1 Publishable summary - CORDIS · 1 Publishable summary 1.1 Executive summary Observational astronomy has dramatically evolved over the last 20 years as a result of the opening up

ARCHES“AstronomicalResourceCross-MatchingforHighEnergystudies”-FP7n°313146,coordinatedbytheUniversityofStrasbourg,finalperiodicreport.

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1 Publishablesummary

1.1 Executivesummary

Observationalastronomyhasdramaticallyevolvedoverthe last20yearsasaresultof theopening up of new observing windows in the electromagnetic spectrum and of thedevelopment of efficient and large area detectors attached to ground-based and space-borneinstruments.Withmulti-wavelengthmeasurementsbecomingavailableforbillionsofstarsandgalaxies,astronomynowranksasa“bigdata”scientificactivityand todaymanyroutineresearchactivitiesrelyoninnovativedataminingtools.However,large-scalemulti-wavelength observational studies remain difficult to achieve for a large majority ofastronomers.One of themost challenging steps of analysis is to associatemeasurementspresent in different catalogues and observed at different wavelengths to a uniqueastrophysicalobjectandtoassessthecorrespondingassociationprobabilities.ThisproblemisparticularlyacuteinthecaseofcosmicX-raysourcesdetectedbytheESAXMM-Newtonsatellite, which due to its specific high-energy optics, yields source positions of lowerprecisionthanavailableatmanyotherwavelengths.Inthiscontext,ARCHES’smaingoalwasto enrich the scientific usability of the catalogue of XMM-Newton sources by providingstatistically qualified radio to X-ray spectral energy distributions for unresolved X-raysources,andprobabilisticidentificationsofextendedX-raysourceswithclustersofgalaxies.In order to fulfil these objectives, careful assessment of the photometric and astrometricqualityofmulti-wavelengthcatalogueswasfirstperformedfollowedbythedevelopmenti)ofaforefrontandsofaruniquemulti-catalogueprobabilisticcross-matchingtoolandii)ofanadvancedintegratedclusterfinderusingopticalandnearinfraredimagingdatatosearchfor clusters of galaxies at any position in the sky. These tools were then applied to anenhancedandcleanedversionoftheXMM-Newtonsourcecataloguetobuildover200,000spectralenergydistributionsofunresolvedX-ray sourcesandover500clustersofgalaxiescandidates. Seven demonstration science cases focused on clusters of galaxies, activegalacticnuclei and stellar activityhighlighted theusabilityofARCHES’s tools andproductsand,most importantly,provided important feedback to thedevelopmentof the tools andthe cross-matched catalogues. ARCHES tools and products were presented to theinternational community in a workshop held in Paris. They are now accessible through avariety of interfaces specific to the project as well as throughmainstream disseminationsystemssuchastheCentredeDonnéesastronomiquesdeStrasbourg.


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1.2 Summarydescriptionofprojectcontextandobjectives

The lastdecadeshavewitnesseda tremendous increaseof theobservationalastronomicaldata flow as a result of the development of new efficient and large area detectorssupplementedwithacomputingpowersofarfollowingMoore’slaw.

Ground-basedand space-borneall-sky surveyshaveprovidedanessential astrometricandphotometricreferenceframeandthefirsttruemapsoftheentiresky.

This ever-increasingwealth ofmulti-wavelength data has fundamentally changed thewayastronomersnowtacklescientificproblems.Thepreviousparadigm,typicallyfocusingonasingle wavelength range, has now evolved towards a systematic fully multi-wavelengthapproach.Infact,ourunderstandingofthephysicsofstarsandgalaxiesnowessentiallyrestson the modelling of their electromagnetic spectra over the widest range of frequencies,spanningfromradiotothehighestenergygamma-rays.

Forinstance,thenumberofcatalogueentriesintheVizierserviceattheCentredeDonnéesastronomiquesdeStrasbourg(CDS)whichwasabout500millionin1999hasreachedalmost18billionasonFebruary2016.Atthe2020horizon,EuropeanspacemissionssuchasGAIAandEUCLIDtogetherwiththeLargeSynopticSurveyTelescope(LSST)willprovideaseveralfoldincreaseofthenumberofcataloguedopticalobjectswhileprovidingmeasurementsofexquisitequality.

Despite theparamountscientific importanceof large-scalemulti-wavelengthobservationalstudies,obstaclesstillremainfortheirefficientusebya largemajorityofastronomers:forexample, essential quality information on some catalogues is difficult to gather, and astandardmethodforadependableandrobustassociationofaphysicalsourcetoinstancesofitindifferentcatalogues(cross-identification)andindiversespectralrangesisstillabsent.

Amongthisplethoraofdata,thehigh-energywindowtotheUniversehasstronglybenefitedfrom the recent availability of the European Space Agency (ESA) XMM-Newton spaceobservatory. This large X-ray telescope routinely observes the sky with an image qualityapproaching that of ground-based optical telescopes, generating one of the key ESAastrophysicaldatabases,thethirdXMM-NewtonX-raycatalogue(3XMM),nowextendingtohalfamilliondetectionsofcosmicX-raysources,thelargestX-raycatalogueevermade.

ARCHES is primarily aimed at increasing the usability and research potential of the XMM-NewtonX-raycatalogue,enhancingitwithkeymulti-wavelengthresourcesinareliablewayand distributing these results to the international community, along with the tools thatmadethispossible.

The ARCHES project started by building an enhanced 3XMM catalogue, cleaned ofpotentially problematic sources, and containing additional useful parameters as well as a


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thorough quality assessment. In parallel, ARCHES developed new tools for probabilisticmulti-catalogue cross-correlation with extensive archival resources. These so far uniquetools allowed us to create high reliability source cross-identifications, based on carefullyselectedarchivalastronomicalcatalogues,soastocoverthewidestrangeinwavelengthandskycoverage.Thesecross-identificationswerethenusedtomeasuretheradiationemittedbyeachsourceinthewavelengthrangesofallcatalogues,buildingfullycalibratedspectralenergydistributions(SEDs)ofX-raysources.AnothertoolspeciallyadaptedtoextendedX-raysourcessearchesforclustersofgalaxiessimultaneouslyinX-rayandoptical-nearinfrareddata, with the goal of producing a science-grade catalogue of clusters of galaxies. Mostimportantly,wevalidatedthequalityoftheseproductsbyusingthemintheframeworkofasmallnumberofpilotprojectstacklingforefrontastrophysicaltopics,providingtherouteforfurtherenhancementandbringinghighlyvaluablefeedbackontoolsandarchivaldata.

ARCHES tools were offered at the end of the project through dedicated interfaces, whilevalidated multi-wavelength SEDs and associated catalogues were made available to theinternationalcommunityusingVirtualObservatoryprotocols.Inthistwo-foldreleaseofdataandtools liesthelegacypotentialofARCHES.Ourprojectwillpavethewayforafull-scaleexploitationoftheimmensewealthofdatanow(andevenmoreinthenearfuture)availabletotheinternationalcommunity.


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1.3 DescriptionofthemainS&Tresults/foregrounds

1.3.1 Selectionofarchivalcataloguesforbuildingspectralenergydistributions

OneofthefirststepsoftheARCHESprojecthasbeentoselectamongthelargecollectionofcatalogues available at the CDS those with the best photometric and astrometric qualitywhile at the same time providing the largest sky coverage. Extracting the final list ofcatalogues fromthe severalhundredavailableatCDShasbeenamajor task involving theentireconsortium.Foreachcatalogue,weidentifiedthemostrelevantinformation,suchasthe number of sources, the wavelength and the sky coverage. We also obtained a firstestimateofthenumberofexpected3XMMassociationsandofthesourcemeanpositionalerror.CDStoolssuchasAladin,theCDStwocataloguecross-matchservice,andthemulti-ordercoveragemaps(MOC)intersectionservicewereextensivelyusedforthatpurpose.Welater used this list of catalogues, containing several hundred catalogues per energy band(optical, infrared...),andthe informationgathered for them, to identify inahomogeneousway those catalogues that will be used for cross-matching with the enhanced 3XMMcatalogue. The list of archival catalogues was thoroughly revised within the entireconsortiumandprioritizeddependingupontheregionoftheskyconsidered(mainlyhighorlowGalacticlatitude).AspecialsetofcataloguesdesignedforbeingusedbytheIntegratedClusterFinderwascompiledwiththeaimtooptimallyderivephotometricredshiftsoverarangeofredshiftsaslargeaspossible.

Finally, it became soon clear that the simultaneous multi-catalogue probabilistic cross-matching tool would not be easily usable if the number of catalogueswere greater thanaboutseven,duetothegeometricallyincreasingnumberofcombinations.Consequently,wehadtoseverelytrimthelistofcataloguestobeusedto24,definingsubsetsofthem,sothatamaximumof7 (includingour“native”enhanced3XMMcatalogue) isusedper individualrun.

1.3.2 TheenhancedXMM-Newtoncatalogue

The prime objective of building an enhanced 3XMM catalogue (3XMMe) of X-ray sourceswastoassemblearesourcethatwouldbesignificantlycleanerthanthebasepublic3XMMcatalogue fromwhich itwas derived and augmentedwith additional information so as toenhanceitsvaluetotheARCHESdemonstrationscienceprogrammesandtothewiderusercommunity. The enhanced 3XMM catalogue (designated 3XMMe) is one of the coreelements of the ARCHES project, representing the X-ray source basis for the cross-correlationswithothermulti-wavelengthcatalogues.Thefinallyreleased3XMMecatalogueis a derivative of the latest increment of the 3XMM catalogue, i.e. 3XMM-DR5, that waspubliclyreleasedinApril2015tailoredforthepurposesoftheARCHESproject.The3XMM-DR5cataloguecontains565962detectionsarisingfrom396910uniquesourcesdrawnfrom


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7781XMMobservations.Thesenumbersincludedetectionsfrom356sub-pointingsmadeinmosaicmode.

Theconstructionoftheenhanced3XMMcatalogueinvolves3mainelements;i)thecleaning(ejection)ofdetectionsthatareconsideredtobeoflowerscientificreliabilityorquality, ii)theapplicationofcriteriatoidentifydetectionsthatareconsideredpotentialcandidatesforthe 3 main science themes (i.e. active galactic nuclei (AGN), clusters of galaxies and thegalacticplane)oftheARCHESproject.Theconstituentdetectionsofuniquesourcesontheskyareexaminedtodecidewhichuniquesources,overall,meetthecriteriatobeassignedtoeachsciencetheme,andiii)theadditionofotherinformationthataugmentsthescientificvalueofthecatalogue.

AlldetectionslocatedinbadmosaicfieldsaffectedbyissueswiththeODF(raw)data,thosepresent in flaggedhighbackgroundfieldsaswellas those locatedatmorethan12arcminfromopticalcentrewereremoved.Anumberoffalsedetections(hotspots)concentratinginlocalised features whenmapped to the separate instrument detector coordinate systemswere also discarded. It was also decided i) to exclude fields where the EPIC camera pndetectorwas off and bothMOS1 andMOS2 detectorswere off or being used inwindowmodes ii) fields with strong diffuse emission iii) fields with less than 5 ks exposure, iv)pointingsforwhichboresightcorrectioncouldnotbeachieved.

Figure1:Positionofthe4082XMM-Newtonobservationsenteringthe3XMMecatalogueasderivedfromthe3XMMDR5(v2.0).WeuseheretheAitoffprojectioninwhichthehorizontalaxisrepresentstheplaneoftheMilkyWay.ThecentreoftheGalaxyisatthecentreofthefigure.Combining theseelements,we find thata totalof280757uniquedetectionsareexcludedfromtheenhanced3XMMcataloguecompared to thebase3XMM-DR5catalogue, leaving285205usabledetections. These remainingdetections are associatedwith219788uniquesources and are drawn from 4802 XMM-Newton observations (see Fig.1). It should be


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emphasized that although almost half the detections in 3XMM-DR5 are removed from3XMMeas a result of this cleaning process,most of the rejected detections are perfectlyvaliddetections.Thepurposeofthiscleaninghasbeentomaximisethequalityandaccuracyofthedetections(anduniquesources)fortheARCHESproject.

1.3.3 Asimultaneousmulti-catalogueprobabilisticcross-matchingtool

Wehave been developing a generic and flexible toolwhich performs potentially complexmulti-cataloguecross-matchesandwhichcomputesprobabilitiesofassociationbasedonanovelstatisticalframework.

It should be stressed that this developmentwas a theoretical challenge since only sparseliteraturerestrictedtothetwocataloguescaseexistedatthestartoftheproject.Apartfrombeing able to process an undeterminednumber of catalogues, the tool had to be flexibleenough so as to handle complex list selections on entry, cope with the heterogeneity ofastronomical catalogues and be able to deal with various cross-matching algorithms.Another issue was computing efficiency that required the implementation of specificindexationtrees.

The complexity of the task and of the hardly predictable progress rate inherent to R&Dactivities led us to adopt an iterative development scheme and to provide incrementalreleases of the tool. Test and validation, both from artificial catalogues and from actualcross-matched multi-wavelength catalogues used in the framework of the science cases,providedinstrumentalandvaluablefeedbacktothesoftwareandtheoreticaldevelopmentofthetool.

Thefirsttaskhasbeentoderiveacriterion,drawnfromstatisticalconsiderations,tobeusedto select a list of potential counterparts to a given source within a set of catalogues. Inaddition to the criterion applied on the full set of catalogues at one time, we havedemonstrated mathematically that the selection can be performed iteratively, i.e. onecatalogueata time,anddoesnotdependon the inputorder: it isbothcommutativeandassociative.

Thecriterion isbasedonthepositionaluncertaintiesofeach individualsource.Hence, thesearchradiiontheskydependoneachcandidateofeachcatalogue.Tobeabletoperformsuch queries efficiently,we conducted a review of the literature in the field of computerscience. We have studied, implemented and compared several data structures beforechoosingtheonewhichbestfittedourrequirements.

Thecurrentversionofthesoftwarecontainsmorethan25,000linesofcode,implementingseveralalgorithmstocomputeprobabilitiesuptoanarbitrarynumberofcataloguesatthesametime.


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Figure2:TheWebinterfacetotheARCHEScross-matchtool.

ThetoolrunsasawebserviceonamachinehostedinStrasbourg.Onatechnologicallevel,itmakesuseofJavaEEwithaTomcatServlet-EnginerunningbehindanApacheHTTPserver.Thesoftwarerunsbothfromacommandlineinterfaceandfromawebinterface(seeFig.2)implementingamoreuser-friendlyinputoftheparameters.Itsessentialfunctionalitiesare;i) to load a data table from a file, from the VizieR CDS server, from a service using a VOprotocol or available through a given URL, ii) tomanipulate the loaded tables e.g. selectcolumns, create new synthetic columns, addmetadata, remove rows: one can select thesubset of data relevant for their purpose and reject some sources applying potentiallycomplex constraints based on scientific considerations; iii) select the data scientificallyrelevantforthecross-matchtobeperformedinawayflexibleenoughtochangeunitson-

ARCHES X-MATCHTOOL

Anonymous Web form Info about this page.

RemotedirectoryUpload afile:

File list:

X-match scriptScript examples

Type, modify or copy/paste here the xmatch script to be executed:

Result log

##############################################################################

# Name: galex_sdss_2mass.xms

# Description: Perform a probabilistic xmatch between galex, sdss and 2mass

# in a given cone of 12 arcminutes. Data is downloaded from VizieR.

# Input files: none

# Output files:

# - galex.vot: galex data

# - sdss9.vot: sdss data

# - 2mass.vot: 2mass data

# - galex_sdss_2mass.vot: cross-match result

# WARNING: the result may not be symetric using successive full joins

##############################################################################

# Load galex data from VizieR

get VizieRLoader tabname=II/312/ais mode=cone center="174.10491 +7.22343" radius

set pos ra=RAJ2000 dec=DEJ2000

set poserr type=CIRCLE param1=0.6

set cols objid,/.*J2000/,/(e_)?[FN]UV/

prefix galex_

save galex.vot votable

# Load sdss data from VizieR

get VizieRLoader tabname=V/139/sdss9 mode=cone center="174.10491 +7.22343" radius

where mode==1 && e_RAJ2000>0.0 && e_DEJ2000>0.0 && rmag<23

set pos ra=RAJ2000 dec=DEJ2000

set poserr type=RCD_DEC_ELLIPSE param1=e_RAJ2000 param2=e_DEJ2000

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the-flyoraddsystematics,iv)chooseoneofthe14cross-matchalgorithmsplusoneofthe10waystojointwotablesandv)setthewaytherelevantinformationismergedtobereadyforthenextcrosscorrelation.

AnadditionalsoftwarewasdesignedtogroupthevariousXMM-Newtonfieldsofviewintoastrophysicallyhomogeneousregionssoastobeabletoderivesensibleprobabilitypriors.

The tool covers a large range of possibilities and allows to test various scenarios beyondthose strictly required for the project butwhichwere important for testing purposes andwerefeltasavaluableandcheapextensionofthecapabilitiesofthetoolthatmayfurtherenlargeitsusability.ForARCHESpurposesweareessentiallyusingboththechisquareandthesimpleconesearchalgorithms(neglectingpropermotions)makingtheLEFTJOINofallcataloguesstartingwithXMM.

Although it is theoretically feasible,we raised a point about the practical computation ofprobabilities when cross-correlatingmore than 6 or 7 catalogues: a combinatory analysisdemonstratesthatthenumberofhypothesistobeconsideredforasinglesourceincreasesdramaticallywiththenumberofcatalogues.

WehavedevelopedanoriginalworkbasedonBayesianprobabilities:forthefirsttimetheeffectof theselectioncriteriahasbeen introduced in thecomputationofprobabilities fortwo catalogues cross-matches.Wehave then resorted toMonte-Carlo simulations to testtheequationsderivedforthetwocataloguescaseandtoextendthemtothreecatalogues.The candidate selection of the simulated catalogues has been performed using the firstversionofthereleasedtool.Hencewehavecross-validatedboththelateroneandthenewtheoretical developments. We have also looked for mathematical simplifications to copewiththecomputationallyextensiveproblemofpriorestimation.ThesolutionwehavefoundreducesanO(NM)problemintoanO(N)+O(M).

Toourknowledge,itisthefirsttoolallowingtocross-correlate,inasinglepass,morethantwo catalogues containing individual elliptical errors with a coherent statistically basedselectioncriterion.

Together with the Integrated Cluster Finder, The ARCHES multi-catalogue cross-matchingtool is at the heart of the ARCHES legacy. It provided multi-wavelength spectral energydistributionsformorethan200,000X-raysourcesextractedfromthe3XMMDR5catalogue.Twomaincatalogueshavebeenproduced,oneall-skyandanotherversionrestrictedtotheGalacticPlane.All-skySEDsarebasedonGALEX5,UCAC4,SDSSDR9,2MASSandtheAllWISEwhiletheGLIMPSEcatalogueisusedat lowGalactic latitudes. Inaddition,candidatesfromtheradioSUMSS,NVSSandFIRSTandfarinfraredAKARIFIScatalogueswereselectedbasedonachi-squarecriterion.


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Figure3:AgraphicalrepresentationofthespectralenergydistributionofanX-raysourceextractedfrom the 3XMMe catalogue. Among other information, the page lists the names of the archivalcataloguesfromwhichthevariousfluxesareextractedaswellastheoverallprobabilityofthetotalcombination(here98%).

1.3.4 Creatingspectralenergydistributions

OneofthemainARCHESobjectiveswastoproduceascientificallyvalidated,VO-compliantsetofspectralenergydistributionsoftheobjectsincludedintheenhanced3XMM-NewtonSerendipitous Source Catalogue (see Fig. 3). Transforming magnitudes and errors intoabsolute fluxes, errors and determining centralwavelengths, all was performed using theSpanish Virtual Observatory Filter Profile Service. In addition, a database was created inorder to test and validate the SEDs and provide a world access to these data byimplementingVOprotocols.


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1.3.5 Anintegratedclusterfinder

One of the ARCHES’s objectives was to develop a software tool, dubbed the IntegratedClusterFinder(ICF),abletosearchforgalaxyclustersatthepositionoftheextendedX-raysourcesregisteredintheXMM-Newtoncatalogue(andvirtuallyinanydirectionofthesky)usingground-andspace-basedmulti-wavelengthimagingandspectroscopicdata.

Extended X-ray sources located at high galactic latitudes are the tracers of clusters ofgalaxies. X-rays are emitted by the hot intergalacticmatter trapped in the deep potentialwellprovidedbythedarkmattermassassembly.Whileclustersofgalaxiesaresingleentitiesat X-ray wavelengths they appear as a group of objects at optical/infrared wavelength.There,onlytheindividualmembergalaxieswithlargelyidenticalredshiftcanberecognized.While the galaxies do not play amajor role in themass budget of a cluster, they are ofutmostimportanceforassessingtherealityoftheclusterthroughameasuredover-densityofgalaxiesandforredshiftdetermination.Thefirstaspectisimportanttosafeguardagainstspurious extended sources, based e.g. on imperfections of the telescope optics or of thedetection process. The cosmological redshift is imprinted into spectral features of themember galaxies and/or the colour of themember galaxies and those properties are thebasisofthedetectionprocesswiththeICF.

The ICF was used to make the important step from a catalogue of detections in multi-wavelengthdatatoascience-gradecatalogueofgalaxyclusters.

We restrict ourselves to high Galactic latitudes in order to avoid problems with sourceconfusionintheGalacticplaneandtoavoidproblemsduetosourceextinctionintheMilkyWay.

TheICFimplementsaredMaPPer-likealgorithmtosearchforclustersinthespacespannedbythepositionsandthecoloursoftheirmembergalaxies.Amajordifferencewithrespecttothe published redMaPPermethod is that prior information on the position of the clusterfromthedetectedX-raypositionisintegratedinourmethod.

Theclusterfindingapproachisbasedonthefactthatluminousredgalaxies(LRGs)have(onthe average) different colours at different redshifts. From a calibrated redshift-colourrelationonecanthusestimatetheredshiftofamembergalaxyand,viasummationoverallpotentialmember galaxies, the redshift of the cluster. The algorithm contains threemainsteps: i) calibrationof the redshift-colour relation: for a chosen setof external catalogues(e.g. SDSS, UKIDSS, AllWISE) one obtains average colours and colour-colour covariancematricesforeachredshift.AnalternativeversionoftheICFthatusespre-fabricatedvaluesofphotometricredshifts(likethoseprovidedwithSDSS,CFHTLSorALHAMBRAcatalogues)hasalsobeendeveloped, ii)estimationof thebackgrounddensity tobe incorporated intothe determination of a multiplicity (abundance of objects) at the cluster position and iii)


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clustersearchproper: Identificationofpossiblemembersandestimationof theredshiftofeachcluster(seeFigs.4&5).

Figure 5: Corresponding finding chart. Coloured 2’ by 2’ SDSS image overlaid with XMM X-raycontours.Redcircle:X-raysourcepositionandextent.Redcrosses:point-likeX-raysources.Yellowand light blue circles: likely clustermemberswith spectroscopic redshift indicated by purple circleandlabelwherepossible.

Figure4:Measureoftheprobabilityoffindingagenuineclusterversusredshift


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Data from various input catalogues in a circular field of radius R = 8 arcmin are acquiredaroundthepositionofeachextended3XMMesource.Therefore,ourapproachisinefficientforthedetectionofclustersatlowredshiftasthoseappearlargerthan8arcminonthesky.Thisradiuscorrespondsto1Mpcco-movingradiusatredshiftz=0.12.Wenote,howeverthatthislimitationdoesnotquestionthevalidityofoursearch,asmostnearbyclusters(z<0.12)arealreadyknown.Also,bright,nearby(henceveryextended)clustersarenotreliablydetected as single entities by the X-ray source detection chain and are thus partiallyscreenedawaybythefiltersappliedtogenerate3XMMe.

TheICFhasbeentestedsuccessfullyagainstseveralsamplesofidentifiedclustersofgalaxies.Appliedtotheenhanced3XMMcatalogueproducedbyARCHES,theICFyieldedacatalogueofclustercandidateswith481detections.

1.3.6 Testsciencecases

Asetof sevendistinctpilot sciencecaseswereselectedat thebeginningof theproject inordertoinvestigatetheusabilityofARCHEStoolsandproductsinarangeofsciencethemesfrom planetary formation to cosmology. ARCHES designed a solid testing and validationprogramme which guaranteed the quality and robustness of the tools. However, asanticipated in the project, using ARCHES products in the framework of science casesprovidedstrongfeedbackwhichallowedustoaddnewfeaturesandrevealedsubtleissuesthat would have naturally escaped the scrutiny of themain stream testing activities. Forinstance,AGNstudiesuncoveredanotableproblemaffectingastrometryinthe3XMM-DR4catalogue. This problem was conveyed to the Survey Science Centre, the consortiumresponsiblefortheproductionoftheXMM-Newtoncatalogues.

1.3.6.1 ActiveGalacticNuclei(AGN)

TheAGNsciencecasesencompasstwopathsofinvestigations,acharacterizationofthemulti-wavelengthpropertiesofobscuredAGNandastudyoftherelationbetweenjetandoverallAGNpropertiesinradio-loudobjects.

i)ObscuredAGN

WehaveconcentratedonusingARCHES tools to trace theobscuredAGNphenomenon inthe optical, X-ray and mid-infrared (MIR) regimes and to compare the obscured AGNpopulationsidentifiedatdifferentwavelengths.

We have used sources in a subset of 3XMMe fields away from the Galactic plane andcompletelycoveredbytheSloanDigitalSkySurvey(SDSS).Inthesefields,X-ray(X),SDSS(S,optical) and WISE (W, infrared) were cross-correlated, building source samples havingdifferentcombinationofassociationprobabilitiesbetweencatalogues(seeFig.6).Theuseof


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theARCHEScross-correlation toolhasbeen instrumental in thisendeavour, since itallowsmatching three catalogues providing full probability information in all combinations. WehavethenusedonlythoseSDSSsourceswithsignificantandluminous[OIII]5007Åemission,to selectAGN (althougha contributionof strong star formation -SF- could also contributesubstantially).

Figure6:Selectionofsources inX-ray(X),optical(S)andinfrared(W):theaxesareprobabilitiesofassociation so that the red volume indicates the sources with high probability (>90%) of beingdetectedinthethreebands;thegreenareashowsthesourceswithhighprobabilityofSXassociation,but no W detection (<10%); the blue area highlights the sources with high probability of SWassociation, but no X detection. This allows investigating what types of AGN are preferentiallydetectedineachband,togaininsightintotheirintrinsicproperties

FortheX-raysourceswithSDSScounterpartsbutnoinfrared(W)match,weobtainedMIRfluxes using the published forced photometry on the SDSS positions and for the sourcesmatchingboththeSDSSandWISEbutvoidofanyX-raydetection,weobtainedX-rayupperlimits from theFLIX server.We finally cross-correlated the three sub-sampleswith2MASSandUKIDSStoobtainnear infraredphotometry.WehavefittedtheSEDsanddevelopeda


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method to obtain X-ray spectral information from the 5-band count rates in the 3XMMecatalogue.Theresult isa largesampleof>1500objectswithwideanduniformoptical-to-MIRSEDandX-rayspectralinformation.OurfirstresultisthattherearealmostnoAGNthatareundetectedinMIR/WISEatthetypicaldepthsof3XMMe.

In the firstplace,weuse theBaldwin,Phillips&Terlevichdiagram that isessentiallya2Dplotofratiosoftwopairsofnarrowemissionlines.MostsourcesdetectedinX,SandWareconsistent with AGN while those not detected in X-rays are likely star forming galaxies.However,someofthenonX-raydetectedsourcesareintheAGNregion.TheX-rayspectralinformationshowsthatthiscouldbebecausetheyareabout0.5dexlessX-rayluminousfortheirMIRluminosityorbecausetheyareabsorbedbytypicalcolumndensitiesof~1024cm-2.

Figure 7: Selection of AGN using MIR-colours, showing essentially the logarithms of the ratiosbetweenWISE bands (2nd and 3rd band along the X-axis and 1st and 2nd along the Y-axis). ThedashedgreylinedelimitstheareawhereAGNareexpectedtolie(Mateosetal.2012,thisproject).The colourof the symbols correspond to theMIR luminosityand showclearly that this criterion iseffective in selecting luminous AGN, but fails to select less luminous ones, probably because thecontributionfromtheirhostgalaxieschangetheirMIR-colours

WehavealsoexaminedanalternativemethodtoselectAGN,whichusesMIRcoloursandisbasedontheeffectivepower-lawshapeoftheSEDofAGNinthatband.Againasexpected,mostsourcesdetectedinS,XandWareintheAGNregionandmostofthosenotdetected


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inX-rayareoutsideit.OurmultiplecriteriatodefineAGNhavealsoallowedustoestimatehowefficientistheMIRAGNselectionmethodasafunctionoftheMIRluminosity.

Finally,wehavecomparedthenumbersofsourcesclassifiedusingeachofthetwocriteriaabove(plusathirdonerelatedtotheintrinsicX-rayluminosity: if it isabove1042ergs-1 inthe2-10keVband,thesourcemustbeanAGN,becausethoseluminositiesareunattainablewithstarformingalone).

We have concluded that, for serendipitous XMM-Newton surveys, the combination ofcataloguesandwavelengthsthatisbestsuitedforAGNstudiesisSDSSintheoptical,WISEinthe MIR and UKIDSS in the Near-IR, combined with 2MASS in the latter band for thebrightest sources and/or for wider coverage. We have also used a variety of SED-fittingmethodsbut,intheend,wehavedecidedtodevelopourownBayesianmethodinPython,using the CIAO-Sherpa package and some Markov Chain Monte Carlo libraries, whichcombined a minimum of indigenous code writing with flexibility in the choosing of thetemplatelibraries.

ii)Radio-loudAGN

We have also compiled and exploited a sample of radio-loud AGN, in particular,demonstratingthevalueofradioemissiontoidentifythepresenceofAGNwherethehostgalaxyemissiondominatesinthemidInfrared.

Using theARCHEScross-matching tool,webuilt theMIXR (Mid-Infrared,X-ray, andRadio)sample by combining theWISE, 3XMMe and FIRST+NVSS source catalogues. MIXR is thelargest, uniform sample to date at these wavelengths, covering a wide range of galaxyproperties,fromstarbursttoquasars.WithourselectionwecanidentifyAGNactivityeveninsourceswherethehostemissiondominates,andefficientlydiagnosestarformation,thusallowingustoderivereliablediagnosticclassificationsthatcanbeusedinothersamples.Thestudysoughtto investigatetherelationshipbetweenradiativeandjetoutput inradio-loudAGN, and its implications for regulating mechanisms for the jet and long-term variabilitytimescales. The results show potential problems in our current understanding of therelationship between AGN and star formation activity: if both the radiative and the jetoutputofanAGNcanvaryby4-5ordersofmagnitudeontimescalesofafewmillionyears,andtheAGNinfluenceonthestarformationinitshostalsohappensinsimilartimescales,itmaynotbepossibletostudytherelationbetweenthembeforewebetterunderstandthelifecyclesofAGN.

Themain objectives of our study involved: i) using theMIXR sample to devise a series ofeffectivediagnosticsthatwillallowthecommunitytopre-classifyextragalacticsourcesevenintheabsenceofredshift,basedontheirradio,mid-IRandX-rayfluxes.Thiswillestablishabaselinethatmightfacilitatesourcetriagewhenthenextgenerationofinstruments(JWST,


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E-ELT,Athena,ALMA,SKA...) startproducingvastamountsofdata, ii)using redshifts fromSDSSDR12toverify theaccuracyof theearlydiagnostics,andexploreAGNactivityversusstarformationcontributioninsourcesdominatedbytheirhosts,examinetheapparentlackof correlation between kinetic (jet) and radiative output in radio-loud AGN, to drawconstraintsonitspossibleoriginanditsimplicationsontheaccretionpropertiesofAGN,andstudy the selection biases that arise from the selection methods in our sample, and inothers,particularlyAGNsampleswithamid-IR/X-rayselection.

1.3.6.2 GalacticSciencecases

WehaveworkedinfourindependentprojectsinordertolearnaboutthenatureoftheX-rayGalacticlandscape.

i)X-rayemissionmechanismsinthehighmassstarpopulationoftheGalaxy,windcollidingbinariesandGamma-Casanalogues

The nature of the low- to intermediate-luminosity (Lx~1032-34 erg s-1) source populationrevealedinhardband(2-10keV)X-raysurveysoftheGalacticplaneispoorlyunderstood.Toinvestigatetheirnature,wecross-correlatedtheXMM-Newton3XMM-DR4surveywiththeinfrared Two Micron All Sky Survey and Galactic Legacy Infrared Mid-Plane SurveyExtraordinaire (GLIMPSE) catalogues.We identified reliable X-ray-infrared associations for690sources.Weselected173sourceshavinghardX-rayspectra,typicalofhardX-rayhigh-mass stars (kT > 5 keV). Roughly 15 per cent of the hard sources are classified in theliterature: ~68 per cent as high-mass X-ray stars single or in binary systems (WR, Be andhigh-mass X-ray binaries - HMXBs), with a small fraction of G and B stars. An infraredspectroscopicpilotobservationattheWilliamHerschelTelescopeallowedustoidentifyfivehard X-ray sources with Wolf-Rayet stars, supergiant stars, Be Gamma-Cas analogues orpossibleinterlopers.Takingadvantageofthesuccessofthispilotsurveywestartedin2016anextendedobservingcampaigncoveringthecentralpartoftheGalacticdisc.

ii)AstudyoftheX-rayemittingWolf-Rayetstars

ThespacedensityofWolfRayet(WR)starsisstillnotwellconstrained.NoristhemechanismproducingcopiousX-rayemission insomeoftheseobjects.WhiletheexpectednumberofsingleandbinaryWRsintheGalaxyvariesfrom1200to6500,onlyabout640GalacticWRsareknownuptodate.Moreover,theoriginofthesometimes-observedhardX-rayemissioninWRsishighlydebated.Therearethreecompetingscenarios:1)intrinsicemission,whereinstabilities in the radiative wind could produce hot shocks 2) accretion onto a compactobject,or3)wind-windinteractioninabinarystar(WR+O,WR+WR).

InordertolearnabouttheX-rayemissionmechanismandtoconstrainthespacedensityofWRsweneedalargeandunbiasedsample.Forthatpurpose,wecross-correlatedthemostrecentcatalogueofWRsintheGalaxywiththeARCHEScatalogue.Toensurethatwehave


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the right X-ray counterpart for eachWRwe visually inspected the ARCHES SEDs and thefindingchartsforalltheWRshavinganX-raycandidate.WeinvestigatedthefractionofWRstars as a function of spectral type and whether this varies with X-ray activity. We alsoinvestigatedapossiblerelationbetweenX-rayfluxandorbitalperiodforknownWRbinaries.

Iii)ModellingofthesolartypestellarpopulationsinX-rays.

InstarssuchastheSun,X-rayemissioniscloselyrelatedtotheexistenceofconvectingcellswhose activity depends on differential rotation. Since stars spin down due to magneticbraking,X-rayemissionisagoodtraceroftheageofthestarsandrevealstheyoungerones.Theaimofthisstudyistoderivethemainpopulationpropertiesofyoungstars,theirspacedensity (toderive the local star formation rate), scaleheight (to constrain themechanismthatscattersyoungstarsawayfromtheGalacticdisc)andtoderivethe importanceoftheoldpopulationwhoseX-rayactivityismaintainbybinaryrotation.

Figure 8: Groups of identified active galactic nuclei (AGN, blue dots) & galactic stars (red dots)separatewellintheFx/Fir+IRcoloursspace.Sourcesofunknownnature(smallgreydots)UnknowncaneasilybeclassifiedinAGNorgalacticstarsusingforinstanceakerneldensitymethod.


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We selected sources in theARCHES cataloguehaving optical and infrared counterparts. Alearningsamplebasedonpublishedcataloguescontainingstarswithknownpropertieswascompiled.Makinguseofthis learningsample,andthroughaprincipalcomponentanalysis,we classified sources as either stars, quasars or galaxies (see Fig. 8). For stars, by fittingstellaratmospheremodelstotheobservedSED,wedeterminedthestellarparameters,suchaseffectivetemperatureandgravity.Wevalidatedtheobtainedresultsbycomparingthemwith spectroscopically determined values taken from the literature. Themodelling of thestellarX-raypopulationwillbedoneusingtheX-raycountmodeldevelopedbyGuilloutetal.1996 and based on the evolution synthesis population model from Besancon. This willprovideuswiththesurfacedensityofsourcesdetectedasafunctionofX-rayflux,ageandspectraltype,atanydirectionoftheGalaxyasafunctionofscaleheight,stellarformationrate,etc...tobecomparedwithourobservations.

iv)Circumstellardiscsaroundlate-typestars

Young late type (F-M) stars are known to be copious X-ray emitters. Their X-ray emissionarisesfromthestellarcorona,anditisdirectlyrelatedtotherotationperiodofthestar.Thefastrotationisusuallytheeffectoftheheritageoftherotationoftheparentalcloudfromwhichthestarwascreated,duetoangularmomentumconservation.

Whilegasdiscsarefoundaroundyoungstarsastheydissipateafter10-20Myr,debrisdiscs'remainwithlifetimesspanningoverGyr(e.g.theKuiperBeltintheSolarSystem).Althoughtheemissionofdebrisdiscsdependsonseveralparameters,itisexpectedthatthefractionalemissionofadebrisdiscdecreaseswithstellarage.Inthiswork,weusetheX-rayluminosity(Lx/Lbol) to calculate the stellar age andwe search for (expected) relations between thestellardiscsandthestellarage.

Atotalof108,037sourcesnotaffectedbybrightstarorgalaxyflagwereselectedfromtheARCHES catalogue and we cross-correlated them with UCAC4 to obtain proper motioninformation.AfterimposinggoodphotometricqualityandastarflagintheUCAC4catalogueweobtained>10,000objects.Wethenselectedonlythosewithsignificantpropermotions(pm>3σpm),obtainingasampleof~5800galacticcandidatesources.

WeusedtheVirtualObservatorytoolVOSAtoidentifyinfraredexcessin~600candidates.Inordertodiscardanysourceknowntobenotasinglestar,wecross-matchedoursamplewiththeSIMBADdatabase.154objectswereremovedfromthesample.

Stellaranddiscparametersoftheremaining~400sourceswerederived.Theseparametersarepresentlybeinganalysedbeforeobtainedthefinallistofbona-fideyoung,late-typestarswithdebrisdisc.


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1.3.6.3 Clustersofgalaxies

TheIntegratedClusterFinder(ICF)wasusedtogenerateacatalogueofclustersbasedontheenhanced 3XMM catalogue. The very first important test to be performed was therobustnessoftheICFredshiftdeterminationwithrespecttoreferenceclustersampleseithercollectedinthisprojectoffoundintheliterature.TheICFpassedthistestwithaconfidencebetween95%and98%(seeFig.9).Clustersuptoredshiftonewerereliablyrecoveredfrompublishedsamples.

Figure9:Comparingtheredshiftsof3XMMclusterscandidatesidentifiedbytheARCHESIntegratedClusterFinderwiththosederivedinformerworks,herethecatalogueofTakeyetal.2013.

ClustercataloguesbasedontheSZ-effect fromthePlancksatelliteor fromtheSouthPoleTelescope became available during the course of the project. These catalogues containpredominantlymassive clusters, given the sensitivityof the current SZ-instruments.Newlydiscovered XMM-Newton clusters on the relatively small survey area however aremainlylowmassobjects.TheoverlapbetweencurrentSZ-clustercataloguesandthosefromXMM-Newton is small, just five clusters were found jointly in both catalogues. The overlap isexcessivelysmalltoderivemeaningfulconclusionsfromacomparison.

The behaviour of the ICF with respect to false positives and to completeness wascharacterized. A paper describing the method of cluster identification, redshift


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determination togetherwith a description of the newly established cluster cataloguewassubmittedtoA&A.

Foralldetectedclustersbasedontheenhancedversionofthe3XMM-DR5cataloguefindingchartswereproduced.TheseshowX-raycontoursontopofanopticalimagefromtheSDSSsurveywithlikelymembergalaxiesoftheclustermarkedaswell.

The X-ray images of all new cluster candidates were inspected and the X-ray spectraextracted. X-ray spectral fits were performed for those clusters with reliable redshiftinformationtodeterminetheclustertemperatureandtheclusterluminosity.

A luminosity-temperature diagram was generated and various strategies were tested tooptimally fit the underlying relation taking biases into account. At the same time, adedicated follow-up program for high-redshift clusters beyond the SDSS limit has startedthatalreadyallowedustoidentify7clusterswithredshiftsbetween0.84and1.22.

1.3.7 DisseminatingARCHESproductsARCHESsuccessalsorestsonthequality,userfriendlinessandefficiencyoftheinterfacestodata.ARCHESdata canbeaccessed in four flavours, as flat files, through specific and richinterfaces designed by the project, through the Virtual Observatory, and in 2016 throughstandardservicesattheCentredeDonnéesastronomiquesdeStrasbourg(CDS).Bothcross-correlatedcataloguesandtheenhanced3XMMcataloguescanbedownloadedascompressedVOtablesfromtheARCHESwebsite.ARCHESdesignedaspecificinterface,theArchesDB,tobrowse,exposeandselectthecross-correlatedcatalogues,theresultingspectralenergydistributionsandthecatalogueofclustercandidates createdbyapplying the IntegratedCluster Finder toextendedX-ray sources inthe enhanced 3XMM catalogue (see Fig. 10). The ArchesDB is an extension of the 3XMMinterfaceoftheSSC,theXCatDB,augmentedwithARCHESdata.Consequently,theArchesDBproposesarichWebinterfaceenablingtheuserstorunverycomplexqueriesandtoeasilybrowsedatathankstonumberofpreviewsofspectra,SEDs,lightcurves,etc...

Thespectralenergydistributions(SEDs)arealsomadeavailablethroughanarchiveinterfacedevelopedbySVO,namelytheCAB-INTAdatabase.

Theenhancedcatalogueandthecross-matchedcatalogueswillalsobepublishedinVizieRatCDS in2016,awaiting the releaseof thescientificpublications.SEDswill alsobestored inVizierinordertoincludetheminthelong-termpreservationpolicyoftheCDS.


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A number of VirtualObservatory interfaces are implemented. The catalogue is publishedintotheVOassimpleconesearchresources(CSP)bytheArchesDBandsooninVizierasanyotherViziercatalogue.TheSSAPVO interface (SimpleSpectrumAccessProtocol) interfacefortheSEDscomeswiththeSVOarchiveandfromVizier inthenearfuture.TheArchesDBoffersaTAP(TableAccessProtocol)accesstotheARCHESDatawithanObsTap(datamodeluses for data discovery) implementation. Amulti-scaled X-ray image (HIPs) covering theARCHESskyhasbeenmadeavailablethroughAladin,theVOskyatlas.Itcanalsobeusedtohelpbrowsingthedataandselectingregionsofinterestonothersinterfaces.

Outreach:

Apart from outreach pages exposed on the ARCHES web site, the project developed anoriginalandversatileoutreachdevicedubbedasthe“ArchesWalker”.Thisprojectaimsathelping the public to discover by themselves different aspects of the ARCHES scientifictargets.TheArchesWalkerisbuiltonthetopofadatacorpuscontainingthedescriptionofasample of sky objects relevant for the ARCHES science. The user can select and displayobjects in variouswavelength. He/she can also explore their neighbourhood or get sometextual data. Two interfaces are available so far: a Web application included within theARCHESWebsite,andadeviceintendedtobeusedonexhibitionboothsthatuseatabletasaremotecontrollerforthedisplay(seeFig.11).

Figure10:ScreenshotoftheArchesDatabase.Theinterfaceallowstheusertoselect3XMMesourcesbased on simple and complex criterions. For each selected entry, the interface displays thumbnailsgivingaccesstotherelevantdata(spectralenergydistributions,findingchartsinseveralbands,X-rayimages, X-ray spectra, X-ray time series, etc..). Source parameters and identifications at otherwavelengthsarealsolisted.


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Figure11:Ayoungfutureastronomerdiscoveringthebeautyofthemulti-wavelengthskyusingtheARCHESwalker.


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1.4Potentialimpact

TheobjectiveofARCHESwastobuildscientifically-validatedspectralenergydistributionsforthemanystars,galaxiesandclustersofgalaxiesdetectedbytheESAX-rayspaceobservatoryXMM-Newton.Thesemulti-wavelengthenhanceddatasetswillgreatlyfacilitatetheopeningof new avenues of investigation and therefore need to bewidely advertised. By bringingtogetherexpertisefromleadinginstitutesinthefieldofmulti-wavelengthanalysis,ARCHEShas opened to investigation new exciting domains of research and will very significantlyincreasetheoverallscientificreturnofthishighlysuccessfulEuropeanspaceobservatoryatamodestcost.

ARCHESdataandproductsaredistributedtotheinternationalcommunitythroughavarietyofchannelsthataltogetherwillunfoldtheimpactofARCHESwork.ARCHEScross-correlatedcataloguesandspectralenergydistributionsarepublishedintheVirtualObservatorythatisbecomingastandarddataaccessmode for theastronomicalcommunity. Inparallel, thesedata can be accessed through the ARCHES web site, through dedicated interfaces (theArchesDB and the CAB database) exposing in a handy manner ARCHES data and theirrelationstootherdatabases.Frommid-2016onARCHESdatawillbealsoaccessiblethroughtheViziercatalogueserviceoftheCentredeDonnéesastronomiquedeStrasbourg(CDS),aworldreferenceforastronomicaldatacurationanddistribution.

As far as tools are concerned, the Integrated Cluster Finder and the ARCHES cross-correlationtoolareinopenaccessonaserverlocatedandmaintainedinStrasbourg.Moreimportantly, the simultaneousmulti-catalogue cross-matching programwill be offered bymid2016asanoptioninthesuccessfulcross-matchingservicedevelopedatCDS.ThisWebservice isusedworldwideandaccessible through themainastronomicaldataanalysisandhandlingsoftwaresuchasTOPCAT.

TheXMM-NewtonsatelliteisthemostscientificallyproductiveEuropeanX-rayobservatoryeverflownandiscurrentlyoneoftheflagshipsoftheEuropeanSpaceAgency'sastronomicalprogramme. On board consumables allow operations to be pursued until 2025 providedgroundsegmentfundingremainsclosetothecurrentlevelandprovideddetectorsarekeptingoodhealth.KeepingthisX-raysatelliteinoperationaslongastechnicallypossiblewouldallow theEuropeancommunity tominimize thegapbetweenXMM-NewtonandATHENA,thenextlargeEuropeanX-raytelescopetobelaunchedaround2028.

In parallel, the German-Russian eRosita X-ray telescope scheduled for launch in 2017willcarryoutthefirstwideenergyrange(0.5-10kev)all-skysurvey,thusprovidinganorderofmagnitudemoresourcesthantheROSATsurveyoperatedinthenineties.


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ARCHES products already constitute a solid basis for carrying out forefront astrophysicalresearchusingdataaccumulatedduringthefirst15yearsofXMM-Newtonoperations.

However, ARCHES’s impact will very certainly extendmuch beyond the date of productsrelease.Fromtheverybeginning,oneofthemainconcernsoftheprojectwastoensurethatenough expertisewould remain close to the participating institutes so as tomaintain thetools in operation and possibly develop them further in order to implement newapplications. As stated above, the ARCHES probabilistic cross-matching tool will be soonincluded in the arrayof CDSweb services under the responsibility of the codedeveloper,recentlyhiredonafixedposition.Althoughthesituationis lessclearfortheICF,therearegoodprospectstokeepareasonablelevelofmaintenanceintheforthcomingyears.

It is importanttonotethattheICFisnotrestrictedtoXMM-Newtondata. Infact,thetoolcanbeusedatvirtuallyanylocationofthesky. IthasbeenthereforeenvisagedtousetheICFtodetectnewclustersofgalaxiesintheformerROSATall-skysurveyandintheeRositaall-skysurveythatwillbereleasedaround2020.

ThesameremarkappliestotheARCHEScross-matchingtool.BeingnotspecifictoX-rays,thealgorithmoffersawiderangeofpotentialapplications.ProposedasaworldwideaccessibleCDSservice,itisexpectedtoplayamajorroleforbuildingthespectralenergydistributionsof thebillionsofastronomicalobjects thatwillbeharvestedat thehorizon2020byGAIA,EUCLID,theLSST,SKA,etc.…


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ListofARCHESrefereedpublications

- “InfraredidentificationofhardX-raysourcesintheGalaxy“,A.NebotGómez-Morán,C.Motch,F.-X.Pineau,F.J.Carrera,M.W.Pakull,F.Riddick,2015,MNRAS,452,884;DOI:10.1093/mnras/stv1020

- “The2XMMi/SDSSGalaxyClusterSurvey.III.ClustersassociatedwithspectroscopicallytargetedluminousredgalaxiesinSDSS-DR10”,A.Takey,A.Schwope,G.Lamer,2014,Astronomy&Astrophysics,Volume564,id.A54,19pp,DOI:10.1051/0004-6361/201322973

- “UncoveringobscuredluminousAGNwithwise”,S.Mateos,A.Alonso-Herrero,F.J.Carrera,A.Blain,P.Severgnini,A.CaccianigaandA.Ruiz”,2013,MNRAS,434,941;DOI:10.1093/mnras/stt953

- “The2XMMi/SDSSGalaxyClusterSurvey.II.TheopticallyconfirmedclustersampleandtheL_X-Trelation”,A.Takey,A.Schwope,G.Lamer,2013,Astronomy&Astrophysics,Volume558,id.A75,17pp,DOI: 10.1051/0004-6361/201220213

- “TheXMM-NewtonBrightSurveysampleofabsorbedquasars:X-rayandaccretionproperties“,Balloetal.,2014,MNRAS,444,2580;DOI:10.1093/mnras/stu1628

- “ExploringtheactivegalacticnucleipopulationwithextremeX-ray-to-opticalfluxratios(fx/fo>50)”,DellaCecaetal.2015,MNRAS,447,3227;DOI:10.1093/mnras/stu2665

- “Submm-brightX-ray-absorbedQSOsatz˜2:insightsintothecoevolutionofAGNandstarformation”,Khan-Alietal.2015,MNRAS,448,75;DOI:10.1093/mnras/stu2719

- “Revisitingtherelationshipbetween6μmand2-10keVcontinuumluminositiesofAGN”,Mateosetal.2015,MNRAS,449,1422;DOI:10.1093/mnras/stv299

- “WISEcoloursandstarformationinthehostgalaxiesofradio-loudnarrow-lineSeyfert1”,Caccianigaetal.2015,MNRAS,451,1795;DOI:10.1093/mnras/stv939

- “TheIntegratedClusterFinderfortheARCHESproject”,Mintsetal.2015,A&A,Submitted.


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OtherARCHESrelatedcontributions

- “AstronomicalResourceCross-matchingforHighEnergyStudies”,posterbyC.MotchattheADASSXXVconferencethattookplaceinSydneyon25-29October2015.ASPinpress

- “Radio-loudAGNthroughtheeyesof3XMM,WISEandFIRST/NVSS”,talkbyB.Mingoatthe"DemographicsandenvironmentofAGNfrommulti-wavelengthsurveys"conferencethattookplaceinChiana(Crete)on21-24September2015.

- “The3XMM-DR4ofWolfRayetstars”,talkbyA.NebotattheInternationalWorkshoponWolfRayetStarsinPotsdam,1-5June2015.

- “TheARCHESproject”,posterbyMotchetal.,AstronomicalDataAnalysisSoftwareanSystemsXXIV(ADASSXXIV),Proceedingsofaconferenceheld5-9October2014atCalgary,AlbertaCanada.EditedbyA.R.TaylorandE.Rosolowsky.SanFrancisco:AstronomicalSocietyofthePacific,2015.,p.437

- “Towardsanext-gencataloguecross-matchservice”,talkbyPineauF.X.;Boch,T.;Derriere,S.andtheArchesConsortium,AstronomicalDataAnalysisSoftwareanSystemsXXIV(ADASSXXIV),Proceedingsofaconferenceheld5-9October2014atCalgary,AlbertaCanada.EditedbyA.R.TaylorandE.Rosolowsky.SanFrancisco:AstronomicalSocietyofthePacific,2015.,p.61

- “Radio-loudAGNthroughtheeyesof3XMM,WISEandFIRST/NVSS”,posterbyB.MingoattheX-rayUniverse2014conference,16-19thJune,Dublin.

- “InfraredidentificationofhardX-raysourcesintheGalaxy”,posterbyA.NebotattheX-rayUniverse2014conference,16-19thJune,Dublin.

- “InfraredidentificationofhardX-raysourcesintheGalaxy”,talkbyA.NebotattheEWASS2014:EuropeanWeekofAstronomyandSpaceSciencetobeheldon30June-4JulyinGeneva,Switzerland.

- “TheARCHESproject”,posterbyC.MotchattheX-rayUniverse2014conference,16-19thJune,Dublin.

- “TheARCHESIntegratedClusterFinder”,talkbyA.MintsattheX-rayUniverse2014conference,16-19thJune,Dublin.

- “TestingtheunifiedmodelofActiveGalacticNucleiinX-rayselectedtype1andtype2quasars”,talkbyS.MateosIbanezattheX-rayUniverse2014conference,16-19thJune,Dublin.

- “OutreachoftheEuropeanARCHESproject”,talkbyL.MichelandA.SchaafattheIVOAmeeting,ESAC,intheeducationsession,Madrid,19-23May2014.


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- “MOCsinARCHES”,talkbyL.MichelattheVOInteropmeeting,heldinHawaii,27-29September2013.IthasbeenfocusedontheusefulnessofVOtoolstosortoutthecatalogueselection.

- “Radio-loudAGNthroughtheeyesof3XMM,WISEandFIRST/NVS”,talkbyB.Mingo,09-2014,Cambridge,UK(NewResultsinX-rayAstronomy).

- “BreakingAGNsampleparadigmswithFIRST/NVSS,WISE,and3XMM”,talkbyB.Mingoetal.2015,Llandudno,UKNationalAstronomyMeeting.

- “TheMIXRsample:Radio-loudAGNthroughtheeyesof3XMM,WISE,andFIRST/NVSS”,B.Mingoetal.,2015,“X-raysurveyswithadvancedmulti-wavelengthcross-identificationmethods”(ARCHESscientificconference),Paris,France,30Nov.-2December2015

- “DiscordantopticalandX-rayclassificationofAGN”,talkbyOrdovás-Pascualetal.2015,“HighlightsofSpanishAstrophysicsVIII”,ProceedingsoftheXIScientificMeetingoftheSpanishAstronomicalSocietyheldonSeptember8-12,2014,inTeruel,Spain,ISBN978-84-606-8760-3.A.J.Cenarro,F.Figueras,C.Hernández-Monteagudo,J.TrujilloBueno,andL.Valdivielso(eds.),p.274-279

- “ExploringXMM-ATLASwiththeARCHEStools”,talkbyCarreraetal.,2015,“X-raysurveyswithadvancedmulti-wavelengthcross-identificationmethods”(ARCHESscientificconference),Paris,France,30Nov.-2December2015

- “[OIII]emittinggalaxiesintheSDSS-dr10/3XMMe/WISEcross-correlation”,byRuizetal.,SpanishX-rayAstronomy2015,Santander,Spain,3-5June2015

- “[OIII]emittinggalaxiesintheSDSS/3XMMe/WISEcross-correlation”,talkbyRuizetal.,“DemographicsandenvironmentofAGNfrommulti-wavelengthsurveys”,Chania,Greece,21-24September2015

- ”[OIII]emittinggalaxiesintheSDSS/3XMMe/WISEcross-correlation“,talkbyRuizetal.,“X-raysurveyswithadvancedmulti-wavelengthcross-identificationmethods”(ARCHESscientificconference),Paris,France,30Nov.-2December2015

- “TheARCHESIntegratedClusterFinder”,talkbyA.Schwope&A.Mints,XMM-SSCConsortiummeeting#28,MSSL,Jan2015

- “TheintegratedClusterFinder”talkbyA.Mints“X-raysurveyswithadvancedmulti-wavelengthcross-identificationmethods”(ARCHESscientificconference),Paris,France,30Nov.-2December2015


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ListofARCHESdeliverables

- D2.2-Reportonthekickoffmeeting- D3.1-Enhancedversionofthe3XMMcatalogue- D4.1-Crosscorrelationtool- D4.2-Cross-correlatedcatalogue- D5.1-SEDtool- D5.2-SEDofXMMsources- D6.1-IntegratedClusterFinder- D6.2-Clustercatalogue- D7.1-Archivalcatalogues:selectioncriteriaandselectedlist- D8.1-Testandvalidationplan- D8.2-ValidationreportsonARCHESproducts- D9.1-AGNsciencecasereport- D10.1-Galacticsciencecasereport- D11.1-Clustersciencecasereport- D12.1-Personneltrainingreport- D13.1-InterfacetocataloguesandSEDs- D13.2-Reportondissemination- D13.3-ScientificWorkshop


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1.5Addressoftheprojectpublicwebsite

www.arches-fp7.eu

Coordinator:Dr.ChristianMotchObservatoireAstronomique11ruedel’université67000Strasbourg,FranceTel:+33368852428Fax:+33368852432E-mail:[email protected](mainbeneficiaries):

UniversitédeStrasbourg

Leibniz-InstitutfürAstrophysikPotsdam

UniversityofLeicester

UniversidaddeCantabria

InstitutoNacionaldeTécnicaAeroespacial(INTA)

Documents

1 Publishable summary - CORDIS · 1 Publishable summary 1.1 Executive summary Observational astronomy has dramatically evolved over the last 20 years as a result of the opening up