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EMU NEWSLETTER ISSUE 10 MAY 2016

Credit:Top,AlexCherney,http://www.terrastro.com/.Bottom,CSIRO

What is EMU?

EMU is a radio sky survey project which will use the new ASKAP telescope to make a deep (10µJy rms) radio continuum survey covering the entire Southern Sky as far North as 30°. It can be characterised as a “Southern NVSS”, except that it will have about 40 times the sensitivity, six times the resolution and will detect 70 million galaxies. As a result, it will be able to probe star forming galaxies up to z=1, AGNs to the edge of the Universe, and will undoubtedly uncover new classes of object.

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From the EditorDearEMUteammembers,

Welcometothe10thissueoftheEMUNewsletter!AconsiderableamounthashappenedsincethelastnewsletterinOctober2015.

IthasbeenabusyandexcitingfewmonthsformembersoftheEMUteamandfortheASKAPproject,withtwelveMk-IIPAFsnowinstalledonASKAPantennas,andBETAofUiciallydecommissioned.WorkcontinuesontheUinalcommissioningandpreparationoftheseantennasandPAFsaheadofEarlyScience.TheUirst36-beamradioimageeverwasalsoproducedbytheMk-IIPAFsinApril(seearticleonpage7).AnotherexcitingmilestonewillbetheUirstASKAPsciencefocussedconference,ASKAP2016,6-10June,heldinSydneyattheUniversityofSydney(seehereformoredetails).IlookforwardtoseeingmanyoftheEMUteaminattendance.

Iwouldencourageyoutosendinsubmissionsforfutureissues.SmallsnippetsorimagesaremostwelcomeasareproUilesofteammembers.Thisnewsletterisonlyasusefulasthecontributionsreceivedfromteammembers.ItservesasbotharecordofthedevelopmentoftheprojectandameanstopromoteideasandissuesthatcanthenbefollowedupthroughdiscussionontheprojectWikihttp://www.askap.pbworks.com.

Ifyouhaveanysuggestionsastowhatyouwouldliketoseeincludedinthenewsletterpleaseletmeknow.

Submissionsforthenextissuearedue:14October2016.Emailreminderswillbesentclosertothedate.

Happyreading!

KateChow Editor

CONTENTS

1FROMTHEEDITOR2PROJECTUPDATES FromtheProjectLeader(includinganASKAPUpdate) TheEMUProjectStructure ASKAP/EMUEarlyScienceUpdate

3EMURELATEDARTICLESASKAPsoftandEMU ASKAP’sUirst36-beamimage!

3EMUKEYSCIENCEPROJECTUPDATES3.1EMUValue-AddedCatalogue3,2CharacterisingtheRadioSky3.3EMUCosmology3.4CosmicWeb 3.5ClustersofGalaxies3.6EMUcosmicstarformationhistoryandstellarmassgrowthforgalaxies3.7Evolutionofradio-loudAGN3.8RadioAGNintheEoR3.9Radio-quietAGN3.10LocalUniverse3.11TheGalacticPlane3.12SCORPIO:CataloguingtheradiostarsinourGalaxy3.13WTF:DiscoveringtheUnexpected

4POSITIONSVACANT

5MEETINGSANDCONFERENCES

6NEWSLETTERSANDPAPERS

EMU NEWSLETTER ISSUE 10 MAY 2016

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Welcome to the10thEMUnewsletter. It seemsavery long time since the project started in 2009,whenASKAPwasstillaconcept–andahigh-riskoneat that!A lothashappened in themeantime,andASKAPisnowarealtelescopeproducingrealimages of the sky, with the Phased Array Feeds(PAFs) per forming up to expectat ions .Unfortunately, there seems to bemore scatteringfrom the dish than hoped, which increases theeffective on-sky system temperature (Tsys/η) byabout 20% compared to the original design, andthis will probably result in a somewhat longerintegration time for EMU to reach its targetsensitivityof10μJy/beamrmsover3πsteradians.

TwelveantennasarenowequippedwithPAFs,andwearenoweagerlyawaitingtheUinalconstructionand commissioning ofASKAP-12, afterwhich theASKAP-12“EarlyScience”phasewillstart.EveninEarly Science we will be making unprecedentedobservationsoftheradiosky,exploringnewpartsof the observational parameter space. Theremaining 24 antennas will be equipped withPAFsoverthenextfewmonths.Ifallgoeswell,thefull EMU survey will start next year, discoveringabout 70million radio sources, compared to the2.5 million discovered so far over the entirehistoryofradioastronomy.

Notonlywill EMUdeliver images and cataloguesof radio sources, but it differs from earlier radiosurveys in building the tools (e.g. both compactand d i f fuse source ex t rac t ion , op t i ca lidentiUication,measuringredshifts,etc.)todeliverthesciencefromthedataonarapidtimescale.TheEMU key science projects and developmentprojects have been preparing for this withobservations and simulations, and incidentallygeneratingahealthy listofpeer-reviewedpapersalong theway.We are now on the home stretch,and probably less than a year away fromproducing the Uirst EMU Early Science papers. Ifyouhavebeenholdingback,waitingforthingstoget moving before you start putting effort intoEMU,nowwouldbeanexcellenttimetostart!

Withbestwishes,

RayNorrisEMUProjectLeader

ASKAPMilestonessincethelastnewsletter:✦BETAfollowed-upontheUirstLIGOdetectionsofgravitationalwaves(seearticlehere)

✦TheUirstASKAPCommunityBusyWeekshavebeen held (three have been held so far; seeFigure1below)

✦ Construction on the MRO Power Station hasbegan, with an array of 5000 solar panelsinstalled earlier this year (see Figure 2 belowandthearticlehere)

✦ BETA was ofUicially decommissioned inFebruary 2016, as work steams ahead onbuilding, testing, and installing the rest of theMk-IIPAFs

✦ PAFs have been used to remove RFI fromobservations without the loss of anyastronomicaldata(seearticlehere)

✦ TheASKAPEarly Science and Survey ScienceTeams have secured 750,000 hours on theMagnussupercomputer(housedinthePawseySupercomputingCentre)tocarryoutadvancedscienceprocessingonASKAPearlysciencedata(seearticlehere).

EMU NEWSLETTER ISSUE 10 MAY 2016

From the EMU Project Leader, including an ASKAP Update Dear member of the EMU team,

Figure 2: Image of the new solar panels thatwill formpartoftheMROpowerstation.Imagecredit:CSIRO

Figure 1: Astronomers working on data reduction forASKAP during the Cirst ASKAP Community Busy WeekheldinMarch2016.Imagecredit:GeorgeHeald(CASS)

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TheEMUProjectStructureThe EMU project consists of about 300 astronomers in 21 countries.Members participate through thevariousEMUprojectsincluding:

• The Key Science projects (see http://askap.pbworks.com/KeyProjects) such as Cosmology,Clusters,etc.

• TheEarlyScienceprojects(seehttp://tinyurl.com/guvvj8e)• TheDevelopmentProjects(seehttp://askap.pbworks.com/DevelopmentProjects)suchasSource

Extraction,Cross-IdentiUication,etc.• The Collaboration Projects (see http://askap.pbworks.com/CollaborationProjects) which

maintainourcollaborationswithothersurveysprojectssuchasSkyMapperandeROSITA

Whilemostof thescience isdrivenbythe leadersof theseprojects,overallmanagementofEMUisbyasmallmanagementteam,shownbelowinFigure3,whomeetbyweeklyteleconference,andKateChow,whoeditsthisnewsletter.

The EMU Management Team

WhyshouldIcontributetoEMU?EMUdatawill be processed in real time and, after validation and quality control,will be placed in thepublicdomain.SoyoumightthinkthatthereisnoadvantagetoparticipatingactivelyinEMU–allyouhavetodoissitbackandwaitforthedatatoappear.I’dliketoexplainwhythatmightnotbeyourbeststrategy.

1) Although the public domain EMU datawill include images and catalogs, there’s amuch richer dataproduct, which is EMU’s value-added catalogue, or EVACAT. EVACAT will be available only to EMUmembers for someproprietary period, For example, in the public domaindata, youmight see a line ofthreeradioblobs,forwhichthecatalogwilllistthreecomponents.EVACATwilltellyouifthethreeblobsarethreedifferentgalaxies,orarethecoreandlobesofanFRIIgalaxy.EVACATwillalsogiveyouoptical/IRidentiUicationandredshift,ifavailable,andwilllinktothePOSSUMdatagivingthepolarisation.Whilethismayseemtrivialforindividualcases,EMUwilldelivermillionsofsuchexamples,fornumerous

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Figure3.TheEMUManagementTeam

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differentscenarios.Furthermore,itmaybenecessaryforASKAPtoobserveeachUieldformorethan12hours,inwhichcasethepublicdomaindataislikelytolistseparateobservationsasseparateimagesandcatalogentries,whilstEVACATwillmergethesetogetherintoacombinedimageandacombinedcatalogueentry.

2)Thereareanumberofoptionsforthesurveystrategy,anditislikelythattheoptimumoptionforonesciencegoalmaynotbeoptimumforanother.Forexample,theGalacticPlaneislikelytorequirequitedifferentparametersfromhigh-latitudeUields.ButevenathighGalacticlatitudes,dowewanttomaximisesensitivity,ordynamicrange,orresolution,orlow-surface-brightnesssensitivity,orsurveyuniformity?Whatdataproductsneedtobestored?Doyoujustwanttheimage,ordoyoualsowantcoveragemaps,rmsmaps,residualmaps?Doyoujustwantcompactsourcesinthecatalog,orextendedsourcestoo?Ifso,whatalgorithmshouldbeused?TheEMUKeyScienceprojectshaveacriticalroleinexaminingtheseissues,performnecessarysimulationsorobservations,givefeedbacktotheinstrumentandsoftwarebuilders,andbuildthetoolsanddatabasesreadyforthedata.Ifyoudon’thaveasayintheplanningprocess,there’sariskthatEMUdatamaybeunsuitableforyoursciencegoal,andreprocessingofthedatamaybeimpractical.

3)AnotherreasonforactiveparticipationistobecomeanexpertuserofASKAP,knowledgeableonthestrengthsandweaknessesofEMUdata,knowingwhatisachievableandwhatisnot,andwhatisrealandwhatislikelytobeanartefact.

4)AnimportantrolefortheKeyScienceProjectsistoensurethatthescienceteamisreadywiththetoolsanddatatheyneedtocapitaliseontheirinsideknowledgetodeliverthesciencefromthedata.Whenthedataarrives,it’sabitlatetostartnegotiatingforaccesstoamultiwavelengthdataset.Someoneelsewillprobablyhavegottherebeforeyou!

5)AndUinally,weexpecttheKeyScienceProjectstodeliveranumberofKeySciencepaperscontainingthemostimportantscienceoutcomesfromEMU.Thesewillprobablybethemosthighly-citedpapersfromEMU,andactivelycontributingtoEMUwillearnyoutherighttobeaco-authoronthesepapers.

Soyouhaveachoice:sitback,donothing,andgetthedefaultpublic-domaindata,oractivelyparticipateandgetaccesstoprivilegedvalue-addeddata,multiwavelengthdatafromothersurveysthroughMOUs,andhaveasayinmakingsurethatEMUdeliversthedatathatYOUwant!

EMU NEWSLETTER ISSUE 10 MAY 2016

Figure 4. Some friendly Emus checking out the land near Boolardy Homestead. ImageCredit:CSIRO

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ASKAP/EMU Early Science Update Josh Marvil TheASKAPEarlyScienceProgramhascontinuedtobereUinedoverthepastseveralmonths.AtCSIRO’smonthlyEarlyScienceForum,severaltopicshavebeendiscussedincludingcommissioningupdates,pilotUields,datapipelines,dataaccessandvalidation,andresourcesforpost-processing.Aseriesofthreecommunitybusyweeks,heldbetweenMarchandMay,werefocusedontheASKAPsoftprocessingpackage,preparationofdatapipelinesandthesciencedataarchive(CASDA).WithinEMU,muchprogresshasbeenmadeonspecifyingtheearlyscienceUieldsandfrequencytunings,butthereremainsmanyobservingstrategyconsiderationstofurtherdeUineoverthecomingmonths.

Aprimarygoaloftheearlyscienceobservationsistoobserveacrossthefullinstrumentalresponseof700-1800MHz.Thiswillrequiremultiplefrequencytuningssincethecorrelatorisonlycapableofprocessing300MHzofbandwidth.TheMk.IIsystemwillbemorelimitedinfrequencyselectionthanwewereaccustomedtowithBETAduetothepresenceof3analogbandpassUilters,wemeanswewillbeunabletocover700-1800MHzrangewith4x300MHzadjacentbands.WeconsidereddifferentconUigurationsofthreebandsthatwouldimposegapsinthefrequencycoverageaswellasaconUigurationusingUivebandswithsubstantialoverlap.AfterconsultationwithPOSSUMandFLASHweconvergedona3-bandconUigurationcovering700-1000MHz(band1),1000-1300MHz(band2)and1500-1800MHz(band3)touseforearlyscience.

TheEMUmanagementteamhasreviewedmorethan25expressionsofinterestandproducedaprovisionalrankingofearlyscienceprojects.Feedbackhasbeenprovidedtoprojectswhichwerenottop-rankedsothattheymaybefurtherreUinedandreconsidered.AlistofUieldswascompiledfromthetop-rankedexpressionsofinterestandtheUieldsthemselveshavenowbeengivenaprovisionalranking.AUield’srankisbasedon1)thenumberandqualityofscienceprojectsusingtheUield,2)theextenttowhichtheobservationwillhelpdebugandcommissionASKAP,3)theextenttowhichtheprojectsuseASKAPsuniquecapability(e.g.,thewideUieldofview)and4)theextenttowhichtheprojectshelpsdriveanEMUkeyscienceproject.Thisprocessisstillopenfordiscussionandyourfeedbackismostwelcome.

Many members of EMU will be in Sydney for the ASKAP 2016 conference on June 6-10, which willshowcaserecentASKAPresultsandplankeyaspectsof futuresurveyssuchasobservingstrategiesanddatasharing.ThereisalsoanEMUinternationalmeetingscheduledfortheendofthepriorweek,June2-3.ThemeetingagendaandremoteconnectioninfoispostedontheEMUwikihere.

EMU NEWSLETTER ISSUE 10 MAY 2016

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EMU NEWSLETTER ISSUE 10 MAY 2016

ASKAPsoft and EMU Josh Marvil and Kate Chow ASKAPsoft is the suite of processing software developed by the ASKAP computing team to handle thepipelineprocessingofASKAPobservations.Ithasbeenprimarilydesignedforfull-scaleASKAPprocessingonahigh-performancecomputingenvironment.ThedesignphilosophyandbackgroundisdetailedintheASKAP Science Processing document,whichwas produced in 2011 to detail the entire ASKAP pipelineprocessingenvironment.AllthescriptshavebeendesignedtobecontrolledbyasingleconUigurationUile,wherein most parameters can be set. The scripts for data processing are run on the supercomputer“Galaxy”, the ASKAP Central Processing machine in the Pawsey Supercomputing Centre. The scriptshandlesallASKAPdatareduction,fromthesplittingandUlaggingof1934-638(thecalibratorradiosource)andsciencedatasets,obtainingandapplyingthebandpasscalibration,averagingofthesciencevisibilities,continuumimaging(withorwithoutself-calibration)andlinearmosaicking,source-Uinding,andspectral-lineimaging(includingcontinuumsubtractionandgainscalibration).

Several components of the full ASKAPsoft data reduction pipeline will need to be commissioned andveriUied prior to general use. In the EMUDevelopment Project D3,wewill focus on the portion of thepipelinerelatedtogridding,weighting,deconvolutionandmosaicking.ThesestepsareperformedbytheASKAPsoftroutinescimagerandlinmos.JointdeconvolutionandjointgriddingofthedatafrommultipleUieldsandbeamswillalsoneedtobetested.ASKAPsoftoffersanumberofgriddingoptionsdescribedonthedocumentationpages.Thecurrentplanisto combineWproject with snapshot imaging (warped snapshots). A large number of parameters areavailabletotunethisalgorithm.Generallyspeaking,griddingaccuracycanbetradedforprocessingspeedandmemoryusage.Defaultvaluesfortheseparametersareinplaceandappeartobeworkingreasonablywell.Aquantitiveanalysiswhichoptimizesthecombinationsoftheseparametersasnotbeenundertaken,butcouldbeinvestigatedusingsimulatedorexistingobservations.

ASKAPsoft'suseofpreconditioningisintendedtomoreefUicientlyreplicatetheeffectsofBriggsweightingandaUVtaper.ThecurrentplanistousetheWienerandGaussianTaper(outertaper)preconditioners.For theWienerpreconditioner, thevalueof robustnesscanbesetcontinuously from-2(uniform) to+2(natural).Basedonsimulatedobservations,arobustnessnear+0.5shouldbeidealforEMU.Inlate2015,weparticipatedinthecommissioningoftheWienerpreconditionerasimplementedincimager.MultiplebugswereidentiUiedandcorrectedbythedevelopers.Afterthoseissueswereresolved,weusedsimulateddatatoverifythattheresultsoverthefullrangeofrobustnessvalueswereaclosematchtoCASA'sresults.Wecomparedanumberofquantitivemetricssuchasimagesensitivity,resolution,peakpositivesidelobe,peaknegativesidelobeandfar-UieldsidelobeRMS.

In ASKAPsoft, deconvolution is performed by one of several solvers after preconditioning has beenapplied. Some solvers supportmultiple scales and/ormultipleTaylor terms. The current plan is to usetheBasisfunctionMFS solverwith 3 Taylor terms (the 2nd order expansion) to image and deconvolveobservations having 300 MHz of bandwidth. The BasisfunctionMFS solver accepts multiple scales,althoughthenumberofscalesandthesizeofeachscaleiscurrentlysomewhatarbitrary;idealchoicesmaybe Uielddependentand/or requiremultiple imaging runs to identify.Other tunableparameters include:loopgain,majorandminorcyclestoppingthresholds,andthesizeofthepsfimageusedintheminorcycle.Large scales have not been extensively tested and a small scale bias parameter may need to beimplemented to prevent very large scales from diverging. Presently, using ASKAP data over a narrowbandwidth (48 MHz), superior results are being demonstrated using the Hogbom solver (underinvestigation).

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EMU NEWSLETTER ISSUE 10 MAY 2016

ASKAP’s first 36-beam image Adapted from the original ASKAP News article written by Flornes Yuen (see here) The Uirst ever 36-beam radio image has been produced during commissioning activities for the ASKAPtelescope!TheimageisshownbelowinFigureX.

The radio image was produced using the nine ASKAP antennas recently installed with the newMk IIPhasedArray Feed (PAF) receiver systems. The PAFswere conUiguredwith 36 dual-polarisation beamsarrangedina6x6squarefootprintandrotatedonthesky.TheteamobservedasingleUieldfor11hours,with48MHzofbandwidthcentredat939.5MHz.The Uield targeted for thisobservation is in theApus('birdofparadise’) constellation.This is the same Uieldpreviouslyused toproduce the Uirstmulti-beamimageevermadewithASKAPPAFs,andusedtoanalysethebeneUitsofASKAP’sthird'roll'axis.ThisareaoftheskyhasbecomeastandardtestUieldfortheACESteam,duetoitsproximitytotheSouthCelestialPoleandbecauseitcontainsanarrangementofseveralstrongsources.

The resulting continuum image was produced using ASKAP’s dedicated imaging package, known asASKAPsoft,andat30squaredegreesisequivalenttothetelescope’sfullUieldofview.

ASKAPsoftwill analyse thedata thatwill Ulow invastquantities from thecompletedASKAP telescope–ratesthatnoothercurrentsoftwarepackagewillbeabletohandle.TheteamrunsASKAPsoftonGalaxy,therealtimecomputerhousedinthePawseySupercomputingCentreinPerth.

This image not only represents the fact that ASKAP’s newest receiver systems work, but also thatASKAPsofthasnowmaturedenoughtodealwithlargequantitiesofdataandproduceimagesofthesamehighqualityasotherwell-establishedsoftwarepackages.

AnicearticlewasalsowrittenforthemainCSIRObloghere,withanexcellentvideoshowingwhyASKAPissuchanamazinginstrument.

Figure5.Thecontinuumimage,producedwithASKAPsoft,hasanrmsofaround300uJy/beamand a Cield of view of 30 square degrees. It contains over 1300 sources. Image Credit: ASKAPCommissioningandEarlyScience(ACES)team

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EMU Key Science Project Updates KSP2:CharacterisingtheRadioSkyProjectLeader:IanHeywood

TheCharacterisingtheRadioSkyKSPsitsattheinterfacebetweentheastrophysicalapplicationsoftheEMUsurveyproducts and the validation of the products themselves. Pick up a typical survey description paper and it willgenerallycontainseveralchecksthatvalidatetheresults.TheseincludeveriUicationofastrometric,photometricandspectral performance,measuring radio source counts, and quantiUication of biases thatmay be present, includingresolutionconsiderationsandmoresubtleeffectssuchasthoserelatedtodeconvolutionandself-calibration.Therearemany approaches to conducting such checks, including the use of Monte Carlo-type simulations that rely oninstrumentalandastrophysicalmodels,andbycross-matchingwithexistingradioobservationsthatoccupysharedregionsofparameterspace.ThesearethebroadgoalsofthisKSP.

Activity related to thisKSPhasmainly involveddevelopingscripts toautomaticallyperformsomeof theactivitiesmentionedabove.Wehaveusedrealobservationstotestthesealready,includingthepilotASKAP-BETAcontinuumsurvey in Tucana (Heywood et al.,MNRAS, 2016) aswell as a 100 square degree JVLA survey at similar angularresolutiontoEMU(Heywoodetal.,MNRAS,2016,submitted),anda4.5squaredegreeJVLAsurveythatismatchedindepth(Heywoodetal.,2016,inprep.).WearealsoworkingcloselywithSouthAfricancolleaguesontechniquestoautomatically reject artefacts from source catalogues and calibrationmodels, led by postgraduate student LeratoSebokolodi.This is anewandverypromisingarea thatwill likelyhaveoverlapwith thegoalsof theWTFKSP. In2016,welookforwardtogettingourhandsondatafromASKAP’scommissioningandEarlyScienceprogram.

KSP4:CosmicWeb ProjectLeader:SheaBrown

PreparationtoutilizeEMUtodetectdiffusesynchrotronemissionwithinthecosmic-webasbeenbuildingmomentumoverrecentmonths.ThisKeyScienceProjecthasgrowntoover30members,andactivitywithintheKSPhasspreadoutintoseveralkey“Experiments”suchas1)DirectDetection;2)FilamentStacking;3)Cross-correlation;4)DistortionofTailedSources;5)DarkMatter;and6)Polarization.MembersoftheCross-correlationgrouphavedevelopedanall-skycross-correlationpipeline,incoordinationwiththeCosmologyKSP,andhavetestedit(seeFigure6overthepage)ontheParkesContinuumHIPASSsurvey(Calabrettaetal.2014).WearecurrentlyplanningtotestthepipelineontheNRAOVLASkySurvey(Condonetal.1998),whichsimulatesmanyofthechallengesthatEMUdatawillpresent.withtheintentionofpublishingtheresults.Tosupportthiseffort,theoreticianFrancoVazzahasjoinedtheteam,andiscontributinginvaluablesimulateddatafromwhichtodesigntheoptimaldetectionalgorithm(e.g.Vazzaetal.2016).TessaVernstromfromtheUniversityofTorontohasalsojoinedtheteam,bringingherexpertisefromsimilarexperimentswiththeMurchisonWideUieldArray.

AparalleleffortbymembersoftheCosmic-WebKSP,inconjunctionwiththeClustersKSPandtheDiffuseEmissionExtractionDevelopmentproject,willensurethatEMUwillbesensitivetolarge-scalediffuseemission,andthatoursource-Uindingandanalysispipelinesfullyaccountforpotentialsystematiceffectsinthedata.ThisisadifUicultandimportantprocess,andwewelcomeanywhoareinterestedinparticipatingtocontactus.

References:Calabretta,M.R.,Staveley-Smith,L.,&Barnes,D.G.,2014,PASA,31,e007Condon,J.J.,Cotton,W.D.,Greisen,E.W.,etal.,1998,AJ,115,1693Vazza,F.,Brueggen,M.,Gheller,C.,Ferrari,C.,&Bonafede,A.,2016,arXiv:1602.07526

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KSP7:Evolutionofradio-loudAGNProjectLeader:AnnaKapinska

Radio-loudAGNwillbethedominantbrightsourcepopulationintheEMUdata,andtheconstructionoflargedeepsamplesout tohighredshiftswill Uinallybeatareachofahand.HighsensitivityofmicroJy levelswillallowus tostudyindetailthelowerluminosityendoftheradio-loudAGNpopulation,andevenwiththeEarlySciencedataweexpecttomeasurevirtuallycompletesamplesofAGN>10^23W/Hzsruptoz=1.

TheoverallgoalofthisKSPistoquantitativelyinvestigatetheradio-loudAGNevolutionandtheAGNimpactontheevolution of galaxies, based on large deep data. This can be broadly split into sub-projects focusing on themeasurementandanalysisof(1)sensitiveradioandkineticluminosityfunctionsasafunctionsofredshiftandsourceproperties,(2)dutycycles,triggeringandlifetimesofradio-loudAGN,and(3)theirhostsandenvironmentsacrosscosmictime.

Butofcourse,thereisalongwayfromplanningtoprovidingoutcomes.Thereisanumberoftechnicalconsiderationsthatmustbe tackled Uirst.These includemeasuringorestimatingredshifts (spectroscopic, template/non-templatephotometricones;D8-D10),distinguishingAGNfromnon-AGNsources,cross-matchingtomulti-wavelengthdatatomeasurehostproperties (D7),andself-identifying(i.e. identifyingmultipleradiocomponentsofoneradiosource;D7) and classifying radio galaxies (D13). Clearly, there is a lot of development work to do! If you would like tocontributeandhavenotputupyourhandyet-letmeknow!

Figure6:ResultsfortheCHIPASSsurveyofthesouthernskywithParkes(1.4GHz,14'beam)correlatedwith4mapsoflarge-scalestructure.1)GalaxiesfromtheLEDAdatabasewithz<0.02(i.e.,verylocal);2)theWISE-2MASScatalog<z>=0.14;andtwoversionsofthelocalgalaxiesthathavebeenrotated/Clippedsothattheynolongercorrespondtotheactualsky.Asyoucansee,bothrealgalaxydistributionsarecorrelatedwithCHIPASS,thoughonscalesontheorderoftheCHIPASSbeam.Thiscorrelation(units ofmKbrightness temperature) is coming fromradio emissionwithin thegalaxies themselves.Wearenowworkingonassessinghowmuchdiffuseemissioncanbecontributingthroughtheiterativeinjectionoffakeradiosignalinordertolimitthecosmic-webemissivity(EMUCosmic-WebKSP,inprep.).

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EMU NEWSLETTER ISSUE 10 MAY 2016

ThereiscurrentlyasmallteameagertoworkontheKSP7goals(26EMUmembers,moremembersarewelcomeatanytime),andtherearefourEarlyScienceProjectsproposedtomapthestepsandtestmethodsontheUirstASKAPdata.Threeoftheseprojects,rankedA,focusontheexploitationofthedatafromtheGAMAsurveyUields:ESP5“RLFsofradio-loudAGN”,ESP6“KLFsofFRIIradiogalaxies”andESP27“TriggeringanddutycyclesofAGN”,addressingourmaingoalsUirstonaselectionofsmallerUieldswithversatiledata.

KSP7willbeinclosetouchwiththeactivitiesafewotherKSPs,especiallyKSP1“EVACAT”,thatwillbeaddressinganumberofcriticaloutputssuchascross-andself-identiUications,redshiftmeasurementsetc,andKSP6“Cosmicstarformationhistory”andKSP9“Radio-quietAGN”tosharesamples,methodsandininterpretingresultsonabroaderscale.

Ifyouwouldliketojointheteamandbedirectlyinvolvedinpreliminaryandearlysciencework,emailmeoraddyournametotheKSP7wikihere.

KSP8:RadioAGNintheEoRProjectLeader:JoseAfonso UpdateprovidedbyJoseAfonso,StergiosAmarantidisandHugoMessiasfortheKSP8team

Over the past few months we have started exploring models of galaxy and structure formation to estimate thenumberofSMBHsthatcouldbedetectedbyEMUatveryhighredshifts.MorespeciUically,wearefollowingseveralcodes, includingsemi-analyticalmodels,toproduceluminosityfunctionsforAGNoverawideredshiftrange.Asanexample,weareusingthelatestversionofthe ’Munich’model(Henriquesetal,2015),whichsimulatesthegalaxypopulationandscalestheMilleniumsimulationstothecosmologyoftheUirstyearPlanckdata.ThismodelconsidersAGN activity in individual galaxies with the central SMBH growing via merging or accretion processes. AGNluminosity functions can be produced, compared with observations for lower redshifts and estimates for higherredshifts up to the EOR developed. Over this work, the limitations of some models, tuned up for non-AGNphenomena,havebecomeapparent.Nevertheless,othermodelshaverevealedthemselvesmuchmoreadequate,andseemtobeabletoprovideinterestingestimatesforEMU,aswellasforotherfutureradiosurveys.

KSP13:SCORPIO:CataloguingtheRadioStarsinourGalaxyProjectLeader:GraziaUmanaUpdateprovidedbyFrancescoCavallarofortheKSP13team

TheSCORPIO(StellarContinuumOriginatingfromRadioPhysicsInOurgalaxy)projectisasurveyofa2x2deg2

regioncenteredatgalacticcoordinatesl=344°.25,b=0°.66conductedwithATCAtotackletheproblemthattheonlyknownradiostarsarethosethathavebeentargetedbecauseoftheirpropertiesatotherwavelengths.(seeUigure1forthewholemap).FurthermoreSCORPIOwillbeusedasapathUinderfortheEMUsurvey.Infact,eventhoughEMUismainlyanextragalacticsurvey,itwillalsoproducethedeepestradioimageyetoftheGalacticPlane.HowmanyGalacticsourcesdoweexpect?Howmanyradiostars?ThesearethescientiUicquestionsthatSCORPIOistryingtoaddressand,withafrequency(ATCACABBL-band),resolution(10by5arcsec)andsensitivity(0.04mJyrms)similartotheEMUones,itwillcertainlyhelp.TheobservationstookplaceinseveralmomentsandwithseveralconUigurations(6A,6C,EW367andEW352).Apaperonthepilotproject,asmallerUieldthatispartofthewholeone,waspublishedin2015(Umanaetal.2015).Wefound614sourcesona2.3deg2area,34ofthemwithaSimbadmatch,487ofthemhaveacounterpartinatleastonecataloguebetweenNOMAD,2MASS,WISE,GLIMPSE,MSX,AKALI,HI-GAL,ATLASGAL,IRAS,RMS,MGPS-2andWBH2005butthespuriouscrossidentiUicationrateoftheinfraredcataloguesishigh.ThankstothebigCABBbandwidth(1.4to3.1GHz)wemanagedtocalculatethespectralindicesformostofthesourcesand,comparingthemwiththeATLASones,wefoundthatSCORPIOhas20%moresourcesthantheATLASones,mostofthemhavingapositiveorUlatspectralindex.ThemodelusedinUigure2wasmadeusingtheGaussianthatUitstheATLAShistogramplusanotherGaussianthatUitstheSCORPIOsourcesurplus.AnotherimportantissuethatweareexploringishowtomapthediffuseemissionoftheGPandhowitcanchangethedynamicrangeoftheobservations.TodothatweaddedtheshortbaselinesfromthecompactconUigurationsineverypointing.ThisisactuallyaworkinprogressbutitshouldteachushowtoreducetheGalacticPlanedatafromEMU.

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EMU NEWSLETTER ISSUE 10 MAY 2016

KSP14:WTF:DiscoveringtheUnexpectedProjectLeader:RayNorris

ThemajorityofdiscoveriesinastronomyhavecomefromunplanneddiscoveriesmadebysurveyingtheUniverseinanewway,ratherthanbytestingahypothesisorconductinganinvestigationwithplannedoutcomes.Forexample,ofthe10greatestdiscoveriesbyHST,onlyonewaslistedinitskeysciencegoals.GiventhatEMUissigniUicantlyexpandingthevolumeofobservationalphasespace,wecanbereasonablyconUidentthatwewillstumbleacrossunexpectednewphenomenaornewtypesofobject.However,thecomplexityoftheinstrumentandthelargedatavolumesmeanthatitmaybenon-trivialtoidentifythem.Ontheotherhand,ifwedon't,thenwemaybemissingoutonthemostexcitingscienceresultsfromEMU.TheWTFprojectinEMUaimstomineEMUdatatodiscoverunexpectedsciencethatisnotpartofourprimarysciencegoals,usingavarietyoftechniquesandalgorithms,especiallymachinelearning(ML)techniques,suchasneuralnetworks.

WereceivedasmallgrantfromAmazonWebServices(AWS),andarecurrentlyusingtheAWSplatformasthebasisofWTF.Ourgoalistoissuedatachallengesinwhichweputuprealandsimulateddatasetscontainingembedded"eastereggs",whicharesimulatedunexpecteddiscoveries,andinvitepeopletotrytheiralgorithmstoseeiftheycanUindtheeastereggs.

EarlierthisyearwestartedputtingupsomedatasetsontheWTFwiki,someofwhichhadembeddedeastereggs,andinvitedsomelocalbeta-testerstotrythemout.Theresponsewasthatpeopleweren'tclearonwhattheyactuallyneededtodowiththem,andalsotherewereissueswithUileformats,toomuchjargonintheexplanations,etc.Aboveall,thestatedproblemwastoopoorlydeUined.Werealisedwewerebeingtooambitious,andneededtostartwithsomethingsimpler.WealsorealisedthatitwasdifUiculttoUindtheunexpectedwhenthealgorithmsweren'tyetverygoodatdiscoveringtheexpected!Sowehavebacktrackedabitandsetupsomesimplerexamplesonthewiki.AsmallgroupofusareputtingupsomesimpledemoexamplesofsourceclassiUicationtogetherwithsomepythoncodetoclassifythem.WehavealsodiscussedtacklingotherMLproblemssuchassourceclassiUicationandcross-identiUication,andarenowdoingthisasapreludetothemoreambitiousWTFgoals.Butitisnot*just*aprelude-theseareimportantprojectgoalsintheirownright..Weplantodevelopmoreinterestingchallenges,withlargertrainingsetsandtargetsets,toseewellMLcodecanworkonrealdata.Iknowthatsomeofyouhavealreadydevelopedalgorithmstodojustthat,andwelookforwardtoseeinghowtheyperformonourdatasets.

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Want to Work on EMU or ASKAP?

Pleasesharewithanyonewhomightbeinterestedinanyofthesepositions.

PositionsatCSIROAstronomyandSpaceScience

Senior Data Scientist in Astrophysics Applications close 17 July 2016. For more information, contact: SimonJohnston(Simon.Johnston@csiro.au),CSIROjobnumber19201.

Tenure-trackFellowshipsatWesternSydneyUniversityWearecurrentlybuildinguptheastrophysicsgroupattheWesternUniversityofSydney(WSU),withafocusonEMUandeScience.Weare invitingexpressionsof interest fortwoclassesofARC-fundedpostdoctoralpositionsatWSU,andareofferingan indeUiniteposition(i.e.a lectureship)atWSUtosuccessfulcandidatesat thecompletionof thefellowship,subjecttonormalperformancecriteria.

There are two types of postdoctoral position to be supported (DECRA and Future Fellowships). Both are verycompetitive and there is no point in applying unless you have an excellent research track record. For moreinformation, see http://askap.pbworks.com/WSUFellowships2016. If you are interested, please emailRay.Norris@gmail.comby6June.

EMU NEWSLETTER ISSUE 10 MAY 2016

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Meetings and Conferences

PleasesendindetailsofanyEMU-relatedmeetingsorconferencescomingup.

EMUInternationalMeetingSydney,Australia,2–3June2016http://askap.pbworks.com/w/page/14049286/FrontPageTheEMUSurveyScienceTeamwillholdameetinginthedaysleadinguptoASKAP2016.

ASKAP2016:ThefutureofradioastronomysurveysSydney,Australia,6–10June2016http://www.atnf.csiro.au/research/conferences/2016/ASKAP/ASKAP 2016will bring together theworld's bestminds in astronomy, engineering and ICT to share cutting-edgeresults from the Australian Square Kilometre Array PathUinder (ASKAP) radio telescope and to discuss futurestrategiesforlargeastronomicalsurveyobservinganddatasharing.

AstronomicalSocietyofAustralia’s(ASA)AnnualScienceMeetingSydney,Australia,3–8July2016http://www.asa2016.org/The2016AnnualScientiUicMeetingwillbehostedbyTheUniversityofSydney.Thiswillbethe50thanniversaryoftheformationoftheAstronomicalSocietyofAustralia.Early-birdregistrationhasbeenextendedto16May.Theprogramisnowavailableonline.

DiscoveryandInnovationinRadioAstronomy:acelebrationofthecareerofRonEkers,‘RonFest2016’Queenstown,NewZealand,13–17September2016http://www.atnf.csiro.au/research/conferences/2016/IDRA16/index.htmlThismeetingisacelebrationofthecareerofProf.RonEkersandisdesignedtocoveradiverserangeoftopicsthatRonhasinUluencedinhiscareer.TheUirstthreedaysarefocusedoninnovationinradioastronomyandhelastdaycoversthebroaderimpactsofRon'scareerincludingpolicy,history,internationalprojectsandwiderscienceareas.Registrationisnowopen.

RFI2016–CoexistingwithRadioFrequencyInterferenceSocorro,NewMexico,USA,17–20October2016http://go.nrao.edu/rUi2016ThisconferencewilldiscusstheimpactofRFIinAstronomy,EarthRemoteSensing,andotherpassiveoractiveUieldsexploitingtheelectromagneticspectrum.Thisisagreatopportunitytodebate(currentandfuturestatusof)interferencecontamination,andreportrecentadvancesmadeinRFImitigationfromatheoreticalandappliedpointofview.Papersubmissionisdue20June2016,andregistrationcloses15September2016.

TheFirstPietroBaracchiConference:Italo-AustralianRadioAstronomyintheEraoftheSKAPerth,WesternAustralia,01–04November2016http://www.atnf.csiro.au/research/conferences/2016/Baracchi/ThisconferenceisdesignedtobringtogetherItalianandAustralianresearchersinradioastronomy,todiscussandexploreexistingandpotentialfutureareasofmutualinterest.Themeetingwillbeopentoallareasofinterestinradioastronomy(science,engineering,andcomputing),withanemphasisontheseareasplayingakeyroleintheeraoftheSKA–aprojectinwhichbothItalyandAustraliaarefoundingmembers.Webregistrationisnowopen.

SPARCS2016Goa,India,6–9November2016The2016meetingoftheSKAPAthUindersRadioContinuumSurveys(SPARCS)willbeheldinGoa,India,justpriortotheSKAsciencemeeting.Moredetail,includingaconferencewebsiteandacallforpresentations,willbeprovidedinthesecondannouncement.Inthemeantimepleaseindicateyourinteresttoattendthemeetingbyemailtosparcs2016@ncra.tifr.res.in

EMU NEWSLETTER ISSUE 10 MAY 2016

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SKA2016:SciencefortheSKAGenerationGoa,India,7–11November2016https://indico.skatelescope.org/event/391/overviewThisconferenceaimstobringtogetherearlycareerresearchersfromtheradioastronomycommunityinordertopresenttheirwork,developnewcollaborations,andpreviewthesciencethatSKA1willdoin2023andbeyond.ThemeetingwillrunforUivedays,includingtwodaysofbreakoutsessionsforthosewishingtodiscussfuturekeyscienceprojectcollaborations.Earlyregistrationcloses10June,withabstractsubmissionsdueinlate-July.

Newsletters

ASKAP Update ASKAPUpdateisaregularseriesdedicatedtoconveyingthelatestnewsabouttheAustralianSquareKilometreArrayPathUinder(ASKAP)projecttointernationalscienceandengineeringcommunities.Itwillalsoprovideadeeperlookat key aspects of ASKAP’s development. ASKAPUpdate replaces the ASKAP ScienceUpdate andASKAPTechnicalUpdatepublications.Thelatestissue,number9,wasreleasedinNovember2015andisavailablehere.

ToreceivenotiUicationofonlinepublicationofeachneweditionofASKAPUpdate,emailtheASKAPUpdateEditor,FlornesYuen(Ulornes.Yuen@csiro.au).

Papers

Published EMU Papers Umanaetal.2015,"SCORPIO:adeepsurveyofradioemissionfromthestellarlife-cycle”,MNRAS,454,902

BanUield et al. 2015, "Radio Galaxy Zoo: host galaxies and radio morphologies derived from visual inspection",MNRAS,453,2326

Hopkinsetal.2015,"TheASKAP/EMUSourceFindingDataChallenge",PASA,32,37H

Fanetal.2015,Matchingradiocatalogueswithrealisticgeometry:application toSWIREandATLAS,MNRAS,451,1299

Raccanelli et al., 2015, Probing primordial non-Gaussianity via iSWmeasurements with SKA continuum surveys,JCAP,01,042

Riggi et al., 2016, Automated detection of extended sources in radio maps: progress from the SCORPIO survey,MNRAS,inpress(arXiv:1605.01852)

Published ASKAP Papers (engineering and scientific) Serra,P.,Koribalski,B.,Kilborn,V. et al. 2015,MNRAS452,2680:ASKAPHI imagingof thegalaxygroup IC1459,(arXiv:1506.04399,acceptedinJune2015)

Allison,J.,etal.2015,MNRAS453,1249:DiscoveryofHIgasinayoungradiogalaxyatz=0.44usingtheAustralianSquareKilometreArrayPathUinder,(arXiv:1503.01265,acceptedinAugust2015)

Chippendale,A.P.,Brown,A.J.,Beresford,R.J.,etal.2015a, MeasuredSensitivityoftheFirstMarkIIPhasedArrayFeedonanASKAPAntenna(arXiv:1509.00544,acceptedforpublicationinICEAA2015-InternationalConferenceonElectromagnetsinAdvancedApplications)

Chippendale,A.P.,Brown,A.J.,Beresford,R.J.,etal.2015b,MeasuredAperture-ArrayNoiseTemperatureoftheMarkII Phased Array Feed for ASKAP (2015arXiv150905489C, accepted for publication in Antennas and Propagation(ISAP),2015InternationalSymposium.

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Published ASKAP Papers continued (engineering and scientific) Allison,J.R.,Sadler,E.M,Moss,V.A.etal,2015,AstronomischeNachrichten:TracingtheneutralgasenvironmentsofyoungradioAGNwithASKAP,(arXiv:1511.03067,acceptedinNovember2015,inproceedingsofthe'5thWorkshoponCSSandGPSradiosources',heldinItalyinMay2015)

Hobbs,G.,Heywood,I.,Bell,M.E.,etcal.2016,MNRAS456,3948 ApilotASKAPsurveyofradiotransienteventsintheregionaroundtheintermittentpulsarPSRJ1107-5907,(arXiv:1512.02702,acceptedinDecember2015)

Heywood,I.,Bannister,K.W.,Marvil,J.etal,2016,MNRAS457,4160-4178,Wide-Uieldbroadbandradioimagingwithphasedarrayfeeds:apilotmulti-epochcontinuumsurveywithASKAP-BETA,(arXiv:1601.05857,acceptedinJanuary2016)

Harvey-Smith,L.,Allison, J.R.,Green, J.A.etal,2016,MNRAS,High-velocityOHmegamasers in IRAS20100-4156:EvidenceforaSupermassiveBlackHole,(arXiv:1604.07537,acceptedinApril2016)

PleasesendindetailsofanyotherEMUorASKAPrelatedpapersyouhavesubmitted.

EMU NEWSLETTER ISSUE 10 MAY 2016

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KEY LINKS

MainEMUwiki: http://www.askap.pbworks.com

ASKAP:http://www.atnf.csiro.au/projects/askap/

anzSKA:http://www.ska.gov.au

TheSKA:https://www.skatelescope.org/

CONTRIBUTIONS

ContributionsaresoughtfromallmembersoftheEMUTeam.Plaintextispreferredandsubmissionofimagesandphotographsiswelcomed!

DEADLINES

ForIssue11pleasesubmitmaterialby14October2016.Emailreminderswillbesentoutseveralweeksbeforehand!

Editor Kate Chow Kate.Chow@csiro.au +61 2 9372 4516

EMU NEWSLETTER ISSUE 10 MAY 2016

Credit:AlexCherney,http://www.terrastro.com/