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CSIRO Astronomy and Space Science

ATNF News

Issue No. 75, October 2013

ISSN 1323-6326

CSIRO Astronomy and Space Science - Undertaking world-leading astronomical
research and operating the Australia Telescope National Facility.

[pic]

CSIRO's Australia Telescope Compact Array - celebrating 25 years of
achievement in 2013.

Editorial

Welcome to the October 2013 issue of ATNF News.

Monday 2 September was the 25th anniversary of the formal opening of the
Compact Array. We report on the public Open Day, formal ceremony and
science symposium held to mark this milestone, and Phil Edwards examines
the telescope's scientific impact.

While the Compact Array celebrates its maturity, work continues apace on
our newest telescope, the Australian SKA Pathfinder. The sixth and final
first-generation phased array feed (PAF) has been installed on an ASKAP
antenna at the Murchison Radio-astronomy Observatory, and commissioning
tests continue. In July came welcome news of a $6m SIEF grant from the
Australian Government and a further $6m from CSIRO: together, these sums
will fund the construction and installation of additional PAFs, bringing
the total to 30. In more good news, the PAF technology has won awards for
its engineering excellence.

The larger SKA project also passed an important milestone this year, with
the SKA Office announcing the international work-package consortia. CSIRO
has received funding from the Australian Government that will enable it to
lead two of the consortia and participate in others.

Observing from the Science Operations Centre in Marsfield is now in full
swing for the Parkes telescope and VLBI sessions, as our Operations report
notes. The same report gives a reassuring update on the Mopra telescope,
which was swept by bushfire in January.

ATNF facilities are used by a thriving astronomical community. Three
science articles in this issue present:

a study of the 'superwind' in NGC 253 that combined observations from Mopra
and ALMA (the Atacama Large Millimeter/submillimeter Array);

a new source catalogue, derived from the AT20G survey, that should prove
useful for selecting populations for future studies and identifying high-
quality calibrators; and

a study of shells and shocks in a star-forming region, RCW 49.

In other news, CASS's Naomi McClure-Griffiths has received a major award
from CSIRO for her scientific achievements, and the Tidbinbilla 70-m
antenna has acquired new capabilities. CASS says 'hello' to a bumper crop
of new science appointments and 'goodbye' to the Parkes Analogue
Filterbanks, finally switched off after many years of service. And there
are our regular updates on graduate students, education and outreach,
engineering developments and publications, along with a new section on
meetings, past and future.

We hope you enjoy this issue of ATNF News. Your comments and suggestions
are always welcome. If you would like to contribute to a future issue,
please contact the newsletter editors, below.

Helen Sim and Tony Crawshaw

ATNF News



From the Chief of CSIRO Astronomy and Space Science

Lewis Ball (Chief of CASS)

This newsletter comes at a very exciting time as CASS, and especially the
ATNF, looks both forward with anticipation and backward with pride. The
Australia Telescope Compact Array is 25 years young and the astronomical
community has celebrated its scientific achievements so far with events in
Narrabri and at the observatory itself in September, with some of the talks
from the 'birthday' symposium being presented again for a second time in
Marsfield. The latest upgrades to the Compact Array, the 4-12 GHz
receivers, are performing well, and the observatory is continuing to
deliver world-class science that is changing our understanding of the
Universe. In recent times the ATNF has also developed other new
capabilities, such as remote operability of Parkes, the Science Operations
Centre in Marsfield coming into full use, and the implementation of On-the-
Fly mapping using the Tidbinbilla 70-metre antenna and a new wide-band

20-GHz receiver system. Of course, adopting new ways of doing things
usually involves, or even requires, moving on from the old ways. The
decommissioning of the Parkes analogue filter banks is an example of a
phenomenally successful instrument that has played its role and now makes
way for new technologies.

The science stories in this newsletter demonstrate the value of ATNF's
complementary capabilities. A new catalogue from the AT20G survey made with
the Compact Array will be useful for many further studies. The study of NGC
253 shows how single-dish data can complement that from a synthesis array,
with Mopra data filling in the gaps of observations made with the world's
largest and most capable millimetre observatory, the $1.6 billion Atacama
Large Millimeter/submillimeter Array. And the RCW 49 science demonstrates
how observations in completely different wavebands (radio, X-ray, optical)
can tell us so much more than observations in one band alone.

The success of the ATNF arises from three sources: its people and their
expertise, its facilities and their capabilities, and its relationships.
This newsletter welcomes a number of exceptional new staff, who bring fresh
ideas, energy and relationships with them. It also welcomes Jim Jackson as
a Distinguished Visitor, notes a number of conferences and workshops, and
details the graduate-student program and a range of outreach activities.
These people and interactions are important aspects of ATNF's role as a
National Facility and support both the astronomical community and the
practice of astronomy.

We also note a range of developments associated with the new kids on the
block, ASKAP and the MWA, and the path to the SKA. After years of work by
many dedicated people ASKAP is getting close to delivering data that will
lead to new science. It has taken its first tentative steps towards the
measurement of the radio sky, and although we will all need to be patient,
we can now start to see the radio waves at the end of the tunnel. And while
ASKAP will deliver outstanding science, it is a stepping-stone to even
bigger things to be enabled by the SKA. With the start of SKA pre-
construction work and the establishment of CSIRO's SKA Centre, led by
CASS's Deputy Chief Sarah Pearce, we are well and truly on that train now.
I hope you find this newsletter informative and exciting, and are looking
forward to the challenges and opportunities of 2014 as much as the staff of
the ATNF.



ATCA 25th Anniversary Science Symposium

Phil Edwards (CASS)

[pic]

The Compact Array. Photo: David Smyth

Following a successful public Open Day on Sunday 1 September, and on-site
commemoration of the opening of the Compact Array on Monday 2 September
(both described on page 6), we celebrated the Compact Array's 25th
Anniversary with a three-day Science Symposium.

The meeting was held in one of the cinemas at the Crossing Theatre in the
town of Narrabri. Top billing on the first day was given to Bob Frater, who
led the construction project ("Prime Minister, we have delivered!") and
John Brooks, the Project Engineer ("Project Management ATNF Style").
Further insights into the history, and pre-history, of the Compact Array
were provided by Dick Manchester, Mal Sinclair, Warwick Wilson, and Mark
Bowen, with Ron Ekers describing the opportunities and challenges presented
by Australia's first National Facility, the ATNF.

The workshop covered all the major fields of research that the Compact
Array has contributed to, including HI studies, the early mosaiced images
of the LMC and SMC, masers, gamma-ray burst afterglows, supernovae, star
formation, polarimetry, intra-day variability, pulsars, clusters, Very Long
Baseline Interferometry, and surveys large, deep and wide.

Peter Tuthill described the Narrabri Stellar Intensity Interferometer, the
forerunner to the Sydney University Stellar Interferometer (SUSI) that now
lives alongside the Compact Array. Robin Wark gave an entertaining review
of Compact Array operations, and showed an early memo from Officer-in-
Charge Graham Nelson which noted that the expected mode of operations was
that observing schedules would be loaded up in the afternoon and the array
left to run unattended overnight - a mode still yet to be realised! Robin
also recognised the efforts of generations of Duty Astronomers who have
provided front-line observing support, identifying Vince McIntyre as the
person who had done the largest (documented) number of DA shifts, with
Maxim Voronkov and Naomi McClure-Griffiths following close behind.

Among the other interesting snippets, facts, and opinions that emerged
during the meeting were:

. that there was an early proposal for an additional two antennas
between the Compact Array and Mopra, which went unfunded;

. that it was Dave Jauncey (CASS) who had proposed the name 'the
Australia Telescope';

. that the design and production of 3,000 VLSI (very-large-scale
integration) chips for the correlator was recognised with the issue of
an Australian postage stamp in 1987;

. John Brooks' 'three people happy' and 'man-month myth' rules*; and

. a recurring appreciation of the fact that the Compact Array is 'a
child-friendly observatory', allowing families to be accommodated on
site and, through its remote-observing capability, providing a means
of observing from one's home institution (or indeed, home!) when
travelling to the Observatory would be disruptive to family life.

Compact Array-themed crosswords were provided to participants on the first
two days, with the first correct entries drawn being presented with a
bottle of wine: Dave McConnell and Stuart Ryder were the successful
cruciverbalists.

The symposium was well attended, with over 60 registered participants. An
encore performance has now been held at Marsfield, allowing those who were
unable to attend to hear these key talks. All presentations will be
archived online, and discussion is under way as to how best to capture in
one document both the information presented at the symposium and
contributions from those who could not be there.

The smooth running of the meeting was thanks to the behind-the-scenes
efforts of staff at Narrabri and Marsfield, with Margaret McFee and Amanda
Gray deserving special mention.

*This requires some explanation. On the first point, John used to tell
disgruntled workers that "if you resign, you'll make three people happy:
you, your boss and your replacement". On the second, John said that if a
job takes one person X months, it will take X people more than one month.
(Ed.)



25 years of Compact Array science

Phil Edwards (CASS)

[pic]

Supernova 1998bw, the subject of the Compact Array's most highly cited
paper. Image: ESO

The ATCA 25th Anniversary Science Symposium provided the opportunity to
look back over the scientific productivity of the Compact Array. It should
be noted up front that the 25th Anniversary of the official Compact Array
opening does not exactly coincide with the start of regular astronomical
observing: operations formally began in 1990, but useful data was being
taken the previous year during the testing and commissioning phase.

One measure of the Compact Array's productivity is the number of refereed
papers produced, and last year this reached a new high, with seventy-six
papers published. A better measure of impact is the number of citations to
those papers, and this was the approach adopted on the occasion of the
Compact Array's 20th birthday: see ATNF News no. 65, October 2008.
Cumulative citation counts naturally favour older papers, and so not
surprisingly, the most highly cited papers from five years ago remain some
of the most highly cited papers today. The exercise was repeated for the
25th symposium, with the NASA/ADS database used to determine the citations,
from all sources, for refereed publications in the ATNF publications
database. From this, papers presenting new Compact Array results were
selected.

Radio emission from the unusual supernova 1998bw and its association with
the gamma-ray burst of 25 April 1998, (Kulkarni et al., 1998, Nature)
remains the Compact Array's most highly cited paper, as it was in 2008,
with over 380 citations. However, the order has changed after that.

The large-scale HI structure of the Small Magellanic Cloud (Stanimirovic et
al., 1999, MNRAS) is currently the second most highly cited paper, but with
Studies of ultracompact HII regions - II. High-resolution radio continuum
and methanol maser survey, (Walsh et al., 1998, MNRAS) breathing down its
neck! A list of the 25 most highly cited papers includes several other
papers on gamma-ray bursts, and other papers on HI imaging of the Small and
Large Magellanic Clouds, as well as several papers on radio observations of
X-ray binary systems. There are also many papers which are not primarily
Compact Array papers but for which Compact Array observations have been
important: for example, The 1000 Brightest HIPASS Galaxies: HI Properties,
(Koribalski et al., 2004, AJ) is based on almost 5,000 hours of Parkes
observations, but with the addition of Compact Array observations of a
number of fields to clarify identifications with optical galaxies.
Similarly, PSR 1259-63 - A binary radio pulsar with a Be star companion,
(Johnston et al., 1992, ApJ) used Parkes to discover the pulsar, but relied
on pinpointing its position with the Compact Array to associate its
companion with a Be star.

The bias against younger papers inherent in cumulative total counts can be
overcome by considering citation count rate with time, and this reveals
three outstanding recent papers. The first, Extragalactic Millimeter-wave
Sources in South Pole Telescope Survey Data: Source Counts, Catalog, and
Statistics for an 87 Square-degree Field (Vieira et al., 2010, ApJ) uses
Compact Array follow-up of the South Pole Telescope discoveries to help
characterise the sources. The Australia Telescope Compact Array Broadband
Backend: description and first results, (Wilson et al., 2011, MNRAS)
combines a detailed description of the CABB system with examples of the
science it is enabling. (The high citation rate of this paper was
acknowledged in a recent email from the journal to the authors, which noted
it had helped raise the journal's impact factor.) Finally, The Australia
Telescope 20 GHz Survey: the source catalogue, (Murphy et al., 2010, MNRAS)
is likely to become one of the Compact Array's most highly cited papers in
absolute terms, in the same way that the paper describing the NRAO VLA Sky
Survey is by far the most highly cited paper produced by the Very Large
Array.

The ATNF Annual Report for 2011 noted that ". the ATNF achieves the best
science outcomes, in terms of publications and citation counts, when
science teams include both Australian and overseas astronomers", and this
is borne out by the list of highly cited Compact Array papers. Twenty-two
of the top 25 papers have overseas-affiliated co-authors, and 21 have ATNF-
affiliated co-authors. The majority also have a 'non-ATNF Australia'
affiliated co-author and, not surprisingly, the largest class of such a
breakdown, constituting almost half the top 25, includes ATNF, and other
Australian, and overseas-affiliated authors.

We look forward to revisiting these studies in five years' time!

The Compact Array's 25 most highly cited papers

Radio emission from the unusual supernova 1998bw and its association with
the gamma-ray burst of 25 April 1998

Kulkarni + 8, Nature, 395, 663 (1998) - 389 citations

The large-scale HI structure of the Small Magellanic Cloud

Stanimirovic + 4, MNRAS, 302, 417 (1999) - 306 citations

Studies of ultracompact HII regions - II. High-resolution radio continuum
and methanol maser survey

Walsh + 3, MNRAS, 301, 640 (1998) - 304 citations

The cored distribution of dark matter in spiral galaxies

Gentile + 4, MNRAS, 351, 903 (2004) - 275 citations

An HI Aperture Synthesis Mosaic of the Large Magellanic Cloud

Kim + 6, ApJ, 503, 674 (1998) - 266 citations

Correlated X-Ray Spectral and Timing Behavior of the Black Hole Candidate
XTE J1550-564: A New Interpretation of Black Hole States

Homan + 8, ApJS, 132, 377 (2001) - 242 citations

Optical and Radio Observations of the Afterglow from GRB 990510: Evidence
for a Jet

Harrison + 19 ApJ, 523, L121 (1999) - 241 citations

Relativistic motion in a nearby bright X-ray source

Tingay + 19, Nature, 374, 141 (1995) - 235 citations

Radio/X-ray correlation in the low/hard state of GX 339-4

Corbel + 4, A&A, 400, 1007 (2003) - 213 citations

A common origin for cosmic explosions inferred from calorimetry of
GRB030329

Berger + 10, Nature, 426, 154 (2003) - 195 citations

Quenching of the Radio Jet during the X-Ray High State of GX 339-4

Fender + 10, ApJ, 519, L165 (1999) - 192 citations

Coupling of the X-ray and radio emission in the black hole candidate and
compact jet source GX 339-4

Corbel + 6, A&A, 359, 251 (2000) - 194 citations

HI Shells in the Large Magellanic Cloud

Kim + 3, AJ, 118, 2797 (1999) - 182 citations

The Radio Structures of Southern 2 Jy Radio Sources

Morganti + 2, MNRAS, 263, 1023 (1993) - 177 citations

The 1000 Brightest HIPASS Galaxies: HI Properties

Koribalski + 39, AJ, 128, 16 (2004) - 173 citations

The Deep X-Ray Radio Blazar Survey. I. Methods and First Results

Perlman + 6, AJ, 115, 1253 (1998) - 165 citations

A Survey for OH (1720 MHz) Maser Emission Toward Supernova Remnants

Frail + 5, AJ, 111, 1651 (1996) - 166 citations

The extended radio emission in the luminous X-ray cluster A3667

Rottgering + 3, MNRAS, 290, 577 (1997) - 154 citations

The Southern Galactic Plane Survey: HI Observations and Analysis

McClure-Griffiths +5, ApJS, 158, 178 (2005) - 152 citations

1E 1547.0-5408: A Radio-emitting Magnetar with a Rotation Period of 2
Seconds

Camilo + 3, ApJ, 666, L93 (2007) - 148 citations

A high-sensitivity survey of radio continuum emission from Herbig Ae/Be
stars

Skinner + 2, ApJS, 87, 217 (1993) - 145 citations

A Long, Hard Look at the Low/Hard State in Accreting Black Holes

Miller +7, ApJ, 653, 525 (2006) - 141 citations

An HI aperture synthesis mosaic of the Small Magellanic Cloud

Staveley-Smith + 4, MNRAS, 289, 225 (1997) - 141 citations

Synthesis images of 6.7 GHz methanol masers

Norris +4, ApJ, 412, 222 (1993) - 140 citations

Chandra Discovery of a 100 kiloparsec X-Ray Jet in PKS 0637-752

Schwartz + 20, ApJ, 540, 69 (2000) - 140 citations



Celebrations at the Compact Array

Helen Sim (CASS)

Albert Einstein doesn't go to many birthday parties these days, but he came
to the Compact Array's on Sunday 1 September. After all, this was a special
event: a public Open Day to celebrate the 25th anniversary of the
telescope's formal opening on 2 September 1988. Einstein (played by Patrick
Helean of Questacon) was just one of more than 800 visitors. The others
were members of the general public, mostly from northwest NSW, who enjoyed
themselves by taking guided tours of antennas and the control building,
viewing the Sun through solar telescopes, listening to presentations about
astronomy, being entertained by Einstein, and talking with CASS staff. The
anniversary also allowed CASS to engage with the community (both local and
national) through the media, promoting the telescope's scientific
contributions. Chris Hollingdrake, former manager of the Parkes
Observatory's visitors centre, was responsible for organising the Open Day,
but it couldn't have happened without the contributions of 50-odd
volunteers, mostly CASS staff, many of whom travelled from Sydney and
Parkes. The staff at the Paul Wild Observatory put in an especially large
effort, shouldering most of the load.

The following day, Monday 2 September, the observatory also hosted a formal
'marquee' event for invited guests. Most attendees had strong connections
to the Compact Array, having built, worked at, or been users of the
telescope. Arriving mid afternoon, guests mingled and renewed their
acquaintance with both each other and the inside of a Compact Array
antenna. In the early evening a representative of the local Gomeroi
community, Ms Jody Sevil, gave a Welcome to Country: speeches followed from
Brett Hiscock (Site Manager - Paul Wild Observatory), Simon Johnston (CASS
Assistant Director - Astrophysics), Ron Ekers (ATNF Foundation Director),
Elaine Sadler (past chair of the National Committee for Astronomy) and Bob
Frater (former Chief of CSIRO's Division of Radiophysics, and responsible
for leading the telescope's construction). Douglas Bock (CASS Assistant
Director - Operations) was the master of ceremonies. The formalities
finished with a three-minute slideshow, heroically compiled by CASS's Robin
Wark, which covered life at the Compact Array over the last 25 years.
Finger food, birthday cake and champagne rounded off the evening. Again,
the success of this event was largely due to the hard work of the Narrabri
staff.

These celebrations were followed by the ATCA's 25th birthday symposium,
held in Narrabri, which is described on page 4.



Engineering update

Graeme Carrad (CASS)

In recent months, CASS Engineering resources have largely been focussed on
aspects of the ASKAP project, but that is by no means all that they have
been committed to.

Compact Array 4-12 GHz receivers

The Compact Array antennas got their new 4-12 GHz (6-cm) receivers in a
timely fashion; however, the spare parts, including a suite of amplifiers,
had to wait for that delivery before they could be given much attention. An
entire spare receiver was delivered in July and other spares will soon be
completed. Documentation also went on the back-burner while we were getting
the receivers on the telescope: we are now focussed on completing this too.

FAST Multibeam Receiver Feasibility Study

The FAST Multibeam Receiver Feasibility Study has progressed, and three
engineers from the National Astronomical Observatories, Chinese Academy of
Sciences (NAOC) visited in October in connection with the project. The
receiver is a weighty part of the receiver suite for the 500 m-diameter
dish currently under construction, and the visitors were keen to discuss
the findings of the feasibility study and take part in measurements of a
single-pixel receiver fabricated from parts representative of those that
might be used in the final 19-pixel receiver. Of similar form to other
hydrogen-line multibeams, this 1.05-1.45 GHz design has had its feed and
orthomode transducer designed by CASS's sister division, now known as CSIRO
Computational Informatics. All other elements have been designed by CASS
engineers and made in the CASS workshops. The low-noise amplifier design
resulted in modules with noise temperatures of around 5 K. Commercial
transistors, whose performance was never expected to match that of the
indium phosphide 'specials' currently used in CASS receivers, were used in
this application. All indications point to the receiver being realisable: a
receiver noise temperature of 7 K has been achieved; a structural analysis
of the cryostat housing indicates that the design is robust; and thermal
calculations show that the receiver package will be able to maintain the
required cryogenic environment. We will deliver a final feasibility report
to the FAST project team in the near future.

Parkes receivers

Effort has also been directed toward studies into possible receivers for
Parkes that fit well with the operating model of more remote control and
fewer receiver changes. Under consideration are a 700 MHz-4 GHz receiver, a
4-24 GHz receiver, and a Phased Array Feed. The sensitivity of any new
receivers must match or excel that of the current receiver suite. We are
investigating designs for the receivers and back ends, considering both the
technologies needed to achieve the wide bandwidths and digitise signals at
the receiver and the strategies needed to cope with radio-frequency
interference (RFI).

Visits and visitors

Alex Dunning recently travelled to the US to meet with Sander Weinreb, a
recognised 'guru' of radio astronomy instrumentation. On the same trip he
visited NRAO's facilities on the east coast, where his interactions with
the staff engendered enthusiasm in both him and them.

October seemed dominated by international visitors as CASS played host to
three engineers from the Max Planck Institute for Radioastronomy (MPIfR) in
Germany. Discussions with the MPIfR representatives, Gundolf Wieching,
GÝnter Knittel and Pablo Tornes Torres, were focussed on making an ASKAP
Design Enhancements (ADE) Phased Array Feed for use on the 100-metre dish
at Effelsberg. MPIfR have been keen to install a PAF, and discussions
centred on the response of a PAF to the challenging RFI environment at
Effelsberg, and how the receiver might be modified to work with the
observatory's existing infrastructure and electronic systems. Members of
the ASKAP commissioning team were able to convey valuable insights into
beamforming and Brian Jeffs, a visitor from Brigham Young University (USA)
at CASS for 11 months, was able to share ideas on dealing with RFI using
beamformers.



Awards

Tony Crawshaw and Helen Sim (CASS)

CSIRO Phased Array Feeds win engineering awards

CSIRO's new phased array feed (PAF) receiver system, developed specifically
for ASKAP and radio astronomy, has now won awards for its engineering at
both the State and national levels.

Earlier this year the PAF was entered in the Engineering Excellence Awards
(Sydney division) of Engineers Australia, winning the Innovations &
Inventions category and receiving an 'honourable mention' in the Research &
Development category.

As a category winner, the PAF was eligible for entry to the national
finals. In late-breaking news, it has received a national Engineering
Excellence Award - an award given to recognise world-class expertise and
innovation.

The PAF is the first chequerboard receiver built specifically for radio
astronomy.

Six first-generation ASKAP PAF systems are already installed on ASKAP
antennas at the Murchison Radio-astronomy Observatory (MRO) in Western
Australia, along with associated digital systems, beamformers and a
hardware correlator. Continued commissioning tests have already produced
the first multibeam image with a three-PAF system, as well as the first
detection of a spectral line with an ASKAP system, another step in
validation of the use of PAFs for radio astronomy.

The PAF systems were developed through a close collaboration between two
areas of CSIRO: Astronomy and Space Science, and Computational Informatics.

Newton Turner Award for Naomi McClure-Griffiths

Dr Naomi McClure-Griffiths, Deputy Astrophysics Group Leader at CSIRO
Astronomy and Space Science, has received CSIRO's prestigious Newton Turner
Award for 2013-2014.

The Award is designed to further the scientific careers of exceptional
senior scientists in CSIRO, and recipients receive a grant to assist their
professional development.

Naomi obtained her doctorate in 2001 from the University of Minnesota and
joined CSIRO Astronomy and Space Science that year, initially as a Bolton
Postdoctoral Fellow. She has more than 90 refereed papers to her name and
has received a number of previous awards, most notably the 2006 Prime
Minister's Malcolm McIntosh Prize for Physical Scientist of the Year.

Naomi's research speciality is the interstellar medium (ISM) of our Galaxy;
she also makes occasional forays into Galactic structure and the Magellanic
System. During the time she's been studying the ISM, the greatest change,
she says, has been our ability to use molecular tracers to better
understand the Galaxy's 'ecosystem': how its stars and gas interact over
time. "The more you learn, the more you realise how complex it is," Naomi
says.

Naomi has led two major surveys, the Southern Galactic Plane Survey (SGPS)
and the Parkes Galactic All-Sky Survey (GASS). She will co-lead the
Galactic Australian SKA Pathfinder Survey (GASKAP), one of ASKAP's large
Survey Science Projects, and will also lead its northern hemisphere
counterpart, the Galactic and Magellanic Evolution Survey (GAMES), which is
to be carried out with the Westerbork Synthesis Radio Telescope.

To make progress on the understanding the life cycle of the ISM, Naomi will
use the funding provided by the Newton Turner award to bring together a
select group of observational astronomers and theoreticians in two tightly
focused meetings in Australia. The first of these, Phase transitions in the
diffuse ISM in late 2013, will address the participants' areas of common
interest and create collaborations; the second meeting will build on those
collaborations.

The Newton Turner Award, named after CSIRO geneticist Dr Helen Alma Newton
Turner (1908-1995), was established by CSIRO in 2008. Dr Turner's work was
focused on genetic improvement of sheep for wool production, and had
national and international impact.



Meetings

Simon Johnston (CASS)

Recent meetings and workshops

The ATNF has hosted and/or played the major part in organising six
international meetings and workshops in the six months from April 2013.

A Neapolitan of Masers: Variability, Magnetism and VLBI, 20-22 May

This meeting, held at the ATNF's Sydney headquarters, brought together
experts to review the current state of important branches of maser
research. It attracted some 50 participants, from 14 countries, and was
followed by two days of informal discussion aimed at developing
collaborations. CASS's Shari Breen, Jimi Green and Ioannis Gonidakis led
the organisation of the meeting.

Maser Workshop 2013

RFI and its impact on the new generation of HI spectral-line surveys, 17-18
June

This technical workshop was held at the ATNF's Sydney headquarters and was
attended by 55 scientists and engineers. It covered spectrum management,
the effects of RFI, and mitigation techniques. Two CASS staff, Lisa Harvey-
Smith and Tim Shimwell, chaired the program organising committee and local
organising committee respectively.

ATNF Conferences - RFI

ASKAP Early Science workshop, 5 August

ASKAP Early Science will be a program of observations that explore new
scientific parameter-space with ASKAP before the construction of the array
is complete. The Early Science workshop, with 70 participants, was held to
generate input to the program from the astronomical community. CASS's Lisa
Harvey-Smith (ASKAP Program Scientist) was the organiser.

ASKAP Early Science workshop

Australia Telescope Compact Array 25th Birthday Symposium, 3-5 September

A three-day science meeting was held in the town of Narrabri as part of the
celebration of the Compact Array's 25th anniversary. It was prefaced by a
formal celebration at the Compact Array on the evening of Monday 2
September (described on page 6). The science meeting was attended by over
60 people, and balanced 'the old' - recollections of the telescope's
construction - with 'the new' - the plans of early-career scientists to use
the telescope and, in particular, exploit the capabilities of the Compact
Array Broadband Backend (CABB). Simon Johnston (CASS Assistant Director -
Astrophysics) chaired both the scientific organising committee and the
local organising committee. This meeting is described in more detail on
page 3.

ATCA 25th Birthday

Evolutionary Paths in Galaxy Morphology, 23-26 September

Galaxy Zoo, the popular citizen-science program, was the trigger for this
meeting. Held at Sydney's Powerhouse Museum, it attracted 94 participants,
from several countries. While being a 'regular' meeting on galaxy
evolution, it also incorporated a good deal of science generated by Galaxy
Zoo and its spinoffs (the Zooniverse), covered how Galaxy Zoo is evolving,
and examined how the automation of galaxy classifications is progressing.
The formal science meeting was complemented by an evening Zooniverse
community workshop for teachers and educators, run by Rob Hollow (CASS) and
Kelly Borden (Adler Planetarium). CASS's Ivy Wong and Julie Banfield led
the local organising committee for the meeting.

GZO conference

Australian ALMA community workshop, 30-31 October

This workshop was held to prepare the Australian astronomical community to
respond to the forthcoming call from ALMA (the Atacama Large
Millimeter/submillimeter Array) for Cycle 2 proposals. It brought together
four ALMA experts (representing North America, East Asia and Europe) with
40 Australian participants who ranged from postdocs to senior researchers.
The workshop covered ALMA's science capability and completed observing
projects, and trained participants in the use of the tools (such as
simulators) needed to write ALMA proposals. CASS's Jill Rathborne chaired
the organising committee.

ALMA workshop


Future meetings and workshops

Phase transitions in the diffuse ISM, 25-27 November 2013

Wentworth Falls, NSW

Phase transitions workshop

Astroinformatics 2013: knowledge from data, 9-13 December 2013

Sydney, NSW

Astroinformatics 2013 workshop

Powerful AGN and their host galaxies across cosmic time, 16-20 June 2014

Port Douglas, Queensland, Australia

Southern Cross VII workshop



ASKAP and SKA news

Flornes Conway-Derley (CASS), Kate Chow (CASS), Carol Wilson (CASS), Steven
Tingay (ICRAR/Curtin) and Judd Bowman (Arizona State University)

The ASKAP team has seen plenty of activity since the last edition of ATNF
News, with the sixth first-generation (Mk I) phased array feed (PAF)
receiver installed onto ASKAP antennas at the Murchison Radio-astronomy
Observatory (MRO); continuing commissioning activities bearing encouraging
results and validating PAFs for radio astronomy; and further progress on
the Mk II PAF as part of the ASKAP Design Enhancements (ADE) project.

While these commissioning activities continue, planning is also underway
for the ASKAP Early Science and CSIRO ASKAP Science Data Archive (CASDA)
programs, with SKA planning and pre-construction work continuing to ramp up
over time.

More recently, the potential of PAFs for radio astronomy has been
recognised by Engineers Australia through its Engineering Excellence Awards
(see page 8) for more details), and additional funding has been secured to
ensure that ASKAP can deliver the scientific capability it needs to achieve
the best possible scientific impact and lasting benefit to Australia.

First spectral-line detection

In October ASKAP made its first-ever detection of a spectral line: an
exciting milestone, given the importance of spectral-line surveys in
achieving ASKAP's science goals. CSIRO researchers performed the
observation remotely from CASS's Science Operations Centre in Marsfield,
Sydney. They used three ASKAP antennas, equipped with the first-generation
phased array feed (PAF) receivers, to observe the source S9 IAU, a cloud of
neutral gas in our Galaxy often used as a calibrator for HI spectral-line
observations. While testing of the spectral-line capabilities with BETA is
still at a preliminary stage and there are many more tests to complete, the
commissioning team is pleased to have made this important step towards the
goal of producing spectral-line image cubes with ASKAP.

ASKAP telescope receives SIEF grant

In July ASKAP was awarded a $6m grant from the Australian Government's
Science and Industry Endowment Fund (SIEF). To achieve its full scientific
potential, ASKAP requires one PAF for each of its 36 antennas. The SIEF
funding, complemented by an additional $6m commitment from CSIRO, will be
used to fund the construction and installation of additional PAFs on the
ASKAP antennas at the Murchison Radio-astronomy Observatory (MRO), bringing
the total to 30, and increasing ASKAP's survey speed by a factor of almost
four.

News from the MRO

Final BETA PAF installed

The sixth and final first-generation ASKAP phased array feed (PAF) system
has been installed on ASKAP antennas at the MRO in Western Australia, along
with its associated digital systems and beamformers. The six antennas
equipped with the first-generation PAFs constitute the Boolardy Engineering
Test Array (BETA), which will be used by the commissioning teams to prepare
for the full fit-out of all 36 ASKAP antennas.

Hardware correlator installed

The new ASKAP hardware correlator and associated firmware have also been
installed at the MRO, making possible the first tests of the ASKAP Science
Processing Pipeline. The correlator and firmware provide greater
sensitivity, bandwidth and spectral resolution than were previously
available. They were developed, tested and validated at CASS's Marsfield
headquarters.

First multibeam image with BETA

[pic]

The first multbeam image made with the ASKAP BETA system. The nine
overlapping beams are confined to the central region inside the red
contour. Three bright extragalactic sources (PKS1610-771, PKS 1549-790 and
PKS 1547-795) are clearly visible.

Following first correlation and phase closure of an astronomical source
using the BETA hardware correlator, in July the ASKAP team produced the
first multibeam image made with the ASKAP BETA system. Unlike the earlier
multibeam image (reported in ATNF News April 2013), this test used the BETA
hardware correlator rather than the interim data-capture and software
correlator system.

The new image was made with ASKAP antennas 1, 3 and 6, close to the core of
the array, which are fitted with the first-generation PAF receivers, along
with the associated digital systems, beamformer and hardware correlator.

The field of view of these antennas comprises nine overlapping beams,
improving on the three beams used for the first ASKAP multibeam image
produced in April 2013.

The success of these initial correlator tests validated the BETA hardware
design and cleared the way for the tests to be repeated using all six first-
generation PAF systems now installed on the ASKAP antennas. However, using
six PAFs rather than three makes these tests more complex.

ASKAP Early Science Program

In May 2013, a program of 'early science' observations on ASKAP was
announced, and the astronomical community was asked for input on the design
of the program.

The Early Science Program will consist of a series of science-focused
observations, carried out by the ASKAP commissioning and early science
team, using an array of 12 ASKAP antennas equipped with CSIRO's second-
generation phased array feed receivers.

The first step in the consultation and planning process was a community
workshop, held early in August at CASS headquarters in Marsfield. This
attracted 70 registered participants, from 14 institutions in five
countries. (See page 9 for more details.)

Discussions at the workshop covered ground-breaking scientific questions
that could be addressed using ASKAP's 12-antenna array, and scientific and
technical issues related to survey planning, data acquisition, and data
access and distribution to the ASKAP Survey Science Teams (SSTs).

For more information about the Early Learning Science Program, please see
www.atnf.csiro.au/projects/askap/science.html.

Science Data Archive

Planning has also been under way for the CSIRO ASKAP Science Data Archive
(CASDA). This is one of three subsystems that make up the computing
components for ASKAP (the others being the Telescope Operating System and
the Central Processor).

The Science Data Archive is the primary mechanism for storing, managing and
sharing fully calibrated and science-ready data products. It will provide
the ASKAP Survey Science Teams with access to processed data products for
analysis.

The team developing the Science Data Archive is drawn from CSIRO Astronomy
and Space Science and CSIRO Information Management and Technology.

An important challenge is that ASKAP is still being commissioned and the
demands on the Science Data Archive will increase with time, meaning that
its design and architecture need to be flexible.

The first stage of the project, which will run until the end of 2013, is to
define the requirements the system must meet.

News from Geraldton

MRO Support Facility officially opened

July saw the new support hub for the Murchison Radio-astronomy Observatory,
the MRO Support Facility (MSF), opened in Geraldton, Western Australia.

The MSF is located within the Geraldton Universities Centre complex, and
will act as the 'home base' for CSIRO staff whose primary role is to
provide remote-operations services for ASKAP. It will also provide support
services for other international projects at the MRO, such as the Murchison
Widefield Array and the future Square Kilometre Array (SKA) telescope.

The MSF has an Operations Room, in which researchers can remotely operate
and monitor projects at the MRO; a Portal Room for regional researchers
awarded time on iVEC's Pawsey Centre supercomputer in Perth; workshops for
repairs of ASKAP equipment; and meeting and conference facilities.

As well as being the official opening of the MSF, July's event was an
opportunity to thank regional stakeholders who have been crucial in the
establishment of the MRO, ASKAP and the MSF itself.

Starstruck at the Murchison Astrofest

The Murchison Astrofest - a one-day astronomy festival held at the
Murchison Settlement in Western Australia - ran as part of National Science
Week in August.

Both professional and amateur astronomers turned out for it. CSIRO's Lisa
Harvey-Smith (ASKAP Project Scientist) and the Australian National
University's Professor Ken Freeman (winner of the 2012 Prime Minister's
Prize for Science) gave keynote talks. Other daytime activities included
guided walks with Wajarri 'bush professor' Alan Egan; sampling a selection
of Aboriginal bush foods, including an Emu-egg omelette; and looking at an
exhibition of local artworks from Wajarri and non-Aboriginal artists.

In the evening a special night-viewing session was held with telescopes set
up by the Geraldton Astronomy Group, Geraldton Grammar School, ICRAR (the
International Centre for Radio Astronomy Research) and the Astronomy Group
of Western Australia. CASS's Education Officer Rob Hollow led a 'sky tour',
interpreting the Murchison skies to the haunting sounds of the didgeridoo.

The Murchison Astrofest is run by the Murchison Shire Council, with support
from CSIRO and other sponsors.

Astrofest was followed by a tour of the MRO for a number of volunteers and
radio-astronomy enthusiasts. This tour was immensely popular, with the
response of the enthusiastic amateurs a reminder of the huge step forward
the telescopes at the MRO represent for radio astronomy.

SKA activities

SKA pre-construction update and planning work

The last six months have been a busy time for SKA-related activities at
CASS, with the planning and pre-construction work increasing. A huge
variety of work has been completed, from funding and hosting agreements and
consortium negotiations to policy decisions and updates.

CSIRO as an enterprise has been providing invaluable help: CSIRO Legal, for
instance, has assisted with the SKA hosting agreements and Memoranda of
Understanding, and CSIRO International has helped facilitate contacts with
European entities over the SKA power studies.

The CSIRO SKA Centre, hosted by CSIRO Astronomy and Space Science and led
by CASS Deputy Chief Sarah Pearce, was established to coordinate CSIRO's
activities in SKA. Dr Mark McKinnon joined CASS in late September (on
secondment from the US National Radio Astronomy Observatory) to lead the
SKA Dish Array Consortium, after Dr Carole Jackson, the previous lead,
accepted a WA Fellowship and moved to Curtin University to be a Professor
of Astrophysics. Dr Kate Chow joined the SKA Team in CASS, working for
Michelle Storey as the Executive Officer for CSIRO SKA Site &
Infrastructure, after her previous role as an OCE Postdoctoral Fellow with
Ray Norris.

Carol Wilson was transferred to CASS from CSIRO Computational Informatics
(CCI) in September and will be responsible for spectrum and radio
interference issues. CASS will continue to support Carol's ITU
(International Telecommunication Union) work on radio standards, which also
benefits CCI and other CSIRO divisions.

CSIRO participation in SKA work-package consortia

The SKA Organisation Request for Proposals (SKAO RfP) closed in June.
During the RfP process, the Department of Industry (then the Department of
Industry, Innovation, Climate Change, Science, Research and Tertiary
Education, DIICCSRTE) ran its own process to conditionally allocate the
$18.8m SKA pre-construction funding to Australian entities, to allow them
to participate in the consortia bids. This process built on the Expressions
of Interest requested by DIICCSRTE in November 2012 from potential industry
partners.

The proposals for grants closed on 15 April, and the results were announced
on 28 May, with eight entities being awarded funds. CSIRO received $9m of
the total available funding of $18.8m, to allow it to lead two consortia
('Dish Array' and 'Infrastructure Australia'), and participate in several
others including 'Assembly, Integration and Verification' and 'Signal and
Data Transport'.

On 27 July the SKA Office announced the outcomes of its RfP process. All
the RfPs in which CSIRO was involved were successful. Negotiations began in
September between the SKA Organisation and the all the SKA pre-construction
consortia to finalise the Statements of Work for the consortium bids.

The 'Dish Array' work-package is an $80m project to manage the research and
design of the dishes and receivers for the SKA: the consortium includes
research and industry partners from South Africa, Canada, China and Italy.
As noted above, Dr Mark McKinnon joined CSIRO in September to lead this
consortium. He is on secondment from the US National Radio Astronomy
Organisation (NRAO), where he has been North American Project Director for
ALMA (the Atacama Large Millimeter/submillimeter Array) and has coordinated
$600m worth of ALMA construction. Mark brings a wealth of experience in
radio astronomy, international collaboration, and interacting with
industry, all of which will be necessary to deliver one of the world's
largest science facilities.

Radio Quiet Zone policy and stakeholder relations

Since 2005, the Australian Communications and Media Authority (ACMA) and
the Western Australian Government have introduced a number of regulatory
measures to protect the radio quietness of the Mid West site for the SKA
and precursor telescopes. The CSIRO Radio Quiet Zone team has worked with
DIICCSRTE (now the Department of Industry) to evaluate the scope of these
measures and identify any additional requirements.

As these regulatory measures have been publicised or updated, government
and industry stakeholders have raised questions about the effect on their
activities. The RQZ team and DIICCSRTE staff have spent considerable time
over the past six months undertaking technical analyses, writing briefing
documents, and meeting with WA Government representatives to explain the
need for these regulatory measures and the effect they may have on industry
in the Mid West.

Collaborator projects

MWA Science Operations under way

In the April 2013 issue of this newsletter it was noted that the MWA had
called for observing proposals from the community for the first semester of
science operations, scheduled to be undertaken in the second half of 2013
(2013B semester).

It is pleasing to report that a set of very high-quality proposals was
received by the deadline at the end of April.

The MWA Time Allocation Committee (TAC), six independent experts from
around the world, considered and ranked the proposals, awarding 620 hours
of observation time across nine approved projects.

The successful projects are listed at MWA astronomers.

The 620 hours of observation are enough to generate approximately 1.5 PB of
data during 2013B. Further, importantly, the 620 hours of observations
include 507 hours of 'dual-use' observing, where multiple science programs
can be pursued in a commensal fashion. This is an important and unique
characteristic of the MWA that flows from its extreme wide-field
capabilities.

To celebrate the fact that the MWA is the first of the three SKA Precursors
to enter the full science operations phase, an operations launch event was
held during the annual meeting of the Astronomical Society of Australia
(ASA) in July, at Monash University in Melbourne. The (then) Minister for
Innovation, Industry, Science and Research, Senator Kim Carr, officiated at
the launch, which was attended by international VIPs and delegates from the
ASA meeting.

The 2013B observing schedule was initiated in early August and the MWA has
been operating in a robust manner since that point, extremely well
supported by power and communications infrastructure and operational staff
at CSIRO's Murchison Radioastronomy Observatory (MRO) and facilities at the
recently commissioned and opened iVEC Pawsey Centre in Perth, as well as by
the iVEC staff operating the Pawsey infrastructure.

Very large volumes of data are now flowing over the 800 km between the
Murchison and Perth and radio astronomy in Australia has well and truly
entered the Big Data regime. The MWA science teams are working hard to keep
up with the data flow, and early imaging and calibration results look
extremely good.

The second Call for Proposals, for semester 2014A (first half of 2014),
closed in October. Whereas the 2013B call was restricted to Guaranteed Time
(GT: for MWA Individual Members and institutions only), the 2014A call now
covered both GT and Open Access (OA: open to any astronomer from any
institution in the world) time allocations.

As the MWA is now moving into its full science operations phase, the
regular six-monthly MWA Project Meetings will now change focus to being
largely scientific meetings to review progress with the different science
projects, disseminate research outcomes, and discuss future scientific
possibilities with the MWA.

These meetings are open to all interested members of the community and the
next meeting will take place in Wellington, New Zealand, in December 2013.

Full details, including registration details, are available at 121 Project
meeting.

Recent publications of note from the MWA include: a study of the potential
for the MWA to be used as a facility for tracking space debris, by Prof.
Steven Tingay et al.; a comprehensive study of the lobes of Centaurus A at
118 MHz, by PhD student Mr Ben McKinley et al.; a 2400-square-degree
polarisation survey at 189 MHz, by Dr Gianni Bernardi et al.; and the full
science case description for the MWA, by Dr Judd Bowman et al. (published
in PASA).

EDGES

EDGES continued to collect data between 80-200 MHz at the MRO during the
year to provide a long-term baseline measurement of low-level radio-
frequency interference and ionospheric conditions. The Arizona State
University (ASU) team visited the site in March and November 2012 to update
the installation. MRO staff have continued to provide on-site support,
including monitoring of fuel, power, and network connectivity. MRO staff
have also performed several minor hardware repairs for the EDGES team.

In parallel with the operation of the existing instrument, the EDGES team
has been preparing a new instrument (EDGES-2) that aims to improve on
performance of the existing experiment by a factor of 10. This development
is supported by a new three-year research grant from the U.S. National
Science Foundation (award number: AST-1207761) awarded in May 2012 to
Principal Investigator Judd Bowman at ASU and Co-Investigator Alan Rogers
at MIT/Haystack.

The first deployment of the new system will begin in late October 2013. In
2012, one postdoc, two postgraduate students, and three undergraduate
students at ASU assisted in EDGES data analysis, instrument design, and
testing.

The MRO and EDGES infrastructure was used in 2012 to support testing of a
prototype receiver and antenna for the Dark Ages Radio Explorer (DARE) NASA
mission concept. DARE mirrors the goals and techniques of EDGES and is
being developed as collaboration between the EDGES group and a team led by
Professor Jack Burns at the University of Colorado.

Hardware for DARE was implemented at JPL, NRAO, and ASU and deployed by the
ASU group to MRO in March 2012. The instrument has been collecting data in
the 40-150 MHz band throughout the year to characterise the hardware and
test absorption models of the ionosphere.





End of an era: the decommissioning of the Parkes Analogue Filterbanks

Dick Manchester and Phil Edwards (CASS)

[pic]

Pulse phase versus radio frequency (?) for the strong, highly dispersed
pulsar PSR B1641-45, recorded using one of the 96 x 3-MHz filterbanks built
for the 20-cm Multibeam system. The dispersive delay is proportional to ?-
2.

On 16 September the Parkes analogue filterbank (AFB) systems were formally
decommissioned, bringing to an end a remarkably successful and productive
series of pulsar observations. While filterbank systems had been
constructed for earlier pulsar searches, the most significant system was
that designed to work with the Parkes 13-beam 20-cm ('Multibeam') receiver.

The Multibeam receiver was originally conceived with the goal of mapping
the sky in the HI spectral line. However, the pulsar group quickly realised
that with some small modifications to the receiver specifications, mainly
increasing the available bandwidth, it would also allow more efficient
pulsar searches. Handling the data from all 13 beams simultaneously,
however, required the construction of a new, dedicated, filterbank system.
As Figure 1 shows, dispersion in the interstellar medium causes pulses to
arrive progressively later at lower frequencies. To obtain the necessary
sensitivity, all pulsar observations must compensate for this delay. The
simplest way to do this is to filter the signal into a number of channels
corresponding to different frequencies and to 'de-disperse' the pulse in
offline processing. For pulsar searches a large number of possible
dispersions must be searched, but for pulsar timing the data are de-
dispersed using the known dispersion measure (DM) of the pulsar.

The filterbank system for the Multibeam receiver consisted of 26 identical
filterbanks, each with ninety-six 3-MHz channels. Each feed of the 13-beam
system has two orthogonal probes recording the total power of incoming
signal and so 26 filterbanks were needed. Construction of the system was an
international collaboration between Jodrell Bank Observatory (JBO), the
Osservatorio Astronomico di Bologna and the ATNF. The filterbanks and one-
bit digitiser system were designed by Andrew Lyne and Tim Iken of JBO, and
constructed at JBO and Bologna during 1996. The design was based on earlier
filterbank systems constructed at JBO for the Parkes 20-cm survey (Johnston
et al., 1992, MNRAS, 255, 401), the Parkes 70-cm pulsar survey (Manchester
et al., 1996, MNRAS, 279, 1235) and the globular-cluster searches (e.g.,
Manchester et al., 1991, Nature, 352, 219).

The local oscillator/down-converter system was designed and constructed at
ATNF. It employed an up-down conversion system to split the incoming 288-
MHz-bandwidth signal for each polarisation/beam into three bands, each
between 64 and 160 MHz, which were fed to separate filterbank boards.
Consequently there were 78 filter boards, which is why the system required
almost three racks in the old control room at Parkes.

After detection, signals from corresponding orthogonal polarisations were
summed and then high-pass filtered, integrated and sampled by a one-bit
digitiser. These samples were then packed and recorded on magnetic tape or
disk for offline analysis. The one-bit digitiser system was also designed
at JBO and constructed there and at Bologna. It proved to be very efficient
for pulsar searching because it was relatively immune to impulsive radio-
frequency interference. Furthermore, it kept data rates from the 13-beam
receiver to levels that were readily manageable at the time. The data-
acquisition system (PMDAQ) was developed by David Loone and Fernando
Camilo, the observation-control program (PMCTRL) by Dick Manchester, the
observer GUI interface by Andrew Lyne, and the monitoring program (PMMON)
by Nichi D'Amico. The Parkes 13-beam pulsar-search system is described in
detail in the paper by Manchester et al. (2001, MNRAS, 328, 17).



New capabilities for the Tidbinbilla 70-m antenna

Shinji Horiuchi (Tidbinbilla)

The Tidbinbilla 70-m radio telescope, also known as Deep Space Station 43
(DSS-43), is one of antennas at the Canberra Deep Space Communication
Complex (CDSCC) at Tidbinbilla near Canberra. The CDSCC is one of three
stations that make up NASA's Deep Space Network (DSN), and the primary
purpose of station's antennas is to track spacecraft and space probes for
NASA and other space agencies. Some antenna time not used for space
communication is scheduled for Host Country radio-astronomy observations
and is open to the astronomical community. The Tidbinbilla 70-m dish is the
most sensitive single-dish antenna in the southern hemisphere. It is used
in VLBI experiments to increase imaging sensitivity and for single-dish
projects such as the observation of water-maser sources and ammonia
emission lines.

Despite its superb sensitivity, two factors have limited the 70-metre's
effectiveness for some kinds of science: a lack of an On-the-Fly (OTF)
mapping mode, and the restricted bandwidth of its analogue spectrometer.
But those limitations have now been overcome.

Tidbinbilla ammonia mapping project

The first moves towards an On-the-Fly mapping system began in late 2010,
when a Summer Vacation Student, Mr Tye Young, started work on a project to
demonstrate the 70-metre's spectral-line mapping capability and apply the
technique to observations of Galactic star-forming regions. Under the
supervision of Shinji Horiuchi and Jimi Green, Tye made test observations
of three large molecular clouds in the Orion Nebula, Sagittarius B2 and the
Carina Nebula, and succeeded in obtaining ammonia molecular-line maps for
all of them. Ammonia is a powerful tracer of the characteristics of
molecular clouds and acts as a natural thermometer, allowing us to measure
the temperature of the gas - one of key parameters in studying star-
formation activity. The Orion Nebula and Sagittarius B2 have been well
studied and can be good targets for test observations. Carina, however, can
be seen only from the southern hemisphere, and ammonia lines had not been
previously detected in this source. But we were able both to make the first
detection of the ammonia and to map it (Young et al., 2013, MNRAS, 435,
3568). These observations have highlighted the potential of the
Tidbinbilla 70-m antenna for sensitive large-scale mapping of ammonia.

The first Tidbinbilla 70-m on-the-fly mapping

[pic]

An observation of the Orion Nebula - one of the first On-the-Fly maps made
with the Tidbinbilla 70-m antenna.

The Carina mapping project was conducted using position-switching
observations. That was appropriate for this source as the ammonia emission
is very weak. Each data point was sampled with frequent position switching
between 'on source' and 'off source' to subtract atmospheric and
instrumental effects, with an integration time of eight minutes in each
position. We mapped a 2.5 x 4.5 arcminute field over a total of 15 hours.
However, for stronger sources and a wider field, the On-the-Fly (OTF)
mapping method, sampling data during a raster scan, would be more
efficient. Graeme Wong from the University of Western Sydney worked with us
recently to develop the Tidbinbilla OTF as part of his PhD project. The OTF
data were calibrated and mapped with ASAP and CASA, thanks to Dr Kanako
Sugimoto who developed the CASA single-dish program and supported a
workaround script to transform the Tidbinbilla data format into one
suitable for CASA. Figure 1 is one of the first OTF maps, an observation of
the Orion Nebula for the radio recombination line of hydrogen at 8.30937
GHz. Here 42 x 35 pixels were sampled over 2.4 hours (the time includes
reference point scans and overhead), with a three-second integration per
point. This is significant improvement in efficiency.

New K-Band System on DSS-43

NASA's Jet Propulsion Laboratory has invested in new wideband K-Band
receiver systems for the Deep Space Network's 70-m dishes. These systems
have two beams, with dual-polarisation feeds for each beam. The Tidbinbilla
70-m has now been outfitted with its new receiver, plus a new wideband down-
converter. The system currently covers 21-25 GHz: this is likely to be
extended to 17-27 GHz in coming years. In addition, the Smithsonian
Astrophysical Observatory has funded a new wideband spectroscopy backend
for Tidbinbilla. The first project to use this new backend with the K-band
frontend will be the Tidbinbilla AGN Maser Survey (TAMS) project led by Dr
Lincoln Greenhill (Harvard-Smithsonian Center for Astrophysics). We expect
that this new system will contribute to future multi-transitional mapping
projects.





New science appointments

Simon Johnston (CASS)

Since the April 2013 edition of ATNF News was published, CASS has welcomed
another seven scientific staff: Joanne Dawson, Laura Gonzalez Gomez, Ian
Heywood, Megan Johnson, Matthew Kerr, Amy Kimball and Paolo Serra. Here
they tell us, in their own words, about their research interests.

Joanne Dawson

Bolton Fellow, PhD: Nagoya University, Japan, 2010

"My primary interest is the interstellar medium in the Milky Way and
nearby galaxies, with particular focus on the mechanisms by which atomic
gas is processed into molecular clouds. My research has addressed the role
of supernova feedback in molecular cloud formation, seeking quantitative
observational evidence of molecular gas formation in the walls of giant
'supershells' in the Galaxy and Large Magellanic Cloud. I am joint Primary
Investigator of a large Parkes project, SPLASH (the Southern Parkes Large-
Area Survey in Hydroxyl), a large-scale, sensitive and unbiased survey of
ground-state OH lines in the Southern Galactic Plane. I am a also member of
the GASKAP project, which will use ASKAP to map the Galactic Plane and
Magellanic system in HI and OH to unprecedented angular resolution."

Laura Gonzalez Gomez

Australis Postdoctoral Fellow, PhD: MPIfR and University of Bonn, 2012

"My research is concerned with understanding the chemical and physical
properties of clumps associated with infrared dark clouds, in the context
of the earliest stages of high-mass star formation. To this end, I have
made use of existing archival data from the Spitzer Space Telescope in the
mid infrared regime to create a catalog of IRDC candidates, and carried out
observations with both single-dish telescopes and interferometers toward
some of those clumps. I have also measured proper motions in star-forming
regions, using VLA radio continuum observations. As Australis Fellow, I
have spent a year working in Santiago at the University of Chile before
coming to CASS."

Ian Heywood

Senior Research Scientist, PhD: University of Manchester, 2005

"My PhD was in stellar astrophysics, observing and modelling the
evolving radio emission from classical nova explosions, and from there I
moved into the field of somewhat more energetic accretion-powered outflows,
namely the jets from active galactic nuclei. At present I'm focusing on
AGN, star formation and galaxy evolution across cosmic time, mainly using
continuum and spectral-line observations at radio wavelengths. I also
maintain a strong interest in new techniques for the calibration and
imaging of data from connected radio-telescope arrays. At CASS I will be
contributing to the commissioning of ASKAP, and I also have a role as
Project Scientist for the CSIRO ASKAP Science Data Archive, an exciting
cross-disciplinary collaboration between CASS and CSIRO Information
Management and Technology."

Megan Johnson

Office of the Chief Executive Postdoctoral Fellow, PhD: Georgia State
University, 2011

"I study the evolution of dwarf galaxies: my current interests are in
understanding the mechanism that triggers starbursts in these galaxies and
how the environment affects their interactions and mergers. At CASS I hope
to gain a deeper understanding of the role of neutral hydrogen, especially
how it connects dwarf galaxies to their environments. I'm involved in
several surveys, including LITTLE THINGS and CHANG-ES (both using the VLA),
LVHIS (led from CASS) and WALLABY (the HI all-sky survey to run on ASKAP)."

Matthew Kerr

Office of the Chief Executive Postdoctoral Fellow, PhD: University of
Washington, Seattle, 2010

"As a PhD student, I studied optimal methods for characterizing the spectra
of gamma-ray sources using data from the Fermi Gamma-ray Space Telescope.
My work was applied - with success - to searching for pulsations from gamma-
ray pulsars and selecting promising unidentified Fermi sources for radio
pulsation searches. Before coming to CASS I worked at Stanford University
on models of pulsar emission and on the challenging spectral analysis of
pulsars at energies from 1 MeV to 100 MeV. I'm currently studying the
timing properties of both gamma-ray and radio pulsars, with hopes of
understanding the timing noise that hampers efforts to detect gravitational
waves with arrays of millisecond pulsars."

Amy Kimball

Office of the Chief Executive Postdoctoral Fellow, PhD: University of
Washington, Seattle, 2010

"My main research area is the study of large samples of powerful active
galactic nuclei (AGNs) using multi-wavelength data from deep-sky surveys in
the radio, optical, and infrared. I am interested in learning how the radio
emission of quasars relates to their properties at other wavelengths,
and understanding the origins of radio-jet production. My current research
projects include observations of host galaxies of ultra-luminous
quasars, exploring the low-frequency radio properties of high-redshift
galaxies, and investigating the origin of radio emission from radio-quiet
quasars."

Paolo Serra

Office of the Chief Executive SL (Science Leader) Research Scientist, PhD:
Kapteyn Astronomical Institute, The Netherlands, 2008

"Before joining CASS, I worked at the Kapteyn Institute and ASTRON in the
Netherlands. My main research interest is galaxy evolution, in particular
the processes that determine the structure, shape and content of galaxies.
Gas is a major player in these processes and my research is strongly
centred on the observation of HI gas in galaxies in different environments.
I combine these observations with data at other wavelengths, and with
simulations, to study the interplay between the different components of
galaxies and test our theoretical understanding of galaxy evolution. I lead
a number of HI surveys using interferometers such as the Westerbork
Synthesis Radio Telescope, MeerKAT and, more recently, the Compact Array.
At CASS I'll work on these projects and on WALLABY, and I hope to be
strongly involved with the commissioning of ASKAP."



Graduate student program

George Hobbs (CASS)

The CASS graduate student program continues to attract high-quality
students from around the world to study a huge array of different
astrophysical problems. Current students are researching galaxies, masers,
pulsars, supermassive black holes, high-velocity clouds, stars and the
interstellar medium. Details of the program are available at
www.atnf.csiro.au/research/student/.

We congratulate the students who have recently completed their PhDs :

Jay Blanchard (University of Tasmania): Linking the radio and gamma-ray
properties of blazars

Justin Bray (University of Adelaide): Ultra-high-energy neutrinos and their
detection with the lunar Cherenkov technique

Xinping Deng (National Space Science Center, Beijing, China): Pulsar timing
and its application in spacecraft navigation

Dan Thornton (Jodrell Bank Centre for Astrophysics): Pulsar and transient
searching with GPUs

Jingbo Wang (Xinjiang Astronomical Observatory, China): Searching for the
gravitational-wave memory effect in pulsar datasets

Caterina Ubach (Swinburne University of Technology): CABB millimetre
observations of proto-planetary disks

We also welcome the following students into the program:

Andreas Herzog (Ruhr University, Bochum, Germany): The broadband spectra of
infrared-faint radio sources

Courtney Jones (University of Tasmania): The Southern Milky Way

Aina Musaeva (University of Sydney): Intermediate-mass black holes in dwarf
galaxies

Glen Rees (Macquarie University): Cosmology using next-generation radio
telescopes

Elise Servajean (Universidad de Chile): The physical and kinematical
structure of massive and dense cold cores

Tye Young (Australian National University): Multiwavelength properties of
dwarf galaxies in the local volume.

If you are interested in joining the program, or wish to learn more about
it, visit Students at ATNFor contact George Hobbs.



Scientific visitors

Naomi McClure-Griffiths (CASS)

The CASS visitors program is designed to provide financial and logistical
support to facilitate working visits. As noted in the April newsletter, the
program is now open to researchers at all levels.

Financial support for visits typically covers the cost of on-site
accommodation at CASS headquarters in Marsfield or its equivalent
(approximately A$500 per week). Visits funded through the program should be
for at least two weeks and could last for up to one year. Visitors may be
located at any of the ATNF sites and are expected to deliver at least one
colloquium or seminar during their stay at the CASS.

We also encourage extended visits of six or twelve months. For these longer
visits it is possible to seek additional funds through CSIRO. Please
contact the Chair of the Visitors Committee, Naomi McClure-Griffiths, for
more information. Potential visitors should make contact with a local
member of staff or the Chair of the Visitors Committee to develop a
proposal. Proposals to the program should include a brief description of a
collaborative project to be conducted during the visit, an estimate of the
dates of the visit and support required, a current CV and a list of
publications. Proposals are reviewed quarterly (in February, May, August
and November).

For more information, see Scientific Visitors.



The superwind of NGC 253

Steven Warren (University of Maryland)

[pic]

The inner 1.5' of NGC 253. H? background image (red) with white CO contours
(SCO?v=5, 10, 25, 100, 250 Jy km s-1 per beam). Expanding molecular shells
are shown as green circles. The CO barycentric velocity is shown at the
lower left in each panel. The beam and a 200-pc scale bar are shown in the
top middle panel. The dashed white circle shows the ALMA primary beam. The
dashed blue line in the top middle panel denotes the approximate edge of
the H? outflow cone. Extra-planar CO emission is apparent at the edges of
this cone throughout the different channel maps, and it appears connected
to the expanding shells.

Mopra data has complemented data from ALMA in a study of the 'superwind of
NGC 253.

Galaxy 'superwinds' are thought to help shape the galactic mass function,
play a critical role in galaxy evolution, and pollute the intergalactic
medium with heavy metals (e.g., Veilleux et al. 2005; Baldry et al. 2008;
Oppenheimer et al. 2010; Dave et al. 2011). These winds are feedback from
either active supermassive black holes (an active galactic nucleus, AGN) or
strong starbursts. Detailed studies of nearby systems frequently focus on
the warm or hot phases of the wind, visible in X-ray or H? emission.
However, most of the mass in the outflowing material is thought to be in
the form of neutral atomic and molecular gas (Walter et al. 2002; Rupke et
al. 2005, 2013; Ferglio et al. 2010; Alatalo et al. 2011). Until recently,
observations of the cooler gas phases have been hindered by the lack of
facilities sensitive to the low-surface-brightness emission as well as the
necessary spatial scales to connect the superwind with either the AGN or
stellar processes (for example, supernovae).

The ionized superwind of NGC 253 emerges from the central ~200 pc, filling
a cone with an opening angle of ~60o, and extends ~10 kpc from the nucleus.
It is unclear whether NGC 253 hosts an accreting black hole, but the low-
luminosity AGN would be energetically sub-dominant to the extreme star-
formation activity. Lobes of H?, UV, and X-ray emission fill the outflow
cone. Imaging of the central region with the Hubble Space Telescope
reveals dark lanes due to dust entrained in the outflow, suggesting the
wind may also carry significant amounts of molecular gas.

We recently observed the nuclear star-bursting galaxy NGC 253 in CO (J=1-0)
with ALMA (the Atacama Millimeter / Submillimeter Array) at 50 pc
resolution (Bolatto et al. 2013). Our ALMA (observations reveal CO emission
spatially coincident with the previously observed ionized outflow, as well
as possible launching mechanisms via stellar-wind and supernova-driven
expanding shells. However, the lack of short spacing information in the
ALMA observations limits our extended flux recovery and results in strong
'negative bowls' in the images.

In order to improve the quality of the observations, the ALMA data
(shortest baselines ~20.2 m) were successfully combined with observations
previously obtained with the 22-m Mopra single dish (Principal
Investigator, JÝrgen Ott). The data were combined in the image plane with
the Miriad software package, using a feathering technique coded in the
immerge routine. The combined image was then used as an input model in
CASA's CLEAN algorithm. This process significantly reduced the impact of
the negative bowls. The final imaging reveals striking CO filaments
perpendicular to the main molecular bar, coincident with the edges of the
outflow cone, and appear to be spatially and spectrally associated with
observed supernova-driven superbubbles (see Figure 1).

We use the observed CO luminosities and velocities to estimate the mass,
mass-loss rate, and energetics of the molecular wind. To compute a lower
bound for the molecular mass in the wind, we adopt an optically thin
conversion factor ?CO—0.34 Msun (K km s-1 pc2)-1, about an order of
magnitude lower than the value characteristic of the Milky Way disk. We
compute an outflow mass of Mmol~6.6x106 Msun. The observed projected
velocities of the CO filaments range from ~30 to 60 km s-1, resulting in a
mass loss rate of ~9 Msun yr-1. This rate is uncertain, but we show that it
takes extremely pessimistic assumptions for the mass-loss rate to become as
low as ~3 Msun yr-1. The nuclear region of NGC 253 has a star-formation
rate of ~3 Msun yr-1, resulting in a mass-loading parameter ?~1-3. It is
not immediately clear if the outflowing gas will escape the halo or
eventually rain back onto the disk. What is clear is that NGC 253 will
exhaust its nuclear star-forming gas in ~60-120 Myr at its current mass-
loss rate, cementing the superwind as an important contributor in the
evolution of NGC 253.

References

Alatalo, K., et al. 2011, AJ 735, 88

Baldry, I. K., Glazebrook, K., & Driver, S. P. 2008, MNRAS, 388, 945-959

Bolatto, A. D., Warren, S. R., Walter, F., et al. 2013, Nature, 499, 450

Dave, R., Oppenheimer, B. D., & Finlator, K. 2011, MNRAS, 415, 11

Feruglio, C., Maiolino, R., Piconcelli, E., et al. 2010, A&A, 518, L155

Oppenheimer, B. D., et al. 2010, MNRAS, 406, 2325-2338

Rupke, D. S., Veilleux, S., & Sanders, D. B. 2005, AJ, 632, 751

Rupke, D. S. N., & Veilleux, S. 2013, ApJ, 768, 75

Walter, F., Weiss, A., & Scoville, N. 2002, AJ, 580, L21



The AT20G high-angular-resolution catalogue

Rajan Chhetri (UNSW/ATNF), Ron Ekers (CASS) Paul Jones (UNSW), Roberto
Ricci (INAF)

[pic]

A visibility-spectra plot using the lower-frequency spectral index for
AT20G sources and 6-km visibility. The dotted line at a 6-km visibility of
0.86 marks our separation between compact and significantly extended
populations. The Y-axis on the right-hand side shows angular scale
corresponding to 6-km visibility. The 'compact' source population is
strongly correlated with the 'flat-spectrum' population, and the 'extended'
source population is strongly correlated with the 'steep-spectrum'
population, as the figure clearly shows. A small number of flat-spectrum
extended thermal Galactic sources detected in the AT20G are marked with
open squares. The negative values of 6-km visibilities are a consequence of
a statistical bias correction.

We have produced a catalogue of high-angular-resolution data for all the
sources in the Southern hemisphere selected at 20 GHz in the AT20G survey.
This catalogue is derived from previously unexploited data obtained with
the ATCA's 6-km antenna during the survey. In the hybrid configurations of
the ATCA, the five antennas in the compact configuration and the 6-km
antenna provide maximum baselines of between 4,300 and 4,500 m. These
baselines provide an angular resolution 20 times greater than that of the
main survey. The large gap between the compact configuration of five
antennas and the 6-km antenna provides only sparse coverage of
interferometer spacings, so imaging is not possible. However, non-imaging
analysis in the visibility domain - in effect, comparing the visibilities
of the sources at long and short baselines - can still be used to separate
sources by size.

Using this approach, we can separate the compact Active Galactic Nuclei or
AGNs (which are 77% of the sources in the AT20G catalogue) from sources
that have extended components at an angular scale of ~ 0.15 arcsec. The
catalogue also identifies compact steep-spectrum sources; an interesting
class of objects that are flat-spectrum but extended; and a population of
thermal sources in both the Milky Way and the Large Magellanic Cloud.

Our cross-correlations with surveys made at other wavelengths with
instruments such as Fermi, ROSAT and WISE give us multiwavelength insights
into the spectral properties of AGNs. Using this work, we have shown that
compact sources (usually associated with flat-spectrum sources) show
spectral curvature at rest-frame frequencies (~30 GHz). Our search for
gravitational lenses in the southern hemisphere based on the catalogue
identified one source that is probably a gravitational lens, and a further
three lens candidates that require further follow-up. A similar search
could be made for supermassive binary black-hole systems resulting from
galaxy mergers.

We expect that this work will be important for a range of applications,
including the selection of different populations for studies (e.g. to
refine models of flat-spectrum and steep-spectrum sources) and the
identification of high-quality calibrators for high-frequency radio
telescope arrays and VLBI observations.

Doi: 10.1093/mnras/stt975


Shells and shocks in the Galactic star-forming region RCW 49

Paula Benaglia & BÄrbel Koribalski

[pic]

The Galactic star-forming region RCW 49 at 843 MHz (greyscale and
contours). The yellow and orange circles mark the core of the cluster
Westerlund 2 and the position of the star WR 20b, respectively, while the
ellipses in dashed lines represent the shells proposed by Whiteoak & Uchida
(1997). Green and cyan rings represent the location of FERMI and HESS high-
energy sources.

RCW 49, also known as G284.4-0.3 (Goss & Shaver 1970), is a very bright,
complex and extended HII region (~ 40' â 50'), largely imaged at radio
continuum and recombination lines. Recent studies using Spitzer data
pointed to the super star cluster Westerlund 2 as RCW 49's ionizing agent
and confirmed that star formation is taking place there (Churchwell et al.
2004). Using Chandra data, Tsujimoto et al. (2007) cataloged hundreds of
cluster members, mostly young stellar object (YSO) candidates and early-
type stars.

Whiteoak & Uchida (1997) obtained radio continuum maps with the Compact
Array at 1.4 and 2.4 GHz and the Molonglo Observatory Synthesis Telescope
(MOST) at 843 MHz. They identified two shell-like structures, shown in
Figure 1: one to the south around the bright star WR 20b (in purple), and
one incomplete shell in the north surrounding Westerlund 2 (in magenta),
with a possible 'blister' toward the west.

A couple of open questions

At least three high-energy objects were recently detected superimposed on
RCW 49: the bright, extended TeV source HESS J1023-575, and two GeV Fermi
sources (2FGL J1022.7-5741 or Fermi-1, 2FGL J1023.5-5749c or Fermi-2).
Despite 50 hours of dedicated monitoring with the High Energy Stereoscopic
System (HESS), and a number of studies focused on determining the nature of
the HESS object, no conclusive result was achieved. Figure 1 displays the
main objects present in the field.

The distance to the ionized region and the super cluster remains highly
controversial. Studies of the stars at different evolutionary stages, and
of the gas from various transitions/frequency bands, yield values from 2.5
to 8 kpc (see, for instance, Vargas àlvarez et al. 2013 and references
therein).

Observing with the ATCA CABB system

[pic][pic]

Images of RCW 49 in radio continuum. Left: at 5.5 GHz, with 2-GHz
bandwidth. Right: at 9 GHz, with 2-GHz bandwidth. The region of the bridge
and part of the southern shell are clearly visible.

We carried out Compact Array observations toward RCW 49 in Feb 2012 using
the Compact Array Broadband Backend (Wilson et al. 2011) in two array
configurations, 6A and 750D, 12 h each. Data at 5.5 GHz and 9.0 GHz were
obtained simultaneously, with a bandwidth of 2 GHz each. The band selection
allowed us to attain very-high-resolution images (relative to the 1.4 and
2.4 GHz ones) at frequencies where any potential non-thermal emission could
still be detected. With those settings we could probe structures of 1-100
arcseconds in extent. The results are presented in a paper by Benaglia,
Koribalski, Peri, Marti, Sanchez-Sutil, Dougherty & Noriega-Crespo (2013,
A&A, 559, A31).

The observations were centered on RCW 49 and covered an area of 30 square
arcminutes. The observing strategy consisted of building a mosaic with 41
pointings, ensuring Nyquist sampling at the higher frequency band. The
integration time for each pointing was approximately 13 minutes.

Data editing, calibration, and image reconstruction were performed with the
multichannel image reconstruction, image analysis and display (Miriad)
routines (Sault et al. 1995). We had to deal with a very extended radio
source, of high dynamic range and substructure sizes at various scales, and
data along 2-GHz bandwidths. We tried various approaches for constructing
the images. The maximum-entropy deconvolution methods proved to be the best
for both minimizing side lobes and dealing with different levels of radio
luminosity from the various pointings.

Figure 2 shows the final images, with an rms noise of 0.6 mJy/beam,
equivalent to three times and twice the theoretical rms values at 5.5 and 9
GHz, respectively. Using the Parkes radio telescope, Churchwell et al.
(1974) measured an integrated flux density from RCW 49 of 180 Jy at 5 GHz.
The integrated flux density from CABB data at 5.5 GHz, above 3?, is 160±15
Jy. A comparison between the two values shows that the interferometer
gathers about 90% of the flux measured by a single-dish telescope, at that
frequency.

The CABB-ATCA zoom modes allowed us to perform a pilot observation of a
radio recombination line. The central frequency was 5005 MHz, where the
H137? transition is expected. The final line data covered 270 channels, of
0.5 km/s width.

Results

The main reason to observe simultaneously at two frequencies was to derive
information about the spectral index. With the 5.5 and 9 GHz data sets we
obtained the spectral index (?) distribution, assuming S proportional to
??. The results showed that the bulk of the emission in the region RCW 49
has a value of approximately zero, consistent with the optically thin
thermal plasma expected from such a large HII region. Nonetheless, the
spectral-index maps hint that some of the plasma in the bridge region may
have spectral-index values that are significantly steeper than -0.1,
suggesting the presence of nonthermal emission due to relativistic
electrons.

Despite the relatively short exposure, the high quality of the data allowed
a 3-sigma detection of the RRL H137? transition toward the regions with
maximum continuum brightness. The area corresponds to the so-called bridge,
at which the two shells proposed by Whiteoak & Uchida (1970) would be
interacting. The RRL emission peaked at 15 km/s.

Previous detections of RRLs in RCW 49 include H109?, centered at 0 km/s
(Caswell & Haynes 1987), and He109?, with a central velocity of -4 ± 1 km/s
(Churchwell et al. 1974), collected with the single-dish Parkes telescope.
Paladini et al. (2013), using narrowband receivers (pre-CABB ATCA, in
2009), measured clear H109? emission toward two sub-regions of the bridge:
they found central velocities of 14.5±1.8 km/s, in full agreement with that
of H137?.

The central velocity of the H137? emission that we detected is similar to
CO-line components (see Ohama et al. 2010 and references therein). The
velocity of +15 km/s corresponds to a kinematic distance of ~6 kpc,
according to the rotation curve in the outer galaxy derived by Brand &
Blitz (1993). The emitting ionized gas corresponds to the brightest
continuum features that form the RCW 49 region. The fact that the ionized
gas and part of the CO gas have similar velocities suggests that the
ionized and the molecular components are physically associated.

The molecular studies already mentioned allow the detection of line
emission characterized by velocities around 0 km/s. Furukawa et al. (2009),
for instance, proposed that there are two main clouds, differentiated by
the velocity (0 and 15 km/s), and that the region could have been formed by
collision of the two clouds. A way to check the hypothesis of 'two
molecular clouds that collided' is to trace the velocity field of the
ionized gas by means of radio recombination lines, over the whole of RCW
49, and compare velocities of the molecular and radio lines.

Radio vs IR emission

[pic]

The core of RCW 49, seen at radio continuum (9 GHz, in red) and NIR bands
(3.6 ?m, in blue and 8 ?m, in light green).

Perhaps the most amazing result is the close match or interplay between
radio and IR (Spitzer-GLIMPSE) emission. Figure 3 represents intensity at
two IR bands

(3.6 mm in blue and 8 mm in green) overlaid onto CABB-ATCA data at 9 GHz
(in red). The radiation is free-free emission from the ionized gas in the
radio and near-IR, and dust (PAH) emission. The Westerlund 2 stars stand
out as the blue agglomerate onto the dark background. There is intense 8-mm
emission (green) in the bridge region. The PAH emission peaks in this band.
Bright emission accounts for a dust-rich region, with the consequent effect
of radiation reddening.

The structures revealed by means of CABB-ATCA data are very similar to
those observed by GLIMPSE. The northern and southern shells, and the bridge
described by Whiteoak & Uchida (1997) are very evident. It is clear that
the HII region is not in an area of uniform density, with a lack of near-IR
emission on the west side of RCW 49 suggesting lower material density to
the west. This explains the possible source of the radio blister structure
on the west side of RCW 49. The next step will be to study the physical
relation between the radio and the IR-emitting gas, eventually making
spectroscopic studies in both regions of the spectrum.

References

Brand, J. & Blitz, L. 1993, A&A, 275, 67

Caswell, J. L. & Haynes, R. F. 1987, A&A, 171, 261

Churchwell, E., Mezger, P. G., Huchtmeier, W. 1974, A&A, 32, 283

Churchwell, E., Whitney, B. A., Babler, B. L. et al. 2004, ApJS, 154, 322

Furukawa, N., Dawson, J. R., Ohama, A., et al. 2009, ApJ, 696, 115

Goss, W. M., Shaver, P. A. 1970, AuJPA, 14, 1

Ohama, A., Dawson, J. R., Furukawa, N., et al. 2010, ApJ, 709, 975

Paladini, R., et al. 2013 (submitted)

Sault, R. J., Teuben, P. J., Wright, M. C. H. 1995, ASPC, 77, 433

Tsujimoto, M., Feigelson, E. D., Townsley, L. K., et al. 2007, ApJ, 665,
719

Vargas àlvarez, C. A., et al. 2013, AJ, 145, 125

Whiteoak, J. B. Z. & Uchida, K. I. 1997, A&A, 317, 536

Wilson, W. E., Ferris, R. H., Axtens, P. et al. 2011, MNRAS, 416, 832





Education and outreach

Rob Hollow (CASS)

CASS staff have been busy over recent months with a diverse range of
outreach and education activities, both in Australia and overseas.

PULSE@Parkes

PULSE@Parkes has now reached over 1000 students. In May, Rob Hollow and Dr
Ryan Shannon spent two weeks in Japan running PULSE@Parkes observing
sessions with Japanese high-school students. Funded by a grant from the
Australia-Japan Foundation, they toured the region affected by the recent
earthquake and tsunami, and several astronomy and space facilities around
Tokyo. Observing sessions were held at the National Astronomy Observatory
of Japan's Mizusawa VLBI Observatory and the Koriyama Space Park.

For schools in Australia, observing sessions for PULSE@Parkes now usually
use the Science Operations Centre and the Interaction Space at Marsfield.
These provide a flexible working area for the sessions, and plenty of space
in which the visiting students can hold discussions with the project
astronomers and our co-supervised PhD students. But, for a change, in
August we conducted our first PULSE@Parkes@Parkes session, in which
students from Parkes High School took part in a PULSE@Parkes session in the
telescope itself. In early September we ran a session with students from
two schools in Geraldton, WA, at the new Murchison Radio-astronomy Support
Facility in that town.

Teacher training and support

The annual Astronomy from the Ground Up teacher workshop took place at
Parkes Observatory in early May. The workshop was booked out, with
educators from several states participating in the three-day event. As well
as touring 'the Dish' and listening to a variety of speakers, the teachers
also had the opportunity to control a model Mars rover at Sydney's
Powerhouse Museum over the Internet. Rob Hollow ran further astronomy-
education workshop sessions at the national science teachers' conference in
Melbourne in July and the NSW science teachers' conference in September. In
National Science Week in August Rob also spent a couple of days giving
talks and running activities at Townsville State High School for students
from several local schools.

Several CASS staff have been involved with CSIRO's Scientists in School
program. In this they are teamed with a school, work closely with teachers
and run activities with students. Other CASS staff have used our small
optical telescopes to run viewing evenings at their local or their
children's schools.

Dr Lisa Harvey-Smith, Dr Yanett Contreras and Rob Hollow received Mentor
Training in Geraldton prior to visiting Pia Wadjarri Remote Community
School near the Murchison Radio-astronomy Observatory in August after the
Murchison Astrofest (an event described on page 14). This tour formed part
of on ongoing mentorship program linking CASS staff with the school.

An exciting new initiative is CASS's formal participation in a new
education program that involves a collaboration of six universities headed
by Macquarie University; CASS; the Australian Astronomical Observatory; and
Las Cumbres Observatory Global Telescope Network. Opening Real Science is a
three-year program designed to improve the quality of pre-service and
current science and mathematics teaching by exposing current and trainee
teachers to real science with astronomy as a key context. An initial
scoping workshop involving participating institutions was held in late
September. The scheme will use existing CASS programs, such as
PULSE@Parkes, and will also open up new opportunities to present CASS's
work to teachers and students.

Other outreach

This year CASS hosted an artist-in-residence, Michaela Gleave. Michaela
presented her exhibition A Day is Longer than a Year, inspired by her time
at CASS, at the Fremantle Arts Centre in June and July. She also curated an
evening of activities at the Museum of Contemporary Art Australia, in which
CASS staff participated. (See below for more about the artist-in-residence
program.) In August CASS supported an event called Journey to the Planets:
Sydney's Willoughby Symphony Orchestra presented Holst's orchestral suite,
The Planets, and CASS ran solar viewing and hands-on activity for children
ahead of the concert. CASS PhD students Vanessa Moss and Glen Rees worked
with Rob Hollow on this event.

Management change at Visitors Centres

Chris Hollingdrake, Manager of the Visitors Centre at the Parkes and Paul
Wild Observatories, left CASS in the middle of the year (but was engaged to
continue work on the preparations for the Compact Array's 25th anniversary
celebrations). In August Glen Nagle, Manager of the Visitors Centre at the
Canberra Deep Space Communication Complex (CDSCC), was appointed as Manager
of all three CASS Visitors Centres. This will allow for a more strategic
and coordinated approach to the management of the VCs. Glen will be based
at CASS's Marsfield headquarters but will spend much of his time at the
other sites.


CASS artist-in-residence

Helen Sim (CASS)

In September Sydney artist Michaela Gleave completed a six-month stint as
an 'artist-in-residence' at CSIRO Astronomy and Space Science in Marsfield.

Michaela works across a range of media including installation, performance,
photography and video. Her creations often question our relationship to
space, matter and time, and involve natural phenomena and tricks of
perception. She has exhibited extensively across Australia and in Germany,
Austria, Hong Kong, Korea and Mexico.

The two main outcomes of her time with CASS were an installation at the
Fremantle Arts Centre in Western Australia and a curated evening event at
the Museum of Contemporary Art Australia in Sydney. The latter included a
ballet based on constellations, a lecture on Indigenous astronomy, CSIRO
telescopes on the roof, and a re-imagining of the Moon landing.

Reflecting on her experience at CASS, Michaela says:

[It] has been a remarkable experience and I feel extremely fortunate to
have been allowed access into this world. . Finding a common ground and a
common language in this environment was a challenging but immensely
interesting process, and whilst I was barely able to scratch the surface of
the field I learned a lot from the process and came out with quite
different impressions than when I went in.

Michaela's residency at CASS was assisted by the Australian Government
through the Australia Council, its arts funding and advisory body.



Operations

Douglas Bock, Phil Edwards, Tasso Tzioumis and Dave McConnell (CASS)

The most visible recent activities of the Operations group have been
restoring Mopra after the bushfire and enabling remote observing with the
Parkes Telescope. However, we continue to grow our group in Geraldton
(there are now 13 staff supporting ASKAP and the MRO) while consolidating
the new wideband capabilities at the Compact Array. On page 17 we honour
the retirement of the Parkes Analogue Filterbanks.

Parkes radio telescope and Marsfield Science Operations Centre

The Parkes telescope can now be routinely operated remotely without any
person at the telescope, and the Science Operations Centre in Marsfield is
the standard observing location. The use of the SOC has increased steadily
since remote observing became available in mid July. The only observers
who now visit the telescope routinely are those using non-standard modes
that require local interaction with instrumentation.

The remote observer accesses the telescope observing systems by connecting
to a VNC session. Two new facilities aid remote observing. The Remote
Observing PORTAL is a web-browser-based interface allowing observers and
support staff to communicate through a 'chat' window, and holds schedules
of up-coming remote observers and the rostered support. Meanwhile, FROG
presents basic information about the current state of the telescope, and
issues warnings derived from both the general monitoring system and the new
Telescope Protection System (TPS). The TPS monitors the systems critical to
telescope safety, contacts Parkes-based staff, and when necessary
interrupts observations to take control of the telescope and place it in a
safe configuration. Under these circumstances the observer will receive an
automated notification on the FROG interface, and should expect to be
contacted by the responding staff member a short time later.

Parkes observations can (and have been) made from any location with a
suitable Internet connection. However, CASS requires observers to conduct
their first remote observations from the Science Operations Centre (SOC) at
the Radiophysics Laboratory, Marsfield, and to conduct at least one
observing session a year from the SOC to retain 'remote qualification'.

Observers are also using the SOC to operate the Mopra telescope and the
Compact Array. Feedback from observers at the SOC has been very positive
but we welcome input as we continue to develop the environment.

Long Baseline Array

The LBA session on 14-19 August 2013 broke new ground: for the first time
all VLBI observing at ATNF antennas was conducted from the SOC. The four
workplaces allocated to each of the ATNF telescopes were used
simultaneously for VLBI observing. The VLBI session ran continuously over
five days, with shifts around the clock. Jamie Stevens (who normally runs
the VLBI at Narrabri) was visiting Sydney and hence all ATNF antennas ran
remotely without any local VLBI experts at the telescopes. Local staff and
the Duty Astronomer provided observatory support, as for all other ATNF
remote observations.

Remote connections were also established to other LBA antennas: the
University of Tasmania's Hobart and Ceduna antennas, the UTas-operated
AuScope VLBI antennas at Katherine and Yarragadee, and the Warkworth
antenna in NZ operated by the Auckland University of Technology. For the
August run these connections were used just to monitor the status at each
site, but all these telescopes may be controlled from the SOC. The
Tidbinbilla antennas and the Hartebeesthoek antennas in South Africa were
also monitored from the SOC.

Monitoring this many antennas is difficult and one would need skates to get
around all the SOC stations! However, the Smart board at the SOC was also
utilised to project an LBA monitoring webpage and view operations at all
telescopes in real time. The webpage uses the Monica monitoring system to
check the telescope status and monitor the VLBI recorders. This system is
very versatile and without it VLBI observing from the SOC would have been
difficult.

We intend this to be the normal LBA observing mode in the future. We would
also like to invite VLBI co-investigators, staff, and students, who in the
past could not get to the observatories, to participate in their
observations from the SOC.

Australia Telescope Compact Array

The 4-cm band upgrade was completed earlier this year, with a single 4-12
GHz band replacing the previous 'C' and 'X' bands. Observers of the
methanol 6.7-GHz line in particular are delighted with the improved
sensitivity provided by the new receivers. Work on the CABB 16-MHz mode is
continuing, as are efforts to understand why reprogramming CABB into its
zoom modes can be such a time-consuming task. Most recently, some trials
have been undertaken to implement an RFI recognition and rejection
algorithm into the CABB system, which offers the possibility of censoring,
in real-time, impulsive or low-duty-cycle but deleterious RFI. As this may
last only a fraction of a second, its excision would allow the remainder of
each (nominally) 10-second cycle to be salvaged. In parallel, a
complementary approach to reduce the impact of 'always-on' RFI is also
being investigated.

We continue to study the use of CASA to reduce ATCA data, recognizing that
certain widefield, multifrequency synthesis observations will be better
handled in CASA - for instance, observations made in hybrid arrays (H214,
H168 or H75) that include CA06 in the imaging, for which w-term effects can
be significant (see the ATCA forum, https://atcaforum.atnf.csiro.au/, for
more details). Miriad continues to be quicker, easier and more familiar to
most users for many ATCA observations, but the development of pipelines and
documentation for CASA reduction will allow users more flexibility in their
data reductions in the future.

Mopra radio telescope

As described in the April issue of ATNF News, the Mopra control building
suffered significant damage in the January bushfire, but the equipment in
the screened room and on the antenna was unscathed. During April mains and
generator power was restored, and the electronic equipment was
professionally cleaned. Tests in early May confirmed that the telescope was
again operational. Under the new operations model, 20 weeks over the winter
season were allocated to the National Astronomy Observatory of Japan and a
consortium of Australian universities led by UNSW and the University of
Adelaide. Operations have gone smoothly over the winter. The L/S receiver
has yet to be reinstalled, but this affects only VLBI observing, and LBA
scheduling has been able to accommodate this.

Time Assignment Committee

The Time Assignment Committee met in July to review proposals for the
2013OCT semester. Strong interest in VLBI observations resulted in the LBA
being the most heavily oversubscribed facility for the 2013OCT semester,
with some of the increased demand arising from the requested participation
of ground-based telescopes in RadioAstron space-VLBI observations.

Some projects that met the ATNF definition of a 'large project' (a total
of more than 400 hours over the projected lifetime of the project) did not
include the required sections in their scientific justification addressing
data analysis and timeline plans, data-release plans, and a recommended
public outreach plan. Large projects (only!) are allowed a five-page limit
so that these additional topics can be described. The requirements for
large projects are clearly set out in section 3.4 of the OPAL users guide,
and the TAC considers all aspects of the proposal in the grading process.





Publications

The following list of publications includes published refereed papers that
use ATNF data or are by CASS authors: the list has been compiled since the
publication of the April 2013 issue of ATNF News. Papers that include CASS
authors are indicated by an asterisk. Please email any updates or
corrections to this list to Julie Tesoriero.

Publication lists of papers that include ATNF data or CASS authors are also
available on the ATNF website at www.atnf.csiro.au/research/publications.

Allison, J.R.; Curran, S.J.; Sadler, E.M.; Reeves, S.N. "Broad, weak 21 cm
absorption in an early-type galaxy: spectral line finding and
parametrization for future surveys". MNRAS, 430, 157-162 (2013).

Aravena, M.; Murphy, E.J.; Aguirre, J.E.; Ashby, M.L.N.; Benson, B.A.;
Bothwell, M.; Brodwin, M.; Carlstrom, J.E.; Chapman, S.C.; Crawford, T.M.;
and 19 co-authors. "Large gas reservoirs and free-free emission in two
lensed star-forming galaxies at z = 2.7". MNRAS, 433, 498-505 (2013).

*Asgekar, A.; Oonk, J.B.R.; Yatawatta, S.; van Weeren, R.J.; McKean, J.P.;
White, G.; Jackson, N.; Anderson, J.; Avruch, I. M.; Batejat, F.; Braun, R.
and 81 co-authors. "LOFAR detections of low-frequency radio recombination
lines towards Cassiopeia A". A&A, 551, L11 (2013).

*Assaf, K.A.; Diamond, P.J.; Richards, A M.S.; Gray, M.D. "Polarization
morphology of SiO masers in the circumstellar envelope of the asymptotic
giant branch star R Cassiopeiae". MNRAS, 431, 1077-1089 (2013).

*Banerji, M.; Glazebrook, K.; Blake, C.; Brough, S.; Colless, M.;
Contreras, C.; Couch, W.; Croton, D.J.; Croom, S.; Davis, T.M.; Jurek, R.J.
and 16 co-authors. "The stellar masses of 40 000 UV-selected Galaxies from
the WiggleZ survey at 0.3 MNRAS, 431, 2209-2229 (2013).

*Bannister, K.W.; Cornwell, T.J. "Memory-efficient w-projection with the
fast Gauss transform". MNRAS, 430, 2390-2400 (2013).

*Barr, E.D.; Guillemot, L.; Champion, D.J.; Kramer, M.; Eatough, R.P.; Lee,
K.J.; Verbiest, J.P. W.; Bassa, C.G.; Camilo, F.; Johnston, S.; Keith,
M.J.; and 12 co-authors. "Pulsar searches of Fermi unassociated sources
with the Effelsberg telescope". MNRAS, 429, 1633-1642 (2013).

*Bernardi, G.; Greenhill, L.J.; Mitchell, D.A.; Ord, S.M.; Hazelton, B. J.;
Gaensler, B.M.; de Oliveira-Costa, A.; Morales, M.F.; Udaya Shankar, N.;
Bunton, J.; and 43 co-authors. "A 189-MHz, 2400-deg2 polarization survey
with the Murchison Widefield Array 32-element prototype". ApJ, 771, A105
(2013).

*Bhattacharyya, B.; Roy, J.; Ray, P.S.; Gupta, Y.; Bhattacharya, D.;
Romani, R.W.; Ransom, S.M.; Ferrara, E.C.; Wolff, M.T.; Camilo, F.; and 10
co-authors. "GMRT discovery of PSR J1544+4937: An eclipsing black-widow
pulsar identified with a Fermi-LAT source". ApJ, 773, L12 (2013).

*Bowman, J.D.; Cairns, I.; Kaplan, D.L.; Murphy, T.; Oberoi, D.; Staveley-
Smith, L.; Arcus, W.; Barnes, D.G.; Bernardi, G. Briggs, F..; Brown, S.;
Bunton, J.D.; and 49 co-authors. "Science with the Murchison Widefield
Array". PASA, 30, e031 (2013).

Bozzetto, L.M.; Filipovic, M.D.; Crawford, E.J.; Sasaki, M.; Maggi, P.;
Haberl, F.; Uro?evic, D.; Payne, J. L.; De Horta, A.Y.; Stupar, M.; and 2
co-authors. "Multifrequency study of SNR J0533-7202, a new supernova
remnant in the LMC". MNRAS, 432, 2177-2181 (2013).

*Braun, R. "Understanding synthesis imaging dynamic range". A&A, 551, A91
(2013).

*Braun, R. "Galaxy formation: The cosmic web in focus". Nature, 497, 191-
192 (2013).

*Bray, J.D.; Ekers, R.D.; Roberts, P. "Noise statistics in a fast digital
radio receiver: the Bedlam backend for the Parkes radio telescope". ExA,
36, 155-174 (2013).

*Breen, S.L.; Lovell, J.E.J.; Ellingsen, S.P.; Horiuchi, S.; Beasley,
A.J.; Marvel, K. "Discovery of four water masers in the Small Magellanic
Cloud". MNRAS, 432, 1382-1395 (2013).

*Brocksopp, C.; Corbel, S.; Tzioumis, A.; Broderick, J. W.; Rodriguez, J.;
Yang, J.; Fender, R. P.; Paragi, Z. "XTE J1752-223 in outburst: a
persistent radio jet, dramatic flaring, multiple ejections and linear
polarization". MNRAS, 432, 931-943 (2013).

*Burgay, M.; Bailes, M.; Bates, S.D.; Bhat, N.D.R.; Burke-Spolaor, S.;
Champion, D.J.; Coster, P.; D'Amico, N.; Johnston, S.; Keith, M.J.; and 11
co-authors. "The High Time Resolution Universe Pulsar Survey - VII.
Discovery of five millisecond pulsars and the different luminosity
properties of binary and isolated recycled pulsars". MNRAS, 433, 259-269
(2013).

*Burgay, M.; Keith, M.J.; Lorimer, D.R.; Hassall, T E.; Lyne, A.G.; Camilo,
F.; D'Amico, N.; Hobbs, G.B.; Kramer, M.; Manchester, R.N.; and 4 co-
authors. "The Perseus Arm Pulsar Survey". MNRAS, 429, 579-588 (2013).

*Burlon, D.; Ghirlanda, G.; Murphy, T.; Chhetri, R.; Sadler, E.; Ajello, M.
"The AT20G view of Swift/BAT-selected AGN: high-frequency radio waves meet
hard X-rays". MNRAS, 431, 2471-2480 (2013).

Burton, M.G.; Braiding, C.; Glueck, C.; Goldsmith, P.; Hawkes, J.;
Hollenbach, D.J.; Kulesa, C.; Martin, C. L.; Pineda, J.L.; Rowell, G.; and
8 co-authors. "The Mopra Southern Galactic Plane CO Survey". PASA, 30, e044
(2013).

*Carretti, E.; Brown, S.; Staveley-Smith, L.; Malarecki, J. M.; Bernardi,
G.; Gaensler, B. M.; Haverkorn, M.; Kesteven, M.J.; Poppi, S. "Detection of
a radio bridge in Abell 3667". MNRAS, 430, 1414-1422 (2013).

*Caswell, J.L.; Green, J.A.; Phillips, C.J. "Parkes full-polarization
spectra of OH masers - I. Galactic longitudes 350œ through the Galactic
Centre to 41œ". MNRAS, 431, 1180-129 (2013).

Cerrigone, L.; Menten, K. M.; Wiesemeyer, H. "Probing the fast outflow in
IRAS 15452 - 5459 with ATCA observations of OH, H2O and SiO masers". MNRAS,
434, 542-551 (2013).

Chakraborti, S.; Ray, A.; Smith, R.; Ryder, S.; Yadav, N.; Sutaria, F.;
Dwarkadas, V.V.; Chandra, P.; Pooley, D.; Roy, R. "The Progenitor of SN
2011ja: Clues from circumstellar interaction". ApJ, 774, A30 (2013).

Chen, X.; Gan, C.-G.; Ellingsen, S.P.; He, J.-H.; Shen, Z.-Q.; Titmarsh, A.

"Newly Identified Extended Green Objects (EGOs) from the Spitzer GLIMPSE II
Survey. I. Catalog". ApJS, 206, A9 (2013).

Chen, X.; Gan, C.-G.; Ellingsen, S.P.; He, J.-H.; Shen, Z.-Q.; Titmarsh, A.
"Newly Identified Extended Green Objects (EGOs) from the Spitzer GLIMPSE II
Survey. II. Molecular Cloud Environments". ApJS, 206, A22 (2013).

*Chhetri, R.; Ekers, R. D.; Jones, P. A.; Ricci, R "The AT20G high-angular-
resolution catalogue". MNRAS, 434, 956-965 (2013).

*Contreras, C.; Blake, C.; Poole, G..B.; Marin, F.; Brough, S.; Colless,
M.; Couch, W.; Croom, S.; Croton, D.; Davis, T.M.; Jurek, R.J. and 16 co-
authors. "The WiggleZ Dark Energy Survey: measuring the cosmic growth rate
with the two-point galaxy correlation function". MNRAS, 430, 924-933
(2013).

*Contreras, Y.; Rathborne, J.; Garay, G. "Structure and radial equilibrium
of filamentary molecular clouds". MNRAS, 433, 251-258 (2013).

*Corbel, S.; Aussel, H.; Broderick, J.W.; Chanial, P.; Coriat, M.; Maury,
A.J.; Buxton, M.M.; Tomsick, J.A.; Tzioumis, A.K.; Harvey-Smith, L.; and 8
co-authors. "Formation of the compact jets in the black hole GX 339-4".
MNRAS, 431, L107-L111 (2013).

*Curran, S.J.; Allison, J.R.; Glowacki, M.; Whiting, M.T.; Sadler, E.M. "On
the H I column density-radio source size anticorrelation in compact radio
sources". MNRAS, 431, 3408-3413 (2013).

*Curran, S.J.; Whiting, M.T.; Sadler, E.M.; Bignell, C. "A survey for the
missing hydrogen in high-redshift radio sources". MNRAS, 428, 2053-2063
(2013).

*Curran, S.J.; Whiting, M.T.; Tanna, A.; Sadler, E M.; Pracy, M.B.;
Athreya, R. "A survey for HI in the distant Universe: the detection of
associated 21-cm absorption at z = 1.28". MNRAS, 429, 3402-3410 (2013).

*Davies, M.L.; Stefan, I.I.; Bolton, R.C.; Carpenter, J.M.; Franzen,
T.M.O.; Grainge, K.J.B.; Green, D.A.; Hobson, M.P.; Hurley-Walker, N.;
Lasenby, A.N.; and 13 co-authors. "The radio source count at 93.2 GHz from
observations of 9C sources using AMI and CARMA". MNRAS, 430, 1961-1969
(2013).

De Rijcke, S.; Buyle, P.; Koleva, M. "FCC046: A candidate gaseous polar
ring dwarf elliptical galaxy in the fornax cluster". ApJ, 770, L26 (2013).

*Delhaize, J.; Meyer, M.J.; Staveley-Smith, L.; Boyle, B.J. "Detection of H
I in distant galaxies using spectral stacking". MNRAS, 433, 1398-1410
(2013).

*DÌaz-Santos, T.; Armus, L.; Charmandaris, V.; Stierwalt, S.; Murphy, E.
J.; Haan, S.; Inami, H.; Malhotra, S.; Meijerink, R.; Stacey, G.; and 19 co-
authors. "Explaining the [C II] 157.7 µm deficit in luminous infrared
galaxies - first results from a Herschel/PACS study of the GOALS sample".
ApJ, 774, A68 (2013).

*Dickey, J.M.; McClure-Griffiths, N.; Gibson, S.J.; GÑmez, J.F.; Imai, H.;
Jones, P.; Stanimirovic, S.; Van Loon, J.; Walsh, A.; Alberdi, A.; and 48
co-authors.

"GASKAP - The Galactic ASKAP Survey". PASA, 30, e003 (2013).

*Eatough, R.P.; Kramer, M.; Lyne, A.G.; Keith, M.J. "A coherent
acceleration search of the Parkes multibeam pulsar survey - techniques and
the discovery and timing of 16 pulsars". MNRAS, 431, 292-307 (2013).

*Emonts, B H.C.; Feain, I.; RÆttgering, H.J.A.; Miley, G.; Seymour, N.;
Norris, R.P.; Carilli, C.L.; Villar-MartÌn, M.; Mao, M.Y.; Sadler, E.M.;
Ekers, R.D.; van Moorsel, G.A.; Ivison, R.J.; Pentericci, L.; Tadhunter,
C.N.; Saikia, D.J. "CO (1-0) detection of molecular gas in the massive
Spiderweb Galaxy (z = 2)". MNRAS, 430, 3465-3471 (2013).

*Espinoza, C.M.; Guillemot, L.; ãelik, æ.; Weltevrede, P.; Stappers, B.W.;
Smith, D.A.; Kerr, M.; Zavlin, V. E.; Cognard, I.; Johnston, S.; Keith,
M.J.; Manchester, R.N.; Shannon, R. and 13 co-authors. "Six millisecond
pulsars detected by the Fermi Large Area Telescope and the radio/gamma-ray
connection of millisecond pulsars". MNRAS, 430, 571-587 (2013).

*Farrar, G.R.; Jansson, R.; Feain, I.J.; Gaensler, B.M. "Galactic magnetic
deflections and Centaurus A as a UHECR source". JCAP, 2013, A023 (2013).

*Ferdman, R.D.; Stairs, I.H.; Kramer, M.; Breton, R.P.; McLaughlin, M.A.;
Freire, P.C.C.; Possenti, A.; Stappers, B.W.; Kaspi, V.M.; Manchester,
R.N.; Lyne, A.G. "The Double Pulsar: Evidence for neutron star formation
without an iron core-collapse Supernova". ApJ, 767, A85 (2013).

*Finn, S.C.; Jackson, J.M.; Rathborne, J.M.; Chambers, E.T.; Simon, R. "The
distribution of infrared dark clouds in the First Galactic Quadrant". ApJ,
764, A102 (2013).

*Foster, J.B.; Rathborne, J.M.; Sanhueza, P.; Claysmith, C.; Whitaker,
J.S.; Jackson, J.M.; Mascoop, J.L.; Wienen, M.; Breen, S.L.; Herpin, F.;
and 16 co-authors. "Characterization of the MALT90 Survey and the Mopra
Telescope at 90 GHz". PASA, 30, e038 (2013).

*Gallaway, M.; Thompson, M.A.; Lucas, P. W.; Fuller, G.A.; Caswell, J.L.;
Green, J.A.; Voronkov, M.A.; Breen, S.L.; Quinn, L.; Ellingsen, S.P.; and 3
co-authors. "The mid-infrared environments of 6.7-GHz methanol masers from
the Methanol Multibeam Survey". MNRAS, 430, 808-821 (2013).

Giannetti, A.; Brand, J.; SÀnchez-Monge, à.; Fontani, F.; Cesaroni, R.;
BeltrÀn, M.T.; Molinari, S.; Dodson, R.; Rioja, M.J. "Physical properties
of high-mass clumps in different stages of evolution". A&A, 556, A16
(2013).

*GÑmez, L.; RodrÌguez, L. F.; Loinard, L. "A one-sided knot ejection at the
core of the HH 111 outflow". RevMexAA, 49, 79-85 (2013).

*Gonidakis, I.; Diamond, P.J.; Kemball, A.J. "A long-term VLBA monitoring
campaign of the v = 1, J = 1-0 SiO masers towards TX Cam - I. Morphology
and shock waves". MNRAS, 433, 3133-3151 (2013).

*Gruppioni, C.; Pozzi, F.; Rodighiero, G.; Delvecchio, I.; Berta, S.;
Pozzetti, L.; Zamorani, G.; Andreani, P.; Cimatti, A.; Seymour, N.; and 93
co-authors. "The Herschel PEP/HerMES luminosity function - I. Probing the
evolution of PACS selected Galaxies to z ~= 4". MNRAS, 432, 23-52 (2013).

*Haan, S.; Armus, L.; Surace, J.A.; Charmandaris, V.; Evans, A.S.; Diaz-
Santos, T.; Melbourne, J.L.; Mazzarella, J.M.; Howell, J.H.; Stierwalt, S.;
and 8 co-authors. "The build-up of nuclear stellar cusps in extreme
starburst galaxies and major mergers". MNRAS, 434, 1264-1286 (2013).

*Hagiwara, Y.; Miyoshi, M.; Doi, A.; Horiuchi, S. "Submillimeter H2O maser
in Circinus Galaxy - a new probe for the Circumnuclear Region of Active
Galactic Nuclei". ApJ, 768, L38 (2013).

*Hezaveh, Y.D.; Marrone, D.P.; Fassnacht, C.D.; Spilker, J.S.; Vieira,
J.D.; Aguirre, J.E.; Aird, K.A.; Aravena, M.; Ashby, M.L.N.; Bayliss, M.;
McIntyre, V. and 56 co-authors. "ALMA observations of SPT-discovered,
strongly lensed, dusty, star-forming galaxies". ApJ, 767, A132 (2013).

*Hong, T; Staveley-Smith, L.; Masters, K.L.; Springob, C.M.; Macri, L.M.;
Koribalski, B.S.; Jones, D.H.; Jarrett, T.H.; Crook, A.C. "2MTF - II. New
Parkes 21-cm observations of 303 southern galaxies". MNRAS, 432, 1178-1188
(2013).

*Huynh, M. T.; Norris, R. P.; Coppin, K. E. K.; Emonts, B. H. C.; Ivison,
R. J.; Seymour, N.; Smail, Ian; Smolcic, V.; Swinbank, A. M.; Brandt, W.
N.; et. al. "Physical conditions of the gas in an ALMA [C II]-identified
submillimetre galaxy at z = 4.44". MNRAS, 431, L88-L92 (2013).

Imai, H.; Katayama, Y.; Ellingsen, S.P.; Hagiwara, Y. "ATCA survey of H2O
masers in the Large Magellanic Cloud". MNRAS, 432, L16-L20 (2013).

*Indermuehle, B,T.; Burton, M,G.; Crofts, J. "Water Vapour Radiometers for
the Australia Telescope Compact Array". PASA, 30, e035 (2013).

*Jones, C.; Dickey, J.M.; Dawson, J.R.; McClure-Griffiths, N.M.; Anderson,
L.D.; Bania, T. M. "HI absorption toward HII regions at small galactic
longitudes". ApJ, 774, A117 (2013).

Jones, P.A.; Burton, M.G.; Cunningham, M.R.; Tothill, N.F.H.; Walsh, A.J.
"Spectral imaging of the central molecular zone in multiple 7-mm molecular
lines". MNRAS, 433, 221-234 (2013).

*Jurek, R.J.; Drinkwater, M.J.; Pimbblet, K.; Glazebrook, K.; Blake, C.;
Brough, S.; Colless, M.; Contreras, C.; Couch, W.; Croom, S.; and 16 co-
authors. "The WiggleZ Dark Energy Survey: star formation in UV-luminous
galaxies from their luminosity functions". MNRAS, 434, 257-281 (2013).

*Kamphuis, P.; Rand, R.J.; JÑzsa, G.I.G.; Zschaechner, L.K.; Heald, G.H.;
Patterson, M.T.; Gentile, G.; Walterbos, R.A.M.; Serra, P.; de Blok, W.J.G.
"HALOGAS observations of NGC 5023 and UGC 2082: modelling of non-
cylindrically symmetric gas distributions in edge-on galaxies". MNRAS, 434,
2069-2093 (2013).

*Kardashev, N. S.; Khartov, V. V.; Abramov, V. V.; Avdeev, V. Yu.; Alakoz,
A. V.; Aleksandrov, Yu. A.; Ananthakrishnan, S.; Andreyanov, V. V.;
Andrianov, A. S.; Ekers, R.D.; and 124 co-authors. "'RadioAstron' - a
telescope with a size of

300,000 km: Main parameters and first observational results". Astronomy
Reports, 57, 153-194 (2013).

*Keith, M.J.; Shannon, R.M.; Johnston, S. "A connection between radio-state
changing and glitch activity in PSR J0742-2822". MNRAS, 432, 3080-3084
(2013).

*Kim, D.-C.; Evans, A.S.; Vavilkin, T.; Armus, L.; Mazzarella, J.M.; Sheth,
K.; Surace, J. A.; Haan, S.; Howell, J.H.; DÌaz-Santos, T.; and 4 co-
authors. "Hubble Space Telescope ACS imaging of the GOALS Sample:
Quantitative structural properties of nearby luminous infrared galaxies
with L IR > 1011.4 L ?". ApJ, 768, A102 (2013).

*Knispel, B.; Eatough, R.P.; Kim, H.; Keane, E.F.; Allen, B.; Anderson, D.;
Aulbert, C.; Bock, O.; Crawford, F.; Eggenstein, H.-B.; Fehrmann, H.;
Hammer, D.; Kramer, M.; Lyne, A. G.; Machenschalk, B.; Miller, R.B.; Papa,
M. A.; Rastawicki, D.; Sarkissian, J. "Einstein@Home Discovery of 24
Pulsars in the Parkes Multi-beam Pulsar Survey". ApJ, 774, A93 (2013).

*Krishnan, V.; Ellingsen, S.P.; Voronkov, M.A.; Breen, S.L. "The first high-
resolution observations of 19.9-GHz methanol masers". MNRAS, 433, 3346-3363
(2013).

*Lagattuta, D.J.; Mould, J.R.; Staveley-Smith, L.; Hong, T.; Springob,
C.M.; Masters, K.L.; Koribalski, B.S.; Jones, D. H. "WISE TF: A mid-
infrared, 3.4 µm extension of the Tully-Fisher Relation using WISE
photometry". ApJ, 771, 88 (2013).

*Levin, L.; Bailes, M.; Barsdell, B.R.; Bates, S.D.; Bhat, N.D.R.; Burgay,
M.; Burke-Spolaor, S.; Champion, D.J.; Coster, P.; D'Amico, N.; Johnston,
S. and 9 co-authors. "The High Time Resolution Universe Pulsar Survey -
VIII. The Galactic millisecond pulsar population". MNRAS, 434, 1387-1397
(2013).

*Lewis, G.F.; Braun, R. McConnachie, A.W.; Irwin, M.J.; Ibata, R.A.;
Chapman, S.C.; Ferguson, A.M.N.; Martin, N.F.; Fardal, M.; Dubinski, J.;
Widrow, L.; Mackey, A.D.; Babul, A.; Tanvir, N.R.; Rich, M. "PAndAS in the
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