The Euclid Consortium Newsletter - Spring 2017

News from the Bridge ear EC members and colleagues.On the eve forts and I would like to thank and congratulate Dof opening the Euclid Consortium Annual them, on behalf of the the Euclid Consortium Meeting in London it is an immense pleasure Board, for their remarkable contributions to to see the vitality of the activities and the pro- the preparation of the mission. I have no doubt gress made since Lisbon last year. After the that with the recent release of the Euclid Flag- instruments’ Critical Design Review (CDR) pe- riods it is up to the payload module and then continue to grow and new superb results will the spacecraft to enter the CDR process that ship Simulation, the scientific activities will

satellite. As the Science Ground Segment and be shown again at the next Annual Meeting in will then provide the final shape of the Euclid- leadingBonn next person year. to Prior promote to open gravitational London, let wave me gressing very well, Euclid researchers have a missionsgive thoughts and toprepare Pierre e-LISA, Binetruy. but Pierre was alsowas a muchthe definition better understanding of the Euclid survey of the are overall also pro po- member of the Euclid Consortium and a most tential of the Euclid mission. It generated a active and enthusiastic supporter of the Euclid - - - verse . flourishing period of excellent and very inter mission and the exploration of the dark uni sortium addressing in great detail all points I wish all of you a very good Euclid Meeting in esting scientific papers from the Euclid Con London and take this opportunity to warmly mission, in particular the statistical analysis thank the SOC, Mark Cropper (chair), Libby regarding all scientific objectives of the Euclid of Euclid data, its performance and the Euclid Daghorn, Tom Kitching, Ofer Lahav, Bob Nichol, forecasts. These papers are listed in https:// Keith Noddle, Richard Massey, Andy Taylor, on www.euclid-ec.org/?page_id=817 and I rec- behalf of all members of the Euclid collabora- ommend you have a look at them. tion. As you will see during the London meeting Yannick Mellier many young scientists are involved in these ef-

From the editors elcome to the spring newsletter of the In order for Euclid to reach its goals, it is es- WEuclid consortium. We are happy to pro- vide with an update of many aspects of the thus in addition to the update from OU-EXT, we Euclid mission - in this issue the emphasis alsosential have that updates we get from the necessary the coordination external group data, is on the bedrock of the mission: the ground segment. We have updates from several of the And last but not least, we are welcoming the Science Data Centres, an update on the third arrivalfor external of Canada data andto the the consortium Javalambre and survey. Ray - Organisational Units. This newsletter also tribution. Scientific Challenge and update from three Carlberg also outlines their external data con hardware - both for the visible and the near-IR instruments,celebrates the so arrival the mission of the isfirst becoming Euclid moreflight Enjoy! Jarle Brinchmann & Stefania Pandolfi, real by the minute.

Contents News from the Bridge 1 Javalambre-Euclid Deep Imaging Survey 15 From the editors 1 OU-EXT 17 The EC Meeting 2017 In London 2 OU-LE3 18 3 19 First Euclid VIS detectors delivered 4 21 Update from ESA Project Scientist and Manager 5 OU-SPE 21 Euclid Developers’ Workshops 7 SocialThe Cluster media of presence galaxies SWG 22 The Sciencefirst NISP Data hardware Centres delivered 8 Weak Lensing Science Performance Verification 23 13 Scientific Challenge # 3 Canada joining the Euclid consortium The Euclid Consortium Newsletter - Spring 2017 T cluding EC memberDidaMarkovic.cluding delegates All by “Entropy” (https://tinyurl.com/lxyqqps) in- include a artandscience and will performance Lucie Green from UCL(http://luciegreen.com Prof.by eventhosted public a with end will day presentations from YannickMellier. The second and pleaseseeannouncementsregarding these The deadline for these contributions isMay 8th nary presentations to the whole conference. ian”(early career researchers) also provideopportunity for an “Young Euclid- workinggroups andOUs.Thesecond day will be arrangedings will by individualscience science and preparations. These splinter meet- meetings onavariety of key aspectsof Euclid The second daydedicatedbe will to splinter reflect onthepresent progress of Euclid. discuss forplans the rest oftheweek aswellas receptiona with allowing delegates to meetand end will day first The segment. ground science testing, surveyand operations, planning andthe lite construction, instrumentdevelopment and talksplenary cluding satelthe on-going about - provide comprehensivea update onEuclid, in- will day first the meetings, EC previous with As http://euclid2017.london and detailsfor the conference canbefound at planned splinter meetings. Registration is open as interactvia thenumerouswith colleagues latest informationthe mission, about as well the of learn to meeting the join to encouraged turalevents for delegates.EC members are All cul and scientific of diverseschedule and full a tohas arrangedand of theUK, city thecapital London (UCL) Science Laboratory (MSSL) atUniversity College the from Cropper Mark Prof. by The Monday June5thto Thursday June8th2017. The next EC meeting will be held in London from he E Local OrganisingLocal Committee (LOC) , chaired uclid , looks forward to welcoming you C onsortium Mullard Space M to make ple- eeting ) - 2017I . ok frad o scesu ad enjoyable and meeting. Pleaseregister successful assoonpossible. a to forward looks The LOCSOC welcomes and youto Londonand details onthewebsite. site. There are alsotravel and accommodation restaurants.Details and activities of variety wide a enjoy and city the exploreto delegatesfor opportunity great a Education in theheartof London. This provides The conference venue is the meetings. further talks from YoungEuclidians splinterand and final day of the meeting will be dedicated to thought-provokingentertaining.and The fourth model. The eventmological tois meant beboth cosmology and key issues withour present cos prominentof the status cosmologistsdebating eventbe released will include two soon, will but debate for conference delegates. Detailsofthis scientific special a with end will day third The programmebe provided will the conference.at tion of students. Morethis schools detailsabout genera- next the to technology and wonder science of the promote to helping experiments spectroscopicand scientist” “meet a include will tolel theECsplinter meetings.These activities hands-on activities at theconference in paral cal schools will beinvited to attend a range of meeting. During the morning, children from lo- EC an such at time first the for Day” “Schools a engagementcontinue ourpublic activities via Euclid, andsplinter meetings. The dayalso will providing more information on thestatusof talks, plenary of mixture a be will daythird The the public. are encouraged to attend alongside membersof on behalf ofthe Local Organising Committee n L ondo ak rpe ad o Nichol Bob and Cropper Mark can be foundbe can ontheweb- UCL Institute of - - An update from the ESA Project Scientist and Manager One very important spacecraft subsystem for tion, and data distribution. In the past years we Euclid is the K-band transponder. Operating at have been busy designing and developing the mission operations, science operations, and the science ground segment. This activity is very ofa transmission data in 4 hours. frequency This is ofunprecedented 26 GHz it enables for an a "human intensive" as the effort concentrates ESAscientific science data mission. rate of 74 One Mbps should providing realise 850Gbit that on system processes, interfaces, algorithms and without the availability of the K-band system software development. To make this a success Euclid would not be able to meet its survey re- we need a very good level of organisation and 2 a willingness by all individuals to make Euclid - quirements (15000 deg in 6 years) with the ist among the various parties. In that respect, required instrument pixel sizes and number of happen, since no contractual relationships ex The choice for the K-band introduced a number the science and IT challenges, currently on go- dithers per field. of technologies which are new for an ESA led ing, of the Science Ground Segment are good op- science mission. It demands a large on-board data storage which has been implemented with make improvements where necessary. Although portunities to experience the interactions and to the solid state mass memory (SSMM), using the interacting with many people working in differ- same hardware technology (Flash NAND) as is ent groups and often with different (cultural) used commonly in USB solid state memories. backgrounds can be tedious, it provides a lot of With a total end-of-lifetime storage capacity of 4 satisfaction to see people collaborating – despite Tbit, the SSMM guarantees a continuous storage - of data without ground contact for three days turn of Euclid. their differences – enabling the best scientific re during the nominal mission. The ESA ground By the end of this year we have to pass the stations in Cebreros and Malargue have been ground segment design review where among upgraded to support the K-band transmission, and the - thatother the review enormous objectives data westream have can to demonstrate be properly fer betweenCCSDS the spacecraft File Delivery at L2 Protocol and the (CFDP)ground processed.that the required The preparation survey can of be this performed review forces and stationhas been about introduced 1.5 million for sciencekm away. data The file protocol trans us to understand the operational activities after in combination with the SSMM is novel, and sup- launch beyond 2020, not only to scope the re- ports automatic retransmission of elements lost sources needed for operations, calibration and during the communications, as if we are doing data validation, but also to envision how the data will be used by the scientists, initially during the ground. proprietary period, and eventually after the data an ordinary FTP between the spacecraft and We mention the development of this (mostly) releases for the best usage by the worldwide sci- hardware to point out that it only makes sense in combination with proper survey planning, data René Laureijs and Giuseppe Racca entific community. handling and data processing, including calibra-

Satellite communication bands The K-band used for Euclid is very different from an astronomer’s K-band, near 2 µm, and be- longs to the set of L, S, C, X, and K bands used for satellite communication (see ESA’s overview). But note that the K-band itself (18–27 GHz) is not used due to water vapour in the Earth’s atmos-

phere - satellites use instead the Ku (12–18 GHz) or Ka bands (26.5–40 GHz). Euclid will use the

Ka band, also used by the Kepler spacecraft. The Euclid Consortium Newsletter - Spring 2017 F significant diffuse optical background (due background optical diffuse significant of presence the in benefit limited gives this Buried Channel (SBC)since Supplementary followingradiation There damage). isno (especially efficiency transfer for charge good schemes clocking in flexibility allows (and hence dynamiccapacity range)and for transfermodulation high function, full-well requirements the meets architecture structuredrain. noanti-blooming with This electrode phase 4 a have pixels image The a spacetelescope. these the largest astronomical imagesfrom be transmittedwill to the ground, making pixels plane focal all Instead, on-board. ing VIS willnotemploy binningor window Euclid Gaia, Unlike images. 610-megapixel that the entire generateVIS instrument will so pixels 4132 x 4096 comprises CCD Each (for observing distant, red-shifted galaxies). wavelengths longer for anti-reflection optimized coating an with silicon resistivity tel- the escope optics. They are fabricated onhigh of resolution the match to pixels good radiationtolerance, 12-micronand noise, low efficiency, high extremely with the demanding requirements of the mission, The CCD detectors are to tailor-made meet MSSL by August. be deliveredEngineering Models) will to Flight Modelsintotal Flightplus Spares and (36 CCDs remaining The e2v. company UK lardScience Laboratory Space by (MSSL) VIS instrument have been delivered to CCDs detectors procured by ESA for the 26 first the 2017, of months first the Over of CCD detectors for theVISinstrument. the development of Euclid withthedelivery An importantmilestone has been passed in irst - seethisoverview forinstance. Gaia on used are techniques Both ing. as fainter ones, reducing charge bleed- sources are observed at the same time are bright very when situtations drains for useful anti-blooming and charge of traps effect the reduce to used are Channels Buried Supplementary E uclid

flight

hardw are Mul

- - delivered With a launch planned close to solar maxi solar to close planned launch a With focal plane. allowingof theCCDsclose butting in theVIS sides the to flex-circuitsattached with bide veloped for Gaia. It is made from silicon car- The CCD package is similar to thedesign de closed duringthisreadout period. shuttermechanical cludes a whichbe will in - 80 seconds.instrument TheVIS almost formance) giving atotalreadout period of per noise optimum (for kpixels/second 70 readout speed of each amplifier is limited to through out four amplifiers simultaneously. read The and quadrants four into divided is image CCD full the that means This fiers. and readbe split out through bothampli reg- ister.operation, Innormal the the imagewill of end each at located amplifiers read-outbe through eitheroftwo readout phase 3 electrode structure allowing theimageto a have pixels register serial The two separate serialregisters. which are clocked inopposite directions to entireinto imagesectionissplit two halves The pixel. 12-micron a in capacity well full cause an SBC would significantly reduce the toVIS integration thelong be- time) and Credit: e2v Euclid VISCCD duringfinalinspection -VIS detectors - - - - background, but is included as a tool for moni- toring and calibrating fast and intermediate trap - ferred charge trails). The Euclid Fine Guidance speciesSensor uses(measuring the same First CCDs Pixel as Response VIS but operates and de with a very short, 2 second integration time. In this case, there will be negligible optical back-

slowground traps and and regular reduce charge the effects injection of charge is likely loss to andbe neededdistortion following in the guide radiation star images. damage to fill

The e2v team responsible for producing the Euclid SurreyThe delivered before CCDsbeing will integrated soon undergo into the extensive VIS fo- CCDs with scientists from MSSL and ESA at the Euclid calibration with the flight electronics at MSSL in VIS CCD delivery meeting. Critical Design Review (CDR) for the VIS instrument is calunderway plane at and CEA this in Paris. will be Meanwhile, followed bythe the CDR astronomy will be to correct the distortion of for the telescope later in the year. The VIS in- mum, one of the major challenges facing Euclid- strument will be integrated into the telescope at ing radiation damage in the CCDs. The CCD op- Airbus facilities in Toulouse in 2018. eratinggalaxy shapestemperature due to will electron be around trapping -120 °C;follow this Alexander Short & Giuseppe Racca is far colder than necessary to eliminate dark Alexander Short is the Instrument Engineer in the ESA Eu- current and has been chosen in order to reduce clid Project team responsible for the CCD procurement and Giuseppe Racca is the ESA Euclid Project Manager. the dominant slow trap species. the effect of radiation damage by "freezing in" been included. This will have negligible correc- tiveIn addition, effect in the a chargepresence injection of the high structure VIS optical has

The first NISP hardware delivered The Euclid mission passed another important

state-of-the art detectors for the Near-Infra- Marseille)(Laboratoire as d’Astrophysiquethe main contributors. de Marseille Other milestone with the delivery of the first three in- institutesand the Centre and industries de Physique across de Particules Europe – dein strument). France, Italy, Germany, Spain, Norway, and red Spectrometer and Photometer (NISP) Denmark – are also involved. Visible imager (VIS) To achieve its objectives, Euclid will carry two USA because such advanced devices were not wide-fieldlight to be sharedinstruments: by both a instruments, so that availableThe NISP in detectors Europe at were the time. procured ESA started in the theand observations NISP. A dichroic can be plate carried enables out in incoming parallel a Euclid-dedicated development programme through both channels, and the arrivals of the with Teledyne Imaging Sensors of Camarillo, California, the leader in the manufacture of closely matched in time. near-infrared detectors used in astronomy. first hardware for the instruments were also - sibility of the Euclid Consortium, with CNES type of detector, in a partnership with NASA, NISP(the French is being space developed agency) under and the respon Following the successful qualification of a new

LAM/CPPM the flight models were designed, procured, The Euclid Consortium Newsletter - Spring 2017 sible to deliver to the groundthe raw all detector detectors byfactor a over Megapixelis impos 100,sinceit 4 the by generated stream data the reduce to required is processing data Onboard ferent wavelengths. incoming, near-infraredsplit that lightinto dif different, low-resolution grisms – gratingprisms The spectroscopic channel is equipped with four 1192 nm, 1192-1544 nm and1544-2000 nm. filters (Y, J and H) covering band the wavelength ranges 900- broad 3 with equipped is channel area covered byMoon. The photometric afull the twice than larger slightly – degrees square 0.53 of view of field a cover will detectors The size. in microns 18 pixels, 2040 × 2040 of posed clude 16 of these detectors. Each of them is com- in- will instrument NISP the completed, When livered to LAM/CPPM inFrance. tremely cold,cryogenic temperatures, were de ex at operate to designed are which electronics proximity with fitted instrument, NISP the for cury cadmium telluride) near-infrared detectors HgCdTethree first (mer the 2017, March 24 On Center before beingdelivered to Europe. the detectorNASA’sat lab Goddard SpaceFlight ry. They were thentested andcharacterised in Laborato- Propulsion Jet NASA’s by tested and detectors, each ofthem iscomposed of2040×pixels andis18microns insize. trometerwill includeinstrument NISP and Photometer such 16 instrument.The (NISP) This picture shows one ofthe state-of-the-artdetectors for Euclid’s Near-Infrared Spec - - - - - payload moduleinthesecondhalfof2018. deliveredbe will for integrationinto theEuclid instrument NISP The LAM. at tests instrument tegratedthe rest with oftheinstrumentfor the in- finally and plane focal NISP the form to bled characterisedTheyCPPM. at assem be then will near-infrared detectorsnow will be thoroughly NISP the of pixel Every instrumentation. craft’s portant step inthedevelopment of the space- im- an is detectors NISP first the of arrival The acterised andassembled. as they are the first part of the “chain” to be char readied, be hardwareto instrument first the are assembled around them.Similarly thedetectors ware todelivered be hard becausethespacecraft- is flight first the are instruments scientific Euclid,In asinotherastronomy missions, the data. Giuseppe Racca, René Laureijs Based onanESA press-release - - - Euclid Developers’ Workshops Since 2014, the SGS Common Tools team (see ), adapted for the pur- pose of the training. newsletter 6 a yearly Euclid Developers' Workshop Day 2 and day 3 were alternating presen- which(part ofaims the to SGS share System common Team) tools, organize rules and best practices between Euclid de- velopers These workshops are open to tations and feedback from projects on the any member of the Euclid Organisational same subject. The talks were addressing Units (OUs) or Science Data Centres (SDC) thatmore know-how complex issues and lessonsthan the learnt tutorial could and and they are all welcome to submit their bethe shared feedback among from the projects participants. were given so own presentations. -

place at CNES Toulouse in 2014 with a building,More specifically, debugging, day testing, 2 covered parallelisa techni- The first one, organized by SDC-FR, took friendly bowling contest as the social tion,cal question optimisation about softwareand documentation. architecture, Day 3 was the opportunity to present the main infrastructure tools (EAS, IAL, Git, event; the second one, organized by SDC- 2015 with a fondue party as social event. Redmine, and others) and common scien- CH, at Campus Biotech Unige in Geneva in The third Euclid developer workshop took place from October 11th to 13th dinner gave a taste of the Bavarian food andtific beer libraries. tradition. Finally, this time the social 2016- near Munich. It was organized by SDC-DE - and hosted at Max-Planck Institute for ex Among the 74 attendees, 19 speakers tronomicalThe next Developers' Observatory Workshop of Trieste, will from be traterrestrial Physics in Garching. - Octoberorganized 10th by to SDC-IT, 12th, basedand hosted at INAF-As at the rienced developers on the development International School for Advanced Stud- environment,provided training tools to andnew practicesand more in expe the ies (SISSA). Science Ground Segment (SGS). It will be structured in three main ses- One of the goals of this last workshop was sions: Beginners, General and Advanced. to provide a complete working knowledge Besides the updates and tutorials from of development for the ground segment: the SGS common infrastructure, this year from the software repository to pipeline - - pipelines;the workshop it will will also benefit cover fromadditional the avail top- (maturityjob submission gate, documentation, including the manageand so ability of examples from more mature SGS on).ment and quality insurance activities SDC - ics, including the EAS query and ingestion The three days of intense work started parison of image processing libraries, de- services (including its REST API), a com precisely with an overview of the devel- sign patterns and tips from the currently developed processing functions and how inside the ground segment. It was fol- to perform their integration tests and val- opment process and project management idation. mostly the basics of software develop- For more information see: https://euclid. mentlowed in by the an local extensive environment tutorial (LODEEN): covering - User_DevWorkshops roe.ac.uk/projects/codeen-users/wiki/ line runner and use of the data model. The Commonproject setup, software job triggering development with theenviron pipe- ment (CODEEN) (see newsletter 4) was Frederic Raison (SDC-DE), Marco Frailis also presented. In order to be as practical (SDC-IT), Maurice Poncet (SDC-FR) and realistic as possible, the tutorial was based on a real code i.e. OU-SIR pipeline The Euclid Consortium Newsletter - Spring 2017 Finland -SDC-FI T ain ih h ntoa aaei scientific academic centercomputing CSC national the with ration The hardware ofSDC-FI is operated incollabo participated inthePlanckmission. tronomy ESO).Before with Euclid thegroup (TuorlaObservatory and Finnish Centre for As- Turku of University and Physics) of Institute ki Helsin and Physics of (Department Helsinki of The Universitypersonnel ofSDC-FI is basedat ried out. car- be to Euclid of aspects scientific the allow will that expertise and infrastructure provide dation of the Science Ground They Segment. CentresScience Data (SDCs) makethe foun up - oftheEuclidpillars Consortium and thenine The ScienceGround(SGS) isoneofthe Segment ed. We have alsoaccessto theCSC computers, disk space; morebe purchased will when need of TB 22 currently has SDC-FI 640. is SDC-FI at CPUs virtual of number maximum the that so newer compute nodes can have 48 virtual CPUs; cloud software.Stack Withhyperthreading the is operatedmachines basedonOpen- asvirtual hardware The each. GB 64 and cores 16 with nodes compute older 10 and each, GB 256 and sists of10newer compute24 cores nodes with ing needed). Currently SDC-FI hardware con- cool- less so cold, (it’s efficiency energyfor part of thecenternorthern location was chosenin jaani Data Center, in north-central Finland. The he ware), islocated onthe inaformer left, papermill. KajaaniCSC The Data Center(site SDC-FIof hard - S cience D a t andislocated intheirKa a C entres - - - - Italy -SDC-IT validation oftheGCprocessing functions). in OU-SIM,in the and inOU-LE3(inparticular Tools (DQCT) SDC-FI participatesCommon Quality intheData e.g. aCray supercomputer. primary SDC of the NIR,SIRandMER The simulated by theSIMPF. DEEN) and process the VIS and NISP raw frames Archive System,COIAL, Model, CommonData - the SGSInfrastructure components (the Euclid PFs,SIR integrateand with NIR them VIS, the of prototypes first the develop and design to was dation (V&V) #2, whichSGS of the ispart Challenge Scientific the coordinated fully success SDC-IT the 2016, and 2015 Between in theSGScommonscientificlibraries. Abstraction Layer (IAL) Resource(DRM) oftheInfrastructure Manager Model, developingmon Data theDistributed the Com EC the of of drafts first the in definition products data the on collaborating (SGS), frastructure of the ECScience Ground Segment in- common the to contributed first SDC-IT The clid mission. gressively involved in theactivities for the Eu- mission. Since2011, the team hasbeenpro- the of products data scientific final the liveryof the raw telemetry processing downto thede and itsend-to-endreduction, data from starting operations flight instrument the for sponsible re- was and mission, ESA Planck the Instrument for (LFI) Frequency Low the of Centre ing Process Data the as originated SDC Italian The ian NationalInstitute for Astrophysics (INAF) Observatory ofTrieste, whichof theItal ispart Astronomicalthe at is based 10 membersand The SDC-IT is currently composed by ateam of for the “editing” of the NISP raw science frames. specification and the delivery of forthe Level 1 responsible pipeline, is it finally, and functions; processing SPE and LE3 the of integration and development the to SDC, auxiliary an cantly,as (PFs) functions ing Italian Science Data Center ScienceData Italian (SDC-IT) work package of the System Team, Plan activities. Its main objective main Its activities. Plan I as cnrbts signifi contributes also It . and theimagehandling eiiain n Vali and Verification Hannu Kurki-Suonio process isthe . ------tion of SDC-IT involved in the development and integration of • - Since September 2016, the team has been deeply- SDC-UKLE3 PFs under the Irfu lead with the contri alsothe NIR, been SIR made and on MER the PFs LE3 targeted processing for thefunctions, Scien bution of Lagrange, IRAP, LERMA, SDC-IT and intific particular Challenge the #3 2-point tests. Significantcorrelation progressfunction andhas The SDC-FR also contributes to the development - ing, where a complete re-engineering and imple- • thementation power inspectrum C++ has for been the performed. LE3 Galaxy Cluster of the following PFs: LE1 as an IAP contribution by the development Since March 2017, the SDC-IT has access to a • new computing infrastructure, providing a total of the VIS part of the LE1 PF • SIM as a contribution to SDC-ES, with SDC-FI : of 800 cores, ~400 TB of raw storage and a Mel- IR as an IRAP contribution to SDC-IT

namely KIDS and DES simulators by the APC, basedlanox 56on GbpsSingularity Infiniband containers interconnection. (http://singu The- NIP-S simulator (aka TIPS) by the CPPM and larity.lbl.gov/virtualization), technologysimplifying currentlythe deployment adopted and is • MER as an IAS and LERMA contribution to VIS simulator by the IAP the update of the SGS reference software infra- SDC-IT and SDC-DE structure. • Marco Frailis SDC-NL EXT as an APC contribution to SDC-DE and •

France - SDC-FR PHZ as a LAM and IRAP contribution to SDC- CH. The Euclid France Science Data Center (SDC-FR) - is one of the 9 Euclid SDCs constituting the Eu- SDC-FR PFs are developed by integrated OU/SDC clid Consortium Science Ground Segment (EC testteams, data called and PFvalidation, Team, OU while activities SDC activities being most are SGS) in addition to the 11 morely devoted focused to algorithmon software definition, design, development, prototyping, (OUs) and its . The SDC-FR en- tests and maintenance. dorses three main responsibilitiesOrganization that are: Units de- At this stage, the SDC-FR is deeply involved in the velopment orProject contribution Office (PO) to the development of Euclid , hosting dedicated article in this issue of the Newsletter). and management of the Euclid SGS continuous SGS Scientific Challenge Number 3 (SC3, see the integration,Processing delivery and Functions deployment (PFs) platform (aka CODEEN) and a computing centre covering integratedIn particular, into the the SDC-FR SC3. provides the VIS PF and contributes to the SIM, MER and EXT PFs release storage needs. a significant part of the EC SGS processing and Common Tools, the SDC-FR hosts, manages and The SDC-FR is led by the French Space Agency maintainsAs a major the contribution common SGSto the continuous SGS System integra Team- (CNES) - tion, delivery and deployment platform (CO- - DEEN, see newsletter 4). CODEEN aims to au- and relies on 11 French scientific labo ratories distributed over 6 locations: Lyon, Mar GitLab repositories, build corresponding bina- seille, Nice, Orsay, Paris and Toulouse. These 11 ries,tomatically run tests, extract generate source software code from documenta the SVN/- SDC-FRlabs are involvementthe following: will APC, imply CPPM, around IAP, IAS, 90 IPNL,FTEs fromIRAP, Irfu,2017 Lagrange, to 2020 LAM,distributed LERMA over and aroundLPSC. This 40 - waretion, checkcomponents quality .This markers, platform compute is hosted trends, and contracts. package RPMs, and deploy each of the SGS soft people under either permanent of fixed-term CernVM-Filemanaged at the System APC labwe and are willnow soon close migrate to being to At the PF development side, the SDC-FR is in ablethe CC-IN2P3 to continuously cloud infrastructure. deploy both Thanksdevelopment to the • charge of the following PFs: UK labs the 9 SDCs. VIS PF under IAP lead with the contribution of and production versions of the existing PFs on • - Another SDC-FR contribution to the SGS System SPE PF under the LAM lead with the contribu The Euclid Consortium Newsletter - Spring 2017 Switzerland -SDC-CH projects/elements/wiki/ (see Makefiles usual lying CMake processes automatically generate under and providedfiles throughCMakeList.txt pository structure. The instructions building are conformingpendent modules to standard a re- inde of number a into organized consequence, softwarea pipeline areas projects,whichEuclid ing andpackagingframework. is usedinall It build CMake-based Python and C++ a is ments common framework. Elements the so-called Ele- and the OU-SHE, respectively. It is also providing following specifications provided by the OU-PHZ terminationsfor and thestrongdetection,lens softwareing for photometric the redshift de develop- is SDC-CH The processing. data Euclid other hand, to prepare analysis pipelines for the infrastructure for theoperations and,onthe ison theonehand,toSDC, its task prepare the University of Geneva. Asfor the other national the of Astronomy of Department the at FTE) (6 The Swiss SDC is composed of a team of 7 people cores, 1PBofdiskand10tapes. For(SPV02). around#2 is 2000 target the 2021, VerificationPerformance Science and SC3 tests, and simulations prototypes, PF for used mainly These resourcesof tapes. 500 TB disk and be will of TB resourcescores,located250 600 to are up the most effectivetime with 2017, In the al cost. toing able purchasehardware new the right at locations are revisited on ayearly basisthusbe- whole EC SGS production needs. Needs and al around 20% of the current estimations of the networktoable and supportsuchasbeing cover number 1(DR1) intermsstorage, ofcomputing, volvement upto 2023 for theEuclidRelease Data committedIN2P3 and yearlast CNES CC-IN2P3the in- LHC. CERN the for Tier-1 the of one is it physics and Astrophysics areas. Inparticular, particle in projects many hosts already centre computing This Lyon. in located (CC-IN2P3) tre structure is hosted by the IN2P3 Computing Cen infrathe SDC-FRcomputing least, not - Last but brary andSpectrumlibrary. developmentby CNESteamli- oftheCatalogues Team Common Tools worth mentioning is the SDC-FR Leadfor the SDC-FR Team https://euclid.roe.ac.uk/ for more information). Maurice Poncet ------oped by the SDC-CH team. It produces It team. SDC-CH the by oped devel - program C++ new a Phosphoros, calling is pipeline the method, fitting template the For troscopic redshifts falling onthesamecolorcell. shift distribution meanvalue toof thatthespec step by is applied shiftingthe photometric red correctionfurther bias color space,a the input spectroscopic redshiftFor sample. of eachcell trainedalgorithm, machine learning a a with combination of the results is then achieved with regionsparameter oftheinput space.Thebest different for optimized and parallel in applied methods, learning machine and fitting template redshift determinationinvolves pipeline.It both overallscheme is emerging for the photometric- Even if different optionscontinueto betested, an ity Density Functions (PDF) made clear about twoabout made clear yearwastime that ago most successful astronomicalsoftware tools), the SExtractorof of (one plans maintenance and parallel,assessment of thelong-terman update ing strong lens)detection andde-blending.In to tests different algorithmsof source (includ- achieved been has function processing SHE the ed work, acollaboration withcolleaguesfrom In theframe ofthestrong lensdetection relat html#photoraptor code (http://dame.dsf.unina.it/dame_photoz. PhotoRaptor the integrate to ongoing also are ent methods and to classifysources. Discussions to optimally combined the results from the differ Primal is used to produce photometric redshifts, Random Forest, canbeinvoked in thepipeline. plementedthis package, in AdaBoostsuch as or way, any of the machinelearningmethods im- learn (http://scikit-learn.org/) package. Inthis scikit- the wrapping project Python compliant thon package has been developed. Itis a Euclid Py Primal the methods, machine-learning For . ch/euclid/phosphoros/ for more information) Euclid mission lifetime (see completed and maintained throughout thefull further be toexpected is Phosphoros extinction. implements anewscheme for handling galactic also includesoptionsto addemission lines andit currently It functions). luminosity as specified axes, (luminosity priors including luminosity can be space parameter the of any along priors input take can Phosphoros example. for history formation star or mass galaxy as such rameters, eter space for determinations of physical pa- produce PDFs along any other axis of the param- of redshiftfunction a ties as values.also can It ) into theEuclid pipeline. providing probabili http://isdc.unige. Probabil ------up to consider the development of a new SEx ourtractor Euclid implementation. colleagues and We provide realized at that the startsame timeing a a newsolid C++basis project for a Euclid could strong benefit lens many detec of-

- turaltion pipeline. design. A singleSDC-CH responsibility members bring is attributed modern toexpertise each code in modular element, object-oriented software interfaces architec are used in a systematic manner and many design

modular framework (together with aperture photometrypatterns are functionalities)at the heart of isthe now new in project. place, asA well as a preliminary proof-of-concept version

theof multi-frame Euclid collaboration model fitting. at the A end first of versionthis year. of the new SExtractor project should be release to - The Centre for Information Technlogy of the Uni- ings and Euclid challenges. It participated in versity of Groningen, hosts the computer systems particularThe SDC-CH into organizes the infrastructure its work around challenges. OU meet It operated by the SDC-NL is not yet involved into the parallel series of sci- component, the Science Analysis System. The the early stage of the Euclid data processing. The EXT pipelines are currently being developed in newentific programs challenges, were which however concerned tested so throughfar only cooperation with SDC-DE. In addition the SDC- two photometric redshift and one strong lens- NL contributes to the development of NIR pipe- ing challenges. This challenge-driven approach lines, which is led by SDC-IT. The archive development and the EXT pipeline for steering large collaborations towards com- development in the SDC-NL draw heavily on the has proven to be an amazingly efficient method many years of development of information sys- it provides a promising path to complete the tems in the University of Groningen. This tech- fullmon analysis goals. Capitalizing system on ontime, the beforerecent thesuccesses, Euclid nology now underpins many active systems, launch. both inside and outside the astronomy domain. Pierre Dubath Inside the astronomy domain it is used by As- tro-WISE (OmegaCAM), the Lofar Long Term Archive, and the Muse processing system. In - tremely Large Telescope. the future it will be used by Micado on ESO’s Ex The Netherlands - SDC-NL The SDC-NL hardware is currently based around - The Netherlands Euclid Science Data Centre (SDC-NL) - cluster.a large GPFS The filedatabase system facilities (10 PByte) are with provided the pro by tronomical Institute and the Centre for Informa- acessing Oracle performed RAC system. on The the storage university system Peregrine is cur- is jointly hosted by the Kapteyn As tion Technology in the University of Groningen, rently being replaced by a and a new high availability database system, Leiden Observatory. The SDC-NL has particu- using Solid State Disk storage.Lustre The SDC-NL files system cur- lartogether responsibilities with significant for the development contributions of from the Euclid Archive System and the EXT pipelines. scientists from the Netherlands in OU-EXT, with The Euclid Archive System is being developed rently has 16 members, including the associated in co-operation with ESA. The SDC-NL has re- Rees Williams sponsibilities for two archive components, the which we work as a unified team.

Storage System. The ESAC Science Data Centre inData Madrid, Processing leads the System development and the of Distributed the third The Euclid Consortium Newsletter - Spring 2017 The USA-SDC-US h rsac cmuiy y rvdn expertinsight into thesurveys,processes, data calibra- providing by community research the processing.data ENSCI supports addition, In performing and assurance, quality data in ing gorithm and software development, participat the EC’sScienceGround providing Segment, al (ENSCI) IPAC at Center shel. SDC-US is part of the Euclid NASA Science Her & Planck ISO, missions ESA previous the space missions, includingNASAinvolvement in ing andarchiving services tolarge a numberof operations data-intensive support, process scientific provides IPAC USA. California, dena, Pasa - in Caltech/IPAC at based is SDC-US The in the IPAC data center. equipment SDC-US dedicated of rack first The . ENSCI participates in - - - - as mitigation initiative Platform Research Pacific the of part as science-DMZ low-friction high-performance, latency to theother SDCs. We are investigating graphicalseparation, andthusbandwidth and issue forparticular One SDC-USisourgeo- lenging) upcomingsciencechallenge3. our first dedicated hardware for the (more chal- integrating are and purchased just have We 2. challenge science and 6 challenge frastructure SDC on2servers,recentin the part taking in- We are currently runningaprototype of the define to Data QuickLookAnalysis for NISP. Center Operation Science the with Theteamcontamination. worksalso closely de spectroscopic and calibration, flux absolute packages,detector-level including calibrations, is responsible for several NIRandSIRwork neers work withOU-NIRandOU-SIR. ENSCI ENSCI/SDC-US scientists andsoftware engi- es. pate inthescienceandinfrastructure challeng workclosely Systemthe with Teampartici- and 5% oftheEuclidabout Weprocessing budget. and archiving effort for Euclid. Weprovide will of thedistributedSDC-US ispart processing US system engineerisBenRusholme. SDC- the Teplitz,and Harry is lead SDC-US and Director is George Helou, the ENSCI science lead engineers workingclosely together. TheENSCI The ENSCI team includesbothscientists and tion, andproducts. Harry TeplitzHarry - - Canada joining the Euclid consortium anadians became provisional members of CEuclid in the fall of 2017. The Canadian Eu- degrees over 117 nights, covering the region clid Consortium has agreed to provide access aboveAll-sky a Universe)declination will of survey0 degrees, ~10000 and outside square (along with French co-Is) to the Canada-France Imaging Survey (CFIS) (point source, SNR=10, 2 arcseconds diameter data products for the purpose of photometric aperture).the galactic plane, to a u-band depth of 23.6 and various scientific redshift estimation. In return Euclid has agreed The CFIS is a legacy survey for the Canadian to provide full membership into Euclid to a and French communities. Alan McConnachie group of about twenty Canadian scientists and .All data are proprietary within the Canadian and French Jean-Charles communities Cuillandre until areFeb. the 1st, co-PIs.2021, ex-officio representatives. - at which point a public release will occur. This da-FranceCFIS (Sea-Fizz) will contain everything from the raw data to is a joint Cana the many advanced products curated by the CFIS Collaboration. The CFIS collaboration is hasCFHT been Largeallo- catedProgram that271 survey to other bands and to enhance the anal- veryysis with interested spectroscopic in collaborations observations. to extend the semesters - nights over six (17A to 19B, from Feb. 1st 2017, to Jan. 31st dian members are: Michael Balogh, Dick Bond, An MOU is being finalized. Provisional Cana Research Council of Canada, the Centre Nation- Nick Cowan, Sebastian Fabbro, Laura Ferrare- 2020). The CFHT is operated by the National Jo Bovy, Ray Carlberg, Scott Chapman, Pat Cote, al de la recherche Scientifique of France and CFIS has two survey components, one in r-band se, Renee Hlozek, Mike Hudson, John Hutchings the University of Hawaii. and one in u-band. CFIS-r WIQD (Wide + Im- (ex officio), JJ Kavelaars, Dustin Lang, Denis Sawicki,Laurin (ex David officio), Schade, Alan Douglas McConnachie, Scott, Kendrick Adam degrees over 154 nights in the r-band. Cover- Smith,Muzzin, Christine Laura Parker, Spekkens, Chris James Pritchet, Taylor, Marcin and ageing theQuality sky above+ Deep) a declinationwill image ~5000of 30 degrees, square Chris Willot. and outside the galactic plane, it will produce - Ray Carlberg source,a panoramic SNR=10, survey 2 witharcseconds exquisite diameter image qual ap- erture).ity (~0.6 CFIS-u arcsecond) LUAU to (Legacy a depth for of the24.1 U-band (point he uclid onsortium ewsletter pring

T E C N - S E 2017 EXTERNAL DA L space would havevolumethe data multiplied as from measurements these Making filters. tiple mul with channel VIS the equip to unjustified considered therefore was it and cameras, field be obtainedfrom theground withlarge wide- ma, extended), sufficiently accurate colours can metric redshifts. Atdepth ofr~24.5(10-sig a colours areOptical essentialto measure photo- redshift calibration sample. Euclid targets, andto provide a spectroscopic re- quirements are to main measure optical colours of all The provide. will instruments NISP ed inaddition to whatthe satellite VIS,NIRand goals, alarge volumearedata ofessential need For theEuclid mission totoable be meetits rad Kuijken (Leiden,chair). Cuillandre (CEA Saclay/Obs. de Paris) and Kon- Jean-Charles (Caltech), Capak Peter of consists be taken by theEuclid spacecraft. Thegroup coordinate theprovisionnot will that of data uclid lished a new workingnew lished a group, the ‘COG’, to ast November the Euclid Consortium estab- well asthe currently ongoing HyperSuprimeCam andKiDS lensingsurveys as indicated, are surveys ground-based complementary various The planes. galactic and ecliptic the avoids it as Euclid-Widesurvey,the of extent full the outlines area green The sky.Euclid The C omplement ary T NEP A GC O bserv CFHT[u] CFHT[u,r] +JST[g] EGS/AEGIS a tions - - - NGP E−GOODS−N OU-SHE processing cannot proceed. ground-basedtherefore, data thefundamental the Without ones. red than differ correction PSF ent a require will galaxies blue known: is galaxy each of SED the if done be only can this and shapes, galaxy VIS observed the correct to order in model PSF accurate an require ments a factor of two in width.The shear measure - Point diffraction-limited Spread Function varies dramatically, by almost nearly the images measurements. Overof theVIS thewideband A second colours liesintheshear use of optical redshift estimation by OU-MER and OU-PHOTZ. readydata, for photometryphotometric and pixel ‘Euclidized’ into data such turning with the Euclidwith is tasked OU-EXT taking. data needs to be acquired, on a timescale compatible ugriz images over the full wide survey therefore principle. Acomprehensivemust’ set of data the ground whatyou from can, spacewhatyou greatat cost: therefore Euclid follows the‘from well as extending the required mission lifetime, G COSMOS roup SEP LMC Blanco [g,r,i,z] HSC SSP KiDS/VIKING DES@Euclid 4kdeg2 Euclid Equa.3kdeg2 Euclid North5kdeg2 Calibration field |Ecliptic lat.|<15deg. Galactic dust Dark EnergySurvey Euclid Wide15kdeg2 E−CDFS/GEMS VVDS−Deep SXDS SGP SMC - No single ground-based survey is at present able to provide all Euclid imaging need: instead - this will take a combination of several surveys algalaxy ambitious shapes. programmes This is another are keyunderway, input to both the (see Figure on the previous page). fromSHE measurementthe Archive and pipelines. with new Also (proposed) here, sever ob- In the South, the eventual plan is to use the LSST servations. survey, but on current planning this facility will The COG is also tracking and coordinating spec- not start operating until 2021. In the meantime, troscopic observations. Several campaigns are the Dark Energy Survey will cover a large part underway, with Keck and VLT, to provide sam- of the Southern Euclid sky and the plan is to use photometric redshift calibration. A total of some Kilo-Degree Survey also overlaps somewhat 100ples nightsof galaxies of 8-10m down telescope to Euclid-Wide time is depthbeing defor- withthese Euclid-Wide data for the infirst the Euclid South: data its datarelease. are Thebe- voted to these programmes. The result will be a ing used already to validate the EXT work. The Northern sky is more complicated. We are comprehensive coverage of galaxy colour space currently contemplating a patchwork of surveys calibration of the photometric redshifts that with spectroscopic redshifts, ensuring adequate - provide the vital third dimension of the Euclid map. in different filters, but the picture is not yet com The beauty of the Euclid mission is that, apart (soon)plete. WithCEFCA’s wide-field JST, there imagers is certainly such the as capac CFHT,- from its primary cosmology science goal, the ityPan-STARRS, to cover the HyperSuprimeCam Northern sky well: on agreementsSubaru and data the satellite will provide will include some have already been made with the French and of the best sky images ever taken. The enormous legacy value this provides will be enhanced tre- (g), and discussions with other potential part- mendously with the complementary multi-col- Canadian CFHT communities (r,u) and CEFCA our imaging the mission has sparked already. to ensure timely coverage of the Euclid North- The collaboration between the many surveys ernners sky are is underway. currently theGetting highest firm priority commitments for the from ground and space that is happening now is COG. Another aspect of shear calibration is to use than the sum of its parts’. an excellent example of a ‘whole that is greater - The COG leads

anddeep thus HST mapimages out (HST the hasintrinsic nearly distribution twice the spa of tial resolution of Euclid, and narrower filters),

The Javalambre-Euclid Deep Imaging Survey in g band (JEDIS-g) The Javalambre-Euclid Deep Imaging Survey the data means that CEFCA will provide a total of in g band (JEDIS-g) will be the contribution of 1250 deg2 in 2023, reaching 2500 deg2 in 2025 the Centro de Estudios de Física del Cosmos de 2 in 2027. The data pro- Aragón (CEFCA, Spain, www.cefca.es) as OU-EXT vided will include raw images, reduced and as- to the Euclid mission. andtrometrically the final 5000calibrated deg images, and catalogues Following a memorandum of understanding constructed from the reduced images. signed between CEFCA and the Euclid Consor- The observations of JEDIS-g will be carried from the - to provide the Sloan g band data of 5000 deg2 bre (OAJ, ) which is a brand new oftium the in Northern September Sky 2016,in common CEFCA with is committed the r data astrophysicalObservatorio facility located Astrofísico at the de Javalam- from Canada-France Imaging Survey (CFIS) tre summit,oajweb.cefca.es Teruel, Spain, which is managed by CEFCA. Pico del Bui at SNR=10. The baseline of the delivery of reaching a depth of ~24.7 for extended objects The Euclid Consortium Newsletter - Spring 2017 aea (JPCam) Camera Panoramic alambre vided the Jav with be proT250 will - 2017/8 the JST/ (Figure 1). During a FoV of 3deg telescope with escope) bre Survey Tel- T250 (Javalam the JST/hand, es. On theother bration purpos features for cali- on specific stellar filters 7 and ters fil- SDSS-like 5 filters:12 of set a tion e2V CCD and (FoV) view of Telescope) 83cm telescopeis an 2deg field a with Survey Auxiliary (Javalambre T80 eras: theJAST/T80the JST/T250. and TheJAST/ cam- view of field large with equipped escopes of theobservatory are two large etendue tel- For this purpose, the two maininstruments (J-PLUS, verse Survey org verse) Astrophysical Survey (J-PAS, JavalambrePAU AcceleratedUni- the (Physics of the for data the of exploitation and production of theOAJThe maingoals andCEFCA are the OAJ (inset) of room clean the in JPCam and (large) JST/T250 of Image 1: Figure ) andthe Javalambre Physics of the Local Uni - equipped with a 9.2k x 9.2k new genera- new 9.2k x 9.2k a with equipped is a 2.5m - - -

of only1/30the original full frame. cutout a is image Pathfinder~0.4”. The is image Pathfinder band image fromThe FWHMofthe(right). SDSS in the PSF g the and (left) filter no exposureswith single 10s six of tion age ofthe central part ofM51resulting from the combina- coaddedim- a of quality imagetheComparison of Figure 2: projects. www.j-plus.es) www.j-pas.

possibility ofcarryingoutobservationsscien at interface between JPCam and JST/T250 the with commissioning of the mechanicalpartsof the alreadyJST/T250at installed tothe carryout is T80Cam, of twin a is Pathfinder,which called sioned off-the-telescope at theOAJ and acamera in commissioning phase. JPCam is being commis of open time since 2016, meanwhile JST/T250 is operating. and finished JAST/T80 is working on J-PLUS and is offering 20% OAJ the Currently, redshifts withintheEuclid project. fordata band thedeterminationof photometric filters inu,g,randibands. complementedbe broad-band with will system filter This ~10000Å. to ~3450Å fromcoverage continuous providing extremes the on band filters broad two plus ~9200Å to ~3700Å from (FWHM~140Å) ters fil- overlapping band narrow 54 of set a system, J-PASfilter optimized photo-z the mount camerawill The covering4.7deg a mosaic of14T80Cam-likea CCDs integrating camera Gpixel 1.2 tion (Figure 1,inset),anewgenera- provide theground-basedg- Sloan eredtoinstrument optimum an efficiency consid been has it optimal 5500Å, around its and T250 Given thelarge etendue oftheJST/ the quality of the skies the of quality the These results highlight Euclidthe Consortium. fordata of theg-band JST/T250 as provider of evaluation first the mated value used for e, itn te esti- the fitting tem, throughputof thesys - measure- ments oftheoverall first the lowed also to obtain al has Pathfinder 2). (Figure ~0.4" FWHM PSF a reached quality 8th March theimage and onthenight of on 20thFebruary light first its received Pathfinder level. tific 2 area ofthesky. - - - - and the performance of the system. the very similar characteristics from those that Finally, CEFCA has already all the hardware systems for processing and storing the images mounted with the same CCD. will come from JPCam since both cameras are coming from the OAJ with a datacenter of more In summary, CEFCA and OAJ will be soon ready than 20 computing nodes with more than 500 to start JEDIS-g to provide the Euclid Consorti-

Jesús Varela storagecores, a space.storage Regarding disk cluster the for software, up to 1.1PB CEFCA of um high quality g-band images from the ground. hasdata developed and a tape is libraryown reduction adding 4.0PBpipeline more based of on open-source code and it is routinely pro- cessing the images from JAST/T80 which have

OU-EXT - - Etial component of the Euclid Mission. The tion calibrates and stacks simulated raw Kilo- xternal ground-based imaging is an essen Degree3. A first Survey version (KiDS) of the and EXT Dark Processing Energy Survey Func lensing tomography will be derived using mul- (DES) observations delivered by OU-SIM. The photometricti-band optical redshifts ground-based required imaging for the covering weak- calibrated images are then input to the MER the Euclid Wide and Deep Surveys. These im- ages will also be used to measure the spectral - energy distribution of stars. This is needed to Processing Function. The main purpose for EXT asis to well. verify functional requirements. Initial vali dation of scientific requirements is performed The Gaia all-sky stellar photometry, spectro- characterize the wavelength dependence of the photometry and astrometry have clear poten- VIS Point Spread Function. at least four different surveys each observed The external images will be acquired through- for Euclid-compliant calibration and validation ent ground-based telescope (see the article on oftial the to ground-based become an excellent surveys. referenceThis has become system thewith Complementary a different wide-field Observations camera onGroup a differ for clear with the Gaia Data Release 1 and with the

differ in their instrumental passbands. Further- more,details). the All surveys surveys have use different Sloan type constraints filters but on OU-EXToutcome has of the created Euclid a newPhotometric architectural Calibration design the allowed atmospheric conditions during ob- forworkshop, the EXT both ground-based in September processing 2016. Therefore in which the Euclid-compliant photometric and astro- metric calibration and validation makes use of Functionservations. to Itdeliver is the to task the ofSGS: the Organizational Gaia in addition to survey-internal relative cali- Unit External Data to develop the Processing Ground-based images that are consistent with bration via observation overlaps. Furthermore the Euclid VIS images in terms of photometry, - over the lifetime of the Euclid mission taking it ensures efficient handling of recalibrations ucts with identical format for all surveys. This advantage of the updated releases of the Gaia PSF characterization and astrometry, prod based images. processing operations. is called the Euclidization of external ground- data. The approach avoids expensive pixel re- OU-EXT together with SDC-NL and SDC-DE are Gijs Verdoes Klein

participating in Euclid’s Scientific Challenge The Euclid Consortium Newsletter - Spring 2017 OU-LE3 S or more scientific working groups. The next The groups. working scientific one more or with organised meetings joint often are Givenscience aspect ofthisOU, themulti there working group. largeforminput simulations cosmological the community withinLE3,theCluster SWG anda This included effort fromvery a active cluster one. first the complementing one, second a of on-going investigationsallowwill the selection and method, one of selection the to led has PF data challenge for the Cluster finding algorithm have candidate prototype algorithms.Arecent the high-priorityand all processing functions Algorithm developmenthas progressed well the LE3SDCefforts. ing theItalian,French andUKcontributionsto Science DataCentres (SDCs) this large TheFinnishandRomanians effort, and spectroscopic Euclid surveys. To cater for selection functionsofboththephotometric tion, galaxy distributionbi-spectrum, orthe statistics codesfor clusters ofgalaxies detec- addition, LE3willalsoprovide higher order correlation functionsandpower spectra. In clustering two-point lensing andgalaxy ing Massmaps,weak such asweak lens Euclid dataproducts liver to ESA thefinal will beusedto de the algorithmsthat ment into theSDCs to develop andimple er. OU-LE3ischarged ing functionsto deliv and over 40process than 500scientists in place,withmore been thelargest OU ment OU-LE3has the ground seg- ince thesetupof - - - - - algorithm selection andimplementation inthe SDC pipeline currently inprogress. Completeness redshiftvs. selecteda of algorithm from the Cluster Challenge byrun whichLE3 toled are complement- the nature ofdark energy anddark matter. on have will we results exciting most the ing Euclidbring will that discoveries,new includ- These becomes public. areproducts thedata availableto the communityafter Euclid data the deliverablesmakethe consortium that will generaterun OU-LE3 code SDCs and will will for Euclid. and those whobe producing will thepipelines betweenplace thosewhothe data using be will for synergies andcollaborative workto take allow and vital are meetings These Sexten. in July in scheduled also Verificationis formance group and Workingfocusing on the ongoing Science Per Clustering Galaxy the joint with meeting A meeting. consortium London the ing takeplanned meetingwill placethis year dur Filipe Abdalla, Jean-Luc Starck &Enzo Bran- chini - - OU-NIR All these activities stimulated a tight posi- have been focused on the preparation of the tive interaction with different actors of the Since the second half of 2016, NIR activities- - ment Team, the Calibration Working Group, Processing Function for the reduction of sim andEuclid the Consortium, OU-SIM. such as the NISP Instru ulated NISP photometric observations within While basic functionalities were already im- At the time of writing, we are currently com- the framework of the Scientific Challenge #3. plemented for the previous challenge, this ar- - ticle later in the newsletter atpleting the SDC-IT, the reduction who provided of a first crucial SC#3 support(see time we are increasing significantly the com for detectors and instrumental features during all the development )process, simulated and field we plexity of the NIR pipeline in order to account are eagerly looking forward for OU-MER to run on NIR data products. throughsuch as the saturation, development non-linearity, of dedicated quantum cali- brationefficiency, pipelines and PSF. for master This is dark being and achieved master few weeks we will be focusing on a thorough part of this will also be used by the OU-SIR Beside completion of the SC#3, in the next forflat the production. pre-processing It is worth of simulated to mention spectro that- - scopic frames. We are also setting forth the tantvalidation Challenge of thewe will NIR be Processing facing this Function, year, the basic structure for relative and absolute pho- Designwhich willReview be theof the basis Euclid for theScience next Ground impor tometric calibration that will be fully imple- Segment at the end of 2017. mented during forthcoming months with the Gianluca Polenta development of further dedicated calibration pipelines.

A zoom on a composite image of a simulated SC3 field from a preliminary version of the stacked frames for the Y, J, and H filters produced by the NIR Processing Function The Euclid Consortium Newsletter - Spring 2017 What isSPE? N T meaning that ithasmore than to becorrect. a99.999%probability C5, class in in redshift this at spectrum the that indicates learning, machine on based algorithm sification obtainedfrom combining the fromPDF the different models, with the redshift correctly clasThe identified. (PDF), function distribution probability redshift posterior the presents panel right top The templates.ence refer on as well as continuum, and absorption, line emission, line on built models different with spectrum line flux > 2×10 > flux line shall be greater than 45%, for an (H pleteness of the redshift measurement, which line. The most relevant requirement is the com- H the of flux the importantly most reliability, and provide spectralmeasurements, the aimisto deliverestimates statistical of its spectroscopy mode. Together with theredshift, slitless the in NISP by observed galaxies the of provide spectroscopic redshift measurements line flux 6x10 a with emitter Hα bright a z=1.1973, redshift a with galaxy simulated a on measurement redshiftPF-SPE P rcie fu ad aeegh calibrated wavelength and flux receives SPE the range 0.9

from -16 erg s

the -16 -1 erg cm cm SPEOU/ -2 Å -1 .The PF-SPE redshift measurements algorithm proceeds by fitting the observed -2 s -1 andaredshift in a) emission a emission processing ments Automated redshift andline(Ha)measure- of the wide survey, it is evidently out of ques- of out evidently is survey,it wide the of deg² 15000 the within expected are spectra of need to befully automated. Tens ofmillions First and foremost, measurements onspectra There are several key challengesfor SPE: axy clustering measurements. importantly LE3,includingthose related to gal availablefor other processing functions,most then deliverablesare SPE the processing, After grism orientations, aswellas associated noise. the wide survey to 4 individual exposures and 3 combined spectrafrom corresponding SIR, for

functio - - - tion to measure the spectra or even control them by hand, contrary to what has been done calibrationcreased, refining necessary the reliabilityprior to running estimates. the Thissur- challenge is the processing speed, as one day of vey,depends which on we the will size need of tothe decide learning on. sample, a observationsfor most galaxy needs surveys to be processed up to now. in less Another than - Testing and performances, next steps lion spectra to be processed per week, as one wantsa day. Theto go expected digging intodata the flow noise leads of theto 4.6 slitless mil tests based on simulations delivered by OU-SIM, spectra images in hope not to miss any faint As the PF is being developed, we run extensive- - sion. simulationsin a parameter available space coveringtoday allow the estimatingrange of ex a continuum sources with significant line emis -2 -1 We have implemented a redshift measurement highpected success line flux rate and down continuum to the 2×10 magnitude. erg cm Thes pipeline, which draws on several key algorithms. -16 - A cross-correlates ob- served spectra with reference (simulated) tem- anline intermediate flux limit, and and give internal confidence result inwhich the relihas processing element (PE) sometimesability of the been SPE algorithms.taken over-enthusiastically This is however

toplates. associate Another a redshiftPE identifies to the emission observed lines lines. and demonstrate that the survey will fully meet the runs informed “artificial intelligence” recipes out of context, and we stress that we do not yet and gets redshift constraints from continuum - Yet another PE extracts continuum information pletecompleteness this work. requirement, and that therefore significant efforts need to be invested to com Indeed our development roadmap is set to al- templates. These PEs are ultimately combined to extract a discretized list of redshifts. - Methods to estimate zspec reliability low verifying compliance with requirements only once the next step of testing and further im Another challenge is to automatically assess on “real sky” simulations currently produced by proving the SPE algorithms will be carried out the reliability of a spectroscopic redshift meas- SIM. These include a realistic magnitude, red- urement. We want to evaluate the probability for a redshift to be right with a high level of cer- most importantly, a realistic handling of spec- shift, and flux distribution of the sources, and, tainty, and do it fully automated. Furthermore, of spectra for each observed grism orientation. tral contamination due to geometric projection as accurately as possible, hence with their as- We have all elements to hope that tests on these sociatedwe need errors.to measure This allowsthe flux maintaining of identified a linestight control on the survey selection function, par- a emitters. state-of-the-art simulations will confirm earlier willresults have that a robustthe requirements spectroscopic will redshift.be met, with,This ticularly on H in the end, about 25 million galaxies which breakthroughThis simple goal gives is us in hope fact verythat complex,we have now and the clustering cosmological probe, at the core of should enable a full realization of the power of thesolving keys itto proved fully solving to be this quite problem. tough. Informed A recent the Euclid mission. by the reliability assessment process used by Olivier Le Fèvre and Christian Surace high redshift spectroscopic surveys, we de- for the OU/PF SPE team vised a machine learning algorithm using the

to produce a homogeneous partitioning of the datashape into of the distinct PDF ofclusters the redshift (classes) measurement via unsu-

pervised classification (Jamal et al., submitted).- In a proof-of-concept analysis, five classes were Inidentified, principle, nicely the reproducingnumber of classes the classes can ofbe gal in- axies in known surveys like the VVDS or VUDS. The Euclid Consortium Newsletter - Spring 2017 S T of simulated clusters. ship bysimulation evaluating theproperties is alsoweighing inonthevalidationof theFlag- clid. forts to verify the science performance of Eu - a numberofreasons as partoftheongoing ef ous sources of bias, itis timely to revisit this for convenient way to compareof vari theimpact - needs. Although these early studies provided a algorithm and performanceEuclid, in calibrationon also but instrument on requirements the time.These results form the basis for the at identified been had that bias of sources the org/abs/1210.7691 led bypaper in a MarkCropper (https://arxiv. framework to propagate biases.This was used abs/1210.7690 per led by Richard Massey (https://arxiv.org/ of theselectionprocess.part Forpa- a instance, parameterslogical was studied in greatas detail of residualThe impact systematics oncosmo mological signalfrom thedata. carefullybeforeextractcos can applied wethe designed to do so, many corrections need to be ies unprecedentedwith accuracy. Although itis galax billion nearlytwo of shapes the measure overcome To this sourceuncertainty, ofstatistical Euclid galaxies. will of ellipticities trinsic percent;a whichthe in- than ismuchsmaller caused byticity gravitationalis about lensing The history. change intheellip the typical is that challenge expansion the and matter total is directlysignal related to thedistribution of of is this ‘cosmic because theamplitude shear’ light by intervening large-scale structures. This of differentialdeflection the by caused galaxies the measuring coherent distortions in theimagesofdistant by theories gravity modified to is constrainthe nature ofdarkenergy andtest Euclid of objectives primary the of One with the Euclid galaxy cluster catalog. SWG to constrain cosmologicalparameters analysisbe used bywill methodology that the of comparing analysis codes and developingthe aim the with Saro Alex and Melin Baptiste tercoordinated cosmologychallenge by Jean- clus- a started has SWG Galaxies of Cluster The he cience C luster P erformance ) presentedgeneral a analytic

of ) to derivebreakdown a of

galaxies The effortled isbeing V erifica SWG

The SWG tion - - - - -

for effects are typically common between galaxies, between common typically are effects systematic galaxies; individual for measured factphotometricshapes and that redshifts are end-to-end simulation. To do this we exploit the of Euclid,havingwithout but to rely on afull performance WL expected the of estimate our (SPV) verificationperformance of thescience As part uting factors have been identified. measurements,contrib- number ofadditional a to progressshape inourunderstandingofthe included in the original studies. Finally, thanks correlations between effects couldnotbeeasily of the variousimpact sources of bias. Moreover, alwaysnot clear howto compute theaggregate tion to do so is that intheinitialformalism it is to revisit theoriginalstudies. Another motiva- timely therefore is it finalized, essentially sign matureof Euclid, status the spacecraftwith de scale-dependencies are considered. Given the parameters might bereduced once the correct cosmological in biases expected the that found Kitching (https://arxiv.org/abs/1507.05334 scenarios recentin a alistic by paperled Tom studyinitial the originalstudies.An ofmore re- parameters could notbeincorporatedthat in on theobserving strategy or time since launch, out-register. Moreover, thebiasesmay depend ciency (CTI) ineffi transfer detector effects such as charge whereas field-of-view; full the from termined de is model PSF the example, For scales. istic arespurious signals introduced oncharacter fects. Inmore realistic scenarios, however, considered scale-independent systematic ef ence for theoriginalpapers implementation, in orderFirst ofall, to avoidpreferimplicit an cia andSimonaMei. work package coordinated byDe Gabriella Lu- Clusters Galaxy of Astrophysics group’s the by Jim Bartlett, Jochen Weller,Jim Bartlett, Lauro Moscardini

theWL-SWG hasstarted workto improve weak occur on the scale of a singleof a occuronthescale read-

lensig ) ------but the measurement process is not. Therefore been discussed in the past, but we were unable as long as the biases are known as a function of - to quantify properly. etc.) we can propagate these biases in a bottom- rors in the point spread function model, imper- galaxy properties (size, shape, color, redshift, As a first set of test cases we have considered er than the previous method of propagating cos- and the impact of masked areas in the survey, up approach, from galaxies to cosmology, rather - butfect wecorrections note that forthe chargepipeline transfer is capable inefficiency to simu- late a much wider range of effects, such as the mological biases into requirements on system compute the residual biases caused by imperfect impact of varying depths in ground-based data. atic effects. By reversing the flow, we can also corrections; these arise because we know the Moreover we can evaluate the impact of instru- ment failures, such as the loss of a NIR detector. limited knowledge is captured by appropriate probabilityrelevant quantities density distributions.with limited precision. This Many people have already contributed to the current work on our versatile pipeline, and we We therefore obtain catalogues of observables that contain realistic residual systematics for different scenarios. Compared to an end-to-end Fenechthank Ruyman Conti, ChristopherAzzollini, Mark Duncan, Cropper, Arun Jerome Kan- simulation, our current approach of starting nawadi,Amiaux, HerveLance Aussel,Miller, AurelienMathias Schultheis,Benoit-Levy, San Ian- at the catalog level has the advantage that it is tiago Serrano, Edo Van Uitert, and Chris Wallis - - leads if you are interested in contributing and much faster, enabling us to explore many differ- for excellent work. Please contact the WL-SWG thonent scenarios. that enables Paniez us to Paykari propagate has the led systematic the ongo Henk Hoekstra, Tom Kitching, Martin Kilbinger signaling work all the to developway to the a modularevaluation pipeline of cosmologi in Py- joining the WL SPV team. cal parameters. The current version of the code uses the MICE simulations as the starting point: : this cosmological simulation provides a catalog Further reading - Massey, R., Hoekstra, H., Kitching, T., et al., 2013, MNRAS, of galaxies in a cosmological setting. We also in- 429, 661 clude a realistic model for Galactic extinction, 431, 3103 Cropper, M., Hoekstra, H., Kitching, T., et al. 2013, MNRAS, westar will counts use andthis Zodiacalas the input light. universe Once the for cata our logs from the flagship simulation are released, Kitching, T., Taylor, A.N., Cropper, M., Hoekstra, H., Massey, - R., & Niemi, S., 2016, MNRAS, 455, 3319 SPV simulations. This unique simulation is also synergiesthe input forbetween similar probes, efforts something for galaxy that cluster has ing. Hence it will enable us to explore possible

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along with any needed credit, your name and supporting short text. The Euclid Consortium Newsletter - Spring 2017 What isit? S Objectives • implementation ofthecomponentsare twofold: developmentSegment drivingplan thesoftware The milestonesEuclid ofthe Science Ground nents. ploy,testinstall, run thesesoftware and compo- de to up set consequently is infrastructure the (SDC's); configuration production any on ning chive data productswith its output and is run - data retrieved from thearchive, updates the ar- input processes requirements, scientific of set of processing functions involved meets agiven isaprocessThis challenge the set ensuringthat Pipeline software development activities. Processing Euclid 2017 year of tives objec- scientific major the of one and Segment, in thedevelopmentof theScienceGroundplan (SC3) #3 Challenge here isScientific Euclid Consortium vocabulary.is setout What The word 'challenge' isa‘catch-all’term in the to befixed... and performances weaknesses corrected, issues features, new terms of management, functional the lessons fromimplement in challenges past objec - tives shouldremember ofthen+1challenge the and Thus 6. challenge Infrastructure 2, challenge Scientific challenges: past the of tion tois important It noteSC3 isthecontinua that cientific ǻ ǻ ǻ ǻ ǻ ǻ ǻ ǻ ǻ ǻ ture componentsmostly: performancefunctional, test of the infrastruc- the Infrastructure dedicated challenges to data filestorage andtransfer), Archive System(central base, data metadata Infrastructure Abstraction Layer (IAL) ORS), archive andorchestrate theproduction (CO - webtoclient enter processingin the plans structure services monitoring and control (M&C) nents and, the supportof the infrastructure compo- on the productionning infrastructure with ecution of a setof processing pipelines run- ex the to dedicated Challenges Scientific the C hallenge #3 of the infra- defined , , - - - Euclid PipelineworkflowforSC3 • • • • • • • from the simulation that act as first element to element first as act that simulation the from implemented and tested for the SC3 starting highlight inthefollowing chapterthe features all we function processing per function Processing ryable/retrievable withEuclid Archive services. que- Archiveso EuclidSystem and the in gested and processed by each Processing function is in- productdata Each supported by eachconnector or fitsfiles. definition and implementation in XML files and/ interface formal a of subject the been has flow work the of box each between connector Each low. be- 1 Figure in depicted is 3 Challenge Scientific intoworkflow implemented pipeline Euclid The mation. sources with astrometric /photometric infor is the merged multi-wavelengthof catalogue productdata output The basic ofthischallenge Consequently, themainobjectives ofSC3are: entific requirements. and itsconformityMER to asubsetof the sci To analyze / check the output data products of SDC’s Prods. data products:on thedifferent VIS/NIR/SIR/EXT input simulated with PFs these run To tion andDeployment component(CODEEN). Continuous Developement the Integration Valida through SDC each on PF each deploy To straction Layer). (EuclidArchive System,Infrastructure Ab - codes Infrastructurewith theSGS components To integrate thedifferent processing functions cessing functions(newfeatures, bugsfixed). To releasepro thecode of theVIS/NIR/SIR - acterization. and/or releasedeffects instrumental andchar- Mission Base(MDB)withnewfeaturesData the trueuniverseimages plus NIR/SIR the and To release codes thesimulation of the VIS/ ternal dataearlier inthedocument). ing Functions (PFs) (see also the articles on ex and EXT/DES EXT/KIDS of theMER, prototypes first the implement and Todesign Process ------• The astrometry catalogues as True input catalogues. No Gaia-like catalogues have been distributed yet • MICECAT v2 Figure 2 shows the the instrumental effects The current galaxy mock is implemented into the simulators.

- lectedIn total with 3x3 lowfields Star have Density been simulatedand moderate and be used in SC3. Those fields have been se

ZodiacalVIS/NIR/SIR/MER/EXT Light contamination. DES/EXT KIDS features This section compiles OUs and correspond- ing primary SDC integrated in the Euclid en- vironment with instrument features to be Figure 1: The Euclid pipeline workflow implemented into Scientific Challenge 3 analyzed during the SC3 Run. be ingested in the pipeline (instead obviously of - the real Data). Those are listed in figure 3 for VIS, NISP-P and NISP-S processing function and in fig Simulation (SIM) features Challenge.ure 4, for the first time, the MER and EXT/DES processing Functions are involved in a Scientific The input true universe catalogue is common Items marked with an asterisk * are not imple- mented for SC3

isto brighter,all simulators might andinclude channels. a brighter However magnitude some Actors limitchannels, cut in like the NISP-S, input cataloguewhere the to detection speed up limit the All the actors of the Science Ground Segment simulation. are involved in this process: • The star model used is the Besançon mod- • - el with the Basel 2.2 Spectral Library (M. tives, contributing to software development, Schultheis). Organization Units (OUs): defining the objec

data model (mostly data product definition)

Figure 2: The features of the simulations The Euclid Consortium Newsletter - Spring 2017 Figure 4:MER/EXT-DES/EXT-KiDS Figure 3:the VIS,NISP-P and NISP-S features implementation, and algorithms' validation. - • Science Data Centers (SDCs): implementing el…). Iterations occur till bugs are corrected and residuals, ghost detection, saturation, PSF mod the processing functions and transverse com- production begins anew. This incomplete list is ponents codes, setting up the development "based on actual events" taking place in SC3. The production infrastructure. • System Team: implementing the transverse Outcomeskey point is that challenges make things real! components (Euclid Archive, IAL, COORS, - M&C, CODEEN), supporting the integration livery to ESA. This delivery is based on the dif- and validation tests and the subversion to git ferentThe SC3 tags results of the in software an official components SGS software used defor migration. • as 100 % of the infrastructure software compo- the different software release, preparation of nentsSC3 production. are implemented This list and is now 50% quite of the significant process- theProject documentation Office: configuration patterns managementto be provided, of ing functions are running on production infra- arbitration of priorities: schedule vs features structure. The SC3 gives the opportunity to get a clear deadline. snapshot and status of the entire SGS and clari- implementation vs bug fixing to meet the Furthermore Instrument Development Teams - also contribute to SC3 by providing the cur- ponent. The documentation produced for SC3 rent best estimates of the instrumental models willfies andbe anconsolidates important the input roadmap for the of eachupcoming com stored in the Mission Data Base and thus used Design Review that the SGS should support this by the simulation code and the related process- year. ing functions. Next stage Benefits - The next challenges should gradually involve • to speed up the interactions between all the - The major benefits of the SC3 are: the Shear (SHE), Spectroscopic (SPE), Photo actors and force them to converge on an ac- cessing functions in the game. metric redshift (PHZ), and level 3 (LE3) pro - All other components SIM/LE1/VIS/NIR/SIR/ faces, MER/EXTs will continue releasing their code curate, unambiguous definition of their inter • to implement these interfaces in their code, according to their own roadmap, and taking into account lessons learnt from SC3: this will con- • • to iterate with their data providers and data to analyze in depth input and output products, customers, notedsist either that in these new features,SIM/LE1/VIS/NIR/SIR/MER/ change requests, bug fixing, validation completion. It should also be- • pate to SC4 to validate their new releases. EXTs components will be requested to partici to prioritize/arbitrate the implementation of • some features or bug fixing, November 2017; to anticipate on potential in- terfaceThe next issues, Scientific the EXT/SIR/NIR/VIS/MERChallenge (SC4) will start SC3 in to clarify ambiguities from requirements and/ - or interfaces definition and reformulate vided, a virtuous cycle takes place. Data are test- Once the first simulation data products are pro interfaceoutput products problem. will be provided to SPE/SHE/ PHZ for a first iteration useful to early identify ed, validated, new bugs are identified though an Christophe Dabin artefactin-depth correction analysis of (astrometry, the data. Processing non-linearity code is tested against its expected performance for Useful links: The SC3 wiki page: https://euclid.roe.ac.uk/projects/ec_sgs_challenges/wiki/20160308_Scientific_Challenge_3 The Euclid Mission Database: http://euclid.esac.esa.int/epdb/ The Euclid Consortium Newsletter - Spring 2017 C port Lead port servations Lead servations EC B NISP-P Instrument Scientist Calibration WGLead SWG LegacyCoordinators ECL Advisory andCoordinationECL Advisory Sup- EC SGSScientist VIS Project Manager Mission Survey Scientist EC Diversity CommitteeLead NISP Project Manager ESA Project Manager EC SGSProject Manager ESA Project Scientist EC Editorial Board Chair Mission System Engineer Science Performance Verification Lead EC Editorial Board co-Chair NISP-S Instrument Scientist EC SGSDeputy Project Manager Science Coordinators COMS Responsible VIS Instrument Lead VIS Instrument Scientist EC Complementary and Ancillary Ob- and Ancillary EC Complementary Euclid Lead Consortium ont act oard

Hannu Kurki-Suonio António daSilva Francisco Castander Romain Teyssier Andrea Cimatti Yannick Mellier Huub Röttgering Ralf Bender Werner Zeilinger Ray Carlberg Mark Cropper list M embers asilva fjc romain.teyssier a.cimatti mellier raymond.carlberg rottgering hannu.kurki-suonio werner.zeilinger bender msc ieec.uab.es Knud Jahnke Stefanie Wachter Chris Conselice Marc Sauvage Sabrina Pottinger Roberto Scaramella Stefanie Wachter MaciaszekThierry Giuseppe Racca Andrea Zacchei René Laureijs Peter Schneider Jerome Amiaux Hervé Aussel John Peacock Anne Ealet Christophe Dabin Henk Hoekstra Eugenie Girin Mark Cropper Ruymán Azzolini Yannick Mellier Jarle Brinchmann Michel Berthe Luigi Guzzo Tom Kitching Will Percival Jochen Weller Konrad Kuijken mssl.ucl.ac.uk astro.up.pt usm.lmu.de iap.fr strw.leidenuniv.nl unibo.it univie.ac.at utoronto.ca uzh.ch helsinki.fi Jason Rhodes Roberto Scaramella Olivier LeFèvre Lucia Popa Hans-Walter Rix Bob Nichol Rafael Rebolo Lopez Per Lilje Kristian Pedersen Sven De Rijcke jahnke wachter marc.sauvage sjp kosmobob wachter thierry.maciaszek Giuseppe.Racca zacchei rlaureij peter jerome.amiaux herve.aussel jap ealet Christophe.Dabin hoekstra girin msc r.azzollini mellier jarle michel.berthe luigi.guzzo t.kitching will.percival jochen.weller christopher.conselice kuijken mssl.ucl.ac.uk roe.ac.uk mssl.ucl.ac.uk strw.leidenuniv.nl cppm.in2p3.fr iap.fr astro.uni-bonn.de mpia.de iap.fr rssd.esa.int oats.inaf.it strw.leidenuniv.nl mpia.de mpia.de strw.leidenuniv.nl mssl.ucl.ac.uk ucl.ac.uk oa-roma.inaf.it brera.inaf.it cea.fr usm.uni-muenchen.de port.ac.uk cea.fr cea.fr cea.fr esa.int lam.fr lpopa rix bob.nichol rrl jason.d.rhodes kosmobob Olivier.LeFevre per.lilje kp sven.derijcke cnes.fr nottingham.ac.uk iac.es space.dtu.dk mpia.de spacescience.ro astro.uio.no oa-roma.inaf.it port.ac.uk jpl.nasa.gov UGent.be lam.fr The Organisational Units OU-VIS - Visual imaging OU-SIM - Simulations of Euclid data Henry McCracken hjmcc iap.fr Santiago Serrano serrano ieec.uab.es Catherine Grenet grenet iap.fr Anne Ealet ealet cppm.in2p3.fr Kevin Benson kmb mssl.ucl.ac.uk OU-MER - Merging of external and Euclid data OU-NIR - Near-IR imaging Adriano Fontana adriano.fontana oa-roma.inaf.it Gianluca Polenta gianluca.polenta @asdc.asi.it Hervé Dole Herve.Dole ias.u-psud.fr Rychard Bouwens bouwens strw.leidenuniv.nl Martin Kuemmel mkuemmel usm.lmu.de

OU-SIR - Near-IR spectroscopy OU-LE3 - Level 3 data Marco Scodeggio marcos lambrate.inaf.it Jean-Luc Starck jstarck cea.fr Yannick Copin y.copin ipnl.in2p3.fr Enzo Branchini branchini fis.uniroma3.it Filipe Abdalla fba star.ucl.ac.uk OU-SPE - Spectroscopic measurements Olivier Le Fèvre Olivier.LeFevre lam.fr OU-SHE - Shear measurements Christian Surace christian.surace lam.fr Andy Taylor ant roe.ac.uk Frédéric Courbin frederic.courbin epfl.ch OU-EXT - Data external to Euclid Tim Schrabback schrabba astro.uni-bonn.de Gijs Verdoes-Kleijn verdoes astro.rug.nl Joe Mohr jmohr usm.lmu.de OU-PHZ - Photometric redshifts Stephane Paltani stephane.paltani unige.ch Francesco Castander fjc ieec.uab.es

The Science Working Groups Weak lensing SWG Chris Conselice christopher.conselice nottingham.ac.uk Henk Hoekstra hoekstra strw.leidenuniv.nl Tom Kitching t.kitching ucl.ac.uk Clusters of galaxies SWG Martin Kilbinger (dpty) martin.kilbinger cea.fr Jochen Weller jochen.weller usm.uni-muenchen.de Lauro Moscardini lauro.moscardini unibo.it Galaxy clustering SWG Jim Bartlett (dpty) bartlett apc.univ-paris7.fr Luigi Guzzo luigi.guzzo brera.inaf.it Will Percival will.percival port.ac.uk CMB Cross-correlations SWG Yun Wang wang ipac.caltech.edu Carlo Baccigalupi bacci sissa.it Nabila Aghanim nabila.aghanim ias.u-psud.fr Galaxy & AGN evolution SWG Andrea Cimatti a.cimatti unibo.it Extrasolar planets SWG David Elbaz delbaz cea.fr Jean-Philippe Beaulieu beaulieu iap.fr Jarle Brinchmann jarle strw.leidenuniv.nl Maria Zapatero-Osorio mosorio iac.es Eamonn Kerins (dpty) eamonn.kerins manchester.ac.uk Milky Way and Resolved Stellar Populations SWG Eline Tolstoy etolstoy astro.rug.nl SNe and Transients SWG Annette Ferguson ferguson roe.ac.uk Charling Tao tao cppm.in2p3.fr Isobel Hook i.hook lancaster.ac.uk Local Universe SWG Enrico Cappellaro (dpty) enrico.cappellaro oapd.inaf.it Bianca Poggianti bianca.poggianti oapd.inaf.it he uclid onsortium ewsletter pring

T E C T N - S 2017 T Pablo Fosalba Cosmological Simulations SWG Jean-Gabriel Cuby Primeval Universe SWG Sune Toft Massimo Meneghetti Romain Teyssier Jean-Paul Kneib Strong lensingSWG Pierre Dubath SDC Switzerland Rees Williams SDC Netherlands Maurice Poncet SDC France Marco Frailis SDC Italy Keith Noddle SDC United Kingdom he he Valeria Pettorino Ariel Sanchez Slack channel S I nter cience -SWG T D a t a C askforce Pierre.Dubath o.r.williams Maurice.Poncet frailis [email protected] valeria.pettorino arielsan euclidist fosalba jean-gabriel.cuby sune romain.teyssier jean-paul.kneib massimo.meneghetti entres oats.inaf.it dark-cosmology.dk ieec.uab.es mpe.mpg.de rug.nl unige.ch cnes.fr gmail.com epfl.ch cea.fr lam.fr oabo.inaf.it Martin Kunz Raphael Gavazzi (dpty) Matteo(dpty) Viel Bruno Altieri Solar System Object SWG Luca Amendola SWGCosmological Theory Christian Neissner SDC Spain Harry TeplitzHarry SDC US Hannu Kurki-Suonio Maximilian Fabricius SDC Germany SDC Finland Tom Kitching neissner hit mxhf hannu.kurki-suonio t.kitching Martin.Kunz gavazzi viel bruno.altieri l.amendola ipac.caltech.edu oats.inaf.it mpe.mpg.de pic.es iap.fr ucl.ac.uk thphys.uni-heidelberg.de sciops.esa.int unige.ch helsinki.fi