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ATNF News
Issue No. 70, April 2011 ISSN 1323- 6326
CSIRO Astronomy and Space Science ­ under taking wor ld leading astronomical research and operator of the Australia Telescope National Facility.


The Par kes Pha sed Ar r ay Feed ( PAF ) pack age, par tially rot ated, showing the chequer board ar r ay minus the weather cover. The abilit y to inver t the PAF pack age dur ing and af ter assembly enables ef f icient f inal cons tr uc tion and, mos t impor t antly, safe tr anspor t and readiness for sk y tes ting. C r e d i t : R u s s B o l t o n , C S I RO

Cover page image
Aus tr alian Square K ilometre Ar r ay Pathf inder (ASK AP) antenna cons tr uc tion. Credit : Antony Schinckel, CSIRO

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Contents
From the Chief of CSIRO A s tronomy and Space Science .......................................................................................... 4 New Depu t y Chief for C ASS ........................................................................................................................................................ 5 Dis tinguished Visitor s.......................................................................................................................................................................... 6 Gr aduate Student Progr am............................................................................................................................................................. 7 Grote Reber Gold Medal Awarded .......................................................................................................................................... 8 CSIRO Chief Visit s Par kes ............................................................................................................................................................... 9 Ruby Payne -Scot t : Fir s t Inter ferometr y in R adio A s tronomy : Aus tr alia Day 1946.................................. 10 Oper ations Engineer ing Cadet ship E xper ience .............................................................................................................. 14 ASK AP and SK A News .................................................................................................................................................................. 16 Compac t Ar r ay 20 /13 cm and 6 /3 cm Receiver Upgr ade ....................................................................................... 20 C ASS Teacher Scholar ship ........................................................................................................................................................... 22 S - PASS : S -band Polar isation All Sk y Sur vey ...................................................................................................................... 24 C AB B Zoom Modes Produce New Science ..................................................................................................................... 28 ATC A Discover s an Ionised Jet A ssociated With a Young High-mass St ar G345. 5+ 01. 5................... 30 SZ and X-r ay Peak s Don't Cor respond ............................................................................................................................... 32 Education and Ou treach................................................................................................................................................................ 34 Oper ations.............................................................................................................................................................................................. 35 Publications Lis t ................................................................................................................................................................................... 37

Editorial
Welcome to this the Apr il edition of ATNF News for 2011. Once again we br ing you ar ticles and news items of interes t, all associated with the oper ation of our National Facilit y. In a feature packed issue, Miller G os s c a p t u r e s t h e p a s t , d e t a i l i n g Ruby Payne-Scot t's pioneer ing wor k in r adio as tronomy and the f ir s t use of a r adio as tronomical inter ferometer at Dover Heights on Aus tr alia Day, 1946 . We're then back to the present day with a number of science ar ticles focused on the lates t i n r a d i o a s t r o n o m i c a l r e s e a r ch . This includes an ar ticle by C ASS scientis t Et tore Car ret ti who provides his lates t update on the S -band Polar isation All Sk y Sur vey (S - PASS). The sur vey has mapped the dif fuse polar ised emission of t he e n t ir e sou t he r n s k y w i t h t he Par kes r adio telescope at 2.3 GHz. In other science repor ts we feature a repor t on the Sunyaev-Zel'dovich ef fec t in gala x y clus ter s and we look at some new science emer ging via the new "zoom" modes of the Compac t Ar r ay spec trometer. We then talk with new C ASS Deput y Chief Sar ah Pearce who joins us from Gr idPP (the UK computing gr id for par ticle physics, s e t u p to d e a l w i t h d a t a f r o m CER N 's L ar ge Hadron Collider) . Welcome aboard Sar ah ! In other news, Mar k Bowen repor ts on receiver upgr ades at the Compac t Ar r ay, C ASS Teacher Scholar Stephen Broder ick enjoys his week with the PULSE @ Par kes projec t team, and we repor t on this year's Grote Reber Gold Medal Award recipient -- Jocelyn Bell Bur nell. As always, we provide our regular in-depth update on CSIRO's ASK AP and SK A related ac tivit y. It's a busy year at the Murchison R adio-as tronomy Obser vator y with the cons tr uc tion of suppor t infr as tr uc ture and ASK AP 's remaining antennas both under way. To conclude, we f inish with our regular Oper ations repor t . We hope you enjoy the issue. Your comments and sug ges tions are always welcome. If you'd like to contr ibute to future editions of the ATNF News, please contac t the newslet ter team. Tony Crawshaw and Joanne Houldswor th The ATNF Newslet ter Production Team (newslet ter @ atnf.csiro.au)

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From the Chief of CSIRO Astronomy and Space Science
Phil Diamond Chief of C ASS

This, the 70 th edition of the ATNF Newslet ter, again demons tr ates the breadth of science under taken with the ATNF facilities ; the quality of the engineer ing that suppor ts the telescopes and the professionalism of the oper ations and other suppor t s taf f that enables the whole endeavour to wor k at a continuing high level.
T h is s e n t i m e n t is s t r o ng l y s u p p o r t e d by the ATNF Steer ing Commit tee, which met on the 10 ­ 11 May at Par kes. The Commit tee was keen to tr avel to one of the telescopes, and will continue to d o s o i n t h e f u t u r e , e ns u r i ng t h a t it rotates around all C ASS /ATNF s i te s in t i m e . T h e C o m m i t te e has a var ied member ship, w i t h t h r e e a s t r onom e r s f r om A u s t r a li a n i ns t i t u t e s , t h r e e f r o m the inter national communit y -- cur rently from China , Ger many and the USA ; t wo other member s are non-as tronomer s representing the broader Aus tr alian communit y and there are t wo ex-of f icio

at tendees from CSIRO, and the Direc tor of the Aus tr alian As tronomical Obser vator y (A AO) . The member ship can be found on the ATNF web site. The Commit tee's pr incipal role is to of fer advice to the ATNF Direc tor. I can safely say that they are not shy in providing such advice, but it is always done in a fr iendly and positive manner. At the recent meeting the agenda covered those topics that you would expec t to be discussed, such as a repor t on recent science results from the ATNF, an update on the s tatus of engineer ing projec ts and on oper ations. A major focus of the meeting was a presentation of the f ir s t complete ver sion of the science and engineer ing oper ations plan for the Aus tr alian Square Kilometre Ar r ay Pathfinder (ASK AP) . It is expec ted that the plan will evolve as we receive i n p u t f r o m b o d i e s s u ch a s t h e Steer ing Commit tee, the User s' Commit tee, the ASK AP Science Sur vey Teams and C ASS s taf f. The Commit tee also received a p r e s e n t a t i o n , a n d e n t e r e d i n to a discussion on the proposed fouryear budget for the ATNF and C A S S a s a w h o l e . T h is b u d g e t w ill

not be f inal until the CSIRO Board for mally approves it on 29 June. The second day of the meeting s tar ted with an update of the s tatus of the Square K ilometre Ar r ay (SK A) projec t ; this was enhanced by the ver y welcome announcement by the gover nment in the previous evening's budget of $ 40.2m for the pre-cons tr uc tion s tage of t h e S K A , s ch e d u l e d to r u n f r o m Januar y 2012 until December 2015. The deliver y of the full amount is contingent upon a successful outcome for Aus tr alia ­ New Zealand in the site selec tion process. I am sure that the highlight of the meeting for the Commit tee was the so-called "hay r ide" on the Par kes telescope itself. The telescope was lowered to almos t 0 degrees elevation, the commit tee s tepped onto the sur face and were then r aised above the obser vator y a s t h e d is h r e t u r n e d t o p o i n t a t the zenith. The tr ick is to walk down the dish sur face as the local hor izontal changes ! All Commit tee m e m b e r s m a na ge d to d o s o a n d were later seen safely to the bus to whisk them of f to the air por t . A great f inale to the day !

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New Deputy Chief for CASS
Tony Cr awshaw (C ASS)

ATNF News Editor Tony Cr awshaw spent some time speaking with Dr Sar ah Pearce, new C ASS Deputy Chief.
Hi Sarah. Welcome to CSIRO and more specif ically to C ASS. Thank you ver y much. I 'm ver y happy to be here ! We're happy as well. Could you tell us something of your background ? I was projec t manager for Gr idPP, which r uns the UK computing gr id for par ticle physics, set up to deal with data from CER N 's ( European Or ganisation for Nuclear Research) L ar ge Hadron Collider. I wor ked for them for six year s, f ir s t of all in a d is s e m i n a t i o n r o l e a n d t h e n a s projec t manager. It was ver y exciting to wor k as (a small) par t of such a lar ge and high prof ile projec t , and I was impressed with how well managed and or ganised the par ticle physics communit y is. Gr idPP was a dis tr ibuted projec t , at 16 UK s i t e s a n d C E R N , s o i t w a s go o d prepar ation for wor k ing in C ASS . A n d pr i o r t o t h a t ? Before I s tar ted with Gr idPP, I wor ked in policy for the UK gover nment and Par liament . Par liament was par ticular ly interes ting ; I was a science adviser, w r i t i n g b r i ef i n g m a t e r i a l o n p o l i c y ques tions to do with IT and physics. I covered some controver sial topics, including missile defence, inter net regulation and nuclear power.
Dr Sar ah Pearce Credit : Tony Cr awshaw, CSIRO

It was fascinating to see behind the scenes how politics wor ked, though in the end I found the adver sar ial nature of the sys tem a bit limiting. So I moved back to science, where I think we all wor k together much more ef fec tively. You're obviously well qualif ied. Where did you study ? I have a degree in physics from Ox ford, then a PhD from Leices ter Univer sit y. For my PhD I wor ked on c a li b r a t i ng t h e m i c r o c h a n n e l p l a t e detec tor s for the Chandr a X-r ay obser vator y, using the Daresbur y s y n c h r o t r o n i n t h e U K . I a l s o we n t to Inter national Space Univer sit y for the summer session in 1994, where I had an ama zing 10 week s in Barcelona -- I 'd highly recommend it to anyone who is interes ted in space science, engineer ing or as tronomy.

And your inspiration in joining C ASS ? Wor k ing for Gr idPP, I really enjoyed being par t of one of the wor ld's lar ges t science projec ts. I 'd also been aiming to move back to as tronomy : although I liked wor k ing in par ticle physics, it was never really "my" f ield. Living in Aus tr alia and look ing to wor k in as tronomy, C ASS was the obvious choice. As well as the wor ld-class wor k at Par kes and the Compac t Ar r ay, there is ASK AP cons tr uc tion and then oper ations to look for ward to. And if the SK A comes to Aus tr alia , C ASS will be at the centre of that process, playing a key role in Aus tr alia's lar ges t science facilit y. So in your role as C ASS Deput y Chief what are your key responsibilities ? M y p os i t i o n o n t h e m a n a g e m e n t team is focussed towards C ASS

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Distinguished Visitor s
Ro b e r t B r a u n ( C A SS )

a s a n o r g a n is a t i o n , r a t h e r t h a n ex ter nally. So I 'm responsible for issues such as s taf f ing, Health Safet y & Environment and communications. I 'm also wor k ing closely on the budget : we're cur rently in the mids t of prepar ing a four year plan as par t of the Str ategic Inves tment Process, which takes in ASK AP cons tr uc tion and the s tar t of oper ations, so it's a ver y useful time to join C ASS and wor k towards that goal. And what do you hope to achieve in the role ? I h o p e to h e l p g u i d e C A S S t h r o u g h the changes that are coming in the nex t few year s. With ASK AP, and p o t e n t i a ll y t h e S K A , t h is p e r i o d is a ver y dynamic one for r adio as tronomy in Aus tr alia . This is an unprecedented inves tment , which will mean new ways of wor k ing and doing science. We need to make sure we can move towards this new e r a w i t h o u t l os i n g t h e e x p e r t i s e a n d excellence that has led to CSIRO's leading position in r adio as tronomy. I k now it's only been a shor t while, but what are your f ir st impressions of C ASS ? I 'm ver y impressed with the dedication of all the s taf f at C ASS . They are at the cut ting edge in their

f ields, whether that's engineer ing, as tronomy, or computer science, and they are all keen to do an outs tanding job that deliver s wor ld-class science. I 'm par ticular ly impressed with how long s taf f seem to wor k for C ASS --there have been sever al long ser vice awards since I got here ! I also appreciate the collegiate atmosphere : ever yone I 've met has been ex tremely helpful and welcoming. Finally, what in par ticular excites you about the f ield of astronomy and space science ? I 've been fascinated with as tronomy in all its facets since I was in school. It s tar ted with some of the popular book s on cosmolog y, such as In search of the big bang by John Gr ibbin and Steven Weinber g's The f ir st three minutes. I found, and s till f ind, the scale of as tronomy compelling. As Douglas Adams said : " Space... is big. Really big. You jus t won't believe how vas tly hugely mindbog gingly big it is..." I think that's what I like about it : as tronomy dwar fs all the other sciences, both in scale and in some of the concepts it explores. Thank s for your time Sarah. My pleasure.

Over the pas t months we have enjoyed wor k ing visits from Ar is Kar as ter giou ( Univer sit y of Ox ford, UK ) and Bill Coles ( Univer sit y of Califor nia San Diego, USA) Upcoming visitor s we expec t include Patr icia Henning ( Univer sit y of New Mexico, USA) , Jose Gomez ( Ins tituto de As trofÌsica de AndalucÌa , Grenada , Spain) , Dale Fr ail ( National R adio As tronomy Obser vator y, USA) , Paul Nulsen ( Har vard-Smithsonian Center for As trophysics, USA) , Mar tin Cohen ( Univer sit y of Califor nia , Ber keley, USA) and Jim Jack son ( Bos ton Univer sit y, USA) . T h e D is t i ng u is h e d V is i t o r s p r o g r a m remains a ver y produc tive means of enabling collabor ative research projec ts with local s taf f, adding subs tantially to the vitalit y of the research environment . Visits can be or ganized for per iods r anging from only a few week s up to one year. For more infor mation please see w w w.atnf.csiro.au /people / distinguished_visitor s.html Prospec tive visitor s should contac t the local s taf f member w i t h t h e m os t s i m i l a r i n t e r e s t s .

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Gr aduate Student Program
Baer bel Kor ibalsk i (C ASS)

We would like to of ficially welcome the following s tudents into the ATNF co-super vision progr am. · Paul Cos ter ( Univer sit y of Swinbur ne) -- Accelerated searches for the most relativistic binar y pulsar s using nextgeneration instr umentation w i t h s u p e r v is o r s D r W ill e m van Str aten ( Univer sit y of Swinbur ne) , Dr Simon J o h ns t o n ( C A S S ) a n d D r Mike Keith (C ASS) . Phoebe de Wilt ( Univer sit y of Adelaide) -- Investigating the connection bet ween star for ming regions and unidentified TeV gamma-ray sources with super visor s Dr Gavin Rowell ( Univer sit y of Adelaide) , Dr K a te B r o o k s ( C A SS ) a n d D r J ill R a t h b o r n e ( C A S S ) . Stuar t Wes ton ( Univer sit y of Auck land, NZ ) -- Development and Astrophysical Applications of the High Per for mance Radio Astronomical Image Processing Pipeline for e-VLBI with s u p e r v is o r s D r S e r g e i G u l y a e v ( Univer sit y of Auck land, NZ ) and Dr Tim Cor nwell (C ASS) .

·

Annie Hughes ( Univer sit y of Swinbur ne) -- Molecular Gas in the Lar ge Magellanic Cloud. Joanne Dawson ( Univer sit y of Nagoya , Japan) --Super shells as Molecular Cloud Factor ies in the Evolving ISM : Obser vations of HI and 12CO in the Galactic Super shells GSH 287+ 0417 and GSH 277+ 00 +36. Sar ah Bur ke-Spolaor ( Univer sit y of Swinbur ne) --Super massive Black Hole Binar ies and Transient Radio Event s : Studies in Pulsar Astronomy. Natasa Vr anesevic ( Univer sit y of Sydney) -- Galactic distr ibution and evolution of pulsar s.

·

Nat asa Vr anesevic

·

·

·

·

Dr Annie Hughes is now a pos tdoc a t t h e M a x P l a n c k I ns t i t u t e i n Heidelber g, Ger many. Dr Sar ah Bur ke-Spolaor is now a Bolton Fellow at CSIRO As tronomy and Space Science. And Dr Jo Dawson is now an Aus tr alian Research Council Super Science Fellow at the Univer sit y of Tasmania . Well done ! A summar y of the ATNF Gr aduate Student Progr am, cur rent and p a s t s t u d e n t s , a s we l l a s n e w application for ms can be found at ht tp ://w w w.atnf.csiro.au /research / graduate /scholar s.html

Sar a B ur ke -Spolaor

Congr atulations to the award of their PhD degree and bes t wishes for their future career goes to the following s tudents.

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Grote Reber Gold Medal Awarded
Ken Keller man ( NR AO)

The 2011 Grote Reber Gold Medal for lifetime innovative contributions to r adio as tronomy will be awarded to Dr Jocelyn Bell Bur nell who is cur rently a Professor of As trophysics at Ox ford Univer sity in England. Bur nell is being honored for her dr amatic 1967 discover y of pulsar s which has had a major impac t on the second half of 20 th centur y as trophysics and her continuing contr ibutions to as trophysics and education.
Jocelyn Bell Bur nell received her fir s t degree in Physics in 1965 from Glasgow Univer sit y in Scotland and her PhD from the Univer sit y of Cambr idge in 1968. Following a t wo year Science Research Council Fellowship, she held a Teaching Fellowship at the Univer sit y of Southampton followed by research a n d m a n a g e m e n t p os i t i o n s a t the Univer sit y College, London and the Royal Obser vator y in Edinbur gh. Af ter a ten year per iod as a Professor of Physics at the Open Univer sit y of the United Kingdom where she s tudied X-r ay sources, she ser ved as Dean of Science at the Univer sit y of Bath. Bell Bur nell is bes t k nown for her role in the discover y of pulsar s. As a r e s e a r ch s t u d e n t i n C a m b r i d ge she was heavily involved in the cons tr uc tion and oper ation of a long waveleng th r adio telescope built to s tudy inter planetar y scintillations at 4 -m waveleng th. L ater, while inspec ting the output char t records, she noticed a peculiar for m of a s ig n a l w h i c h h a d a p e r i o d i c p u l s e r ate close to one second. Like Grote Reber, she initially had to convince her bet ter es tablished colleagues that her obser vations were impor tant for as tronomy and not due to ex ter nal inter ference or to a spur ious ins tr umental ef fec t . S h e ha s p r ev io u s l y b e e n h o n o r e d by many pr izes and recognitions, including the Alber t Michelson Medal of the Philadelphia Fr ank lin I ns t i t u t e , t h e J R o b e r t O p p e n h e i m e r Memor ial Pr ize from the Miami Center for Theoretical Studies, the Tinsley Pr ize from the Amer ican As tronomical Societ y, and the Her schel Medal from the Royal As tronomical Societ y. She has ser ved as President of the Royal As tronomical Societ y, is a Fellow of the Royal Societ y, is cur rently the President of the Ins titute of Physics, and in June 20 07, she was made Dame Commander of the Br itish Empire ( DBE ) by Queen Elizabeth II .

Jocelyn Bell Bur nell Credit : Univer sit y of Bath The 2011 Reber Medal will be presented to Dame Jocelyn in Augus t 2011 at the X X X UR SI G e ne r a l A s se m b l y in I s t a n b ul , Tur key. The Reber Medal was es tablished by the Tr us tees of the G r ot e R e b e r Fo u n d a t i o n to h o n o r the achievements of Grote Reber and is adminis tered by the Queen Vic tor ia Museum in L aunces ton, Tasmania . Nominations for the 2012 Medal may be sent to Mar tin G e o r ge , Q u e e n V i c to r ia M u s e u m , Welling ton St , L aunces ton, Tasmania 7250, Aus tr alia or by email to : mar tin @ qvmag.tas.gov.au to be received no later than 15 Oc tober 2011.

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CSIRO Chief Visits Par kes
E r i k Le ns s o n ( C A S S )

CSIRO Chief E xecutive Megan Clar k at Par kes. Credit : John Sar k issian, CSIRO

CSIRO Chief E xecutive Megan Clar ke visited the Par kes Obser vator y on 21 March 2011, accompanied by her husband Trent. The visit included an inspec tion of the refur bished Visitor s Centre, as well as discussion of as tronomical obser ving trends with ATNF Science Oper ations and As trophysics s taf f.
A s i t e t o u r w i t h E ng i n e e r i ng Oper ations included the 12-m ASK AP Tes t Bed and a discussion with Andrew Hunt and Tim Ruck ley about the new Par kes 64 -m a n te n na M a s te r C o n t r o l Pa n e l ( MCP) , a key achievement for the Par kes Obser vator y March 2011 shutdown. Megan appreciated the r e t r o l o o k w h ils t n o t i ng t h e a ll n e w computer controllable elec tronics and agreed that there is s till a place

for the analogue human inter face. S h e w a s a ls o i n t e r e s t e d i n t h e n e w Par kes backend switch, its impac t o n e x is t i ng a n d f u t u r e o b s e r v i ng and how remote obser ving might develop with sys tems providing tac tile feedback and vir tual realit y technolog y. Ken Reeves took Trent up the dar k centr al column for a look at the "Cr icket Pitch" on the sur face of the Dish. Megan and Trent then enjoyed infor mal discussions and mor ning tea with s taf f at Par kes Quar ter s.

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Ruby Payne-Scot t : Fir st Inter ferometr y in Radio Astronomy: Australia Day 1946
Miller Goss ( NR AO)

At sunrise on Aus tr alia Day 1946 (26 Januar y) , Ruby PayneScot t (Figure 1) obser ved the sun at Dover Heights, the f ir s t use of a r adio as tronomical inter ferometer.
She had been employed by the Council for Scientif ic and Indus tr ial Research, Division of R adiophysics since 1941. Payne-Scot t used a 20 0 - MHz antenna , a por tion of a shore defence r adar sys tem ( Figure 2) , cons tr uc ted dur ing the ear ly year s of Wor ld War II ( W WII ) . By ear ly 1946 the Aus tr alian Ar my had allowed the Radiophysics L abor ator y ( RPL) to use the receiving aer ial for r adio as tronomy research. A " Lloyds mir ror" inter ference pat ter n was obser ved by recording the i n t e ns i t y v a r i a t i o ns a s t h e r is i ng s u n appeared over the sea . Inter ference occur red bet ween the direc t and ref lec ted r ays from the sea , leading to a ser ies of ma xima and minima ( "lobes" ) . With the clif f height of about 90 metres, the fr inge s e p a r a t i o n w a s s l ig h t l y l e s s t h a n t h e size of the quiet sun. The ef fec tive baseline of the inter ferometer is t wice the clif f height . Radio as tronomical obser vations of the ac tive sun had, however, already begun in Oc tober, 1945. J L Pawsey, Ruby Payne-Scot t and L L McCready had s tar ted obser vations of the sun using the Royal Aus tr alian Air Force 20 0 - MHz aircr af t war ning r adar antenna at Collaroy, nor th

Figure 1: Ruby Payne -Scot t as a young s tudent in the 1930s , possibly while she was a s tudent at the Univer sit y of Sydney 1929 ­ 1932, wor k ing on a BSc degree in physics . Goss and McGee have wr it ten a biogr aphy : Under t he Radar : The Fir st Woman in Radio Astronomy : Ruby Payne-Scot t, published by Spr inger, 20 09. The book was launched in Sydney and Canber r a in late 20 09, sponsored by the Univer sit y of Sydney School of Physics and CSIRO. ( Photo from the Bill Hall family collec tion)

of Dover Heights. Dur ing these o b s e r v a t i o ns ( p u b lis h e d i n N a t u r e i n ear ly 1946) , the solar emission was d e t e c t e d w i t h t h e s i ng l e a n t e n n a sys tem only. No fr inges or lobes we r e d e t e c t e d d u e t o t h e w i d e dis tr ibution of the sunspots over the sun's sur face. The R PL group d i d d e t e r m i n e t h a t t h e b r ig h t n e s s temper ature far exceeded the expec ted temper ature of the quiet sun at 20 0 MHz. In addition, the r adio intensit y was closely

cor related with the sunspot area as obser ved at the Commonwealth Solar Obser vator y at Mt Stromlo. On Aus tr alia Day 1946 , the situation was quite dif ferent ; a compac t group of sun-spots dominated the sun. The lobe pat ter n was obser ved as the sun rose shor tly af ter 5 am local t i m e . T h e r a d i o s u n a c t u a l l y r os e a b o u t e ig h t m i n u t e s e a r l i e r t h a n o p t i c a l s u n r is e d u e t o t h e i n c r e a s e d refr ac tion at r adio waveleng ths compared to optical refr ac tion. The

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Figure 2 : RPL field s tation, Ar my Reser ve, Dover Heights ; the For tress Fire Command Pos t was in this reser ve, 2.2 k m south of the Macquar ie Lighthouse and 2 k m nor th of Bondi Beach. The location is 7 k m eas t of the centre of Sydney. Date, 18 Febr uar y 1943. This 20 0 - MHz antenna , associated with the main block house, was used for the solar r adio as tronomy sea-clif f obser vations on Aus tr alia Day, 1946 . The view is to the nor th with Nor th Head clear ly visible. Note the ships possibly waiting for the submar ine net at the entr ance to Sydney har bour. (ATNF his tor ical photogr aphic archive B81-1)

r adio lobe pat ter n was obser ved for about an hour due to the lar ge pr imar y beam of the r adio antenna (about 10 degrees) . The presence of deep minima implied a small angular size of less than about 7 a r c m in , w i t h a r e su l t a n t br ightness temper ature in excess of a billion degrees. About t wo week s later ( 7 Febr uar y 1946) , a prominent sunspot appeared, one of the major sunspots in recorded his tor y (about 0. 5 per cent of

solar sur face was covered by the spot) . The 20 0 - MHz r adiation increased in intensit y by a fac tor of ten compared to a few week s ear lier. Numerous obser vations were obtained until the end of March 1946 . In addition to the limit on the size, the location of t h e r a d i o e m is s i o n f r o m t h e s u n could be deter mined with an accur acy of a few arc min. The R PL group found that the emission o r ig i n a t e d f r o m a r e g i o n o n t h e

sun apparently coincident with the m a j o r o p t i c a l s u ns p o t . B a s e d o n cur rent k nowledge, Type I bur s ts we r e b e i n g d e t e c t e d . T h e s e c a n be associated with fundamental f r e q u e n c y p l a s m a e m is s i o n , in the presence of enhanced magnetic fields near sunspots. The " Lloyd's mir ror" or sea-clif f inter ferometer made use of the techniques used dur ing Wor ld War II for "r adio direc tion finding" using r adar s for aircr af t war ning at metre

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waveleng ths. This remar k able r adio inter ferometer consis ted of a single antenna ; a major dr awback was that obser vations could only be car r ied o u t a t s u n r is e o r s u ns e t w h e n r adio refr ac tion ef fec ts were quite pronounced. The techniques used by Payne-Scot t in ear ly 1946 used t h e s a m e m e t h o d o log y p io n e e r e d by numerous groups in Aus tr alia , t h e U K a n d t h e U S d u r i ng W W I I for use in r adar. In Aus tr alia , John Jaeger, an applied mathematician who wor ked at R PL, had wor ked out the theor y of the lobe pat ter ns in 1943. In the UK , both J A R atclif fe and Fred Hoyle had independently c a r r i e d o u t s i m il a r s t u d i e s . In the publication of the exciting results from the seaclif f inter ferometr y from 1946 (publication Augus t 1947 ) , Pawsey, Payne-Scot t and McCready sug ges ted, for the fir s t time, the pr inciples of aper ture synthesis using the method of Four ier summation. T h e ot h e r g r o u p t ha t m a d e r a p i d advances in the 1945 ­ 1946 er a was the Cavendish L abor ator y of the Univer sit y of Cambr idge, under the leader ship of R atclif fe a n d M a r t i n Ry l e . A f t e r a r e m a r k a b l y shor t per iod of ins tr umental developments in ear ly 1946 , Ryle and Vonber g were ready to obser ve the sun in July 1946 , when another prominent sunspot appeared. They obser ved the sun at 175 MHz with a " Michelson" inter ferometer with a var iable spacing up to 140 waveleng ths (240 metres) . They

Figure 3 : The mos t commonly published photogr aph of Ruby Payne -Scot t . This was t aken at the Pot t s Hill Reser voir, likely in late 1948. "Chr is" Chr is tiansen is to the r ight with Alec Lit tle in the middle. Payne -Scot t and Lit tle were wor k ing on obser vations of the sun at 97 MHz using the newly cons tr uc ted swept-lobe inter ferometer. (ATNF His tor ical Photogr aphic Archive : B14315 and Hall family collec tion)

found that the solar emission was less than 10 arc min in size, and associated the r adio emission with the sunspot due to the compac t size of the r adio emission. In contr as t to the Sydney data , the position o n t h e s u n w a s n ot d e t e r m i n e d . I n a g r e e m e n t w i t h o t h e r g r o u ps

i n t h e U K a n d A u s t r a l i a , Ry l e and Vonber g detec ted circular polar isation from Type I bur s ts a t t h is t i m e . I n t h e n e x t d e c a d e s , the Michelson inter ferometer became the ins tr ument of choice for r adio as tronomer s.

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Figure 4. A photo of a numb (dr ink ing a cup of tea) , Alec Car ter and Joe Pawsey. The telescopes at Pot t s Hill. This t h is g r o u p d is a g r e e w i t h t h e

er of the R PL s t af f at Pot t s Hill circa 1950. From lef t to r ight , Ruby Payne -Scot t Lit tle, Geor ge Fair weather (a technician s t anding in the door) , possibly Alan location is in front of one of the tr ailer s used for ins tr ument ation of the r adio photo is damaged with numerous spot s , likely ink . Some colleagues that k new identification of Alan Car ter. ( Bill Hall family collec tion)

The life of Ruby Payne-Scot t has recently been summar ised by W M Goss ( NR AO) and R X McGee ( Division of Radiophysics , retired) . Under the Radar : The Fir st Woman in Radio Astronomy: Ruby PayneScot t was published by Spr inger in 20 09. A number of highlights of her life and career (CSIR and CSIRO from 1941 to 1951) are descr ibed, including a detailed account of the fir s t recorded r adio as tronomy o b s e r v a t i o ns i n A u s t r a li a c a r r i e d out in March 194 4 by Pawsey and Payne-Scot t . The mos t innovative

per iod of her career as a r adio as tronomer was the per iod 1949 ­ 1951, wor k ing at the Pot ts Hill (Sydney) site with Alec Lit tle as they developed the swept lobe inter ferometer. The motions of the Type IV outbur s ts were tr acked in real time by obser ving the sun 25 times per second. In Figures 3 and 4, t wo group photos of some of the individuals at the Pot ts Hill site from this per iod are shown. Prominent r adio as tronomer s of this er a were present : Pawsey, Chr is tiansen, Payne-Scot t and Lit tle.

Advances in techniques in this immediate pos t War per iod have had a major impac t on the development of r adio as tronomy in the 20 th centur y. The major sunspot ac tivit y of 1946 ­ 1947 was a major s timulus as r adio inter ferometr y development acceler ated. A book about Payne-Scot t for a non-scientific audience is cur rently in prepar ation by Goss : Mak ing Waves : The Stor y of Ruby Payne-Scot t : Australian Pioneer Radio Astronomer.

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Oper ations Engineering Cadetship Experience
Peter Mir t schin (C ASS)

Dur ing the 2010 calendar year, Oper ations under took a cadet engineer progr am. This progr am was targeted at giving t wo third year engineer ing s tudents indus tr ial engineer ing wor k exper ience at C ASS obser vator ies.
An emphasis was for the cadets to gain an "end-to-end" appreciation of oper ational r adio as tronomy s y s t e m s e ng i n e e r i ng u n d e r t h e guidance of a professional mentor/ super visor. The projec t wor k was n o t li m i t e d t o o p e r a t i o n a l s y s t e m s , but could involve engineer ing research or development wor k in line with the development projec ts under way at the Obser vator ies. Another goal was to provide a benefit to C ASS oper ations in an area that might not other wise occur by car r ying out a defined projec t t h a t a l ig n e d w i t h t h e i n t e r e s t s of both the cadet and C ASS . Cathy Mitchell was the successful candidate located at Par kes. Her projec t entailed some inves tigative wor k in the area of vibr ation analysis. The ultimate aim of this wor k is to develop an automated s y s t e m w h i ch c a n m o n i to r t h e vibr ation signature of a telescope i n o p e r a t i o n . S h o u l d s o m e t h i ng detr imental occur, such as a failed

b e a r i n g , t h e v i b r a t i o n s ig n a t u r e c h a ng e c a n b e d e t e c t e d a n d r e p o r t e d to o p e r a to r s i n a t i m e l y manner. Cur rently this func tion is car r ied out by the obser ver noticing abnor mal noises. With automation and obser ver s being located remotely, this new monitor ing method becomes impor tant for maintaining the integr it y of the s tr uc tures. Her ef for ts have been a great fir s t s tep. Ben McKay was the successful c a d e t a s s ig n e d t o N a r r a b r i a n d h i s projec t was to provide improved monitor ing inter faces bet ween the obser vator y computing environment and real wor ld monitor points t h a t a r e d is p e r s e d t h r o u g h o u t the obser vator ies. These points are cr ucial for the ongoing oper ation of the obser vator y. Ben's initial focus was to provide improved methods for MoniC A to access Aus tr alia Telescope (AT ) s e r i a l d a t a s e t b u s e s . M o n i C A is a sof t ware application used at the obser vator ies for monitor ing and archiving of telescope monitor points. AT datasets are inter face hardware which enables computer s to monitor physical measurements of key par ameter s within the obser vator y. AT datasets are i n t e g r a l i n t h e e x is t i ng o b s e r v a t o r i e s and there is a growing need for multiple s takeholder sof t ware applications to have simultaneous

access to these dataset buses. A s tandalone R PC ( Remote Procedure Call) ser ver application has been completed which enables this to take place. In addition, it also provides the option for Modbus (an indus tr y reques t and reply protocol) controller s to monitor AT dataset m o n i to r p o i n t s , i f r e q u i r e d . T h e second s tage of the projec t was to enable MoniC A to access Modbus devices direc tly. This has enabled MoniC A to ver y easily access any commercial of f the shelf Modbus equipment that may be ins talled at an obser vator y. Of cour se, there a r e t h e u s u a l cr i t e r ia , s u ch a s R a d i o Frequency Inter ference tes ting, that has needed to take place before ins talling commercial equipment . Specifically at Par kes, with the completion of this sof t ware, MoniC A & LOboss sof t ware suites are now able to tr ansparently and simultaneously access the same dataset buses with no perceived degr adation in per for mance of either application. LOboss continues to be the application for configur ing the Par kes conver sion r ack . At this point in time, Modbus e q u i p m e n t t h a t h a s b e e n i ns t a ll e d at the obser vator ies includes gener ator and mains control and monitor ing as well as sever al temper ature and humidit y sensor s. The sof t ware developed is designed to be suf ficiently gener ic

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that it could be implemented on mos t Linux plat for ms. So thank s to the wor k of Ben we have seen sever al improvements. Fir s tly, the obser vator y sof t ware can now have reliable multiple access to the under lying monitor ing hardware. At Par kes this has enabled the number of points monitored by MoniC A to be doubled whils t r e t a i n i n g t h e e x i s t i n g p u r p os e w r i t t e n obser ving tools. Look ing for ward to the future it will facilitate a centr al monitor ing sys tem without complex i n t e g r a t i o n i n t o t h e o b s e r v i ng sof t ware. Secondly, by enabling an indus tr ial s tandard protocol to be used with MoniC A the cur rent control and monitor ing hardware can easily be expanded by the use of commercial equipment , These achievements have been a bonus for the Developmental Projec t , Par kes Equipment Control and Monitor ( PECM ) , as it moves towards completion. There are p l a ns t o f u r t h e r e x t e n d t h e n u m b e r of points monitored by MoniC A at Par kes in the coming months. Thank s to Euan Troup for some ear ly wor k on this sof t ware and also to John Reynolds for sof t ware changes to LOboss to enable MoniC A access. I would also like to thank all those involved in enabling the c ad e t s h i p p r og r a m . I t ha s b e e n a great success in its fir s t year.

Cathy Mitchell Photo : Peter Mir tschin, CSIRO

Ben McKay Photo : Peter Mir tschin, CSIRO

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ASK AP and SK A News
Flor nes Conway- Der ley (C ASS)

2011 will be a cr itical year in the development of CSIRO's Aus tr alian Square Kilometre Ar r ay Pathfinder (ASK AP) . Following the successful cons tr uc tion of the fir s t s i x A S K A P a n t e n na s a t t h e Murchison Radio-as tronomy Obser vator y ( MRO) in 2010, the over all technical build of ASK AP continues to r amp up.

ASK AP Antennas
Dur ing late 2010, five new ASK AP antennas were delivered and i ns t a ll e d a t t h e M u r c h is o n R a d i o as tronomy Obser vator y ( MRO) in Wes ter n Aus tr alia , br inging the total number of antennas on site to six. At the same time, the fir s t antenna (built in ear ly 2010 ) under went a number of retrofits to br ing it as close as possible to the produc tion design of the r e m a i n i ng A S K A P a n t e n n a s . Comprehensive site acceptance tes ts and initial commissioning ac tivities were also completed on the new antennas, including the fit-out of inter nal par ts such as the suppor t floor, mez zanine and inter nal cable tr ays. An impor tant feature of the a n t e n n a d e s ig n i s t h e a b i l i t y t o s e t reflec tor accur acy at the fac tor y acceptance tes t s tage ; this allows

Member s of CE TC54 in front of an ASK AP antenna at the MRO in Oc tober 2010. Credit : Ter r ace Photogr apher s .

t h e a n t e n na to b e e r e c t e d a t t h e MRO, with no fur ther adjus tment required, while maintaining a specified sur face accur acy. The reflec tor dishes are specified to a sur face accur acy of 1.0 mm, which allows for as tronomycapable oper ation up to 10 GHz. However, the sur face accur acy ac tually achieved on the fir s t six

delivered dishes at the been closer to 0. 5 mm for as tronomy-capable to be doubled to 20 G

MRO has , which allows oper ation Hz .

Not only does this design feature allow for an increased r ange of o p e r a t i o n , b u t i t a ls o d r a m a t i c a ll y saves on ins tallation time. The guar antee of "in-the-field" sur face alignment provides a reliable

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· Ins tallation of 390 k m of optical fibre cable bet ween the MRO a n d G e r a l d to n b e g a n i n O c to b e r 2010. In Apr il 2011, one of four segments was fully completed, with par tial completion in the other areas. The high capacit y li n k w ill b e u s e d t o t r a ns m i t lar ge volumes of data from the MRO for processing ; · A dr y fit-up of the fir s t full-sized Phased Ar r ay Feed ( PAF ) was completed in December 2010, and t wo full (analogue and digital) receiver sys tems are being assembled in prepar ation for preliminar y sys tem integr ation tes ts at the Par kes Tes tbed Facilit y ( PTF ) and on an ASK AP antenna at the MRO ; · Integr ation has commenced on the MATES ( Mar sfield ASK AP Tes t Engineer ing Sys tem) dur ing the fir s t half of 2011, which includes a skeletal PAF receiver w i t h p a r t i a l m o n i t o r i ng a n d control func tions ; dummy heat l o a d s a n d t e m p e r a t u r e m o n i t o r i ng have provided a useful tes tbed for the PAF water cooling sys tem ; · The fir s t meeting of ASK AP PIs ( Pr incipal Inves tigator s) for 2011 was held at Mar sfield in Febr uar y. Following a successful one year review in November, the teams have been wor k ing on source finding and s i m u l a t i o n a lg o r i t h m s w i t h t h e A S K A P C o m p u t i ng t e a m ;

Trench dig ging under way near the B oolardy homes tead. Credit : Bar r y Tur ner, CSIRO

and fas t build process for a " tr aditional panel" s t yle antenna . All 36 ASK AP antennas are being manufac tured by the 54th Research Ins titute of China Elec tronics Technolog y Group Cor por ation (k nown as CE TC54) based in Shijia zhuang, China . Member s of the ASK AP Antenna team recently visited the CE TC54 fac tor y in China

to per for m fac tor y acceptance tes ting. The nex t batch of antennas will ar r ive at the MRO in May, with all 36 antennas expec ted to be built by the end of 2011.

ASK AP General
Key ASK AP updates since the previous issue of the ATNF News went to pr int include :

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Aaron Saunder s , Paul Cooper and Eliane Har k voor t with dr y fi t-up PAF. Credit : Wheeler Studios

· ASK AP was included as par t of the Pawsey Centre's ear ly a d o p t e r s p r o g r a m , c h os e n a s a lar ge projec t that could use the additional computing power to open new avenues of research ; · A new ver sion of the ASK AP sof t ware imaging pack age (ASK APsof t) was released in Febr uar y ; the upgr ade includes enhancements to the vir tual tes t o p e r a t i n g s y s t e m , a we a t h e r s t a t i o n e m u l a t i o n a n d d ig i t a l receiver engineer ing GUI . The t e s t p a c k a g e w ill b e u s e d t o t e s t o b s e r v a t i o ns a n d m e a s u r e m e n t s made dur ing integr ation of the new full-sized PAF ins talled on the PTF in the coming months.

ASK AP antenna contr ac t to date with CE TC54's capacit y to fully assemble and precision align a ll a n t e n n a s i n t h e i r f a c t o r y i n Shijia zhuang before shipping to A u s t r a li a ; r e s u l t i ng i n a f a s t b u il d time and with no adjus tment of the reflec tor sur faces being required once on-site at the MRO. "This was an excellent oppor tunit y to show the antennas to the CEO of CE TC and to continue to explore China's exper tise in producing lowcos t antennas at a cos t-specification for the SK A ," says Carole Jack son. Also in late 2010, the MRO had visits from the MRO Indigenous L and Use Agreement ( ILUA) L i a i s o n C o m m i t t e e a s we l l a s s tudents from Pia Wajar r i, a remote communit y located near Boolardy. The MRO ILUA Liason Commit tee Meeting coincided with a visit to the MRO by C ASS chief Dr Phil Diamond and CSIRO's ASK AP Projec t Direc tor Ant Schinckel, which provided the oppor tunit y to meet infor mally with the Wajar r i

representatives. At the conclusion of the Meeting, ILUA member s viewed, for the fir s t time, the six n e w l y i ns t a ll e d A S K A P a n t e n n a s on a tour of the MRO. The Wajar r i people have provided CSIRO a lis t of Wajar r i names that will be used for key infr as tr uc ture at the MRO in the future.

Industr y Engagement News
The tender for the cons tr uc tion of suppor t infr as tr uc ture was recently awarded to McConnell Dowell Cons tr uc tor s (Aus t .) P t y. Ltd., representing a significant miles tone in the ongoing development of the MRO site. The projec t commences immediately, and involves the cons tr uc tion of sever al k ilometres of access roads and tr ack s, power and data infr as tr uc ture, a centr al control building and 30 r adio antenna concrete foundations, as well as ancillar y wor k s. The design tender for the Murchison Suppor t Facilit y ( MSF )

At the MRO
In December 2010, senior s taf f from China Elec tronics Technolog y Group Cor por ation (CE TC) visited the CSIRO As tronomy and Space Science headquar ter s in Sydney. Both par ties were keen to recognise the success of the

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Mr Tu Tianjie, President of CE TC 54, with Chief of CSIRO A s tronomy and Space Science, Dr Philip Diamond. Credit : Tony Cr awshaw, CSIRO.

at Ger aldton was awarded to Aurecon and final detailing for the design wor k s are under way. The fir s t t wo Redback-2 digital signal processor boards will soon be ready for full integr ation tes ting over the coming months. Puz zle Precision, a supplier of high-end digital sys tems, are cur rently deliver ing the major components of the ASK AP digital sys tems, upon deliver y the b o a r d s a r e f u ll y t e s t e d a n d r e a d y for ASK AP sys tems integr ation.

the development of the PAF SK A Concept Descr iptions, which will be key inputs to the Concept Design Reviews (CoDR s) due to take place bet ween Apr il and Oc tober 2011.

engineer. "This minimises the number of ex ter nal components needed to build a receiver, which also leads to a reduc tion in size, weight , power and cos t ." Once fabr icated, the chips will b e t e s t e d a n d i n t e g r a t e d i n to a demons tr ator ar r ay that will per for m the entire analogue processing in the phased ar r ay feed pack age, and contr ibute significantly toward development of receiver s for the SK A .

First Silicon-onSapphire Prototype SK A Receiver Chip
A significant miles tone was achieved in the development of a r adio receiver on a chip, with the fir s t chip design now fabr icated as par t of collabor ation bet ween C ASS and Silanna (for mer ly Sapphicon Semiconduc tor) . The chip is being manufac tured at Silanna's foundr y in Sydney, and integr ates much of the elec tronics required to process one channel's wor th of data in a Phased Ar r ay Feed ( PAF ) or Aper ture Ar r ay (A A) receiver into a single integr ated circuit . "The chip, w 2 . 8 m m , a ls o circuitr y and S u z y J a ck s o n h i ch m e a s u r e s ju s t 2 . 8 x includes precision bias digital control," says , A S K A P e le c t r onic s

SK A Ac tivities
Work Package Discussions Continue
Discussions with inter national par tner s on SK A Technolog y Wor k Packages ( PrepSK A WP2) continue, focussed on SK A-related research and development such as dish ar r ays, digital sys tems, computing, signal tr anspor t and sys tems. C ASS is coordinating

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Compac t Array 20 /13 cm and 6 /3 cm Receiver Upgr ade
Mar k B owen (C ASS)

In December 2010 the ins tallation of t wo upgr aded 1 ­ 3 GHz receiver s on the Compac t Ar r ay her alded the subs tantive completion of the second phase of the Compac t Ar r ay 20 /13 cm and 6 /3 cm receiver upgr ade. Though the RF signal path of the receiver s is complete, an upgr ade of the receiver control and monitor elec tronics is s till under way. The exis ting receiver elec tronics packages are over 20 year s old and the upgr ade will moder nise them in line with the cur rent millimetre-wave sys tems, ensur ing our ability to suppor t them into the future. This wor k will be completed dur ing the f ir s t half of 2011 and can be accomplished on the antennas without removal of the receiver s.

Af ter the successful demons tr ation of a protot ype 1 ­ 3 GHz receiver in late 20 09, the roll out of fully upgr aded receiver sys tems was commenced in June 2010. A fur ther t wo receiver s were ins talled in Augus t , with the ins tallation of these t wo receiver s also br inging the fir s t phase of the upgr ade projec t to a conclusion. The 20 /13 cm and 6 /3 cm u pg r ad e ha s t h r e e s t a ge s ; t h e fir s t of these included, among other things, the retrofit of new fins to the 20 /13 cm receiver or thomode tr ansducer s (OMTs) . The OMT refit was designed to improve the beam shape in the upper half of the receiver frequency r ange. The discover y of low frequency bias oscillation bet ween pair s of Low Noise Amplifier s ( LNAs) in some upgr aded receiver s dur ing S e p t e m b e r r e s u l t e d i n a h ia t u s i n the ins tallation of the remaining receiver sys tems while a suitable fix was developed. Modifications to the LNA bias circuitr y cured the problem and subsequent receiver s were modified pr ior to ins tallation. The remaining unmodified receiver s Santiago Cas tillo ins talling an upgr aded 1 ­ 3 GHz receiver sys tem. Credit : Henr y Kanoniuk , CSIRO.

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Initial tes ting of the gain s tages, par t of a 4 ­ 12GHz Low Noise Amplifier. Credit Alex Dunning, CSIRO.

are being retrofit ted dur ing the fir s t half of 2011 as par t of nor mal scheduled maintenance. The per for mance of the upgr aded receiver s has exceeded e x p e c t a t i o ns . T h e s y s t e m temper ature ( Tsys) has been measured at ~ 20 K over the band 1.1 ­ 3.0 GHz, an improvement in over all noise per for mance of bet ween 25% - 30 % over the or iginal ATC A L / S receiver sys tems. Jamie Stevens has also char ac ter ised the beam pat ter ns of the upgr aded ATC A antennas bet ween 1.1 ­ 3.1 GHz. The pr imar y beams are symmetr ical within 6 % , independent of frequency. These upgr aded receiver s are now designated as ATC A 16 -cm receiver sys tems. The third and final phase of the projec t is an upgr ade of the 6 /3 -

cm receiver sys tems which will follow a similar development path to the 16 -cm receiver sys tems. The provision of A $1.471M from As tronomy Aus tr alia Limited (A AL) as par t of the Education Inves tment Fund ( EIF ) is funding the completion of this phase of the projec t . The A AL funding will commence in July 2011 ending in June 2013 when the projec t will be completed. The development of cr yogenic 4 ­ 12 GHz LNAs is cur rently under way. To ensure the feasibilit y of the third phase of the projec t , this wor k is being car r ied out by C ASS as par t of the second p ha s e . S u b s t a n t ia l p r og r e s s toward a suitable LNA has been made with tes ting of a protot ype scheduled for ear ly 2011.

When completed, the upgr ade of the exis ting Compac t Ar r ay centimetre receiver s will enable the use of the full capabilit y of the Compac t Ar r ay Broadband Backend (C ABB ) at centimetre waveleng ths. The upgr ade will tr ansfor m the piecemeal cover age of the 1 ­ 12 GHz obser ving spec tr um deliver ing almos t complete cover age in t wo frequency bands 1 ­ 3 GHz and 4 ­ 12 GHz.

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S -PASS : S -band Polarisation All Sk y Sur vey
Et tore Car ret ti (C ASS)

Abstract
The S -band Polar isation All Sk y Sur vey (S - PASS) has mapped the dif fuse polar ized emission of the entire souther n sk y with the Par kes r adio telescope at 2.3 GHz with a resolution of 9'. Aimed at inves tigating the CMB Galac tic foreground and the Galac tic magnetic field, the projec t has required a special setup to cover half a sk y with such a resolution. The obser vations are now completed and the data reduc tion is in progress. With their huge spatial dynamic r ange (360o to 9' ) and high frequency, S - PASS maps deliver a completely new view of the polar ised sk y showing interes ting new features and s tr uc tures at all Galac tic latitudes.

Here we are again t wo year s later t o t a l k a b o u t t h e b e a u t i f u l p o l a r is e d sk y of S - PASS (see Apr il 20 09 issue) . At that time S - PASS was 60 % complete and the data reduc tion s till in an embr yonic s tage, but the fir s t results were showing the high potentialit y of this projec t already. Now, t wo year s later, the sur vey is completed and the resulting maps show the dif fuse polar ised sk y with an unprecedented combination of angular scale dynamic r ange, sensitivit y, and frequency, deliver ing a new view of the polar ised sk y. Unlike previous lower frequency sur veys af fec ted by severe Far aday depolar isation, the dif fuse emission from the Galac tic disc is now unveiled (expec t for a few degree across t h e G a l a c t i c P l a n e ) o p e n i ng a n e w

power ful window to inves tigate the magnetic field of our own Gala x y. But let's s tep back a bit and introduce the projec t fir s t . The S -band Polar isation All Sk y Sur vey (S - PASS) is a projec t to map the dif fuse polar ised synchrotron emission of the entire souther n sk y at 2.3 GHz (Car ret ti et al. 20 07 ) . Car r ied out with the Par kes r adio telescope, the sur vey is aimed at inves tigating t wo cut ting-edge cases of the present as trophysics research : the Galac tic magnetic field, whose lar ge scale s tr uc ture is s t ill a p u z z l e , a n d t h e d e t e c t i o n of the B - Mode of the Cosmic Microwave Background (CMB ) polar ised component , for which the synchrotron emission is one of the s tronges t foreground contaminants.

The s tr uc ture of the Galac tic magnetic field is s till lar gely unk nown. The obser vations show that the ordered component of t h e d i s c i s a l ig n e d a l o n g t h e s p i r a l ar ms, but sever al details of the m o d e l a r e s t ill u n d e r d e b a t e , like number and position of field rever sals (field rever sal means that the field direc tion is preser ved, but a complete rever sal of the heading occur s) . Many data sets are consis tent with one rever sal only, which would make our Gala x y s i m il a r t o t h e e x t e r n a l g a l a x i e s obser ved so far (e.g., Sun et al. 20 08, van Eck et al. 2010 ) , while some author s find that rever sals might occur at any spir al ar m to i n t e r - a r m r e g i o n t r a ns i t i o n , w h i c h would make our Gala x y unique (e.g. Han et al. 20 06) . Moreover, some recent results seem to challenge t h e a l ig n m e n t w i t h t h e s p i r a l a r m s in the outer Gala x y where the field could jus t take a r ing-like shape (e.g. Van Eck al. 2010 ) . The field in the Galac tic halo is even less under s tood, essentially for lack of data in this low emit ting region. Models have been proposed (e.g., Han 20 02, Sun et al. 20 08 ) and the asymmetr y recently discovered in the ver tical component of the local field ( Mao et al. 2010 ) has sug ges ted that a combination of dipole and quadr upole components m i g h t d e s c r i b e we l l t h e l a r g e s c a l e field. However, all the proposed models are poor ly cons tr ained

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both by the lack of the contamination s tr uc tures, like the that can introduce

da t a a nd by lar ge local b ig r a d i o l o o p s , a n o m a li e s .

More data are thus necessar y to under s tand how the Galac tic magnetic field is ar r anged. One of the goals of S - PASS is to help cover this gap, measur ing the polar ised synchrotron emission of the entire souther n sk y. The dif fuse polar ised emission encodes a wealth of infor mation on the magnetic field by R o t a t i o n M e a s u r e ( R M ) , p o l a r is a t i o n a ng l e , p o l a r is a t i o n f r a c t i o n , a n d R M synthesis, which can unlock how t h e e m is s i o n is o r g a n is e d a l o ng t h e line of sight deliver ing a 3D view of t h e i n t e r s t e ll a r m e d i u m ( I S M ) . T h e cover age of the entire souther n sk y allows inves tigation of the field in all the possible environments : plane, disc, halo, disc-halo tr ansition. The other goal of S - PASS is to s tudy the polar ised component of the CMB , which car r ies the signature of the Gr avitational Wave Background (GWB ) emit ted at the Inflation time ( Kamionkowsk i & Kosowsk y 1998, Kinney et al. 20 06 , Boyle et al. 20 06) . This is the only r adiation that can tr avel the Univer se from its ver y ear ly s tages (10 -34 s af ter the B ig B a n g ) u p t o u s m os t l y u n t o u c h e d and gives us the chance to probe the physics of the Big Bang at ener g y densities so high, that no par ticle acceler ator on Ear th can par allel.

The CMB signal is weak , however (10 0 nK the cur rent upper limit) , weaker than the foreground Galac tic synchrotron emission, which thus needs to be removed for a successful detec tion of the cosmological signal. It is something like peer ing through the fog of our Gala x y to a have an unobs tr uc ted view of the far end of the visible Univer se. The goal of S - PASS is to measure with high precision the Galac tic emission to make p os s i b l e C M B d e t e c t i o n s w i t h the lowes t possible er ror. To realise such goals S - PASS has obser ved the entire souther n s k y a t 2 . 3 G H z w i t h h ig h s ig n a l to-noise r atio also in the lowes t emission regions of the halo. The obser vations have been conduc ted from Oc tober 20 07 to Januar y 2010 for a total of about 20 0 0 h, keeping t h e t e a m b u s y o b s e r v i n g a l l n ig h t long for six months in t wo and a half year s -- almos t a retreat ! The frequency is high enough to keep Far aday Rotation ef fec ts under control down to disc latitudes, as shown by the precur sor projec t Par kes Galac tic Mer idian Sur vey ( PGMS , Car ret ti et al. 2010 ) , w h i l e t h e h ig h s e n s i t i v i t y e n a b l e s both high ef ficient foreground cleanings and sensitive rotation measute ( RM ) measurements (the expec ted sensitivit y in the h a l o is s o m e 2 r a d / m 2 w h e n combined with 1.4 GHz data) .

A projec t like S - PASS has posed sever al challenges, pr imar ily to m i n i m is e t h e g r o u n d e m is s i o n contamination and to enable absolute calibr ation, and a special s c a n n i ng s t r a t e g y b a s e d o n l o ng A zimuth (A z) scans has been developed to this pur pose. Ground e m i s s i o n i s m os t l y e l e v a t i o n d e p e n d e n t , a n d A z s c a ns a r e i d e a l t o m i n i m i s e i t . Lo n g a z i m u t h scans (115o) can cover the entire Declination r ange of interes t in j u s t o n e go t h u s p r e s e r v i ng t h e infor mation on all angular scales. The mapping of all the desired R ight Ascension r ange is ensured by the Ear th rotation, that in combination with A Z scans, lets the telescope dr aw zig-zag pat ter ns in the sk y each day. The full cover age of the sk y is realised by precisely t i m i n g t h e s c a n s t a r t e a c h n ig h t , so that day af ter day the zigzags are appropr iately spaced to ensure a unifor m sk y cover age. The vas t area to obser ve and the small pixel size (4. 5' ) have required a high scan speed to conduc t the sur vey in a sensible time dur ation. T h e s c a n r a te ha s b e e n p u s h e d u p to 15o /min, a significant fr ac tion of the slewing speed (24o /min) : not a bad per for mance for a 10 0 0 -tons 64 -m telescope near ly 50 year s old ! To recover the power on all angular scales a "basket weaving" technique (scan crossing) is required. Basket

23


weaving is a tr ick y job with a zimuth scans. However, the same Dec r ange can be obser ved either when t h e s k y r is e s o r s e t s , b u t w i t h a dif ferent path in the sk y. Two sets of scans has then been obser ved, one e a s t w a r d a n d o n e we s t w a r d , w h o s e combination realises an ef fec tive scan crossing ( Figure 1) . This, along with the modulation of the signal by par allac tic angle var iation a l o ng t h e s c a n , h a s p e r m i t t e d full recover y of the emission on all angular scales (for details see Car ret ti 2011, Car ret ti et al. 2011) . As example, Figure 2 shows the final map of Stokes Q. This is absolutely c a li b r a t e d a n d a t f u ll r e s o l u t i o n deliver ing a spatial dynamic r ange of 240 0 (360o to 9' ) , maybe one of the highes t ever obtained in r adio as tronomy. Thank s both to the high r e s o l u t i o n a n d h ig h f r e q u e n c y t h a t reduce Far aday Rotation ef fec ts, the map shows an unprecedented amount of detail. The emission i s s m o o t h b o t h a t h ig h G a l a c t i c latitude and in the disc down to 5o ­10o from the plane even in the inner Gala x y, symptomatic that Far aday depolar isation is mar ginal almos t down to the Galac tic plane. This unveils the disc, which was s t r o ng l y d e p o l a r is e d u p t o l a t i t u d e |b| ~ 30o in previous sur veys taken at 1.4 GHz ( Figure 3) . S - PASS thus opens a new window to inves tigate the magnetic field in the disc with polar ised dif fuse emission. Ver y lar ge scale s tr uc tures are v i s i b l e a t h ig h G a l a c t i c l a t i t u d e s . The mos t obvious is the ver tical s tr uc ture along longitude l= 0o that

Figure 1: Combination of eas t and wes t scans . The t wo set s span the same Declination r ange bu t with a dif ferent path in the sk y. The resulting crossing enables an ef fec tive basket weaving.

Figure 2 : S - PASS Stokes Q map. Galac tic coordinates centred at the Galac tic Centre are used. Longitude increases lef t ward.

Figure 3 : All-sk y map of polar ised intensit y emission at 1.4 GHz. This image is combination of the Dominion R adio A s trophysical Obser vator y (nor th) and Villa Elisa sur vey (sou th) and is in Galac tic coordinates centred at the Galac tic Centre. Longitude increases lef t ward.

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s t r e t ch e s f r o m t h e s o u t h G a la c t i c pole up to the nor th end of the map for a total leng th of near ly 150o. Br ight ex tended emission made of sever al r idges is also obvious in the i n n e r G a la x y a t n o r t h la t i t u d e s (b ~ 0o ­30o) and wes t of l= 0o. I n t h e o u t e r G a l a x y t h e p o l a r is e d emission is detec ted down to the Galac tic plane, even if modulation by Far aday Rotation is obvious. Prominent features in the disc are t wo heavily depolar ised regions on either sides of the Galac tic centre and the Gum nebula in the outer Gala x y. The for mer s well m a t c h b r ig h t H I I r e g i o n s w h os e high elec tron column densit y is the likely cause of the depolar isation. The lat ter is centred at l~260o and s tretches for 30o ­ 40o in longitude and +/- 15o in latitude and closely follows the H emission associated to the Gum Nebula . In the same area the Vela Nebula is also clear ly visible. At high Galac tic latitudes the e m i s s i o n i s s m o o t h a n d we a k . T h e lar ge scale emission closely follows that of Wilk inson Microwave Anisotropy Probe ( WMAP) maps, even though with much higher S / N . The S - PASS emission is thus mos tly free from Far aday Rotation ef fec ts and its analysis will give a sounding basis to es timate and clean the Galac tic emission contamination in CMB data . Moreover, the lowes t emission regions that will be identified in S - PASS can be ideal tar gets for CMB g r o u n d b a s e d e x p e r i m e n t s , w h i ch seek for the cosmic signal in small

s k y a r e a s . F o r e g r o u n d e m is s i o n is also a s trong contaminant for Epoch of Reionisation exper iments like Murchison Widefield Ar r ay, w h os e o b s e r v a t i o n s m ig h t b e conveniently pointed to the S - PASS lowes t emission regions as well. Now the time of data analysis and inves tigations s tar ts. A fir s t catalogue of near ly 50 0 0 point source R Ms has been ex tr ac ted already, while R M analysis of t h e d i f f u s e e m is s i o n a n d C M B foreground analysis will s tar t soon. In summar y, S - PASS obser vations have been successfully completed in t wo and half year s of long o b s e r v i n g n ig h t s . T h e d i s c e m i s s i o n look s unveiled at las t and promises new insights into the s tudy of this par t of the Gala x y, while the h ig h S / N a t h ig h l a t i t u d e p r o m i s e s both a big improvement in the foreground cleaning ef ficiency and a bet ter under s tanding of the lar ge scale Galac tic field. The data analysis has now begun and t h e n e x t t i m e we w r i t e o n t h e s e p a g e s we h o p e t o r e p o r t o n t h e new findings that this projec t will have car r ied out . Stay tuned.

S - Band Polar isation All Sk y Sur vey, Par kes projec t P560. Car ret ti E., Haver kor n M ., McConnel D., Ber nardi G ., Cor tiglioni S ., McClure- Gr if fiths N . M ., Poppi S ., 2010, MNR AS , Car ret ti E., 2011, in The Dynamic ISM : A celebration of the CGPS, ASP Conf. Ser., 438 Car ret ti E., et ., 2011, in prepar ation Han J . L ., 20 02, in Astrophysical Polar ised Backgrounds, AIP Conf. Ser., 609, 96 Han J . L ., Manches ter R . N ., Lyne A .G ., Qiao G . J ., van Str aten W., 20 06 , ApJ , 642, 868 Kamionkowsk i M ., Kosowsk y A ., 1998, PRD, 57, 685 K inney W. H ., Kolb E.W., Melchior r i A ., R iot to A ., 20 06 , Phys. Rev. D, 74, 023502 Sun X . H ., Reich W.,Waelkens A ., Enúlin T. A ., 20 08, A & A , 47 7, 573 Tes tor i J .C ., Reich P., Reich W., 20 08, A & A , 484, 733 Van Eck C . L ., Brown J .C ., Stil J . M . , R a e K . , M a o, S . A . , Gaensler B . M ., Shukurov A ., Taylor A . R , Haver kor n M ., K ronber g P. P., McClureGr if fiths N . M ., 2010, submit ted to ApJ , arXiv :1012.2938 Wolleben M ., L andecker T. L ., Reich W., Wielebinsk i R ., 20 06 , A & A , 4 48, 411

References
Boyle L . A ., Steinhardt P. J ., & Turok N ., 20 06 , Phys. Rev. Let t . 96 , 111301 Car ret ti E., Staveley-Smith L ., Haver kor n M ., Ber nardi G ., C o r t ig l i o n i S . , G a e n s l e r B . , Kes teven M ., Poppi S ., 20 07,

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CABB Zoom Modes Produce New Science
Ma xim Voronkov, James Ca swell and James Green (C ASS)

The eager ly anticipated "zoom" modes of the new Aus tr alia Telescope Compac t Ar r ay spec trometer (also k nown as C A B B ) b e c a m e o p e r a t io na l

mid 2010 and have begun to yield new scientific results.
Recently put into press is a m a s e r s t u d y w h i c h d e m o ns t r a t e s the capabilit y of simultaneously obser ving eight spec tr al lines at ver y

high spec tr al resolution ( Voronkov et al., MNR AS , in press ; ht tp ://dx.doi. or g /10.1111/j.1365-2966.2011.18297.x) including a new t ype of methanol maser at 23.4 GHz. These results are shown in Figure 1. The top f u ll s p e c t r a l li n e s a r e a r e l a t e d

F ig u r e 1: B a c k g w h i c h w e h av e ma se r s , r espe c simult aneously

round map is the 8 .0 micron IInfr ared Ar r ay Camer a ( IR AC) Spit zer Space Telescope image of 357.97- 0.16 on mar ked the r adio mea surement s of var ious maser species (circle and squares show class I and class II methanol tively ; crosses show water ma ser s) . Alongside the map we show the eight spec tr a of the class I maser s t aken in C AB B high resolu tion multiple zoom mode.

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ser ies of methanol tr ansitions well k nown as maser s, and clear ly reveal the slowly changing proper ties (amplitude and s tr uc ture) as we pass down the ser ies. The bot tom line is a tr ansition of methanol not previously k nown as a maser, and it

can be seen to be the s tronges t of all the lines. The new modes also allowed a s tudy of an enigmatic OH maser showing both s trong circular and linear polar isation, now recently p u b l i s h e d ( F i g u r e 2 , a n d C a s we l l & Green, 2011, MNR AS , 411, 2059 ;

ht tp ://dx.doi.or g /10.1111/j.13652966.2010.17856.x) . This projec t d e m o ns t r a t e s t h e n e w c a p a b ili t y of recording full polar ization at a s p e c t r a l r e s o l u t i o n e ig h t t i m e s bet ter than was possible before. Fur ther more, the full zoom mode c a p a b ili t i e s a r e b e i ng e x p l o i t e d i n a sur vey of the magnetic fields in high-mass s tar for mation regions (entitled " MAGMO" ) , which aims to deter mine the magnetic fields a c r os s t h e G a l a x y t h r o u g h t h e measurement of Zeeman split ting of OH maser s. This sur vey will obser ve four tr ansitions of OH maser s simultaneously, with a lar ge frequency cover age at each tr ansition (equivalent to ~30 0 k m /s) , in all four Stokes par ameter s. The new zoom modes are cur rently being used in a wide var iet y of projec ts r anging from the s tudies of per iodic maser flares to the mapping of HI in near by gala xies.

Figure 2 : Det ailed spec tr a of the 1667- MHz OH tr ansition towards OH24.329+ 0.145 (2010 July) . The upper panel shows R HC (solid) and LHC (da shed) polar isations . The lower panel shows the Stokes par ameter s Q (solid) and U (dashed) revealing significant linear polar isation.

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ATCA Discover s an Ionised Jet Associated With a Young High-mass Star G345. 5+ 01. 5
Andres Guzman ( PhD s tudent , Univer sit y of Chile / C ASS)

We have discovered, using ATC A , a ver y good example of an ionised jet associated with a ver y young high-mass s tar. The presence of this jet for ms impor tant obser vational evidence that cons tr ains the theor y of high-mass s tar for mation.
A n i n t r ig u i n g d a t u m a b o u t t h e process of for ming high-mass s tar s (greater than 8 solar masses) is the common presence of massive and fas t-moving molecular bipolar outf lows, t ypically of sever al solar masses and velocities in excess of tens k m /s. Are these more power ful ver sions of the out f lows that are readily obser ved toward ver y young low-mass s tar s and consequently do they imply one gener ic diskmediated accretion for mation process for all s tar s across the s tellar mass spec tr um ? Conf ir mation of this would be via direc t obser vation of an accretion disk sur rounding a high-mass s tar. Unfor tunately the sites of high-mass s tar for mation hamper such obser vations because they are located far from E a r t h , e m b e d d e d i n d e ns e , d u s t y molecular clouds, and evolve on fas t time-scales. Obser vation of ionised jets of fer an alter native, albeit indirec t, means to conf ir m a disk-accretion for mation process.

So far there are about a dozen repor ted detec tions of ionised jets towards young high-mass s tar s. If t h e s e i o n is e d j e t s a r e a n a l o g u e s t o their low-mass counter par ts then these jets are intimately linked to the accretion-disk for mation process and power the obser ved massive molecular bipolar out f lows. An ionised jet towards a high-mass young s tellar objec t ( HMYSO) can be obser ved through its r adio continuum emission at centimeter waveleng ths. This ther mal freefree continuum emission is more commonly associated with the i o n is e d g a s t h a t s u r r o u n d s m o r e developed, but s till young, highmass s tar s (refer red to as ultr acompac t HII regions) . We are able to dis tinguish this t ype of emission from jets using a combination of s p e c t r a l a n d d e t a il e d m o r p h o l o g i c a l infor mation. The wide spec tr al cover age (1 to 10 0 GHz) and the high-angular resolution of the Aus tr alia Telescope Compac t Ar r ay (ATC A) make it well-suited to get ting this infor mation. In fac t the ATC A has already discovered one of the bes t examples of an i o n i s e d p r o t os t e l l a r j e t ( I R A S 16547- 4247, Brook s et al. 20 03) . We are near ing to completion a sys tematic search using the ATC A to look for more detec tions of ionised jets toward HMYSOs. Here we repor t on the discover y of an

ionised protos tellar jet towards the source G345.4938+ 01.467 7 (hereaf ter G345. 5+ 01. 5) . G345. 5+ 01. 5 is associated with the Infr ared As tronomical Satellite ( IR AS) source 16562-3959, and is believed to be a high-mass s tar in for mation at a dis tance of 1.6 k pc. The pr incipal source is detec ted by sever al infr ared sur veys (e.g. Midcour se Space E xper iment ( MSX ) , Spit zer- GLIMPSE [Galac tic Legacy Infr ared Mid- Plane Sur vey E x t r a o r d i n a i r e ] ) f r o m w h i c h we deduce it has ~ 60,0 0 0 times the solar luminosit y, and the centr al objec t cor responds to a s tar of 15 times the mass of the Sun. The objec t is also associated with a massive (~ 10 0 0 solar masses) and dense (10 4 -105cm-3) core of cold gas and dus t . Figure 1 shows an image of the ATC A 8.6 - GHz continuum emission. The image shows f ive sources r o u g h l y a l ig n e d a n d s y m m e t r i c a l l y of fset with respec t to the centr al source, which we identif y as the ionised jet . We inter pret the outer four sources as lobes where the high-velocit y gas ejec ted from the j e t h a s i m p a c t e d t h e s u r r o u n d i ng s , gener ating shock-ionised gas (GuzmÀn et al. 2010 ) . They are the r adio equivalent of optical Her big- Haro objec ts. All of the f ive emission sources were obser ved at four dif ferent frequencies.

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Figure 1: ATC A 8.6 - GHz continuum emission image of the newly discovered ther mal ionised jet sys tem in the high-mass s t arfor ming site G345. 5+ 01. 5. Dat a were t aken on June 20 0 8, Oc tober 20 0 8 and Febr uar y 20 09. The synthesised beamsize is 1.62'' x 1.01'' and indicated in the bot tom lef t cor ner.

This allows us to obtain spec tr a towards each of the lobes and the jet, the lat ter being a power law with a spec tr al index equal to + 0.85 and consis tent with freef r e e e m is s i o n f r o m a t h e r m a l j e t . Using the Atacama Pathf inder E Xper iment (APE X ) telescope in Chile we have also discovered a CO molecular out f low that e x te n d s i n t h e je t d i r e c t io n a n d ha s its blue-shif ted par t towards the

eas t , coincident with the eas ter n r adio lobe (GuzmÀn et al. 2011) Of the small lis t of HMYSOs k nown t o h a r b o r a t h e r m a l i o n is e d j e t , G345. 5+ 01. 5 has taken the lead as the mos t luminous. In second place is IR AS 16547- 4247. Both of these jets were discovered with ATC A and we look for ward to their followup s tudies at higher frequencies using the Atacama L ar ge Millimeter/ submillimeter Ar r ay (ALMA) .

References
Brook s, K . J ., Gar ay, G ., Mardones, D. & Bronfman, L ., ApJ 20 03, 594, L131 GuzmÀn A ., Gar ay, G . & Brook s, K . J ., ApJ 2010, 725, 734 GuzmÀn A ., Gar ay, G ., Brook s, K . J . , R a t h b o r n e , J . M . & G Ý s te n , R ., ApJ 2011, submit ted

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SZ and X-ray Peak s Don't Correspond
H e le n S im , C A SS

Two independent s tudies have been made with the Compac t Ar r ay of the Sunyaev-Zel'dovich (SZ ) ef fec t in gala x y clus ter s. They show that the relationship bet ween the SZ ef fec t and X-r ay br ightness is complex, sug ges ting that we have much more to lear n about the processes involved in clus ter merger s.
When Cosmic Microwave B a c k g r o u n d ( C M B ) p h o t o ns encounter a cloud of elec trons, they under go inver se Compton scat ter ing. For frequencies above 218 GHz, the CMB br ightness increases, while for frequencies below that value, it decreases. This spec tr al dis tor tion is k nown as the Sunyaev-Zel'dovich ef fec t . The amplitude of the dis tor tion depends only on the proper ties of the elec tron cloud : in the case of t h e r m a l e l e c t r o ns , i t is p r o p o r t i o n a l t o b o t h t h e e l e c t r o n d e ns i t y a n d t h e e l e c t r o n t e m p e r a t u r e . T h e h ot , dense, ionised gas found in gala x y clus ter s is a source of such elec trons. Hot clus ter gas is commonly s tudied through its ther mal X-r ay emission : this, however, is more dependent on elec tron densit y, but l e s s d e p e n d e n t o n te m p e r a t u r e , than the SZ ef fec t . As a result , the SZ ef fec t will tend to tr ace the hot, low-densit y gas in a clus ter (which may be a bet ter indicator of the clus ter's lar ge-scale s tr uc ture) , while the X-r ay luminosit y will be a bet ter tr acer of clumpiness (and thus per haps highlight shor tter m ac tivit y in the clus ter) . Two teams have used the capabilities of fered by the Compac t Ar r ay Broadbank Backend (C ABB ) to make the fir s t subarcminuteresolution obser vations of the SZ ef fec t in gala x y clus ter s under going mer ger s. They have then compared these to X-r ay emission maps. In one s tudy, Marcella Massardi, Ron Eker s, Simon Ellis and Ben Maughan tar geted the clus ter CL J 0152-1357. This is one of the mos t massive clus ter s k nown (with a total mass of 1015 solar masses) , and lies at a redshif t of 0.83. Previous s tudies have shown that clus ter s w i t h z 5 a r e m o r e s t r u c t u r a ll y complex, and less vir ialized, than clus ter s at low redshif ts ; and that clus ter s of z > 0.8 tend to be clumpy, sug ges ting they are closer to the epoch of clus ter for mation. The team had obser ved this clus ter in 20 05, before the advent of C ABB , with the Aus tr alia Telescope Compac t Ar r ay (ATC A) in its mos t compac t configur ation ( H75, with baselines from 30 m to 75 m) . They detec ted a (negative) peak in the SZ ef fec t in the clus ter's nor theas t subclump, displaced about 35 arcsec to the nor thwes t of the X-r ay peak . The of fset was u n e x p e c te d a n d , a s t h e d e te c t io n was at a level of jus t 3. 5 s, it was not convincing. In 20 09, af ter the upgr ade to C ABB , they repeated the obser vation of the X-r ay peak in the nor theas t subclump. Again, they saw the peak in the SZ ef fec t of fset from the X-r ay peak-- by about 45 arcsec to the nor th ; a n d t h is t i m e , t h e d e t e c t i o n w a s at a ver y convincing 10 s level. An Ac tive Galac tic Nuclei (AGN ) could have locally heated the gas in the region of the SZ ef fec t minimum. But there is no sign of an X-r ay or r adio AGN in the region, and the clus ter gala xies present in t h is r e g i o n a r e s u b l u m i n o u s , s o s u c h heating seems unlikely. The team has a ls o r u l e d o u t a s t r o m e t r i c e r r o r s as an explanation for the of fset . In the second s tudy, Siddhar th Malu, R avi Subr ahmanyan, Mar k Weir inga and Delampady N a r a s i m h a e x a m i n e d t h e we l l k nown Bullet Clus ter, a clus ter collision (or mer ger) with a redshif t 0.296 . The s tronges t SZ feature was again significantly of fset from the X-r ay emission peak ; indeed other SZ features in this clus ter were all of fset from the lesser peak s in X-r ay emission. This implies that , in this clus ter, the peak in intr aclus ter gas temper ature is of fset from the peak in gas densit y. Through the higher-resolution S Z o b s e r v a t i o n s m a d e p os s i b l e by C ABB , these t wo s tudies have shown, for the fir s t time, that the SZ ef fec t does not cor respond well to X-r ay br ightness in non-vir ialised clus ter s. The finding implies that the physics of clus ter mer ger s is more complicated than our cur rent models provide for, and throws into ques tion the combined use of X-r ay and SZ obser vations to der ive cosmological par ameter s.

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Figure 1: A false-colour X-r ay image from the Chandr a X- R ay obser vator y of the Bullet Clus ter, with super imposed contour s of the pressure /temper ature dis tr ibution in the gas, deter mined from SZ obser vations with the Aus tr alia Telescope Compac t Ar r ay. The hot tes t gas, seen by the SZ obser vations (contour s) , is displaced from the denses t gas regions, which are tr aced by the X-r ay emission (grey-scale tones) . Only t wo other clus ter s are k nown to show such a displacement , which may indicate an ener getic clus ter mer ger. Inter ferometer s are bes t suited for such SZ obser vations and the Compac t Ar r ay is the only one capable of these measurements for souther n clus ter s such as the Bullet Clus ter. Credits : ATC A data : S . Malu et al. Chandr a data cour tesy of the Chandr a X-r ay Obser vator y Center, oper ated by the Smithsonian As trophysical Obser vator y on behalf of NASA . NB : For reference, please see the colour image published on the inside back page of this newslet ter.

Publications
M . Massardi, R .D. Eker s, S .C . Ellis, and B . Maughan. High Angular Resolution Obser vation of the Sunyaev-Zel' dovich

Ef fect in the Massive z 0.83 Cluster CL J0152 ­ 1357. ApJ Let ter s, 718 : L1- L 5 (2010 ) S . S . Malu, R . Subr ahmanyan, M . H . Weir inga , and D. Nar asimha .

Compact Sunvaev-Zeldovich " Hole" in the Bullet Cluster. Submit ted to The Astrophysical Jour nal.

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Education and Outreach
R o b H o l l ow ( C A S S )

PULSE @ Parkes
A miles tone mar ked the s tar t of the four th year of CSIRO's PULSE @ Par kes projec t, with the fir s t ever s e s s i o n h e l d f r o m a s c h o o l t a k i ng place in Febr uar y 2011. Hos ted by Penr ith Anglican College, s tudents f r o m G l e n m o r e P a r k H ig h S c h o o l , Caroline Chisholm College and Penr ith Anglican College took direc t control of the Par kes r adio telescope from a control desk set up in the school's music per for mance space. C ASS s taf f member s, Dr Geor ge Hobbs and Rob Hollow were assis ted by PhD s tudent Stefan Ozlowsk i from Swinbur ne Univer sit y. The session was a great success and provided a wonder ful oppor tunit y for s tudents and t e a ch e r s f r o m t h e t h r e e l o c a l s c h o o ls t o m e e t a n d i n t e r a c t . In March, the fir s t PULSE @ Par kes Teacher Scholar, Stephen Broder ick from St Ur sula's College in Toowoomba , spent a successful we e k a t C A S S h e a d q u a r t e r s at Mar sfield. He wor ked with the projec t team in developing new outreach related resources. Stephen's ar ticle about his time w i t h C A S S c a n a ls o b e s e e n i n this issue of the ATNF News. I n a f u r t h e r u p d a te , A l e x M a t h ew s from Univer sit y of Wes ter n A u s t r a l i a s p e n t t e n we e k s a s a C ASS Summer Vacation Scholar

wor k ing on PULSE @ Par kes modules and science. He has developed a new module that allows s tudents to deter mine the per iod of a pulsar. It is cur rently being tes ted by an ex ter nal group of teacher s and should go live soon.

s tudents with developments in r adio as tronomy including the Aus tr alian Square K ilometre Ar r ay Pathfinder (ASK AP) and the Square Kilometre Ar r ay (SK A) .

CASS Summer Vacation Program
Ten scholar s from across Aus tr alia s p e n t t h e ir su m m e r ba s e d e i t h e r at Mar sfield or Par kes, wor k ing on a diver se r ange of projec ts under the super vision of C ASS s taf f. The s tudents also had the oppor tunit y to use the Aus tr alia Telescope Compac t Ar r ay in Januar y for shor t obser ving proposals of their own choosing dur ing an obser ving tr ip to Nar r abr i. Ever y s tudent gave a presentation of their wor k at a joint symposium w i t h su m m e r v a c a t io n s t u d e n t s f r o m t h e A u s t r a li a n A s t r o n o m i c a l O b s e r v a t o r y a n d t h e A u s t r a li a n G e m i n i S c h o l a r s b a s e d i n C h il e . The C ASS s tudents then finished their progr am by par ticipating in the Big Day In at Macquar ie Univer sit y with other summer s tudents from across the CSIRO Infor mation Sciences Group. C A S S D i r e c t o r D r P h il D i a m o n d gave the keynote address at this t wo-day event , inspir ing the

Other Education and Outreach Activity
The annual one-day Astrophysics for Physics Teacher s wor k shop was held at Mar sfield in late March 2011. Par ticipating teacher s from across NSW lear nt about new ways and a c t i v i t i e s t o e ng a g e a n d c h a ll e ng e s tudents. Speaker s included Dr J i m i G r e e n , D r G e o r ge H o b bs a n d Rob Hollow from C ASS , Dr Fred Watson from the A AO and Geof f Wyat t from Sydney Obser vator y. Rob also presented sessions to teacher s at the Sydney Obser vator y as well as at the Science Teacher s' Association of Vic tor ia Physics Teacher Conference in Febr uar y. The s tudents and s taf f from Pia Wadjar r i Remote Communit y S c h o o l t o u r e d t h e M u r c h is o n R a d i o O b s e r v a t o r y t o i ns p e c t the fir s t six dishes of ASK AP in December. This was the fir s t site visit by the s tudents. Wor k is continuing on an Indigenous Education resource for the Wadjar r i Yamatji communit y in conjunc tion with the building of ASK AP.

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CASS Teacher Scholar ship
Stephen B roder ick

Teacher Stephen Broder ick was the recipient of the fir s t C ASS Teacher Scholar ship. The scholar ship provided Stephen with the oppor tunity to wor k alongside the PULSE @ Par kes team in a research environment. He spent a week at the C ASS Mar sfield site, meeting with scientis ts and outreach s taf f, and lear ning about the progr am and the ATNF more gener ally. Stephen will also develop as tronomy related educational resources in the coming months and will have the oppor tunity to remain involved in future PULSE @ Par kes ac tivity. An account of his enjoyable week follows :

I have been teaching mathematics and science at St Ur sula's College in Toowoomba for 25 year s, so I saw the CSIRO Teacher Scholar ship as a unique oppor tunit y to combine my love of as tronomy and mathematics. Af ter ar r iving at the CSIRO main gate in Mar sfield, (reminiscent of a scene out of Mission Impossible) , I proceeded to tur n a combination lock (successfully I might add) in var ious d i r e c t i o ns u s i ng t h e s e c r e t n u m b e r until my key and ins tr uc tions on how to reach the lodge were revealed. The lodge was my on site accommodation for the week . Two over seas pos t gr aduate s tudents and a visiting professor from Melbour ne were also s taying at the lodge. The lodge would r ival any three or four s tar motel. Ever y thing you could possibly imagine was available in the lodge, including toothpick s, bicycles, and combination lock s, punc ture k its, etc. The Mar sfield site is ver y pic turesque and is nes tled amongs t lots of gum trees which consequently at tr ac t many var ieties of par rots, native birds and exotic insec ts. The spec tacular sunsets from my window in the lodge were fr amed by the t wo iconic 12-metre r adio telescopes. On Monday Rob Hollow gave me a tour of the CSIRO facilities which included the As tronomy and Space Science division, libr ar y, canteen and var ious wor k shops which included

Rober t Hollow, Jonathan K hoo, Stephen Broder ick and Dr Geor ge Hobbs. Credit : Helen Sim, CSIRO

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full scale models of var ious sec tions of the 12 metre r adio telescopes cur rently being cons tr uc ted in Wes ter n Aus tr alia as par t of the Aus tr alian Square K ilometre Ar r ay Pathf inder (ASK AP) telescope. The hallways are decor ated with eye catching educational pos ter s which show a progression in technolog y and precision depending on which direc tion you tr avel in. L ater in the day we met with G e o r ge H o b bs a n d J o na t h o n K hoo to discuss my role which was mainly wor k ing on the web based PULSE @ Par kes s tudent modules. My k nowledge of pulsar s was greatly enr iched hour by hour and one of my favour ite as tronomical objec ts is now the pulsar PSR J 0 437- 4715 (my s tudents also k now about PSR J 0 437- 4715 and a r e f a m ili a r w i t h i t s s o u n d f il e ) . On Wednesday I was pr ivileged to be involved in a meeting chaired by Rober t Br aun who was the head of the As trophysics sec tion. The meeting showcased var ious developments on site, including the progress of sever al projec ts and the research findings by p os t g r a d u a t e s w a s a l s o s h a r e d . Discussions were encour aging and

illuminating, providing alter native s o l u t i o ns a n d m o r e q u e s t i o ns t h a n answer s. The robus tness of some well k nown s tandard theor ies was a ls o q u e s t i o n e d . I t w a s b r e a t h t a k i ng witnessing the level of think ing a n d r e a s o n i ng w i t h i n t h e r o o m . It was science in the mak ing. On Wednesday af ter noon, elec tr ical engineer Mar k Bowen gave me a guided tour of the engineer ing s e c t i o n . H e e x p la i n e d w ha t happened to the r adio signal af ter it ar r ived at the focus cabin and entered the multibeam receiver. For example the multibeam receiver at Par kes (which was built in the CSIRO wor k shop) can look at 13 points in the sk y simultaneously. Each receiver uses vacuum and l i q u i d h e l i u m t o a m p l i f y t h e s ig n a l . Eventually the integr it y of the vacuum break s down and the receiver s need to be resealed. On Thur sday I at tended a lec ture a t t h e A u s t r a li a n A s t r o n o m i c a l O b s e r v a t o r y o n t h e d is t r i b u t i o n of dar k mat ter. The lec ture was ver y interes ting and gener ated lots of discussion. Once again t h e r e we r e m o r e q u e s t i o n s t h a n answer s and plent y of food for thought . (Speak ing of food, the

CSIRO canteen provided a huge r ange of culinar y delights and lunch time was always enjoyable lis tening to var ious scientis ts and computer progr ammer s s p e a k i ng a b o u t t h e i r t r i u m p hs . ) Fr iday was my las t day and I felt contented that I had lear nt a lot in such a shor t time ; however, my jour ney with pulsar s has only jus t begun. I am ver y gr ateful to all of the s taf f at the CSIRO Mar sf ield site especially Rob Hollow, Geor ge Hobbs and Jonathon K hoo for allowing me to wor k with them. All of the s taf f at CSIRO appeared focused on a common goal -- the advancement of scientif ic k nowledge. I feel conf ident that I can give my s tudents accur ate career advice about what a scientis t at CSIRO does and I have also regis tered St Ur sula's College in the Scientis t in Schools projec t as I see the connec tion bet ween schools and scientis ts as an enter pr ising and positive s tep in Aus tr alian Education. My week at CSIRO has cer tainly been the highlight of my t e a c h i ng c a r e e r t o d a t e a n d I l o o k for ward to reading about future achievements in CSIRO newslet ter s.

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Operations
D o ug la s B o ck ( C A S S )

Sever al upgr ades are coming to their conclusion this year. Upgr aded "16 cm" receiver s replacing the 20 cm and 13 cm receiver s are now available on all Aus tr alia Telescope Compac t Ar r ay (ATC A) antennas (see r e p o r t e ls e w h e r e i n t h is is s u e ) . The new receiver s have increased s e ns i t i v i t y a n d b a n d w i d t h t o complement C ABB , the Compac t Ar r ay Broadband Backend. Meanwhile, the 64 - MHz mode for C ABB is now being released. This will subs tantially improve the capabilit y for ex tr agalac tic millimetre-wave obser vations this winter. Together the upgr ades are a major enhancement to the ATC A . Ins tallation of the Univer sit y of New South Wales water vapour r adiometer s has also recently be completed. These will be char ac tised dur ing the coming winter. Dur ing March, Par kes was shut down for four week s to enable the M C P ( M a n u a l C o n t r o l P a n e l ) to be replaced. While the front panel s t ill l o o k s l a r g e l y t h e s a m e , t h e inter nal wor k ings of the MCP have been completely over hauled. This, t o g e t h e r w i t h t h e "s w i t c h m a t r i x " ins talled las t year (that automates

signal chain reconf igur ation) will e n a b l e r e m o t e o b s e r v i ng w i t h t h e Par kes Telescope. Also suppor ting r e m o t e o b s e r v i n g a r e s ig n i f i c a n t upgr ades to the Par kes power s u p p l y a n d d is t r i b u t i o n s y s t e m s , which are under way and will continue for the nex t few year s. In Febr uar y, CSIRO and the Auck land Univer sit y of Technolog y (AUT ) for mally agreed to collabor ate on Ver y Long Baseline Inter ferometr y ( VLBI ) obser vations. As a result , the AUT 12-m War k wor th r adio telescope is now commonly available for VLBI sessions at 20, 13, and 3 cm. A single A S K A P a n t e n n a is a ls o s o m e t i m e s available at 20cm. These antennas are reques ted explicitly in proposals. T h e A u s t r a li a n N a t i o n a l Da t a Ser vice (ANDS)/ATNF Data Management Projec t has recently been successfully completed. This projec t produced a public archive of sever al impor tant Par kes p u ls a r d a t a s e t s a n d e s t a b lis h e d the fr amewor k for including all Par kes data in the future. This will complement the ATC A and Mopr a data already available in the Aus tr alia Telescope On-line Archive. The data may be accessed at ht tp ://datanet.

csiro.au /dap /. For more details, see the repor t in the Apr il 2010 News.

April 2011 Time Assignment
T h e T i m e A s s ig n m e n t C o m m i t t e e ( TAC) met at Mar sf ield on 2 ­ 4 Febr uar y to consider proposals for the 2011 Apr il semes ter (2011APRS) . A total of 212 proposals were reviewed ; 132 for the Compac t Ar r ay, 38 for Mopr a , 29 for Par kes, 12 for the Long Baseline Ar r ay ( LBA) and one for Tidbinbilla . With ongoing enhancements to OPAL (ATNF Online Proposal Applications & Link s) , the Time Assignment Commit tee now has bet ter access to proposals and TAC comments from previous semes ter s, and is paying closer at tention to ensure resubmit ted proposals have addressed the comments made on previous submissions. A resubmission that does not consider any of the feedback provided by the TAC is unlikely to be reviewed favour ably ! In the pas t , proposal teams have been notified individually on the outcome of their proposal review by the TAC , and again once the schedules have been released. From

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Apr il 2011, a single message is b e i n g s e n t t o a l l p r o p os e r s . T h e f ir s t, soon af ter the TAC has met , advises all proposer s that the TAC gr ades and comments are available in OPAL . The second notif ies all proposer s that the schedules have been released and provides link s to the detailed infor mation available from the schedule webpages. Abs tr ac ts of all accepted proposals are now available in ADS .

bet ween the t wo 64 - MHz channels p os s i b l e . I t i s e x p e c t e d t h a t t h e 6 4 M H z m o d e w ill b e e x p a n d e d w i t h the full thir t y-t wo 64 - MHz channels available per IF ear ly in the semes ter. Wor k has commenced on the 6 / 3 c m ( " C / X " ) u p g r a d e , w h i c h w ill provide cover age over the r ange 4.0 ­12.0 GHz and thus f ill the gap b e t we e n t h e e x i s t i n g 6 c m a n d 3 c m bands. The f ir s t protot ype receiver may be ready for ins tallation toward the end of the 2011APR S . Two week s dur ing the semes ter have been allocated for C2479 ATC A Character isation of the f ir st BETA f ields, in order to char ac ter ise the t wo 30 square degree f ields that will become the f ir s t science f ields obser ved on BE TA (the f ir s t six antennas of ASK AP) . The f ields are centred on the Circinus gala x y and the For na x clus ter (and including For na x A) . The " Science Oper ations Centre" p il o t o b s e r v i ng m o d e t r i a ll e d l a s t year for Mopr a (see Oc tober 2010 ATNF News) will be ex tended to selec ted ATC A projec ts this year.

June, pr imar ily for refur bishment of the focus cabin tr anslator r ails. It is expec ted that all receiver s will be removed from the focus cabin for this wor k to be under taken.

Notes on Mopra
Owing to the relocation of Balt Inder muele to Sydney, mos t Mopr a suppor t will now be delivered from Mar sf ield. In the 2011APR S , "on-site" obser ving w ill b e s u p p o r t e d f r o m M a r s f i e l d (where a dedicated obser ving room will be set up) or at Nar r abr i. Recent changes to the Mopr a Spec trometer ( MOPS) have enabled " f a s t m a p p i ng " o b s e r v a t i o ns t o be made, with a cor relator cycle time of 256 milliseconds r ather than the s tandard 2 seconds, for a reduced number of MOPS zoom bands (no more than four is recommended) . In order to allow a seamless tr ansition bet ween fas tm a p p i ng o b s e r v a t i o ns a n d r e g u l a r o b s e r v a t i o ns , i t is i n t e n d e d f r o m ear ly 2011APR S to change the cycle time for all Mopr a obser vations from the cur rent 2.0 seconds to 2.0 48 seconds. We will ensure that all Mopr a user s are made aware w h e n t h is c h a ng e is m a d e , a n d t h a t old scr ipts (assuming a 2.0 sec cycle time) will be handled gr acefully.

Notes on the Compact Array
The 2011APRS will commence w i t h t h e "s t a n d a r d " C A B B 1 M H z continuum mode available, and with up to 16 zoom bands per IF (inter mediate frequency) available in the 1M - 0. 5k mode. The 64 - MHz C ABB mode will, for the f ir s t few week s, have a single 64 - MHz band in each IF, which will have 20 48 c h a n n e l s a c r os s i t . ( T h u s , i f t h e 64 - MHz mode is selec ted for an IF, the total bandwidth in that IF will be 64 MHz and not 2 GHz) . For continuum plus spec tr al line s tudies, having one IF set with the 6 4 - M H z m o d e a n d t h e ot h e r w i t h the s tandard 20 48 1- MHz-wide c h a n n e l i s p os s i b l e . F o r s p e c t r a l l i n e s tudies, 64 MHz is available in both I F s -- w i t h s e p a r a t i o ns u p t o 7 G H z

Notes on Parkes
The 2011APR S schedule for Par kes has a three-week shutdown per iod, from Monday 23 May to Fr iday 10

36 Issue No . 70, Apr il 2011


Publications List

Publication lis t s for paper s which include ATNF dat a or C ASS au thor s are available on the Web at w w w.at nf.csiro. au /research /publications. Plea se email any updates or cor rec tions to this lis t to Julie.Tesor iero @ csiro.au This lis t includes published refereed paper s compiled since the Oc tober 2010 issue of ATNF News. Paper s which i n c l u d e C A S S a u t h o r s a r e i n d i c a t e d by a n a s te r is k . *Abdo, A . A . ; Ajello, M . ; Antolini, E . ; B a l d i n i , L . ; B a ll e t , J . ; B a r b i e lli n i , G . ; Bar ing, M . G . ; Ba s tier i, D. ; B echtol, K . ; B ella z zini, R . ; and 14 4 coau thor s . " Fer mi lar ge area telescope obser vations of gamma-r ay pulsar s PSR J1057-5226 , J1709- 4 429, and J1952+3252". ApJ , 720, 26 - 4 0 (2010 ) . *Acker mann, M . ; Ajello, M . ; Baldini, L . ; B a ll e t , J . ; B a r b i e lli n i , G . ; B a s t i e r i , D. ; B echtol, K . ; B ella z zini, R . ; B erenji, B . ; Bloom, E . D. ; and 161 coau thor s . " Fer mi-lat search for pulsar wind nebulae around gamma-r ay pulsar s". ApJ , 726 , 35 -35 (2011) . Aver sa , Alan G . ; Johnson, Kelsey E . ; B rogan, Cr ys t al L . ; Goss , W. M . ; Pisano, D. J . " Ver y L ar ge Ar r ay and ATC A Search for Nat al St ar Clus ter s in Near by St ar-for ming Gala xies". AJ , 141, 125 (2011) . Bailes , M . "Cur ious proper ties of the rec ycled pulsar s and the potential of high precision timing". NewAR , 54, 86 86 (2010 ) . *Bates , S . ; Johns ton, S . ; Lor imer, D. R . ; K r amer, M . ; Possenti, A . ; B ur gay, J . ; St apper s , B . ; Keith, M . J . ; Lyne, A . ; Bailes , M . ; McL aughlin, M . A . ; O' B r ien, J .T. ; Hobbs , G . "A 6 . 5 - GHz Multibeam Pulsar Sur vey". MNR AS , 411, 1575 -1584 (2011) . *B ell, M . E . ; Tzioumis , T. ; U t tley, P. ; Fender, R . P. ; ArÈvalo, P. ; B reed t , E . ; McHardy, I . ; Calvelo, D. E . ; Jamil, O. ;

KÆrding, E . "X-r ay and r adio var iabilit y i n t h e l ow - l u m i n o s i t y a c t i v e g a l a c t i c nucleus NGC 7213". MNR AS , 411, 4 02 (2011) . *B enaglia , P. ; R ibÑ, M . ; Combi, J . A . ; Romero, G . E . ; Chat y, S . ; Kor ibalsk i, B . ; Mir abel, I . F. ; Rodr Ìguez, L . F. ; Bosch, G . " R adio and IR s tudy of the massive s t ar-for ming region IR AS 16353 - 4636". A & A , 523, A62 (2010 ) . *B ietenholz, M . F. ; Soder ber g, A . M . ; Bar tel, N . ; Ellingsen, S . P. ; Hor iuchi, S . ; Phillips , C . J . ; Tzioumis , A . K . ; Wier inga , M . H . ; C h ug a i , N . N . " V L B I O b s e r v a t io ns of the Type I b /c SN 20 09bb ". ApJ , 725 4 (2010 ) . * B l a ke , C . ; B r o u g h , S . ; C o l l e s s , M . ; Couch, W. ; Croom, S . ; Davis , T. ; Dr ink water, M . J . ; For s ter, K . ; Gla zebrook , K . ; Jellif fe, B . ; and 11 coau thor s . " The Wig gleZ Dar k Ener g y S u r v ey : t h e s e l e c t i o n f u n c t i o n a n d z = 0.6 gala x y power spec tr um". MNR AS , 4 06 8 03 (2010 ) . B oz zet to, L . M . ; Filipovic, M . D. ; Cr aw ford, E . J . ; Bojicic, I . S . ; Payne, J . L . ; Medik , A . ; Wardlaw, B . ; de Hor t a , A .Y. " Multifrequenc y r adio obser vations of a SNR in the LMC . The case of SNR J 0527- 6549 ( DEM 120 4) ." SerAJ , 181, 43 - 49 (2010 ) . *B r aine, J . ; Gr atier, P. ; K r amer, C . ; Xilour is , E . M . ; Rosolowsk y, E . ; B uchbender, C . ; Boquien, M . ; Calzet ti, D. ; Quint ana- L acaci, G . ; Tabat abaei, F. ; and 16 coau thor s . "Cool gas and dus t in M 33 : Result s from the HER schel M 33 E x tended Sur vey ( HER M33ES)". A & A , 518, L69 (2010 ) . * B r a u n , R . ; H e a ld , G . ; B e ck , R . " T h e Wes ter bor k SINGS sur vey. III . Global magnetic field topolog y". A & A , 514, A42 (2010 ) . * B r ow n , S . ; D u e s t e r h o e f t , J . ; R u d n i c k , L . " M u l t iple s ho ck s t r u c t u r e s in a r ad io

selec ted clus ter of gala xies". ApJ , 727, L 25 (2011) . * B r ow n , S . ; D u e s t e r h o e f t , J . ; R u d n i c k , L . " M u l t i p l e S h o c k St r u c t u r e s i n a R a d i o selec ted Clus ter of Gala xies". ApJ , 727, L 25 - L 25 (2011) . *B rown, S . ; Far nswor th, D. ; Rudnick , L . "Cross- cor relation of dif fuse synchrotron and lar ge -scale s tr uc tures". MNR AS , 4 02, 2- 6 (2010 ) . *B uitink , S . ; Scholten, O. ; Bacelar, J . ; B r aun, R . ; de B r uyn, A .G . ; Falcke, H . ; Singh, K . ; St apper s , B . ; Strom, R .G . ; Yahyaoui, R . "Cons tr aint s on the flux of ultr a-high ener g y neu tr inos from Wes ter bor k Synthesis R adio Telescope obser vations". A & A , 521, A47-A47 (2010 ) . *B ur ke -Spolaor, S . ; Bailes , M . ; Eker s , R . ; Macquar t , J .- P. ; Cr aw ford, F., III . " R adio b u r s t s w i t h e x t r a g a la c t i c s p e c t r a l char ac ter is tics show ter res tr ial or igins". ApJ , 727, 18 (2011) . *Calvelo, D. E . ; Fender, R . P. ; Russell, D. M . ; Gallo, E . ; Cor bel, S . ; Tzioumis , A . K . ; B ell, M . E . ; Lewis , F. ; Maccarone, T. J . " Limit s on the quiescent r adio e m is s io n f r o m t h e b la ck h o l e b i na r i e s GRO J1655 - 4 0 and X TE J1550 -56 4". MNR AS , 4 09, 839- 845 (2010 ) . *Caswell, J . L . ; B reen, S . L . "An unbiased pilot sur vey for Galac tic water maser s". MNR AS , 4 07, 2599-2610 (2010 ) . * C a s we l l , J . L . ; B r e e n , S . L . ; E l l i n g s e n , S . P. "A water maser sur vey towards the galac tic centre". MNR AS , 410, 1283 1294 (2011) . * C a s we l l , J . L . ; G r e e n , J . A . " B l u e s h i f t e d ou t flow from 24.329+ 0.145". MNR AS , 411, 2059-2066 (2011) . Cer nuda , I . "Cosmic-r ay elec tron a n is ot r o p i e s a s a to o l to d is cr i m i na te bet ween exotic and as trophysical sources". A s tropar ticle Physics , 34, 5969 (2010 ) .

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*Champion, D. J . ; Hobbs , G . B . ; Manches ter, R . N . ; Edwards , R .T. ; Backer, D.C . ; Bailes , M . ; B hat , N . D. R . ; B ur ke Spolaor, S . ; Coles , W. ; Demores t , P. B . ; and 12 coau thor s . " Mea sur ing the ma ss of solar sys tem planet s using pulsar timing". ApJ , 720, L 201- L 205 (2010 ) . *Chandola , Yogesh ; Saik ia , D. J . ; Gupt a , N . " H I g a s i n t h e r e j u ve n a t e d r a d i o gala x y 4C29.30 ". MNR AS , 4 03, 269273 (2010 ) . *Clay, R .W. ; Whelan, B . J . ; Edwards , P.G . "Cent aur us A at ultr a-high ener gies". PASA , 27, 439- 4 48 (2010 ) . *Cluver, M . E . ; Jar ret t , T. H . ; K r a anKor teweg, R .C . ; Kor ibalsk i, B . S . ; Appleton, P. N . ; Melbour ne, J . ; Emont s , B . ; Woud t , P. A . "Ac tive disk building i n a l o c a l H I - M a s s i ve L I RG : t h e s y n e r g y bet ween gas , dus t , and s t ar for mation". ApJ , 725, 1550 -1562 (2010 ) . Cr aw ford, E . J . ; Filipovic', M . D. ; Haber l, F. ; Piet sch, W. ; Payne, J . L . ; de Hor t a , A .Y. " Multi-frequenc y s tudy of Local G r o u p s u p e r n ov a r e m n a n t s . T h e cur ious case of the L ar ge Magellanic Cloud SNR J 0528 - 6714". A & A , 518 , (2010 ) . *Crof t , Steve ; Bower, Geof frey C . ; Acker mann, Rob ; Atk inson, Shannon ; Backer, Don ; Backus , Peter ; Barot t , William C . ; Bauer meis ter, Amber ; B lit z, Leo ; Bock , Dougla s ; and 41 coau thor s . Er r atum : " The Allen Telescope Ar r ay t went y- centimeter sur vey - a 690 deg (2) , 12 epoch r adio dat a set . I . cat alog and long- dur ation tr ansient s t atis tics". ApJ , 724, 827- 827 (2010 ) . Cui , L D i ng , Net w r ad io A 23 ( ., Liu, X ., Liu, J ., Song, H .G . & Z. " The follow-up European VLB I or k obser vations of t welve GPS sources at 5 GHz". A & A , 518 , 2010 ) .

Davies , L . J . M . ; B remer, M . N . ; St anway, E . R . ; B ir k inshaw, M . ; Lehner t , M . D. " Limit s on the molecular gas content of z ~ 5 LBGs". MNR AS , 4 0 8, L31- L35 (2010 ) . *Dawson, J . ; McClure - Gr if fi ths , N . ; K aw a m u r a A . ; M i z u n o , N . ; Onishi, T. ; Fukui, Y. " Super shells as molecular cloud fac tor ies : Par sec-scale obser vations of HI and 12CO ( J =10 ) in GSH 287+ 0 4 -17 and GSH 27 7+ 0 0 +36". ApJ , 728, 127 (2011) . Dedes , C . ; Leur ini, S . ; Wyrowsk i, F. ; Schilke, P. ; Menten, K . M . ; Thor wir th, S . ; O t t , J . "A s tudy of three sou ther n highma ss s t ar-for ming regions". A & A , 526 , A 59 (2011) . *Defr aigne, P. ; Manches ter, R . ; Mat sak is , D. ; Petit , G . ; Hosok awa , M . ; Leschiu t t a , S . ; Zhai, Z.- C . "Commission 31: Time". IAUTB 6 , 14 0 -141 (2010 ) . * D i c ke l , J . R . ; G r u e n d l , R . A . ; M cI n t y r e , V. J . ; Amy, S .W. "A 4.8 and 8.6 GHz sur vey of the small magellanic cloud : the images". AJ , 14 0, 1511-1518 (2010 ) . *Dickel, J . R . ; McInt yre, V. J . ; Gr uendl, R . A . ; Milne, D. K . ER R ATU M : "A 4.8 and 8.6 GHz sur vey of the lar ge Magellanic Cloud. I . The Images". (20 05, AJ , 129, 790 ) AJ , 14 0, 1567 (2010 ) . *Eatough, R . P. ; Molkenthin, N . ; K r amer, M . ; N o u t s o s , A . ; Ke i t h , M . J . ; S t a p p e r s , B .W. ; Lyne, A .G . " Selec tion of r adio pulsar candidates using ar tificial neur al net wor k s". MNR AS , 4 07, 24 43 -2450 (2010 ) . Elson, E .C . ; de Blok , W. J .G . ; K r a anKor teweg, R .C . "A search for noncircular flows in the ex tended HI disc of NGC 2915". MNR AS , 411, 20 0 -210 (2011) .

* Ferdman, R . D. ; St air s , I . H . ; K r amer, M . ; McL aughlin, M . A . ; Lor imer, D. R . ; Nice, D. J . ; Manches ter, R . N . ; Hobbs , G . ; Lyne, A .G . ; Camilo, F. ; and 7 coau thor s . Er r atum : "A precise mass measurement of the inter mediate -mass binar y pulsar PSR J18 02-2124". ApJ , 713, 710 (2010 ) . Filipovic, M . D. ; Cr aw ford, E . J . ; Jones , P. A . ; White, G . L . " R adio - continuum jet s a r o u n d t h e p e cu l i a r g a l a x y p a i r E S O 295 - IG 022". SerAJ , 181, 31-37 (2010 ) . *Ford, H . A . ; Lock man, F. J . ; McClure Gr if fi ths , N . M . " Milk y Way Disk- Halo Tr ansition in H I : Proper ties of the Cloud Population". ApJ , 722, 367-379 (2010 ) . *Ford, H . A . ; McClure - Gr if fi ths , N . M . ; Lock man, F. J . ; Bailin, J . ; Calabret t a , M . R . ; K alber la , P. M .W. ; Mur phy, T. ; Pisano, D. J . " E r r a t u m : " H I c l o u d s i n t h e l ow e r h a l o . I . The galac tic A sur vey pilot region". AJ , 710, 1868 (2010 ) . *Freudling, W. ; St aveley-Smith, L . ; C a t i n e lla , B . ; M i n ch i n , R . ; C a la b r e t t a , M . ; Momjian, E . ; Zwa an, M . ; Meyer, M . ; O' Neil, K . " Deep 21 cm H I Obser vations at z ~ 0.1: The Precur sor to the Arecibo Ultr a Deep Sur vey". ApJ , 727, 4 0 (2011) . Ghir landa , G . ; Ghisellini, G . ; Tavecchio, F. ; Foschini, L . "Cor relation of Fer mi L ar ge Area Telescope sources with the 20 - GHz Aus tr alia Telescope Compac t Ar r ay r adio sur vey". MNR AS , 4 07, 7918 03 (2010 ) . *Glioz zi, M . ; Panessa , F. ; L a Fr anca , F. ; Saviane, I . ; Monaco, L . ; Foschini, L . ; Kedzior a- Chudc zer, L . ; Sat yapal, S . ; Sambr una , R . M . "Q2122- 4 4 4 : A naked ac tive galac tic nucleus fully dressed". ApJ , 725, 2071-207 7 (2010 ) .

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Goulier mis , D. A . ; Schmeja , S . ; K lessen, R . S . ; de Blok , W. J .G . ; Walter, F. " H i e r a r c h i c a l St e l l a r St r u c t u r e s i n t h e Local Group Dwar f Gala x y NGC 6822". ApJ , 725, 1717-1734 (2010 ) . *Gr atier, P. ; B r aine, J . ; Rodr iguezFer nandez, N . J . ; Schus ter, K . F. ; K r amer, C . ; Xilour is , E . M . ; Tabat abaei, F. S . ; Henkel, C . ; Cor belli, E . ; Isr ael, F. ; and 15 coau thor s . " Molecular and atomic ga s in the Local Group gala x y M 33". A & A , 522, A3 (2010 ) . *Green, J . A . ; Caswell, J . L . ; Fuller, G . A . ; Avison, A . ; B reen, S . L . ; Ellingsen, S . P. ; Gr ay, M . D. ; Pes t aloz zi, M . ; Quinn, L . ; Thompson, M . A . ; Voronkov, M . A . " The 6 - G H z m e t ha nol m ul t ib e a m ma s e r cat alogue ­ II . Galac tic longitudes 6° to 20°". MNR AS , 4 09, 913 -935 (2010 ) . *Guzman, A . E . ; Gar ay, G . ; B rook s , K . J . "A s tr ing of r adio emission a ssociated with IR AS 16562-3959 : A collimated j e t e m a n a t i n g f r o m a l u m i n o u s m a s s i ve young s tellar objec t". ApJ , 725, 734 -741 (2010 ) . *Hamacher, " M e te o r s in Dreamings". Inter nationa D.W. & Nor r is , R . P. Au s t r a lia n A b o r ig i n a l WGN - Jour nal of the l Meteor 38 , 87-98 (2010 ) .

H2O maser s". MNR AS , 4 0 8, 1438 -1451 (2010 ) . * H o b bs , G . ; A r ch i ba ld , A . ; Ar zoumanian, Z. ; Backer, D. ; Bailes , M . ; B hat , N . D. R . ; B ur gay, M . ; B ur ke -Spolaor, S . ; Champion, D. ; Cognard, I . ; and 48 coau thor s . " The Inter national Pulsar Timing Ar r ay Projec t : using pulsar s as a g r av i t a t i o n a l w av e d e t e c t o r - a r t . n o . 0 84 013". Class . & Quant . Gr avit y, 27, 84 013 - 84 013 (2010 ) . *Holt , J . ; Tadhunter, C . N . ; Mor ganti, R . ; Emont s , B . H .C . " The impac t of the war m ou t flow in the young (GPS) r adio source and ULIRG PK S 1345+12 (4C 12. 50 )". MNR AS , 410, 1527-1536 (2011) . Ishiyama , T. ; Mak ino, J . ; Ebisuzak i, T. "Gamma-r ay signal from ear th-mass dar k mat ter microhalos". ApJ , 723, L195 - L 20 0 (2010 ) . *Jack son, S . A . ; Gough, R . ; Moghe, Y. " Receiver Integr ation for Mid-band Square K ilometer Ar r ay Demons tr ator Applications". In : IEEE Compound Semiconduc tor Integr ated Circuit Symposium, Monterey, C A USA , Oc tober 3 - 6 , 2010. *Jack son, S . A ; Moghe, Y. ; Gough, R .G . ; Jack son, C . A . " Highly integr ated Silicon on Sapphire receiver for nex tgener ation r adio telescopes". In : Wor k shop on the Application of R adio Science 2010, Canber r a , 11-12 Januar y, 2010. *James , C .W. ; Protheroe, R . J . ; Eker s , R . D. ; Alvarez- Mußiz, J . ; McFadden, R . A . ; Phillips , C . J . ; Rober t s , P. ; B r ay, J D. " LU NASK A exper iment obser vational l i m i t s o n U H E n e u t r i n os f r o m Cent aur us A and the Galac tic Centre". MNR AS , 410, 885 - 889 (2011) .

Johns ton, H . M . ; B roder ick , J .W. ; Cot ter, G . ; Mor ganti, R . ; Huns tead, R .W. " The ex tr aordinar y r adio gala x y MRC B1221423 : probing deeper at r adio and optical waveleng ths". MNR AS , 4 07, 721 (2010 ) . *Jones , D. I . ; Crocker, R . M . ; O t t , J . ; Protheroe, R . J . ; Eker s , R . D. "Aus tr alia Telescope Compac t Ar r ay r adio continuum 1384 and 2368 MHz obser vations of Sagit t ar ius B". AJ , 141, 82 (2011) . Jones , P. A . ; B ur ton, M .G . ; Tothill, N . F. H . ; C u n n i ng ha m , M . R . " S p e c t r a l i m a g i ng of the Sagit t ar ius B2 region in multiple 7-mm molecular lines". MNR AS , 411, 2293 -2310 (2011) . *K alber la , P. M .W. ; McClure - Gr if fi ths , N . M . ; Pisano, D. J . ; Calabret t a , M . R . ; Ford, H . A . ; Lock man, F. J . ; St aveleySmith, L . ; Ker p, J . ; Winkel, B . ; Mur phy, T. ; New ton- McGee, K . "GASS : the Par kes Galac tic all-sk y sur vey. II . Str ayr adiation cor rec tion and second dat a release". A & A , 521, A17 (2010 ) . * Ke i t h , M . J . ; J a m e s o n , A . ; v a n St r a t e n , W. ; Bailes , M . ; Johns ton, S . ; K r amer, M . ; Possenti, A . ; Bates , S . D. ; B hat , N . D. R . ; B ur gay, M . ; and 6 coau thor s . " The h i g h t i m e r e s o l u t i o n u n i ve r s e p u l s a r sur vey - I . sys tem configur ation and initial discover ies". MNR AS , 4 09, 619627 (2010 ) . *Kes teven, M . "Over view of R FI m i t ig a t i ng m e t h o d s i n e x is t i ng a n d n e w sys tems". PoS , Proceedings of the R FI (2011) . *K im, S . ; Kwon, E . ; Madden, S .C . ; Meixner, M . ; Hony, S . ; Panuz zo, P. ; S a u v a ge , M . ; Ro m a n - D u v a l , J . ; G o r d o n , K . D. ; Engelbr acht , C . ; and 20 coau thor s . " C o l d d u s t cl u m p s i n d y n a m i c a l l y h o t gas - ar t . no. L75, A & A , 518, L75 - L75 (2010 ) .

*Hancock , P. J . ; Sadler, E . M . ; Mahony, E . K . ; R icci, R . "Obser vations and proper ties of candidate high-frequenc y GPS r adio sources in the AT 20G sur vey". MNR AS , 4 0 8 , 1187-1206 (2010 ) . H a s s a n , A . H . ; F l u ke , C . J . ; B a r n e s , D.G . " Inter ac tive visualization of the lar ges t r adioas tronomy cubes". New A s tronomy, 16 , 10 0 -109 (2011) . * H i n d s o n , L . ; T h o m ps o n , M . A . ; U r q u h a r t , J . S . ; C l a r k , J . S . ; D av i e s , B . " The G305 s t ar-for ming complex : wide area molecular mapping of NH3 and

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*Koca , J . ; B r ig gs , F. H . ; Reynolds , J . " R adio frequenc y inter ference removal through the application of spatial filter ing techniques on the Par kes Multibeam Receiver ". AJ , 14 0, 20 86 2094 (2010 ) . L anger, W. D. ; Velusamy, T. ; Pineda , J . L . ; Goldsmith, P. F. ; Li, D. ; Yor ke, H .W. "C+ detec tion of war m dar k ga s in dif fuse clouds". A & A , 521, L17 (2010 ) . *L a zendic, J . S . ; Wardle, M . ; Whiteoak , J . B . ; B u r to n , M . G . ; G r e e n , A . J . " Multi-waveleng th obser vations of the super nova remnant G349.7+ 0. 2 inter ac ting with a molecular cloud". MNR AS , 4 09, 371-388 (2010 ) . * Lev i n , L . ; B a il e s , M . ; B a te s , S . ; B ha t , N . D. R . ; B ur gay, M . ; B ur ke -Spolaor, S . ; D'Amico, N ., Johns ton, S . ; Keith, M . ; K r amer, M . ; and 5 coau thor s . "A r adio loud magnet ar in X-r ay quiescence". ApJ , 721, L33 - L37 (2010 ) . *Liu, G .- C . ; Bir k inshaw, M . ; Prot y W., Jiun- Huei ; H ., Paul T. P. ; Locu tus H ., Chih-Wei ; L ., Yu-Wei ; L ., K ai-Yang ; M ., Sandor M . ; Nishiok a , H . ; Koch, P. M . ; and 19 coau thor s . "Cont amination of the centr al sunyaev-zel' dovich decrement s in AMiBA gala x y clus ter obser vations". ApJ , 720, 60 8 - 613 (2010 ) . Longmore, S . N . ; Pillai, T. ; Keto, E . ; Zhang, Q. ; Qiu, K . " Is protos tellar heating suf ficient to halt fr agment ation ? A case s tudy of the ma ssive protoclus ter G8.68 - 0.37 ". ApJ , 726 , 97-97 (2011) . *Lopez-Sanchez, A . R . " Ma ssive s t ar for mation in Wolf- R ayet gala xies . V. St ar-for mation r ates , ma sses and the impor t ance of gala x y inter ac tions". A & A , 521, A63 (2010 ) . *Lopez-Sanchez, A . R . ; Mesa- Delgado, A . ; Lopez- Mar tin, L . ; Es teban, C . " The ionized gas at the centre of IC 10 : a possible localized chemical pollu tion by Wolf- R ayet s t ar s". MNR AS , 411, 2076 2092 (2011) .

Lyne, r ad io A s tro (2010

A .G . "A new population of tr ansient neu tron s t ar s". New nomy Reviews , 54 118 -1221 ).

*Macquar t , J .- P., Bailes , M . ; B hat , N . D. R . ; Bower, G .C . ; B unton, J . D. ; Chat ter jee, S . ; Colegate, T. ; Cordes , J . M . ; D'Addar io, L . ; Deller, A . ; and 29 coau thor s . " The commensal real-time ASK AP fas t-tr ansient s (CR AF T ) sur vey. PASA , 27, 272-282 (2010 ) . Maddison, S .T. ; Wr ight , C . M . ; Lommen, D. ; B ur ton, M . ; Wilner, D. ; Bour ke, T. " Resolving s tr uc ture in the HD10 0546 disk - signatures of planet building" ? Highlight s of A s tronomy, 15, 741-741 (2010 ) . *Manches ter, R . N . " The Par kes pulsar timing ar r ay projec t". Highlight s of A s tronomy, 15, 233 -233 (2010 ) . *Manches ter, inter ac tions a in t he dou ble A s tronomy R R . N . " Magnetospher ic nd emission proper ties pulsar sys tem". New eviews , 54, 152-157 (2010 ) .

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Figure 1: A false - colour X-r ay image from the Chandr a X- R ay obser vator y of the B ullet Clus ter, with super imposed contour s of the pressure /temper ature dis tr ibu tion in the ga s , deter mined from SZ obser vations with the Aus tr alia Telescope Compac t Ar r ay. See page 31 for fur ther det ails .

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F o r f u r t h e r i n fo r m at i o n : C S I R O A s t r o n o my & S p a c e S c i e n c e Email enquir ies : atnf- enquir ies @ csiro. au Email newslet ter : newslet ter @ atnf.csiro. au Web centr al : w w w. atnf.csiro. au Web newslet ter : w w w. atnf.csiro. au / news / newslet ter, Web ou tr each : ou tr each. atnf.csiro. au

Ross For sy th s t ands in the receiver cage of one of the Aus tr alian Square K ilometre Ar r ay Pathfinder antenna s at the Murchison R adio -a s tronomy Obser vator y. C r e d i t : C S I RO