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The EST and SOLARNET projects

The EST and SOLARNET projects. FRANCESCA ZUCCARELLO and the EST & SOLARNET TEAMS. Today : several national European solar facilities on Tenerife and La Palma. EST A large aperture 4-meter telescope to be built in the Canary Islands

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The EST and SOLARNET projects

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  1. The EST and SOLARNET projects FRANCESCA ZUCCARELLO and the EST & SOLARNET TEAMS

  2. Today: severalnationalEuropeansolarfacilitieson Tenerife and La Palma

  3. EST • A large aperture 4-meter telescope • to be built in the Canary Islands EST is promoted by EASTEuropean Association for Solar Telescopes: • a consortiumformedbyinstitutionsfrom 15 Europeancountrieswith the aim, amongothers, ofundertaking the developmentof the EuropeanSolarTelescope, tokeepEurope on the frontlineofSolarPhysics. Countries represented in EAST

  4. Countries represented in EAST Countries directly involved in the EST Design Phase Budget: 6.7 M€ FP-7 EC funding: 3.2 M€ 1 Feb 2008 - 30 June 2011 Project Coordinator: M. Collados (IAC) 29 partners plus 9 collaborating institutions

  5. EST goal is to provide ananswer to the following questions • How does the magnetic field evolve andemerge to the surface ? • How is energy transported from the photosphere to the chromosphere ? • How is the energy released deposited in the upper atmosphere ? • Why does the Sun have a hot chromosphere and a hot corona ? • What causes the explosive events (flares, filament eruptions, CMEs) ?

  6. Telescope and instrumentation key requirements • EST must specialise in simultaneous spectropolarimetry of the photosphere and the chromosphere • Must have superb optical quality, with very high throughput • Must have integrated high-order AO and MCAO • Must have spectrograph capabilities from blue to near-IR (with several simultaneous spectral regions) • Must have narrow-band tunablefiltergraphs from blue to near-IR, simultaneously accessible • Must have complementary imaging channels to observe photospheric and chromospheric layers (G-Band, Hα,…)

  7. Design baseline • 4-meter diameter • On-axis Gregorian configuration • Alt-Az mount • Simultaneous instrument stations (each with several wavelength channels) - Broad-band imager - Narrow-band tunable imager - Grating spectrograph • MCAO integrated in the optical path

  8. Diameterof the primarymirror: 4070 mm • Diameterof the secondarymirror: 800 mm • Spatialresolution on the solar disk: 30 km (goal 20 km)

  9. Beam from telescope NB1 (390-550 nm) Upper floor BB3 Ha CaII IR 30-70 BB1 CaII core 10-90 BB2 CaII wing BLUE NBNIR 1 (700-900 nm) D3 VIS RED 10-90 NB3 (700-900 nm) D1 D2 25/75 NIR GREEN-RED NBNIR2 900-1100 nm) 75-25 D4 NB2 (550-700 nm) Lower floor SPvis SPNIR

  10. IntegratedInfrastructureInitiative (I3) INFRA-2012-1.1.26 ResearchInfrastructuresforHigh-ResolutionSolarPhysics Grant Agreement no. 312495 • Purpose: • I3 combine in thiscall • Networkingactivities, • TransNational and Servicesactivities • Joint Researchactivities. Coordinatorinstitution : IAC

  11. SOLARNET : AIMS • Integrating the major European infrastructures in the field of high-resolution solar physics • Realise Trans-national Access to external European users • Enhance and spread data acquisition and processing expertise to the Europe-wide community • Increase the impact of high-resolution data by offering science-ready data and facilitating their retrieval and usage • Encourage combination of space and ground-based data by providing unified access to pertinent data repositories

  12. Data reduction and Archives • Pipelines • • GREGOR: GFPI, GRIS,BLISS • • SST: CRISP, TRIPPEL, CHROMIS • • THEMIS: MTR, TUNIS • • VTT: TESOS, LARS • • DST: IBIS, ROSA • Data Compression • ImageRestoration • SolarVirtualObservatory (SVO)

  13. SOLARNET : AIMS • Foster synergies between different research communities by organising meetings where each presents state-of-the-art methodologies • Train a new generation of solar researchers through setting up schools and a mobility programme

  14. SOLARNET : AIMS • Developprototypesfornew-generation post-focus instruments • Studylocal and non-localatmosphericturbulence, their impact on imagequality, and waysto negate theireffects • Improvedesignsof future largeEuropeanground-andspace-basedsolartelescopes

  15. SOLARNET: AdvancedInstrumentationDevelopment • Fourinstrumentstobedeveloped: • LargediameterEtalonDevelopment (100 – 300 mm) • Severallayouts are explored • Imageslicerfor 2D spectroscopy • Design developedfor EST hasbeenadaptedforGRIS@GREGOR • Microlens-fedspectrograph • mustbeadapted and optimizedforpolarimetricmeasurements • Fast ImagingPolarimeter • based on fast, low-noisepnCCDsensor

  16. Wavefrontcontrol • AdaptiveOptics (AO) • MulticonjugateAdaptiveOptics (MCAO) Simulations and Tests • Implementationofan AO prototypeforTHEMIS • Developmentofan innovative heatrejecterprototypeforGREGOR • AtmosphericSeeingCharacterization • Applicationof CFD techniquesforlocalseeingoptimization

  17. SynopticObservations SolarPhysicsResearch Network Group (SPRING) • 4workinggroups: • Synopticmagneticfields • Solarseismology • Transientevents • Solarawareness

  18. Previousexperience, limitations and advantages Ground-basedtelescopes: WavelengthrangelimitedbyEarth atmosphere absorption Radio observations (usefulforinstanceto investigate flares/CMEsproperties) not at the sameresolutionasopticalobservations (future: ALMA) Acquisitiontimeintervalseverelylimitedbychanges in seeingconditions Day/night constraints Higherangularresolution Possibilitytorepair, upgrade instruments Changeof the target in realtime Unique observations in the Hα line (patrol observations, but too low spatial resolution)

  19. Previousexperience, limitationsand advantages • Satellite Instruments: • Telemetry and data transfer limitation • Effectsofenergeticparticlesemittedduringsolarexplosiveevents • Instruments: itisnotpossibleto upgrade or repair • Lostof satellite control (see, e.g. SOHO) • Limitedtimeintervalof satellite observations (10 - 15 y ?) • Public release data • Pipelines (forinstance, Solar Software) almostimmediatelyavailable • Wellorganized data archives and repository

  20. Synergies, advantagesof GB and Satobservations • EST and ATST-DKIST have the advantageofmuchhigher data return, but are limitedtotheirvantagepoints on the Sun-Earthline. • Depending on the orbitalconfiguration, significantsynergy can beachievedbycombiningSolarOrbiter’sremote-sensing data witheitherhigh-resolution and/or high-cadenceco-spatial data fromotherobservatoriesthatprovideadditionalspatialcoverage • Authorswhouse high resolution GB data veryoften “like” to put them in a widercontext and thereforeusealsoSat data • The oppositeoccurslessoften (probablybecauseanaccessiblearchivedoesnotyetexists or because the pipelines are notalwaysavailable, butremember the SOLARNET goals and the work going on !!)

  21. Synergies, advantagesof GB and Satobservations • CoordinatedObservationalCampaigns: A Challenge • Tillnow the target mustbeselectedtwodays in advance: • willitbepossibletoshortenthistimeinterval ? • Howabouthaving the sametimecadence in data acquisition ? • Flaresissue

  22. Conclusions • The EST project is promoted by EAST (European Association for Solar Telescopes) • The Design Phase has been financed by EC (29 partners: 14 scientific institutions and 15 industries) • A new budget has been allocated to the EST-EAST community by EU: SOLARNET • Synergies with ATST-DKIST, Solar Orbiter and other GB and Sat facilities are necessary in order to achieve a better knowledge of the Sun. • EST website: http://www.iac.es/proyecto/EST • SOLARNET website:

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