Existing Planned and Envisaged - extras.springer.comextras.springer.com/2006/978-1-4020-4351-2/Jenam/Session5/5Cpalle.… · Existing Planned and Envisaged ... • MDSP: Simultaneous

ExistingExistingPlannedPlanned andand

Envisaged Envisaged facilities for Observational facilities for Observational

Solar Physics at E.N.O.Solar Physics at E.N.O.

Pere L. PalléInstituto de Astrofísica de Canarias

Pere L. PallPere L. Palléé JENAMJENAM’’0404Granada. Sept.16Granada. Sept.16thth 20042004

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Contents . . Contents . .

•• The context ..The context ..•• Brief historical overview to understand Brief historical overview to understand

WHY and HOW WHY and HOW ……..•• Present facilities and their Present facilities and their ““scientific & scientific &

technologicaltechnological”” valuevalue……•• WhatWhat’’s Nexts Next……

– The near future– The envisaged future– The dreams . . .


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The context The context ……....

•• The Solar Physics domain . . .The Solar Physics domain . . .– “The Sun is the only ASTRONOMICAL object that

CRITICALLY MATTERS to humankind”Jack Harvey (NSO, USA)

– “ The Sun is the ROSETTA STONE of astrophysics, but we haven’t been able to decrypt it entirely” (…yet)

Goran Scharmer (SST, ENO)


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Observing the Sun . .Observing the Sun . .

Courtesy: Kevin Reardon (EGSO)

NSO. SacPeakENO


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Observing the SunObserving the Sun……....

• E.N.O. is lodging the best “battery” of ground-based observational Solar Physics facilities (Optical & IR):

– Quantity, Quality, Complementarities and innovative technological developments

– Allows access to most of the Sun’s layers: from the CORE to the outer ATMOSPHERE


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Historical Historical ““WHYWHY”” and and ““HOWHOW””....•• JOSO (Joint Organization for Solar Observations): JOSO (Joint Organization for Solar Observations): ““ To To

promote international cooperation and TO FIND an promote international cooperation and TO FIND an outstanding site for a NEW European Solar Observatoryoutstanding site for a NEW European Solar Observatory””(1969)(1969)– Systematic and coordinated investigations of the meteorological

and astronomical properties.– Campaign:

• 1969 till 1980 (!! One Solar Activity Cycle !!)

• Participation of 55 observers from 8 European countries

• 40 sites initially selected

• 15 extensively tested

• 2 finalists…. both in the CANARY ISLANDS

– Izaña. Tenerife ( Observatorio del Teide- OT)– Roque de los Muchachos. La Palma (ORM)


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•• Official conclusions:Official conclusions:– Both Canarian sites ONE ORDRE OF MAGNITUDE better

than any other tested site– “Image blurring and granulation images better at Izaña

than at Roque de los Muchachos”

•• The The ““Agreement on Cooperation in AstrophysicsAgreement on Cooperation in Astrophysics”” (1979)(1979)– Up to 19 countries and 60 institutions present up to now– IAC responsibility on MANAGING 20% + 5% OBSERVING TIME on

BEHALF and USE of the “WHOLE” astrophysical community – Together with the scientific and technical facilities provided by the

IAC at its headquarters in La Laguna (Tenerife) jointly constitute ..

the "European Northern Observatory" (ENO). the "European Northern Observatory" (ENO).


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Some historical highlightsSome historical highlights……•• 1964: First 1964: First ““nightnight”” telescope at OT ( telescope at OT ( ⇒⇒ 1982)1982)•• 1971: First scientific solar images (1971: First scientific solar images (RazdowRazdow ⇒⇒ 19811981))


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Some historical highlightsSome historical highlights……•• 1964: First 1964: First ““nightnight”” telescope at OT ( telescope at OT ( ⇒⇒ 1982)1982)•• 1971: First scientific solar images (1971: First scientific solar images (RazdowRazdow ⇒⇒ 19811981))


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Outstanding science drivers..Outstanding science drivers..

•• Main (most) solar phenomena (affecting live on Main (most) solar phenomena (affecting live on Earth) are intricately related to SMALLEarth) are intricately related to SMALL--SCALE SCALE MAGNETIC processes whose INNER WORKINGS MAGNETIC processes whose INNER WORKINGS are BEYOND what current telescopes can observeare BEYOND what current telescopes can observe


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Outstanding science drivers..Outstanding science drivers..

•• Main (most) solar phenomena (affecting live on Earth) are Main (most) solar phenomena (affecting live on Earth) are intricately related to SMALLintricately related to SMALL--SCALE MAGNETIC processes SCALE MAGNETIC processes whose INNER WORKINGS are BEYOND what current whose INNER WORKINGS are BEYOND what current telescopes can observetelescopes can observe

•• Need to observe the Sun & its magnetic activities at Need to observe the Sun & its magnetic activities at HIGHER RESOLUTION on three fronts:HIGHER RESOLUTION on three fronts:– Spatial (on solar surface and atmosphere)– Spectral (narrow δλ -> better measurement of magnetic fields and

thermodynamics)– Temporal (high cadence image & spectra of rapidly evolving ev)

•• Further . . :Further . . :– Exploit infrared solar spectrum– Polarization with greater precision– Larger fields of view


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The Observatories The Observatories ……


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The Observatories The Observatories ……

TenerifeLa Palma


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OT:TWO operational Solar Telescopes (VTT and THEMIS)A Solar Laboratory ( instrumentation of unique program)GREGOR telescope under construction

ORM:TWO operational Solar Telescopes (SST and DOT)Candidate for the ATST (tbc December’04)


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DOTDOT

SSTSST


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THEMISTHEMISGREGORGREGORVTTVTT


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VNT *VNT *

Solar LabSolar LabGCT *GCT *


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Razdow*

VNT* GCT

SVST*

VTT

DOT

THEMISSST


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VTTVTTVakuumVakuum TurmTurm TeleskopTeleskop

•• Operated:Operated:– Kiepenheuer Institut für Sonnenphysisk (KIS)– Universitäts-Sternwarte Göttingen– Max Plack-Institut für Aeronomie– Astrophysikalisches Institut Potsdam

•• Aperture 70 cm; Focal 4600 cm Aperture 70 cm; Focal 4600 cm •• Evacuated Reflector, TourEvacuated Reflector, Tour•• Wavelength range: 0.35 Wavelength range: 0.35 µµm m –– 2 2 µµmm•• Instrument Capabilities: V, IR, AO, HRS, IVP, VPInstrument Capabilities: V, IR, AO, HRS, IVP, VP•• Instruments:Instruments:

– POLIS (1”), TESOS (0.”5), GFP (0.”2), TIP (1”)– Correlation Tracker , KAOS (AO) and now MCAO ! ! (14SEP04)


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TheThe instrumentinstrument: TIP: TIP

M. Collados IACM. Collados IACThe Tenerife InfraredPolarimeter (TIP) has

been used attached to theGerman VTT of

Observatorio del Teide

FULL STOKES POLARIMETER

Wavelength range: 1-1.8 µm

Pixel size: 0.38´´ x 30 mA

Modulation frequency: 2 HzExposure time: 50 ms

Spectral range: 7.5 AField of view: 40´´ x 40´´


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TheThe analyzeranalyzer

Two ferroelectric liquidcristals (FLCs) are in charge of modulating the

incoming light

FLCs: Fixedretardance and two

axis positions

Incominglight

BeamsplitterFLC 1 & 2

FLC 2: λ/4

FLC 1: λ/2

The four Stokes parametres are measured simultaneously every 0.56 s.Temporal modulation: the same pixel is used


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Spectral imagesSpectral images

II

QQ

UU

VV

SiISiI HeIHeI Tell. Tell.


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THEMISTHEMISTelescope Telescope HeliographiqueHeliographique pour pour ll’’EtudeEtude dudu MagnetismeMagnetisme et et

des des InestabilitiesInestabilities SolairesSolaires

•• Operated:Operated:– INSU- CNRS– CNR

•• Aperture 90 cm; Focal 5760 cm Aperture 90 cm; Focal 5760 cm •• Evacuated Evacuated CassegrainCassegrain CoudCoudéé•• Wavelength range: 0.4 Wavelength range: 0.4 µµm m –– 0.8 0.8 µµmm•• Instrument Capabilities: V, HRS, VP, Instrument Capabilities: V, HRS, VP, CorrCorr--Track.Track.

•• UNIQUE CAPABILITY TO UNIQUE CAPABILITY TO VP at simultaneous VP at simultaneous λλii•• Instruments:Instruments:

– MTR and MSDP (1”) Configuration modes– IPM (0.”7)


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THEMISTHEMIS


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THEMISTHEMIS


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•• Stokes parameters I (intensity), Q and U (linear polarization) aStokes parameters I (intensity), Q and U (linear polarization) and V nd V (circular polarization) for the three simultaneously observed li(circular polarization) for the three simultaneously observed lines: (from nes: (from top to bottom) He Dtop to bottom) He D3 3 , , HHαα and the Ca II line at 8542and the Ca II line at 8542ÅÅ. Each plot, . Each plot, shows wavelength in the horizontal axis, and spatial direction ashows wavelength in the horizontal axis, and spatial direction along the long the prominence in the vertical one . Image courtesy of A. prominence in the vertical one . Image courtesy of A. LLóópezpez AristeAriste (THEMIS) (THEMIS)


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•• MDSP: Simultaneous 2D spectral imagesMDSP: Simultaneous 2D spectral images((--0.75, 0.75, --0.50, 0, +0.50 and +0.75A at 8542 A )0.50, 0, +0.50 and +0.75A at 8542 A )


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Solar LaboratorySolar Laboratory

•• Operated:Operated:– IAC– Collaboration with U. Birmingham, NSO, HAO and U. Thsing-Hua

•• Node of Node of HelioseismologyHelioseismology International Networks:International Networks:– BiSON: Full disk K769.9 nm radial velocity– GONG+: High resolution (5”) I,V and magneth. at Ni 676.8 nm – ECHO: Medium (25”) I,V at KI769.9 nm– TON: High resolution (2”) CaK 393.4 nm

•• Long Term (solar cycles) programsLong Term (solar cycles) programs


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SSTSSTSwedish Solar TelescopeSwedish Solar Telescope

•• Operated:Operated:– Institute for Solar Physics (RSAS)

•• Aperture 97 cm; Focal 2030 cm Aperture 97 cm; Focal 2030 cm •• Evacuated Refractor, turretEvacuated Refractor, turret•• Upgrade from 50 cm SVST (1985 Upgrade from 50 cm SVST (1985 ––2002)2002)•• Wavelength range: 0.35 Wavelength range: 0.35 µµm m –– 0.8 0.8 µµmm•• Instrument Capabilities: V, AO, HRSInstrument Capabilities: V, AO, HRS•• Low order AO + real time frame selection+ image Low order AO + real time frame selection+ image

restoration restoration => resolution better than 0.=> resolution better than 0.””12 12 arcsecarcsec (90 Km)(90 Km)•• Instruments:Instruments:

– Narrow band filters (0.”1)– Future spectroscopy and VP (LPSP)


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80 “57000 Km


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40 “29000 Km

28 “


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3D images3D images……

Structures: 200Structures: 200--450 Km height450 Km height


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DOTDOTDutch Open TelescopeDutch Open Telescope

•• Operated:Operated:– Universiteit Utrecht

•• Aperture 45 cm; Focal 200 cm Aperture 45 cm; Focal 200 cm •• Open Open newtoniannewtonian•• Wavelength range: 0.35 Wavelength range: 0.35 µµm m –– 0.8 0.8 µµmm•• Instrument Capabilities: Narrow band photometryInstrument Capabilities: Narrow band photometry•• Alternative to AO: Speckle reconstruction (pros & cons)Alternative to AO: Speckle reconstruction (pros & cons)•• OPEN DOME demonstration concept: VALIDOPEN DOME demonstration concept: VALID•• First solar telescope to regularly obtain 0.First solar telescope to regularly obtain 0.””2 images over 2 images over

hourshours•• Instruments:Instruments:

– Narrow band filters (0.”2)


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The near future: GREGOR The near future: GREGOR Operational 2005 at OTOperational 2005 at OT

Upgrade of the 45 cm GCTUpgrade of the 45 cm GCT•• Operated:Operated:

– Kiepenheuer Institut für Sonnenphysisk (KIS)– Universitäts-Sternwarte Göttingen– Max Plack-Institut für Aeronomie

•• Aperture 150 cm; Focal 7500 cm Aperture 150 cm; Focal 7500 cm •• Expected Seeing = Diffraction limit = 0.Expected Seeing = Diffraction limit = 0.””1 = 70 Km 1 = 70 Km •• Open Gregory Open Gregory CoudCoudéé•• Wavelength range: 0.35 Wavelength range: 0.35 µµm m –– 12 12 µµmm•• Instrument Capabilities: V, IR, AO, HRS, IVP, VPInstrument Capabilities: V, IR, AO, HRS, IVP, VP•• Lightweight optics (Lightweight optics (SiCSiC) and mechanics) and mechanics•• Instruments:Instruments:

– FP spec; Polarim spectrographs: Visible/Near UV and IR (TIP-II)


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The envisaged future:The envisaged future:4m. ATST4m. ATST

Advanced Technology Solar TelescopeAdvanced Technology Solar Telescope

•• Unique tool to study the Sun Unique tool to study the Sun

•• Will replace major existing Solar Facilities (within USA)Will replace major existing Solar Facilities (within USA)

•• Expected lifetime 30Expected lifetime 30--40 years40 years

•• Addresses scientific challenges of todayAddresses scientific challenges of today

•• Look ahead when defining requirements (e.g. Multi Look ahead when defining requirements (e.g. Multi Conjugate Adaptive Optics) Conjugate Adaptive Optics)

•• Able to adapt to new scientific challengesAble to adapt to new scientific challenges

•• Flexibility/AdaptabilityFlexibility/Adaptability


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The ATST in contextThe ATST in context……


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Science requirements..Science requirements..

•• Key drivers of telescope design:Key drivers of telescope design:– Image Quality

• Diffraction limited optical spectroscopy & polarimetry

• Near IR spectral polarimetry

• Near IR coronal magnetometry

– Polarization• Optical and IR polarimetry use

– Scattered Light• Near IR coronal magnetometry


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Telescope requirementsTelescope requirements•• Aperture:Aperture: 4 m4 m•• Resolution:Resolution: diffraction limited:diffraction limited:

-- within within isoplanaticisoplanatic patch (AO)patch (AO)-- over ~2 over ~2 arcminarcmin using MCAO (upgrade) using MCAO (upgrade)

•• Adaptive Optics:Adaptive Optics: StrehlStrehl ratio: >0.3 , goal of S > 0.6 ratio: >0.3 , goal of S > 0.6 during good seeingduring good seeing

•• FOV:FOV: 3 3 arcminarcmin (goal 5 (goal 5 arcminarcmin))•• Wavelength Coverage:Wavelength Coverage: 300 nm 300 nm -- 28 micron28 micron•• Polarization Accuracy: Polarization Accuracy: 1010--44 (low instrumental polarization)(low instrumental polarization)•• Polarization Sensitivity:Polarization Sensitivity: limited by photon statistics down to 10limited by photon statistics down to 10--5 5

•• Low Scattered Light:Low Scattered Light: e.g. sunspots: 1% of surrounding photospheree.g. sunspots: 1% of surrounding photosphereCorona: < 10Corona: < 10--55 at R= 1.1Rat R= 1.1R ; ; λλ= 1= 1µµ

•• Coronagraph:Coronagraph: in the NIR and IRin the NIR and IR•• Flexibility:Flexibility: e.g., Combine various poste.g., Combine various post--focus instrumentsfocus instruments•• Adaptability: Adaptability: e.g., try out new ideas, bring your own e.g., try out new ideas, bring your own

instrumentinstrument


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ATST Baseline Design..ATST Baseline Design..•• Aperture: 4mAperture: 4m•• Gregorian Gregorian •• OffOff--AxisAxis

– Unobstructed Aperture– Clean PSF, High Strehl– Easy access to: prime focus, heat stop, occulting, secondary– No hot objects in beam > Internal seeing control easier– Scattered light control– Rotating spiders cause problems with WFS flat field

•• AltAlt--AzAz•• Conventional Adaptive Optics (MCAO upgrade)Conventional Adaptive Optics (MCAO upgrade)•• Tip/tilt secondaryTip/tilt secondary•• Internal Seeing Control (thermal control of optics&structure)Internal Seeing Control (thermal control of optics&structure)•• Contamination Control Contamination Control •• Enclosure Enclosure -- HybridHybrid


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ATST Concept


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ATST Concept


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Science Instruments..Science Instruments..


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The Candidate SitesThe Candidate Sites

Big Bear Solar Observatory, CaliforniaBig Bear Solar Observatory, CaliforniaMeesMees Solar Observatory, Solar Observatory, HaleakalaHaleakala, Hawaii, HawaiiNSO/Sacramento Peak Observatory, New MexicoNSO/Sacramento Peak Observatory, New MexicoObservatorioObservatorio AstronAstronóómicomico NacionalNacional, San Pedro , San Pedro MMáártirrtir, Baja California, Mexico, Baja California, MexicoObservatorioObservatorio RoqueRoque de Los de Los MuchachosMuchachos, La Palma, , La Palma, Canary Islands, SpainCanary Islands, SpainPanguitchPanguitch Lake, UtahLake, Utah


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ATST TimelineATST TimelineWith and Without Long Lead ItemsWith and Without Long Lead Items

20032003 2005200520042004 20062006 20072007 20082008 20092009 20102010 20112011 20122012 20132013

Technology DevelopmentTechnology

Development

Concept & DesignConcept & Design

Final Select SiteScientific and Technical Advisory GroupsScientific and Technical Advisory Groups

IntegrationIntegrationPDR

CDR

Demonstrate High-Order AO system

CoDR

IntegrationIntegration

Mirror ProcurementMirror Procurement

Mirror ProcurementMirror Procurement

Schedule with Early Mirror Procurement

Schedule with mirror Procurement at

beginning of construction phase

ConstructionConstruction

OperationOperation


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••European Solar Physics Community already European Solar Physics Community already present:present:

•• Scientific Advisor CommitteeScientific Advisor Committee•• Science Working GroupScience Working Group•• Site Survey Working GroupSite Survey Working Group

••Proposal at FPProposal at FP--6 6 ……


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The dreams:The dreams:GISOTGISOT

A peculiar approach for a solar ELTA peculiar approach for a solar ELT…………..

Aperture shape 1 consisting of a central axial mirror with 4 m diameter and six off-axis mirrors with 2 m diameter, which form together an approximately elliptical shape of the aperture.


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Open framework structure of the telescope tube.


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Fig. 8Fig. 8

Open framework of the whole telescope structure.


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Fig. 9a/bFig. 9a/b

GISOT parked and tent closed.Complete concept of the GISOT


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ConclusionConclusion

•• We are already in the GOLDEN AGE of the We are already in the GOLDEN AGE of the Solar Solar Physics ResearchPhysics Research....

•• E.N.O. (institutions, facilities and developments) E.N.O. (institutions, facilities and developments) plays (will continue playing) a key roleplays (will continue playing) a key role……

Existing Planned and Envisaged - extras.springer.comextras.springer.com/2006/978-1-4020-4351-2/Jenam/Session5/5Cpalle.… · Existing Planned and Envisaged ... • MDSP: Simultaneous

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