Existing Planned and Envisaged facilities for Observational Solar Physics at E.N.O. Pere L. Pallé Instituto de Astrofísica de Canarias

Transcription

1 Existing Planned and Envisaged facilities for Observational Solar Physics at E.N.O. Instituto de Astrofísica de Canarias

2 Contents.. The context.. Brief historical overview to understand WHY and HOW. Present facilities and their scientific & technological value What s s Next The near future The envisaged future The dreams... Pag.- 2

3 The context.. 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) Pag.- 3

4 Observing the Sun.. NSO. SacPeak ENO Courtesy: Kevin Reardon (EGSO) Pag.- 4

5 Observing 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 Pag.- 5

6 Historical WHY and HOW.. JOSO (Joint Organization for Solar Observations): To promote international cooperation and TO FIND an outstanding site for a NEW European Solar Observatory (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) Pag.- 6

7 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 Agreement on Cooperation in Astrophysics (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). Pag.- 7

8 Some historical highlights 1964: First night telescope at OT ( 1982) 1971: First scientific solar images (Razdow( 1981) Pag.- 8

9 Some historical highlights 1964: First night telescope at OT ( 1982) 1971: First scientific solar images (Razdow( 1981) Pag.- 9

10 Outstanding science drivers.. Main (most) solar phenomena (affecting live on Earth) are intricately related to SMALL-SCALE SCALE MAGNETIC processes whose INNER WORKINGS are BEYOND what current telescopes can observe Pag.- 10

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12 Outstanding science drivers.. Main (most) solar phenomena (affecting live on Earth) are intricately related to SMALL-SCALE SCALE MAGNETIC processes whose INNER WORKINGS are BEYOND what current telescopes can observe Need to observe the Sun & its magnetic activities at 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.. : Exploit infrared solar spectrum Polarization with greater precision Larger fields of view Pag.- 12

13 The Observatories Pag.- 13

14 The Observatories La Palma Tenerife Pag.- 14

15 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) Pag.- 15

16 SST DOT Pag.- 16

17 GREGOR VTT THEMIS Pag.- 17

18 Solar Lab GCT * VNT * Pag.- 18

19 THEMIS SST SVST* VTT DOT VNT* GCT Razdow* Pag.- 19

20 VTT Vakuum Turm Teleskop Operated: Kiepenheuer Institut für Sonnenphysisk (KIS) Universitäts-Sternwarte Göttingen Max Plack-Institut für Aeronomie Astrophysikalisches Institut Potsdam Aperture 70 cm; Focal 4600 cm Evacuated Reflector, Tour Wavelength range: 0.35 µm 2 µm Instrument Capabilities: V, IR, AO, HRS, IVP, VP Instruments: POLIS (1 ), TESOS (0. 5), GFP (0. 2), TIP (1 ) Correlation Tracker, KAOS (AO) and now MCAO!! (14SEP04) Pag.- 20

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23 The instrument: : TIP M. Collados IAC The Tenerife Infrared Polarimeter (TIP) has been used attached to the German VTT of Observatorio del Teide FULL STOKES POLARIMETER Wavelength range: µm Spectral range: 7.5 A Field of view: 40 x 40 Pixel size: 0.38 x 30 ma Exposure time: 50 ms Modulation frequency: 2 Hz Pag.- 24

24 The analyzer Two ferroelectric liquid cristals (FLCs) are in charge of modulating the incoming light FLCs: Fixed retardance and two axis positions Incoming light FLC 1: λ/2 FLC 2: λ/4 FLC 1 & 2 Beamsplitter Temporal modulation: the same pixel is used The four Stokes parametres are measured simultaneously every 0.56 s. Pag.- 25

25 Spectral images I Q U V SiI HeI Tell. Pag.- 26

26 THEMIS Telescope Heliographique pour l Etude du Magnetisme et des Inestabilities Solaires Operated: INSU- CNRS CNR Aperture 90 cm; Focal 5760 cm Evacuated Cassegrain Coudé Wavelength range: 0.4 µm 0.8 µm Instrument Capabilities: V, HRS, VP, Corr-Track. UNIQUE CAPABILITY TO VP at simultaneous λ i UNIQUE CAPABILITY TO Instruments: MTR and MSDP (1 ) Configuration modes IPM (0. 7) Pag.- 27

27 THEMIS Pag.- 28

28 THEMIS Pag.- 29

29 Stokes parameters I (intensity), Q and U (linear polarization) and a V (circular polarization) for the three simultaneously observed lines: (from top to bottom) He D 3, Hα and the Ca II line at 8542Å.. Each plot, shows wavelength in the horizontal axis, and spatial direction along a the prominence in the vertical one. Image courtesy of A. López Ariste (THEMIS) Pag.- 30

30 MDSP: Simultaneous 2D spectral images (-0.75, -0.50, 0, and +0.75A at 8542 A ) Pag.- 31

31 Solar Laboratory Operated: IAC Collaboration with U. Birmingham, NSO, HAO and U. Thsing-Hua Node of Helioseismology International Networks: BiSON: Full disk K769.9 nm radial velocity GONG+: High resolution (5 ) I,V and magneth. at Ni nm ECHO: Medium (25 ) I,V at KI769.9 nm TON: High resolution (2 ) CaK nm Long Term (solar cycles) programs Pag.- 32

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38 SST Swedish Solar Telescope Operated: Institute for Solar Physics (RSAS) Aperture 97 cm; Focal 2030 cm Evacuated Refractor, turret Upgrade from 50 cm SVST ( ) Wavelength range: 0.35 µm 0.8 µm Instrument Capabilities: V, AO, HRS Low order AO + real time frame selection+ image restoration => resolution better than arcsec (90 Km) Instruments: Narrow band filters (0. 1) Future spectroscopy and VP (LPSP) Pag.- 39

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41 Km Pag.- 42

42 Km Pag.- 43

43 3D images Structures: Km height Pag.- 44

44 Operated: Universiteit Utrecht DOT Dutch Open Telescope Aperture 45 cm; Focal 200 cm Open newtonian Wavelength range: 0.35 µm 0.8 µm Instrument Capabilities: Narrow band photometry Alternative to AO: Speckle reconstruction (pros & cons) OPEN DOME demonstration concept: VALID First solar telescope to regularly obtain images over hours Instruments: Narrow band filters (0. 2) Pag.- 46

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48 The near future: GREGOR Operational 2005 at OT Upgrade of the 45 cm GCT Operated: Kiepenheuer Institut für Sonnenphysisk (KIS) Universitäts-Sternwarte Göttingen Max Plack-Institut für Aeronomie Aperture 150 cm; Focal 7500 cm Expected Seeing = Diffraction limit = = 70 Km Open Gregory Coudé Wavelength range: 0.35 µm 12 µm Instrument Capabilities: V, IR, AO, HRS, IVP, VP Lightweight optics (SiC( SiC) ) and mechanics Instruments: FP spec; Polarim spectrographs: Visible/Near UV and IR (TIP-II) Pag.- 52

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54 The envisaged future: 4m. ATST Advanced Technology Solar Telescope Unique tool to study the Sun Will replace major existing Solar Facilities (within USA) Expected lifetime years Addresses scientific challenges of today Look ahead when defining requirements (e.g. Multi Conjugate Adaptive Optics) Able to adapt to new scientific challenges Flexibility/Adaptability Pag.- 58

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56 The ATST in context Pag.- 60

57 Science requirements.. 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 Pag.- 61

58 Aperture: Resolution: Adaptive Optics: Telescope requirements FOV: Wavelength Coverage: 4 m diffraction limited: - within isoplanatic patch (AO) - over ~2 arcmin using MCAO (upgrade) Strehl ratio: >0.3, goal of S > 0.6 during good seeing 3 arcmin (goal 5 arcmin) 300 nm - 28 micron Polarization Accuracy: 10-4 (low instrumental polarization) Polarization Sensitivity: limited by photon statistics down to 10-5 Low Scattered Light: Coronagraph: Flexibility: Adaptability: e.g. sunspots: 1% of surrounding photosphere Corona: < 10-5 at R= 1.1R ; λ= = 1µ 1 in the NIR and IR e.g., Combine various post-focus instruments e.g., try out new ideas, bring your own instrument Pag.- 62

59 ATST Baseline Design.. Aperture: 4m Gregorian Off-Axis 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 Alt-Az Az Conventional Adaptive Optics (MCAO upgrade) Tip/tilt secondary Internal Seeing Control (thermal control of optics&structure) Contamination Control Enclosure - Hybrid Pag.- 63

60 ATST Concept Pag.- 67

61 ATST Concept Pag.- 68

62 Science Instruments.. Pag.- 69

63 The Candidate Sites Big Bear Solar Observatory, California Mees Solar Observatory, Haleakala,, Hawaii NSO/Sacramento Peak Observatory, New Mexico Observatorio Astronómico Nacional,, San Pedro Mártir,, Baja California, Mexico Observatorio Roque de Los Muchachos,, La Palma, Canary Islands, Spain Panguitch Lake, Utah Pag.- 70

64 ATST Timeline With and Without Long Lead Items Scientific Scientific and and Technical Technical Advisory Advisory Groups Groups Final Select Site Technology Development Concept & Design Demonstrate High-Order AO system Schedule with Early Mirror Procurement Schedule with mirror Procurement at beginning of construction phase CoDR PDR Pere L. CDR Pallé Mirror Procurement Mirror Procurement Construction Integration Integration Operation Pag.- 71

65 European Solar Physics Community already present: Scientific Advisor Committee Science Working Group Site Survey Working Group Proposal at FP-6 Pag.- 72

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67 The dreams: GISOT A peculiar approach for a solar ELT. Aperture shape 1 consisting of a central axial mirror with 4 m diameter and six offaxis mirrors with 2 m diameter, which form together an approximately elliptical shape of the aperture. Pag.- 74

68 Open framework structure of the telescope tube. Pag.- 75

69 Fig. 8 Open framework of the whole telescope structure. Pag.- 76

70 Fig. 9a/b Complete concept of the GISOT GISOT parked and tent closed. Pag.- 77

71 Conclusion We are already in the GOLDEN AGE of the Solar Physics Research.. E.N.O. (institutions, facilities and developments) plays (will continue playing) a key role Pag.- 78