardi, G.; Gaensler, B.M.; including the unambiguous detection Kesteven, M.J.; Poppi, S.; Brown, of three torsionally excited lines S.; Crocker, R.M.; Purcell, C.; and 2 toward G 358.931-0.030”. ApJ, 876, coauthors. “S-band Polarization All‑Sky L25 (C) Survey (S-PASS): survey description Legend and maps”. MNRAS, 489, 2330-2354 (P) * Authors include ATNF staff A ASKAP C ATCA M Mopra O Other staff paper P Parkes S SKA T Tidbinbilla (CDSCC) V VLBI

61 *Corbet, R.H.D.; Chomiuk, L.; Coe, M.J.; Dénes, H.; Jones, P.A.; Tóth, L.V.; *Duncan, K.J.; Sabater, J.; Röttgering, Coley, J.B.; Dubus, G.; Edwards, P.G.; Zahorecz, S.; Koo, B.-C.; Pinter, S.; H.J.A.; Jarvis, M.J.; Smith, D.J.B.; Best, Martin, P.; McBride, V.A.; Stevens, J.; Racz, I.I.; Balázs, L.G.; Cunningham, P.N.; Callingham, J.R.; Cochrane, R.; Strader, J.; Townsend, L.J. “Discovery M.R.; Doi, Y.; and 5 coauthors. Croston, J.H.; Hardcastle, M.J.; and of the galactic high-mass gamma‑ray “Exploring the pattern of the Galactic 17 coauthors. “The LOFAR Two-metre binary 4FGL J1405.1-6119”. ApJ, H I foreground of GRBs with the ATCA”. Sky Survey. IV. First data release: 884, 93 (C) MNRAS, 489, 3778-3796 (C) Photometric and rest-frame magnitudes”. A&A, 622, 3 (O) *Coriat, M.; Fender, R.P.; Tasse, C.; Di Teodoro, E.M.; McClure-Griffiths, Smirnov, O.; Tzioumis, A.K.; Broderick, N.M.; De Breuck, C.; Armillotta, L.; *Dzudzar, R.; Kilborn, V.; Meurer, G.; J.W. “The twisted jets of Circinus X-1”. Pingel, N.M.; Jameson, K.E.; Dickey, Sweet, S.M.; Drinkwater, M.; Bekki, K.; MNRAS, 484, 1672-1686 (C) J.M.; Rubio, M.; Stanimirović, S.; Audcent-Ross, F.; Koribalski, B.; Kim, Staveley-Smith, L. “Molecular gas in J.H.; Putman, M.; and 16 coauthors. Coti Zelati, F.; Papitto, A.; de Martino, the outflow of the Small Magellanic “The neutral hydrogen properties of D.; Buckley, D.A.H.; Odendaal, A.; Li, Cloud”. ApJ, 885, L32 (A) galaxies in gas-rich groups”. MNRAS, J.; Russell, T.D.; Torres, D.F.; Mazzola, 483, 5409-5425 (C) S.M.; Bozzo, E.; and 5 coauthors. *Di Teodoro, E.M.; McClure-Griffiths, “Prolonged sub-luminous state of N.M.; Jameson, K.E.; Dénes, H.; Dickey, *Eden, D.J.; Liu, T.; Kim, K.-T.; the new transitional pulsar candidate J.M.; Stanimirović, S.; Staveley‑Smith, Juvela, M.; Liu, S.-Y.; Tatematsu, K.; CXOU J110926.4-650224”. A&A, L.; Anderson, C.; Bunton, J.D.; Di Francsco, J.; Wang, K.; Wu, Y.; 622, 211 (C) Chippendale, A.; and 3 coauthors. “On Thompson, M.A. and 153 coauthors. the dynamics of the Small Magellanic “SCOPE: SCUBA-2 continuum *Croston, J.H.; Hardcastle, M.J.; Mingo, Cloud through high-resolution ASKAP observations of pre-protostellar B.; Best, P.N.; Sabater, J.; Shimwell, H I observations”. MNRAS, 483, evolution – survey description and T M.; Williams, W.L.; Duncan, K.J.; 392‑406 (A) compact source catalogue “. MNRAS, Röttgering, H.J.A.; Brienza, M.; and 485, 2895-2908 (O) 6 coauthors. “The environments Dickey, J.M.; Landecker, T.L.; Thomson, of radio-loud AGN from the LOFAR A.J.M.; Wolleben, M.; Sun, X.; Carretti, Eisner, B.A.; Ott, J.; Meier, D.S.; Two‑Metre Sky Survey (LoTSS)”. E.; Douglas, K.; Fletcher, A.; Gaensler, Cannon, J.M. “A spectral analysis A&A, 622, 10 (O) B.M.; Gray, A.; and 4 coauthors. of the centimeter regime of nearby

“The Galactic Magneto-ionic Medium galaxies: RRLs, excited OH, and NH3”. *Curran, S.J.; Hunstead, R.W.; Survey: Moments of the Faraday ApJ, 882, 95 (C) Johnston, H.M.; Whiting, M.T.; spectra”. ApJ, 871, 106 (P) Sadler, E.M.; Allison, J.R.; Athreya, *Elagali, A.; Staveley-Smith, L.; Rhee, R. “Ionization of the atomic gas in *Dobie, D.; Murphy, T.; Kaplan, D.L.; J.; Wong, O.I.; Bosma, A.; Westmeier, redshifted radio sources”. MNRAS, Ghosh, S.; Bannister, K.W.; Hunstead, T.; Koribalski, B. S.; Heald, G.; For, 484, 1182-1191 (O) R.W. “An optimised gravitational wave B.-Q.; Kleiner, D.; and 18 coauthors. follow-up strategy with the Australian “WALLABY early science – III. An H I *Dai, S.; Lower, M.E.; Bailes, M.; Square Kilometre Array Pathfinder”. study of the spiral galaxy NGC 1566”. Camilo, F.; Halpern, J.P.; Johnston, S.; PASA, 36, e019 (A) MNRAS, 487, 2797-2817 (A) Kerr, M.; Reynolds, J.; Sarkissian, J.; Scholz, P. “Wideband polarized radio *Dobie, D.; Stewart, A.; Murphy, Falkendal, T.; De Breuck, C.; Lehnert, emission from the newly revived T.; Lenc, E.; Wang, Z.; Kaplan, D.L.; M.D.; Drouart, G.; Vernet, J.; Emonts, Magnetar XTE J1810-197”. ApJ, 874, Andreoni, I.; Banfield, J.; Brown, B.; Lee, M.; Nesvadba, N.P.H.; Seymour, L14 (P) I.; Corsi, A.; and 20 coauthors. “An N.; Béthermin, M.; Kolwa, S.; and ASKAP search for a radio counterpart 3 coauthors. “Massive galaxies on the *de Gasperin, F.; Dijkema, T.J.; to the first high-significance neutron road to quenching: ALMA observations Drabent, A.; Mevius, M.; Rafferty, star-black hole merger LIGO/Virgo of powerful high redshift radio D.; van Weeren, R.; Brüggen, M.; S190814bv”. ApJ, 887, L13 (A,C) galaxies”. A&A, 621, 27 (C) Callingham, J.R.; Emig, K.L.; Heald, G.; and 10 coauthors. “Systematic effects Duchesne, S.W.; Johnston-Hollitt, M. *Farah, W.; Flynn, C.; Bailes, in LOFAR data: A unified calibration “The remnant radio galaxy associated M.; Jameson, A.; Bateman, T.; strategy”. A&A, 622, 5 (O) with NGC 1534”. PASA, 36, e016 (C) Campbell‑Wilson, D.; Day, C.K.; Deller, A.T.; Green, A.J.; Gupta, V. and 19 coauthors. “Five new real-time detections of fast radio bursts with UTMOST”. MNRAS, 488, 2989-3002 (O)

62 Australia Telescope National Facility | Annual Report 2019–20 Feng, Y.; Li, Di; Li, Y.-R.; Wang, *Garon, A.F.; Rudnick, L.; Wong, O.I.; *Gürkan, G.; Hardcastle, M.J.; Best, J.-M. “Constraints on individual Jones, T.W.; Kim, J.-A.; Andernach, H.; P.N.; Morabito, L.K.; Prandoni, I.; Jarvis, supermassive binary black holes using Shabala, S.S.; Kapinska, A.D.; Norris, M.J.; Duncan, K. J.; Calistro Rivera, observations of PSR J1909-3744”. R.P.; de Gasperin, F.; and 2 coauthors. G.; Callingham, J.R.; Cochrane, R.K.; Res. Astron. Astrophys., 19, 178 (P) “: The distortion and 10 coauthors. “LoTSS/HETDEX: of radio galaxies by galaxy clusters”. Optical . I. Low-frequency Fissel, L.M.; Ade, P.A.R.; Angilè, F.E.; AJ, 157, 126 (O) radio properties of optically selected Ashton, P.; Benton, S.J.; Chen, C-Y.; quasars”. A&A, 622, 11 (O) Cunningham, M.; Devlin, M.J.; Dober, *Ghirlanda, G.; Salafia, O.S.; Paragi, B.; Friesen, R; and 30 coauthors. Z.; Giroletti, M.; Yang, J.; Marcote, Han, W.; Wang, N.; Wang, J.; Yuan, J.; “Relative alignment between the B.; Blanchard, J.; Agudo, I.; An, T.; He, D. “Using single millisecond pulsar magnetic field and molecular gas Bernardini, M.G.; Beswick, R.; and 26 for terrestrial position determination”. structure in the Vela C giant molecular coauthors. “Compact radio emission Ap&SS, 364, 48 (P) cloud using low- and high-density indicates a structured jet was tracers”. ApJ, 878, 110 (M) produced by a binary neutron star *Hancock, P.J.; Anderson, G.E.; merger”. Science, 363, 968-971 (O) Williams, A.; Sokolowski, M.; *For, B.-Q.; Staveley-Smith, L.; Tremblay, S.E.; Rowlinson, A.; Crosse, Westmeier, T.; Whiting, M.; Oh, *Glowacki, M.; Allison, J.R.; Moss, B.; Meyers, B.W.; Lynch, C.R.; Zic, A.; S.‑H.; Koribalski, B.; Wang, J.; Wong, V.A.; Mahony, E.K.; Sadler, E.M.; and 15 coauthors. “A VOEvent-based O. I.; Bekiaris, G.; Cortese, L.; and Callingham, J.R.; Ellison, S.L.; Whiting, automatic trigger system for the 12 coauthors. “WALLABY early M.T.; Bunton, J.D.; Chippendale, A.P.; Murchison Widefield Array”. PASA, science – V. ASKAP H I imaging of the and 4 coauthors. “An ASKAP survey for 36, e046 (O) Lyon Group of Galaxies 351”. MNRAS, HI absorption towards dust-obscured 489, 5723-5741 (A) quasars”. MNRAS, 489, 4926-4943 (A) Harada, R.; Onishi, T.; Tokuda, K.; Zahorecz, S.; Hughes, A.; Meixner, M.; *Franzen, T.M O.; Vernstrom, T.; *González-Lópezlira, R.A.; Mayya, Y.D.; Sewilo, M.; Indebetouw, R.; Nayak, O.; Jackson, C.A.; Hurley-Walker, N.; Ekers, Loinard, L.; Álamo-Martínez, K.; Heald, Fukui, Y.; and 7 coauthors. “Formation R.D.; Heald, G.; Seymour, N.; White, G.; Georgiev, I.Y.; Órdenes-Briceño, of high-mass stars in an isolated S.V. “Source counts and confusion Y.; Lançon, A.; and 4 coauthors. environment in the Large Magellanic at 72-231 MHz in the MWA GLEAM “Spectroscopy of NGC 4258 globular Cloud”. PASJ, 71, 44 (M) survey”. PASA, 36, e004 (O) cluster candidates: Membership confirmation and kinematics”. ApJ, *Hardcastle, M.J.; Croston, J.H.; Fujita, Y.; Kawachi, A.; Akahori, T.; 876, 39 (O) Shimwell, T.W.; Tasse, C.; Gürkan, G.; Nagai, H.; Yamaguchi, M. “First Morganti, R.; Murgia, M.; Röttgering, detection of PSR B1259-63/LS 2883 Gorgone, N.M.; Kouveliotou, C.; H.J.A.; van Weeren, R.J.; Williams, W.L. in the millimeter and submillimeter Negoro, H.; Wijers, R.A.M.J.; Bozzo, “NGC 326: X-shaped no more”. MNRAS, wavelengths with ALMA”. PASJ, 71, L3 E.; Guiriec, S.; Bult, P.; Huppenkothen, 488, 3416-3422 (O) (C) D.; Göğüs, E.; Bahramian, A.; Kennea, J.; Linford, J.D.; and 19 coauthors. *Hardcastle, M.J.; Williams, W.L.; *Galluzzi, V.; Puglisi, G.; Burkutean, “Discovery and identification of MAXI Best, P.N.; Croston, J.H.; Duncan, S.; Liuzzo, E.; Bonato, M.; Massardi, J1621-501 as a Type I X-ray burster K.J.; Röttgering, H.J.A.; Sabater, J.; M.; Paladino, R.; Gregorini, L.; Ricci, with a super-orbital period”. ApJ, Shimwell, T.W.; Tasse, C.; Callingham, R.; Trombetti, T.; and 10 coauthors. 884, 168 (C) J.R.; and 13 coauthors. “Radio-loud “ALMA Band 3 polarimetric follow-up AGN in the first LoTSS data release. The of a complete sample of faint PACO *Gotthelf, E.V.; Halpern, J.P.; Alford, lifetimes and environmental impact of sources”. MNRAS, 489, 470-486 (C) J.A.J.; Mihara, T.; Negoro, H.; Kawai, jet-driven sources”. A&A, 622, 12 (O) N.; Dai, S.; Lower, M.E.; Johnston, S.; *Galvin, T.; Huynh, M.; Norris, R.P.; Bailes, M.; and 4 coauthors. “The 2018 *Heesen, V.; Buie, E., II; Huff, C.J.; Wang, X.R.; Hopkins, E.; Wong, O.I.; X-ray and radio outburst of Magnetar Perez, L.A.; Woolsey, J.G.; Rafferty, Shabala, S.; Rudnick, L.; Alger, M.J.; XTE J1810-197”. ApJ, 874, L25 (O) D.A.; Basu, A.; Beck, R.; Brinks, Polsterer, K.L. “Radio Galaxy Zoo: E.; Horellou, C.; and 9 coauthors. Knowledge transfer using rotationally Gross, J.; Williams, B.F.; Pannuti, T.G.; “Calibrating the relation of low- invariant self-organizing maps”. PASP, Binder, B.; Garofali, K.; Hanvey, Z.G. frequency radio continuum to star 131, 108009 (C) “Multiwavelength study of the X-ray formation rate at 1 kpc scale with bright supernova remnant N300-S26 LOFAR”. A&A, 622, 8 (O) in NGC 300”. ApJ, 877, 15 (C)

63 *Heesen, V.; Whitler, L.; Schmidt, P.; *James, C. W.; Ekers, R. D.; Macquart, *Kaplan, D.L.; Dai, S. Lenc, E.; Zic, A.; Miskolczi, A.; Sridhar, S.S.; Horellou, J.-P.; Bannister, K. W.; Shannon, R. Swiggum, J.K.; Murphy, T.; Anderson, C.; Beck, R.; Gürkan, G.; Scannapieco, M. “The slope of the source-count C.S.; Cameron, A.D.; Dobie, D.; Hobbs, E.; Brüggen, M.; and 6 coauthors. distribution for fast radio bursts”. G.; and 3 coauthors. “Serendipitous “Warped diffusive radio halo around MNRAS, 483, 1342-1353 (A,P) discovery of PSR J1431-6328 as a highly the quiescent spiral edge-on galaxy polarized point source with the NGC 4565”. A&A, 628, L3 (O) *James, C.W.; Bannister, K.W.; Australian SKA Pathfinder”. ApJ, 884, Macquart, J.-P.; Ekers, R.D.; Oslowski, 96 (A,P) *Hisano, S.; Yonemaru, N.; Kumamoto, S.; Shannon, R.M.; Allison, J.R.; H.; Takahashi, K. “Detailed study Chippendale, A.P.; Collier, J.D.; *Kaur, D.; Bhat, N.D.R.; Tremblay, of detection method for ultralow Franzen, T.; and 6 coauthors. “The S.E.; Shannon, R.M.; McSweeney, S.J.; frequency gravitational waves with performance and calibration of Ord, S.M.; Beardsley, A.P.; Crosse, B.; pulsar spin-down rate statistics”. the CRAFT fly’s eye fast radio burst Emrich, D.; Franzen, T.M.O.; and 13 MNRAS, 487, 97-103 (O) survey”. PASA, 36, 009 (A,P) coauthors. “A high time-resolution study of the millisecond pulsar *Ho, A.Y.Q.; Phinney, E.S.; Ravi, V.; *James, C.W.; Bray, J.D.; Ekers, J2241‑5236 at frequencies below Kulkarni, S.R.; Petitpas, G.; Emonts, R.D. “Prospects for detecting 300 MHz”. ApJ, 882, 133 (O) B.; Bhalerao, V.; Blundell, R.; Cenko, ultra‑high‑energy particles with FAST”. S.B.; Dobie, D.; and 7 coauthors. Res. Astron. Astrophys, 19, 19 (O) *Kirsten, F.; Bhat, N.D.R.; Meyers, “AT2018cow: A luminous millimeter B.W.; Macquart, J.-P.; Tremblay, S.E.; transient”. ApJ, 871, 73 (C) Jameson, K.; McClure-Griffiths, N.; Ord, S.M. “Probing pulsar scattering Liu, B.; Dickey, J.; Staveley-Smith, L.; between 120 and 280 MHz with the *Hobbs, G,; Dai, S.; Manchester, R.N.; Stanimirovic, S.; Dempsey, J.; Dawson, MWA”. ApJ, 874, 179 (O) Shannon, R.M.; Kerr, M.; Lee, K.-J.; J.; Denies, H.; Bolatto, A.; Wong, T. Xu, R.-X. “The role of FAST in pulsar “An ATCA survey of HI absorption *Kleiner, D.; Koribalski, B.S.; Serra, timing arrays”. Res. Astron. Astrophys, in the Magellanic Clouds: I. HI gas P.; Whiting, M.T.; Westmeier, T.; 19, 20 (O) temperature measurements in the Wong, O.I.; Kamphuis, P.; Popping, Small Magellanic Cloud”. ApJS, A.; Bekiaris, G.; Elagali, A. and *Hong, T.; Staveley-Smith, L.; Masters, 244, 7 (C) 12 co‑authors. “WALLABY early K.L.; Springob, C.M.; Macri, L.M.; science – IV. ASKAP HI imaging of Koribalski, B.S.; Heath Jones, D.; *Jankowski, F.; Bailes, M.; van Straten, the nearby galaxy IC520”. MNRAS, Jarrett, T.H.; Crook, A.C.; Howlett, C.; W.; Keane, E.F.; Flynn, C.; Barr, E.D.; 488, 5352‑5369 (A) Qin, F. “2MTF – VII. 2MASS Tully-Fisher Bateman, T.; Bhandari, S.; Caleb, M.; survey final data release: distances for Campbell-Wilson, D.; and 8 coauthors. Klose, S.; Nicuesa Guelbenzu, 2062 nearby spiral galaxies”. MNRAS, “The UTMOST pulsar timing A.M.; Michałowski, M.J.; Hunt, L.K.; 487, 2061-2069 (P) programme I: Overview and first Hartmann, D.H.; Greiner, J.; Rossi, results”. MNRAS, 484, 3691-3712 (O) A.; Palazzi, E.; Bernuzzi, S. “Deep *Ilie, C.D.; Johnston, S.; Weltevrede, P. ATCA and VLA radio observations of “Evidence for magnetospheric effects *Johnston, S.; Karastergiou, A. “The short‑GRB host galaxies. Constraints on the radiation of radio pulsars”. period-width relationship for radio on star formation rates, afterglow flux, MNRAS, 483, 2778-2794 (P) pulsars revisited”. MNRAS, 485, and kilonova radio flares”. ApJ, 887, 640‑647 (P) 206 (C) *Ingallinera, A.; Umana, G.; Trigilio, C.; Norris, R.; Franzen, T.M.O.; Cavallaro, *Johnston, S.; Kramer, M. “On the *Koay, J.Y.; Jauncey, D.L.; Hovatta, F.; Leto, P.; Buemi, C.; Schillirò, F.; beam properties of radio pulsars with T.; Kiehlmann, S.; Bignall, H.E.; Bufano, F.; and 3 coauthors. “Study interpulse emission”. MNRAS, 490, Max-Moerbeck, W.; Pearson, T.J.; of the galactic radio sources in the 4565-4574 (P) Readhead, A.C.S.; Reeves, R.; Reynolds, SCORPIO survey resolved by ATCA at C.; Vedantham, H. “The presence *Joseph, T.D.; Filipović, M.D.; 2.1 GHz”. MNRAS, 490, 5063-5077 (C) of interstellar scintillation in the Crawford, E.J.; Bojičić, I.; Alexander, 15 GHz interday variability of 1158 *Jackson, J.M.; Whitaker, J.S.; E.L.; Wong, G.F.; Andernach, H.; OVRO‑monitored blazars”. MNRAS, Rathborne, J.M.; Foster, J.B.; Contreras, Leverenz, H.; Norris, R.P.; Alsaberi, 489, 5365-5380 (O) Y.; Sanhueza, P.; Stephens, I.W.; R.Z.E. and 46 coauthors. “The ASKAP Longmore, S.N.; Allingham, D. EMU Early Science Project: radio *Kumamoto, H.; Imasato, Y.; Yonemaru, “Asymmetric line profiles in dense continuum survey of the Small N.; Kuroyanagi, S.; Takahashi, K. molecular clumps observed in Magellanic Cloud”. MNRAS, 490, “Constraints on ultra‑low-frequency MALT90: Evidence for global collapse”. 1202‑1219 (A) gravitational waves with statistics of ApJ, 870, 5 (M) pulsar spin‑down rates”. MNRAS, 489, 3547‑3552 (O)

64 Australia Telescope National Facility | Annual Report 2019–20 *Kumar, P.; Shannon, R.M.; Osłowski, *Li, W.; Pober, J.C.; Barry, N.; Hazelton, *Luken, K.J.; Norris, R.P.; Park, L.A.F. S.; Qiu, H.; Bhandari, S.; Farah, W.; B.J.; Morales, M.F.; Trott, C.M.; “Preliminary results of using k-nearest Flynn, C.; Kerr, M.; Lorimer, D.R.; Lanman, A.; Wilensky, M.; Sullivan, neighbors regression to estimate the Macquart, J.-P.; and 4 coauthors. “Faint I.; Beardsley, A.P.; and 37 coauthors. redshift of radio-selected data sets”. repetitions from a bright Fast Radio “First season MWA Phase II EoR power PASP, 131, 108003 (O) Burst source”. ApJ, 887, L30 (A,P) spectrum results at Redshift 7”. ApJ, 887, 141 (O) *MacLeod, G.C.; Sugiyama, K.; *Lalbakhsh, A.; Afzal, M.U.; Esselle, Hunter, T.R.; Quick, J.; Baan, W.; K.P.; Smith, S.L. “Wideband near-field Liu, B.; Li, D.; Staveley-Smith, L.; Qian, Breen, S.L.; Brogan, C.L.; Burns, R.A.; correction of a Fabry-Perot resonator L.; Wong, T.; Goldsmith, P. “Tracing Caratti o Garatti, A.; Chen, X.; and antenna”. IEEE Trans. Antennas the formation of molecular clouds in a 11 coauthors. “Detection of new Propag., 67, 1975-1980 (O) low-metallicity Galaxy: An H I narrow methanol maser transitions associated self-absorption Survey of the Large with G358.93‑0.03”. MNRAS, 489, *Lalbakhsh, A.; Afzal, M.U.; Magellanic Cloud”. ApJ, 887, 242 (C,P) 3981‑3989 (C) Esselle, K.P.; Smith, S.L.; Zeb, B.A. “Single‑dielectric wideband partially *Liu, K.; Young, A.; Wharton, R.; *Macquart, J.-P.; Shannon, R.M.; reflecting surface with variable Blackburn, L.; Cappallo, R.; Chatterjee, Bannister, K.W.; James, C.W.; Ekers, reflection components for realization S.; Cordes, J.M.; Crew, G.B.; Desvignes, R.D.; Bunton, J.D. “The spectral of a compact high-gain resonant G.; Doeleman, S.S.; and 13 coauthors. properties of the bright fast radio cavity antenna”. IEEE Trans. Antennas “Detection of pulses from the Vela burst population”. ApJ, 872, L19 (A) Propag., 67, 1916-1921 (O) pulsar at millimeter wavelengths with phased ALMA”. ApJ, 885, L10 (O) *Mahatma, V.H.; Hardcastle, M.J.; Lau, J.C.; Rowell, G.; Voisin, F.; Williams, W.L.; Best, P.N.; Croston, Blackwell, R.; Burton, M.G.; Braiding, Louvet, F.; Neupane, S.; Garay, G.; J.H.; Duncan, K.; Mingo, B.; Morganti, C.; Wong, G.F.; Fukui, Y.; Casanova, S. Russeil, D.; Zavagno, A.; Guzman, A.; R.; Brienza, M.; Cochrane, R.K.; “Probing the origin of the unidentified Gomez, L.; Bronfman, L.; Nony, T. “Lack and 12 coauthors. “LoTSS DR1: TeV gamma-ray source HESS J1702‑420 of high-mass pre-stellar cores in the Double‑double radio galaxies in the via the surrounding interstellar starless MDCs of NGC 6334”. A&A, 622, HETDEX field”. A&A, 622, 13 (O) medium”. MNRAS, 483, 3659-3672 (M) 99 (M) *Maitra, C.; Haberl, F.; Filipović, *Leahy, D.A.; Hopkins, A.M.; Norris, *Lower, M.E.; Bailes, M.; Shannon, M. D.; Udalski, A.; Kavanagh, P. J.; R.P.; Marvil, J.; Collier, J.D.; Taylor, E.N.; R.M.; Johnston, S.; Flynn, C.; Carpano, S.; Maggi, P.; Sasaki, M.; Allison, J.R.; Anderson, C.; Bell, M.; Bateman, T.; Campbell-Wilson, D.; Norris, R. P.; O’Brien, A.; and 13 Bilicki, M.; and 18 coauthors. “ASKAP Day, C.K.; Deller, A.; Farah, W.; and coauthors. “Discovery of a very young commissioning observations of the 13 coauthors. “Detection of a glitch high‑mass X-ray binary associated GAMA 23 field”. PASA, 36, e024 (A) in PSR J0908‑4913 by UTMOST”. Res. with the supernova remnant MCSNR Notes AAS, 3, 192 (O) J0513-6724 in the LMC”. MNRAS, 490, Lebofsky, M.; Croft, S.; Siemion, A.P.V.; 5494‑5502 (A) Price, D.C.; Enriquez, J.E.; Isaacson, *Lu, J.; Peng, B.; Xu, R.; Yu., M.; Dai, S.; H.; MacMahon, D.H.E.; Anderson, D.; Zhu, W.; Yu, Y.; Jiang, P.; Yue Y.; *Marasco, A.; Fraternali, F.; Heald, Brzycki, B.; Cobb, J. and 15 coauthors. Wang, L. “The radiation structure of G.; de Blok, W.J.G.; Oosterloo, T.; “The Breakthrough Listen Search for PSR B2016+28 observed with FAST”. Kamphuis, P.; Józsa, G. I.G.; Vargas, Intelligent Life: Public data, formats, Sci.China Phys.Mech.Astron., 62, C.J.; Winkel, B.; Walterbos, R.A.M.; reduction, and archiving”. PASP, 131, 959505 (O) and 2 coauthors. “HALOGAS: the 124505 (P) properties of extraplanar HI in disc Ludlam, R.M.; Shishkovsky, L.; galaxies”. A&A, 631, 50 (O) *Lee-Waddell, K.; Koribalski, B.S.; Bult, P.M.; Miller, J.M.; Zoghbi, A.; Westmeier, T.; Elagali, A.; For, B.-Q.; Strohmayer, T.E.; Reynolds, M.; Marcel, G.; Ferreira, J.; Clavel, M.; Kleiner, D.; Madrid, J.P.; Popping, Natalucci, L.; Miller-Jones, J.C.A.; Petrucci, P.-O.; Malzac, J.; Corbel, S.; A.; Reynolds, T.N.; Rhee, J.; and Jaisawal, G.K.; and 10 coauthors. Rodriguez, J.; Belmont, R.; Coriat, 12 coauthors. “WALLABY early “Observations of the ultra-compact M.; Henri, G.; Cangemi, F. “A unified science – II. The NGC 7232 galaxy X-Ray binary 4U 1543-624 in outburst accretion-ejection paradigm for black group”. MNRAS, 487, 5248-5262 (A) with NICER, INTEGRAL, Swift, and hole X-ray binaries. IV. Replication ATCA”. ApJ, 833, 39 (C) of the 2010-2011 activity cycle of GX 339‑4”. A&A, 626, 115 (C)

65 *McCauley, P.I.; Cairns, I.H.; White, *Mora-Partiarroyo, S.C.; Krause, M.; Murray, C.E.; Peek, J.E.G.; Di Teodoro, S.M.; Mondal, S.; Lenc, E.; Morgan, J.; Basu, A.; Beck, R.; Wiegert, T.; Irwin, E.M.; McClure-Griffiths, N.M.; Dickey, Oberoi, D. “The low-frequency solar J.; Henriksen, R.; Stein, Y.; Vargas, C.J.; J.M.; Dénes, H. “The 3D kinematics of corona in circular polarization”. SoPh, and 6 coauthors. “CHANG-ES XIV: gas in the Small Magellanic Cloud”. 294, 106 (O) Cosmic-ray propagation and magnetic ApJ, 887, 267 (A) field strengths in the radio halo of *Men, Y.; Aggarwal, K.; Li, Y.; NGC 4631”. A&A, 632, 10 (O) *Murugeshan, C.; Kilborn, V.; Palaniswamy, D.; Burke-Spolaor, Obreschkow, D.; Glazebrook, K.; Lutz, S.; Lee, K.J.; Luo, R.; Demorest, P.; *Mora-Partiarroyo, S.C.; Krause, M.; K.; Dzudzar, R.; Dénes, H. “Angular Tendulkar, S.; Agarwal, D.; and 2 Basu, A.; Beck, R.; Wiegert, T.; Irwin, momentum regulates H I gas content coauthors. “Non-detection of fast J.; Henriksen, R.; Stein, Y.; Vargas, and H I central hole size in the discs of radio bursts from six gamma-ray burst C.J.; Heesen, V.; and 7 coauthors. spirals”. MNRAS, 483, 2398-2412 (C) remnants with possible magnetar “CHANG‑ES XV: Large-scale magnetic engines”. MNRAS, 489, 3643-3647 (O) field reversals in the radio halo of NGC *Namkham, N.; Jaroenjittichai, P.; 4631”. A&A, 632, 11 (O) Johnston, S. “Diagnostics of timing *Meyers, B.W.; Tremblay, S.E.; Bhat, noise in middle-aged pulsars”. MNRAS, N.D R.; Shannon, R.M.; Ord, S.M.; *Morabito, L.K.; Matthews, J.H.; Best, 487, 5854-5861 (P) Sobey, C.; Johnston-Hollitt, M.; Walker, P.N.; Gürkan, G.; Jarvis, M.J.; Prandoni, M.; Wayth, R.B. “The emission and I.; Duncan, K. J.; Hardcastle, M.J.; *Nguyen, H.; Dawson, J.R.; Lee, M.-Y.; scintillation properties of RRAT J2325- Kunert-Bajraszewska, M.; Mechev, Murray, C.E.; Stanimirović, S.; Heiles, 0530 at 154 MHz and 1.4 GHz”. PASA, A.P.; and 7 coauthors. “The origin of C.; Miville-Deschênes, M.-A.; Petzler, A. 36, e034 (P) radio emission in broad absorption “Exploring the properties of warm and line quasars: Results from the LOFAR cold atomic hydrogen in the Taurus *Mingo, B.; Croston, J.H.; Hardcastle, Two‑metre Sky Survey”. A&A, 622, and Gemini regions”. ApJ, 880, 141 (O) M.J.; Best, P.N.; Duncan, K.J.; 15 (O) Morganti, R.; Rottgering, H.J.A.; *Nikiel-Wroczynski, B.; Berger, A.; Sabater, J.; Shimwell, T.W.; Williams, *Morello, V.; Barr, E.D.; Cooper, S.; Herrera Ruiz, N.; Bomans, D.J.; Blex, W.L.; and 8 coauthors. “Revisiting Bailes, M.; Bates, S.; Bhat, N.D.R.; S.; Horellou, C.; Paladino, R.; Becker, the Fanaroff-Riley dichotomy and Burgay, M.; Burke-Spolaor, S.; A.; Miskolczi, A.; Beck, R.; and 7 radio-galaxy morphology with the Cameron, A.D.; Champion, D.J.; coauthors. “Exploring the properties LOFAR Two‑Metre Sky Survey (LoTSS)”. and 14 coauthors. “The High Time of low-frequency radio emission MNRAS, 488, 2701-2721 (O) Resolution Universe survey – XIV. and magnetic fields in a sample of Discovery of 23 pulsars through compact galaxy groups using the *Miniutti, G.; Saxton, R.D.; Giustini, GPU‑accelerated reprocessing”. LOFAR Two‑Metre Sky Survey (LoTSS)”. M.; Alexander, K.D.; Fender, R.P.; MNRAS, 483, 3673-3685 (O) A&A, 622, 23 (O) Heywood, I.; Monageng, I.; Coriat, M.; Tzioumis, A.K.; Read, A.M.; *Morgan, J.S.; Macquart, J.-P.; Chhetri, *Norris, Ray P.; Salvato, M.; Longo, G.; and 4 coauthors. “Nine-hour X-ray R.; Ekers, R.D.; Tingay, S.J.; Sadler, Brescia, M.; Budavari, T.; Carliles, S.; quasi‑periodic eruptions from a E.M. “Interplanetary Scintillation with Cavuoti, S.; Farrah, D.; Geach, J.; Luken, low‑mass black hole galactic nucleus”. the Murchison Widefield Array V: K.; and 7 coauthors. “A comparison Nature, 573, 381-384 (C) An all-sky survey of compact sources of photometric redshift techniques using a modern low-frequency radio for large radio surveys”. PASP, 131, *Miskolczi, A.; Heesen, V.; Horellou, telescope”. PASA, 36, 002 (O) 108004 (O) C.; Bomans, D.-J.; Beck, R.; Heald, G.; Dettmar, R.-J.; Blex, S.; Nikiel- *Morokuma-Matsui, K.; Serra, P.; *O’Sullivan, S.P.; Machalski, J.; Van Eck, Wroczynski, B.; Chyzy, K. T.; and Maccagni, F.M.; For, B.-Q.; Wang, C.L.; Heald, G.; Brüggen, M.; Fynbo, 4 coauthors. “CHANG-ES XII. A J.; Bekki, K.; Morokuma, T.; Egusa, J.P.U.; Heintz, K.E.; Lara-Lopez, M.A.; LOFAR and VLA view of the edge-on F.; Espada, D.; Miura, R.E. and 3 Vacca, V.; Hardcastle, M.J.; and 20 star‑forming galaxy NGC 3556”. A&A, coauthors. “Complex distribution and coauthors. “The intergalactic magnetic 622, 9 (O) velocity field of molecular gas in NGC field probed by a giant radio galaxy”. 1316 as revealed by Morita Array of A&A, 622, 16 (O) *Mooney, S.; Quinn, J.; Callingham, ALMA”. PASJ, 71, 85 (O) J.R.; Morganti, R.; Duncan, K.; Morabito, L.K.; Best, P.N.; Gürkan, G.; Hardcastle, M.J.; Prandoni, I.; and 6 coauthors. “Blazars in the LOFAR Two‑Metre Sky Survey first data release”. A&A, 622, 14 (O)

66 Australia Telescope National Facility | Annual Report 2019–20 *Onić, D.; Filipović, M.D.; Bojičić, Parikh, A.S.; Russell, T.D.; Wijnands, *Piro, L.; Troja, E.; Zhang, B.; Ryan, I.; Hurley-Walker, N.; Arbutina, B.; R.; Miller-Jones, J.C.A.; Sivakoff, G.R.; G.; van Eerten, H.; Ricci, R.; Wieringa, Pannuti, T.G.; Maitra, C.; Urošević, Tetarenko, A.J. “Rapidly evolving M.H.; Tiengo, A.; Butler, N.R.; Cenko, D.; Haberl, F.; Maxted, N.; and 20 disk‑jet coupling during re-brightenings S. B.; and 5 coauthors. “A long-lived coauthors. “Murchison Widefield in the black hole transient MAXI neutron star merger remnant in Array and XMM-Newton observations J1535−571”. ApJ, 878, L28 (C) GW170817: Constraints and clues from of the Galactic supernova remnant X-ray observations”. MNRAS, 483, G5.9+3.1”. A&A, 625, 93 (O) *Parthasarathy, A.; Shannon, R.M.; 1912‑1921 (C) Johnston, S.; Lentati, L.; Bailes, *Oosterloo, T.; Morganti, R.; M.; Dai, S.; Kerr, M.; Manchester, *Polzin, E.J.; Breton, R.P.; Stappers, Tadhunter, C.; Raymond Oonk, J.B.; R.N.; Osłowski, S.; Sobey, C.; and B.W.; Bhattacharyya, B.; Janssen, G.H.; Bignall, H.E.; Tzioumis, T.; Reynolds, C. 2 coauthors. “Timing of young radio Osłowski, S.; Roberts, M.S.E.; Sobey, “ALMA observations of PKS 1549-79: pulsars – I. Timing noise, periodic C. “Long-term variability of a black a case of feeding and feedback in a modulation, and proper motion”. widow’s eclipses – A decade of PSR young radio ”. A&A, 632, 66 (O) MNRAS, 489, 3810-3826 (P) J2051-0827”. MNRAS, 490, 889-908 (O)

*Ord, S.M.; Tremblay, S.E.; McSweeney, *Perera, B.B.P.; DeCesar, M.E.; Price, D.C.; Croft, S.; DeBoer, D.; Drew, S.J.; Bhat, N.D.R.; Sobey, C.; Mitchell, Demorest, P B.; Kerr, M.; Lentati, J.; Enriquez, J.E.; Foster, G.; Gajjar, V.; D.A.; Hancock, P.J.; Kirsten, F. “MWA L.; Nice, D.J.; Osłowski, S.; Ransom, Gizani, N.; Hellbourg, G.; Isaacson, tied-array processing I: Calibration and S.M.; Keith, M.J.; Arzoumanian, Z.; H.; and 6 coauthors. “Breakthrough beamformation”. PASA, 36, e030 (O) and 65 coauthors. “The International Listen observations of asteroid (514107) Pulsar Timing Array: second data 2015 BZ509 with the Parkes Radio *Orenstein, B.J.; Collier, J.D.; Norris, release”. MNRAS, 490, 4666-4687 (P) Telescope”. RNAAS, 3, 19 (P) R.P. “The redshift distribution of infrared-faint radio sources”. MNRAS, *Peters, C.; van der Horst, A.J.; *Price, D.C.; Foster, G.; Geyer, M.; 484, 1021-1030 (O) Chomiuk, L.; Kathirgamaraju, A.; van Straten, W.; Gajjar, V.; Hellbourg, Barniol Duran, R., Giannios, D.; G.; Karastergiou, A.; Keane, E.F.; *Osłowski, S.; Shannon, R.M.; Ravi, Reynolds, C.; Paragi, Z.; Wilcots, Siemion, A.P.V.; Arcavi, I.; and 23 V.; Kaczmarek, J.F.; Zhang, S.; Hobbs, E. “Observational constraints on coauthors. “A fast radio burst with G.; Bailes, M.; Russell, C.J.; van late‑time radio rebrightening of GRB/ frequency-dependent polarization Straten, W.; James, and 18 coauthors. supernovae”. ApJ, 872, 28 (V) detected during Breakthrough “Commensal discovery of four fast Listen observations”. MNRAS, radio bursts during Parkes Pulsar *Petroff, E.; Oostrum, L.C.; Stappers, 486, 3636‑3646 (P) Timing Array observations”. MNRAS, B.W.; Bailes, M.; Barr, E.D.; Bates, S.; 488, 868‑875 (P) Bhandari, S.; Bhat, N.D.R.; Burgay, M.; *Prochaska, J.X.; Macquart, J.-P.; Burke-Spolaor, S.; and 17 coauthors. McQuinn, M.; Simha, S.; Shannon, *Oswald, L.; Karastergiou, A.; “A fast radio burst with a low R.M.; Day, C.K.; Marnoch, L.; Ryder, Johnston, S. “Understanding the dispersion measure”. MNRAS, 482, S.; Deller, A.; Bannister, K.W.; and radio beam of PSR J1136+1551 through 3109-3115 (P) 9 coauthors. “The low density and its single pulses”. MNRAS, 489, magnetization of a massive galaxy 310‑324 (O) *Petrov, L.; de Witt, A.; Sadler, E.M.; halo exposed by a fast radio burst”. Phillips, C.; Horiuchi, S. “The second Science, 366, 231-234 (A,C) Paice, J.A.; Gandhi, P.; Charles, P.A.; LBA calibrator survey of southern Dhillon, V.S.; Marsh, T.R.; Buckley, compact extragalactic radio sources – *Qian, L.; Pan, Z.-C.; Li, D.; Hobbs, D.A.H.; Kotze, M. M.; Beri, A.; LCS2”. MNRAS, 485, 88-101 (V) G.; Zhu, W.-W.; Wang, P.; Liu, Z.-J.; Altamirano, D.; Middleton, M.J.; and Yue, Y‑L.; Zhu, Y.; Liu, H.-F.; and 12 6 coauthors. “Puzzling blue dips in *Pineda, J.L.; Horiuchi, S.; Anderson, coauthors. “The first pulsar discovered the black hole candidate Swift J1357.2 L.D.; Luisi, M.; Langer, W.D.; Goldsmith, by FAST”. Sci.China Phys.Mech.Astron., – 0933, from ULTRACAM, SALT, ATCA, P.F.; Kuiper, T.B.H.; Bryden, G.; Soriano, 62, 959508 (O) Swift, and NuSTAR”. MNRAS, 488, M.; Lazio, T.J.W. “Electron densities 512‑524 (C) and nitrogen abundances in ionized *Qiu, H.; Bannister, K.W.; Shannon, gas derived using [N II] fine‑structure R.M.; Murphy, T.; Bhandari, S.; and hydrogen recombination lines”. Agarwal, D.; Lorimer, D. R.; Bunton, ApJ, 886, 1 (T) J.D. “A survey of the Galactic plane for dispersed radio pulses with the Australian Square Kilometre Array Pathfinder”. MNRAS, 486, 166-174 (A)

67 *Ralph, N.O.; Norris, R.P.; Fang, G.; *Rowlinson, A.; Stewart, A.J.; Sano, H.; Matsumura, H.; Yamane, Y.; Park, L.A.F.; Galvin, T.J.; Alger, M. J.; Broderick, J.W.; Swinbank, J.D.; Wijers, Maggi, P.; Fujii, K.; Tsuge, K.; Tokuda, Andernach, H.; Lintott, C.; Rudnick, R.A.M.J.; Carbone, D.; Cendes, Y.; K.; Alsaberi, R. Z. E.; Filipović, M. L.; Shabala, S.; Wong, O.I. “Radio Fender, R.; van der Horst, A.; Molenaar, D.; Maxted, N.; and 18 coauthors. Galaxy Zoo: Unsupervised clustering G.; and 9 coauthors. “Identifying “Discovery of shocked molecular of convolutionally auto-encoded transient and variable sources in radio clouds associated with the shell-type radio‑astronomical images”. PASP, 131, images”. A&C, 27, 111-129 (O) Supernova Remnant RX J0046.5−7308 108011 (O) in the Small Magellanic Cloud”. ApJ, Russell, T.D.; Tetarenko, A.J.; Miller- 881, 85 (M) Ravi, V. “The observed properties of Jones, J.C.A.; Sivakoff, G.R.; Parikh, fast radio bursts”. MNRAS, 482, 1966- A.S.; Rapisarda, S.; Wijnands, R.; Sano, H.; Rowell, G.; Reynoso, E. M.; 1978 (P) Corbel, S.; Tremou, E.; Altamirano, D. Jung-Richardt, I.; Yamane, Y.; Nagaya, and 12 coauthors. “Disk-jet coupling in T.; Yoshiike, S.; Hayashi, K.; Torii, K.; *Reardon, D.J.; Coles, W.A.; Hobbs, the 2017/2018 outburst of the galactic Maxted, N.; and 6 coauthors. “Possible G.; Ord, S.; Kerr, M.; Bailes, M.; Bhat, black hole candidate X-ray binary evidence for cosmic-ray acceleration N.D.R.; Venkatraman Krishnan, MAXI J1535-571”. ApJ, 883, 198 (C) in the Type Ia SNR RCW 86: Spatial V. “Modelling annual and orbital correlation between TeV gamma rays variations in the scintillation of the *Sabater, J.; Best, P.N.; Hardcastle, M.J.; and interstellar atomic protons”. ApJ, relativistic binary PSR J1141-6545”. Shimwell, T.W.; Tasse, C.; Williams, 876, 37 (C) MNRAS, 485, 4389-4403 (P) W.L.; Brüggen, M.; Cochrane, R.K.; Croston, J.H.; de Gasperin, F.; and 11 *Schmidt, P.; Krause, M.; Heesen, *Reynolds, T.N.; Westmeier, T.; coauthors. “The LoTSS view of radio V.; Basu, A.; Beck, R.; Wiegert, T.; Staveley-Smith, L.; Elagali, A.; For, AGN in the local Universe. The most Irwin, J.A.; Heald, G.; Rand, R.J.; Li, B.-Q.; Kleiner, D.; Koribalski, B.S.; massive galaxies are always switched J.-T.; Murphy, E.J. “CHANG-ES XVI: Lee-Waddell, K.; Madrid, J.P.; Popping, on”. A&A, 622, 17 (O) An in‑depth view of the cosmic- A.; and 14 coauthors. “WALLABY ray transport in the edge-on spiral early science – I. The NGC 7162 galaxy *Sadler, E.M.; Chhetri, R.; Morgan, galaxies NGC 891 and NGC 4565”. A&A, group”. MNRAS, 482, 3591-3608 (A,C,P) J.; Mahony, E.K.; Jarrett, T.H.; Tingay, 632, 12 (O) S. “Interplanetary scintillation *Riggi, S.; Vitello, F.; Becciani, U.; studies with the Murchison *Schnitzeler, D.H.F.M.; Carretti, E.; Buemi, C.; Bufano, F.; Calanducci, A.; Wide‑field Array – IV. The hosts of Wieringa, M.H.; Gaensler, B.M.; Cavallaro, F.; Costa, A.; Ingallinera, sub‑arcsecond compact sources at Haverkorn, M.; Poppi, S. “S-PASS/ATCA: A.; Leto, P.; and 6 coauthors “CAESAR low radio frequencies”. MNRAS, 483, a window on the magnetic universe source finder: Recent developments 1354‑1373 (O) in the Southern hemisphere”. MNRAS, and testing”. PASA, 36, e037 (O) 485, 1293-1309 (C) Sandhu, P.; Raja, R.; Rahaman, M.; *Rodman, P.E.; Turner, R.J.; Shabala, Malu, S.; Datta, A. “Study of diffuse *Segal, G.; Parkinson, D.; Norris, R.P.; S.S.; Banfield, J.K.; Wong, O.I.; emission in cluster MACSJ0417.5-1154 Swan, J. “Identifying complex sources Andernach, H.; Garon, A. F.; Kapinska, from 76 MHz to 18 GHz “. JApA, 40, in large astronomical data using a A.D.; Norris, R.P.; Rudnick, L. “Radio 17 (C) coarse-grained complexity measure”. Galaxy Zoo: observational evidence PASP, 131, 108007 (O) for environment as the cause of radio *Sanidas, S.; Cooper, S.; Bassa, C.G.; source asymmetry”. MNRAS, 482, Hessels, J.W.T.; Kondratiev, V.I.; *Servajean, E.; Garay, G.; Rathborne, 5625-5641 (O) Michilli, D.; Stappers, B.W.; Tan, J.; Contreras, Y.; Gomez, L. “ALMA C.M.; van Leeuwen, J.; Cerrigone, observations of a massive and dense Romano, D.; Burton, M.G.; Ashley, L.; and 13 coauthors. “The LOFAR cold clump: G305.137+0.069”. ApJ, 878, M.C.B.; Molinari, S.; Rebolledo, D.; Tied-Array All‑Sky Survey (LOTAAS): 146 (O) Braiding, C.; Schisano, E. “The G332 Survey overview and initial pulsar molecular cloud ring: I. Morphology discoveries”. A&A, 626, 104 (O) *Shimwell, T.W.; Tasse, C.; Hardcastle, and physical characteristics”. MNRAS, M.J.; Mechev, A.P.; Williams, W.L.; Best, 484, 2089-2118 (M) P.N.; Röttgering, H.J.A.; Callingham, J.R.; Dijkema, T.J.; de Gasperin, F.; and 97 coauthors. “The LOFAR Two-metre Sky Survey. II. First data release”. A&A, 622, 1 (O)

68 Australia Telescope National Facility | Annual Report 2019–20 *Shternin, P.; Kirichenko, A.; Zyuzin, D.; Thomson, A.J.M.; Landecker, T.L.; *Trott, C.M.; Watkinson, C.A.; Jordan, Yu, M.; Danilenko, A.; Voronkov, M.; Dickey, J.M.; McClure-Griffiths, N.M.; C.H.; Yoshiura, S.; Majumdar, S.; Shibanov, Y. “Tracking the footprints Wolleben, M.; Carretti, E.; Fletcher, Barry, N.; Byrne, R.; Hazelton, B.J.; of the radio pulsar B1727–47: Proper A.; Federrath, C.; Hill, A.S.; Mao, S.A.; Hasegawa, K.; Joseph, R.; and 35 motion, host supernova remnant, and and 5 coauthors. “Through thick or coauthors. “Gridded and direct Epoch the glitches”. ApJ, 877, 78 (C,P) thin: Multiple components of the of Reionisation bispectrum estimates magneto‑ionic medium towards the using the Murchison Widefield Array”. *Smith, D.A.; Bruel, P.; Cognard, I.; nearby H II region Sharpless 2-27 PASA, 36, e023 (O) Cameron, A.D.; Camilo, F.; Dai, S.; revealed by Faraday tomography”. Guillemot, L.; Johnson, T.J.; Johnston, MNRAS, 487, 4751-4767 (P) Urquhart, J S.; Figura, C.; Wyrowski, S.; Keith, M.J.; and 8 coauthors. F.; Giannetti, A.; Kim, W.-J.; Wienen, “Searching a thousand radio pulsars Titus, N.; Stappers, B.W.; Morello, M.; Leurini, S.; Pillai, T.; Csengeri, for gamma-ray emission”. ApJ, V.; Caleb, M.; Filipović; , M.D.; T.; Gibson, S.J.; and 3 coauthors. 871, 78 (P) McBride, V.A.; Ho, W.C.G.; Buckley, “ATLASGAL – molecular fingerprints D.A.H. “Targeted search for young of a sample of massive star-forming Smith, I.A.; Ryder, S.D.; Kotak, R.; Kool, radio pulsars in the SMC: Discovery clumps”. MNRAS, 484, 4444-4470 (M) E.C.; Randall, S.K. “ALMA, ATCA, and of two new pulsars”. MNRAS, 487, Spitzer observations of the luminous 4332‑4342 (P) Urquhart, R.; Soria, R.; Pakull, M. W.; extragalactic Supernova SN 1978K”. Miller-Jones, J.C.A.; Anderson, G. E.; ApJ, 870, 59 (C) *Tobin, J.J.; Bourke, T.L.; Mader, S.; Plotkin, R. M.; Motch, C.; Maccarone, Kristensen, L.; Arce, H.; Gueth, F.; T. J.; McLeod, A. F.; Scaringi, S. *Sobey, C.; Bilous, A.V.; Grießmeier, Gusdorf, A.; Codella, C.; Leurini, S.; “A newly discovered double-double J.-M.; Hessels, J.W.T.; Karastergiou, A.; Chen, X. “The formation conditions candidate microquasar in NGC 300”. Keane, E.F.; Kondratiev, V I.; Kramer, of the wide binary class 0 protostars MNRAS, 482, 2389-2406 (C) M.; Michilli, D.; Noutsos, A.; and 15 within BHR 71”. ApJ, 870, 81 (P) coauthors. “Low-frequency Faraday *Van Eck, C.L.; Haverkorn, M.; Alves, M rotation measures towards pulsars Tramonte, D.; Ma, Y.-.Z.; Li, Y.-.C.; I.R.; Beck, R.; Best, P.; Carretti, E.; Chyzy, using LOFAR: probing the 3D Galactic Staveley-Smith, L. “Searching for H I K.T.; Enßlin, T.; Farnes, J.S.; Ferrière, K.; halo magnetic field”. MNRAS, 484, imprints in cosmic web filaments with and 6 coauthors. “Diffuse polarized 3646-3664 (O) 21-cm ”. MNRAS, emission in the LOFAR Two‑meter Sky 489, 385-400 (P) Survey”. A&A, 623, 71 (O) *Stacey, H.R.; McKean, J P.; Jackson, N.J.; Best, P.N.; Calistro Rivera, G.; *Troja, E.; van Eerten, H.; Ryan, G.; *Vernstrom, T.; Gaensler, B.M.; Callingham, J.R.; Duncan, K.J.; Gürkan, Ricci, R.; Burgess, J.M.; Wieringa, Rudnick, L.; Andernach, H. “Differences G.; Hardcastle, M.J.; Iacobelli, M.; M.H.; Piro, L.; Cenko, S.B.; Sakamoto, in Faraday rotation between adjacent and 8 coauthors. “LoTSS/HETDEX: T. “A year in the life of GW 170817: the extragalactic radio sources as a probe Disentangling star formation and rise and fall of a structured jet from a of cosmic magnetic fields”. ApJ, 878, AGN activity in gravitationally lensed binary neutron star merger”. MNRAS, 92 (O) radio‑quiet quasars”. A&A, 622, 18 (O) 489, 1919-1926 (C) Voisin, F.J.; Rowell, G.P.; Burton, M.G.; *Stairs, I.H.; Lyne, A.G.; Kramer, M.; *Trott, C.M.; Fu, S.C.; Murray, S.G.; Fukui, Y.; Sano, H.; Aharonian, F.; Stappers, B.W.; van Leeuwen, J.; Tung, Jordan, C.H.; Line, J.L.B.; Barry, N.; Maxted, N.; Braiding, C.; Blackwell, A.; Manchester, R.N.; Hobbs, G.B.; Byrne, R.; Hazelton, B.J.; Hasegawa, R.; Lau, J. “Connecting the ISM to TeV Lorimer, D.R.; Melatos, A. “Mode K.; Joseph, R.; and 19 coauthors. PWNe and PWN candidates”. PASA, 36, switching and oscillations in PSR “Robust statistics towards detection e014 (M) B1828-11”. MNRAS, 485, 3230-3240 (P) of the 21 cm signal from the Epoch of Reionization”. MNRAS, 486, *Wang, L.; Gao, F.; Duncan, K.J.; *Stein, Y.; Dettmar, R.-J.; Irwin, J.; 5766‑5784 (O) Williams, W.L.; Rowan-Robinson, M.; Beck, R.; Wezgowiec, M.; Miskolczi, Sabater, J.; Shimwell, T.W.; Bonato, A.; Krause, M.; Heesen, V.; Wiegert, M.; Calistro-Rivera, G.; Chyży, K.T.; T.; Heald, G.; and 3 coauthors. and 8 coauthors. “A LOFAR-IRAS “CHANG‑ES. XIII. Transport processes cross-match study: the far-infrared and the magnetic fields of NGC 4666: radio correlation and the 150 MHz indication of a reversing disk magnetic luminosity as a star-formation rate field”. A&A, 623, 33 (O) tracer”. A&A, 631, 109 (O)

69 *Wang, W.; Lu, J.; Zhang, S.; Chen, *Yan, W.M.; Manchester, R.N.; Wang, Conference papers X.; Luo, R.; Xu, R. “Pulsar giant N.; Yuan, J.P.; Wen, Z.G.; Lee, K.J. pulse: Coherent instability near light “Periodic Q-mode modulation in PSR *Bastholm, E. Guzman, J.C.; Voronkov, cylinder”. Sci.China Phys.Mech.Astron., J1825-0935 (PSR B1822-09)”. MNRAS, M.; Lahur, P. “Challenges of real-time 62, 979511 (O) 485, 3241-3247 (P) processing in HPC environments: the ASKAP experience”. In: SPIE *Wenger, T.V.; Dickey, J.M.; Jordan, *Zhang, L.; Hobbs, G.; Manchester, Proc., Astronomical Telescopes & C.H.; Balser, D.S.; Armentrout, W.P.; R.N.; Li, D.; Wang, P.; Dai, S.; Wang, Instrumentation, Austin, United States, Anderson, L D.; Bania, T.M.; Dawson, J.; Kaczmarek, J.F.; Cameron, A.D.; 10-15 June, 2018, 10707, 107070J (A) J.R.; McClure-Griffiths, N M.; Shea, J. Toomey, L; and 6 coauthors. “Wide “The Southern H II Region Discovery bandwidth observations of pulsars C, *Chanapote, T.; Asanok, K.; Dodson, Survey. I. The bright catalog”. ApJS, D, and J in 47 Tucanae”. ApJ, 885, L37 R.; Rioja, M.; Green, J.A.; Kramer, B.H. 240, 24 (C) (P) “LBA high resolution observations of ground- and excited-state OH masers *Williams, W.L.; Hardcastle, M.J.; Best, *Zhang, L.; Li, D.; Hobbs, G.; Agar, towards G351.417+0.645”. In: IAU 336: P.N.; Sabater, J.; Croston, J.H.; Duncan, C.H.; Manchester, R.N.; Weltevrede, P.; Astrophysical Masers: Unlocking the K.J.; Shimwell, T.W.; Röttgering, Coles, W.A.; Wang, P.; Zhu, W.; Wen, Mysteries of the Universe, Cagliari, Italy, H.J.A.; Nisbet, D.; Gürkan, G.; and 31 Z; and 52 coauthors. “PSR J1926-0652: 4-8 September, 2017, 336, 329-330 (V) coauthors. “The LOFAR Two-metre Sky A pulsar with interesting emission Survey. III. First data release: Optical/ properties discovered at FAST”. ApJ, Dannerbauer, H. “Impact of infrared identifications and value- 877, 55 (P) environment on molecular gas added catalogue”. A&A, 622, 2 (O) reservoirs probed in distant cluster *Zhang, S.-B.; Hobbs, G.; Dai, S.; and field galaxies”. In: Linking Galaxies *Wolleben, M.; Landecker, T.L.; Toomey, L.; Staveley-Smith, L.; Russell, from the Epoch of Initial Star Formation Carretti, E.; Dickey, J.M.; Fletcher, A.; C.J.; Wu, X.-F. “A new fast radio burst to Today, Sydney, Australia, 18-22 McClure-Griffiths, N.M.; McConnell, in the data sets containing the Lorimer February, 2019, 89 (C) D.; Thomson, A.J.M.; Hill, A.S.; burst”. MNRAS, 484, L147-L150 (P) Gaensler, B.M.; and 5 coauthors. “The *Dunning, A.; Baquiran, M.; Global Magneto-Ionic Medium Survey: *Zhao, G.-Y.; Jung, T.; Sohn, Bong Beresford, R., Bourne, M.; Bowen, Polarimetry of the Southern sky from Won; Kino, M.; Honma, M.; Dodson, M.; Brothers, M.; Bunton, J.; Carter, 300 to 480 MHz”. AJ, 158, 44 (P) R.; Rioja, M.; Han, S.-T.; Shibata, N.; Castillo, S.; Chen, Y.; and 29 K.; Byun, D.-Y.; and 20 coauthors. coauthors. “New receiver technology *Wu, C.; Wong, O.Ivy; Rudnick, L.; “Source-frequency phase-referencing for Radio Astronomy”. In: 2019 IEEE Shabala, S.S.; Alger, M.J.; Banfield, observation of AGNs with KAVA AP-S Symposium on Antennas and J.K.; Ong, C.S.; White, S.V.; Garon, A.F.; using simultaneous dual-frequency Propagation and USNC-URSI Radio Norris, R.P.; and 6 coauthors. “Radio receiving”. JKAS, 52, 23-30 (O) Science Meeting, Atlanta, USA, 7-12 July, Galaxy Zoo: CLARAN – a deep learning 2019, 403-404 (P) classifier for radio morphologies”. *Zhao, R.-S.; Yan, Z.; Wu, X.-J.; Shen, MNRAS, 482, 1211-1230 (O) Z.-Q.; Manchester, R.N.; Liu, J.; Qiao, *Dunning, A.; Bourne, M.; Bowen, G.-J.; Xu, R.-X.; Lee, K.-J. “5.0 GHz TMRT M.; Castillo, S.; Carter, N.; Chung, *Xie, Y.-W.; Wang, J.-B.; Hobbs, G.; observations of 71 pulsars”. ApJ, 874, Y.S.; Doherty, P.; George, D.; Hayman, Kaczmarek, J.; Li, D.; Zhang, J.; Dai, 64 (O) D.B.; Jeganathan, K. and 13 coauthors. S.; Cameron, A.; Zhang, L.; Miao, “Recent centimetre band receiver *Zhou, S.Q.; Zhou, A.A.; Zhang, J.; Liu, C.-C.; and 5 coauthors. “Flux density development at CSIRO Australia”. In: M.Q.; Liu, H.Y.; Zhang, L.; Feng, Z.W.; measurements for 32 pulsars in the 2019 URSI Asia-Pacific Radio Science Zhu, X.D.; Wu, D. “A very large slow 20 cm observing band”. Res.Astron. Conference, New Delhi, India, 9-15 glitch in PSR J1602-5100”. Ap&SS, 364, Astrophys, 19, 103 (P) March 2019, 1p. (O) 173 (P) *Xue, M.; Ord, S.M.; Tremblay, S.E.; Bhat, N.D.R.; Sobey, C.; Meyers, *Zic, A.; Stewart, A.; Lenc, E.; Murphy, B.W.; McSweeney, S.J.; Swainston, T.; Lynch, C.; Kaplan, D. L.; Hotan, N.A. “MWA tied-array processing II: A.; Anderson, C.; Bunton, J.D.; Polarimetric verification and analysis Chippendale, A.; and 2 coauthors. of two bright southern pulsars”. PASA, “ASKAP detection of periodic and 36, e025 (O) elliptically polarized radio pulses from UV Ceti”. MNRAS, 488, 559-571 (A)

70 Australia Telescope National Facility | Annual Report 2019–20 *Dunning, A.; Bourne, M.; Bowen, *Heesen, V.; Basu, A.; Brinks, E.; Heald, Shastri, P.; Dopita, M.; Banfield, J.; M.; Castillo, S.; Carter, N.; Chung, G.; Fletcher, A.; Horellou, C.; Hoeft, Thomas, A.; Longbottom, F.; Sundar, Y.S.; Doherty, P.; George, D.; Hayman, M.; Chyży, K. “Stellar feedback in M.N.; Duggal, C.; Groves, B.; Kharb, P.; D.B.; Jeganathan, K. and 12 coauthors. dwarf irregular galaxies with radio Davies, R.; and 6 coauthors and the S7 “Receivers to meet radio astronomy continuum observations”. In: IAU 344, collaboration. “The environments of field of view and bandwidth Dwarf galaxies: from the deep Universe accreting supermassive black holes in demands”. In: 16th Australian to the present, Vienna, Austria, 20-24 the nearby Universe: A brief overview Symposium on Antennas, Sydney August, 2018, 344, 255-258 (O) of the Southern Seyfert spectroscopic Australia, 12-14 February, 2019, 2pp. (O) snapshot survey (S7)”. In: Women in *Jameson, K. “The first large, Physics, Birmingham, UK, 16-20 July, *Dunning, A.; Jeganathan, Y.S.; unbiased ALMA survey of CO at parsec 2017, AIP Conf. Proc., 2109, 090003 (C) Bourne, M.; Bowen, M.; Castillo, resolution in the Small Magellanic S.; Carter, N.; Doherty, P.; George, Cloud”. In: ALMA2019: Science Results *Smart, K.; Dunning, A.; Smith, S.; D.; Hayman, D.; Mackay, S.; and 9 and Cross-Facility Synergies, Cagliari, Carter, N.; Bourne, M.; Doherty, P.; coauthors. “Ultra-wideband (UWB) Italy, 14-18 October, 2019, 26pp. (O) Castillo, S. “Pattern measurements Receiver for Radio Astronomy”. In: of cryogenically cooled ultra- ICEAA-IEEE APWC 2019, Granada, Spain, Johnson, M.C.; McQuinn, K.B. W.; wideband feed horn”. In: 13th 9-13 September, 2019, 0343-0346 (O) Cannon, J.; Martinkus, C.; Skillman, European Conference on Antennas E.; Bailin, J.; Ford, H.A.; Hunt, L.; and Propagation, Krakow, Poland, 31 *Ekers, R.D. “The Prague IAU Westmeier, T.; Wong, O. .; Kamphuis, March-5 April, 2019, 4pp. (P) General Assembly, Pluto and the IAU P. “The Hi Neighborhoods Around processes”. In: IAU 349, Under One STARBIRDS”. In: IAU 344, Dwarf *Smith, S.; Smart, K.; Carter, N.; Sky: The IAU Centenary Symposium, galaxies: from the deep Universe to the Weily, A.; Nikolic, N.; Kekic, I. “A 20 Vienna, Austria, 27-31 August, 2018, present, Vienna, Austria, 20-24 August, GHz switched beam lens antenna 349, 51‑57 (O) 2018, 344, 280-282 (P) for airborne communications applications”. In: International Fusiara, P.; Schoonderbeek, G.; *Koribalski, B. “Star formation and gas Conference on Electromagnetics in Pragt, J.; Hiemstra, L.; Kuindersma, in Galaxies”. In: Linking Galaxies from Advanced Applications, Granada, Spain, S.; Schuil, M.; Hampson, G. “Design the Epoch of Initial Star Formation to 9-13 September, 2019, 1084-1088 (O) and fabrication of full board direct Today, Sydney, Australia, 18-22 February, liquid cooling heat sink for densely 2019, 68 (O) packed FPGA processing boards”. In: 2018 International Conference on *Koribalski, B.S. “Neutral hydrogen in ReConFigurable Computing and FPGAs, nearby dwarf galaxies”. In: IAU 344, Cancun, Mexico, 3-5 December, 2018, Dwarf galaxies: from the deep Universe 8pp. (O) to the present, Vienna, Austria, 20-24 August, 2018, 344, 288-291 (C) *Granet, C.; Zhou, M.; Sørensen, S.; Smart, K.; Ness, J.; Kot, J. “Reflectarray Nishimura, Y.; Shimonishi, T.; compact antenna test range concept”. Watanabe, Y.; Sakai, N.; Aikawa, Y.; In: 13th European Conference on Kawamura, A.; Kohno, Ko.; Yamamoto, Antennas and Propagation, Krakow, S. “Molecular composition of local Poland, 31 March-5 April, 2019, 5pp. (O) dwarf galaxies: Astrochemistry in low‑metallicity environments”. In: IAU *Guzman, J.C.; Marquarding, M. 344, Dwarf galaxies: from the deep “Managing the ASKAP computing Universe to the present, Vienna, Austria, project: From inception to early 20-24 August, 2018, 344, 182-185 (M) science operations”. In: ASP Conference Series, Astronomical Data Analysis Software and Systems XXVI, Trieste, Italy, 16-20 October, 2016, 521, 276 (A) Legend

* Authors include ATNF staff A ASKAP C ATCA M Mopra O Other staff paper P Parkes S SKA T Tidbinbilla (CDSCC) V VLBI

71 I: Abbreviations

This list does not include units of measure or chemical symbols.

ABBREVIATION DESCRIPTION ABBREVIATION DESCRIPTION

ACMA Australian Communications and Media GASKAP Galactic ASKAP survey Authority GPU Graphics Processing Unit ADC Analog to digital converter IAU International Astronomical Union AO Officer in the Order of Australia ICRAR International Centre for Radio Astronomy ARC Australian Research Council Research

ARQAWA Australian Radio Quiet Zone (WA) IEEE Institute of Electrical and Electronics Engineers

ASKAP Australian SKA Pathfinder ILUA Indigenous Land Use Agreement

ASTRON Netherlands Institute for Radio Astronomy LBA Long Baseline Array

ATCA Australia Telescope Compact Array LIGO Laser Interferometry Gravitational Wave Observatory ATNF Australia Telescope National Facility LNA Low Noise Amplifier ATOA Australia Telescope Online Archive MMIC Mircowave Monolithic Integrated Circuit ATSC ATNF Steering Committee MRO Murchison Radio-astronomy Observatory ATUC ATNF User Committee MWA Murchison Widefield Array AusSRC Australian SKA Regional Centre NAOC National Astronomical Observatories, Chinese BIGCAT Broadband Integrated GPU-Correlator Academy of Sciences for the Australia Telescope NAPA Non A-Priori Assignable CABB Compact Array Broadband Backend NASA National Aeronautics and Space Administration CASDA CSIRO ASKAP Science Data Archive NRAO National Radio Astronomy Observatory (USA) CAS Chinese Academy of Sciences NSW New South Wales CASS CSIRO Astronomy and Space Science PAF Phased Array Feed CDSCC Canberra Deep Space Communication Complex PI Principal Investigator CRAFT Commensal Real-time ASKAP Fast Transients POSSUM Polarisation Sky Survey of the Universe's CSIRO Commonwealth Industrial and Scientific Magnetism Research Organisation RACS Rapid ASKAP Continuum Survey DAP Data Access Portal RFI Radio Frequency Interference DINGO Deep Investigation of Neutral Gas Origins RFSoC Radio Frequency System on a Chip DISER Department of Industry, Science, Energy and Resources SAGE Science in Australia Gender Equity

EDGES Experiment to Detect the Global Epoch SKA Square Kilometre Array of reionisation Signature SKAO SKA Organisation EMU Evolutionary Map of the Universe STEM Science Technology Engineering and ESA European Space Agency Mathematics

ESO European Southern Observatory TAC ATNF Time Assignment Committee

FAST Five hundred meter Aperture Spherical UWB Ultra Wideband Telescope (China) VAST Variables And Slow Transients FLASH First Large Absorption Survey in HI VLBI Very Long Baseline Interferometry FPGA Field Programmable Gate Array WA Western Australia FRB Fast Radio Burst WALLABY Widefield ASKAP L-band Legacy All-sky Blind FTE Full Time Equivalent survey

72 Australia Telescope National Facility | Annual Report 2019–20

CSIRO Australia Telescope National Facility operated by CSIRO Astronomy and Space Science www.csiro.au/atnf

Sydney Murchison Radio-astronomy PO Box 76 Observatory Support Facility Epping NSW 1710 PO Box 2102 +61 2 9372 4100 Geraldton WA 6531 +61 8 9923 7700 Perth PO Box 1130 Paul Wild Observatory Bentley WA 6102 1828 Yarrie Lake Road +61 8 6436 8500 Narrabri NSW 2390 +61 2 6790 4000 Parkes Observatory PO Box 276 Parkes NSW 2870 +61 2 6861 1777

As Australia’s national science agency and innovation catalyst, CSIRO is solving the greatest challenges through innovative science and technology.

CSIRO. Unlocking a better future for everyone.

Contact us 1300 363 400 csiro.au/contact csiro.au

B&M | 20-00255