est and the future of european solar astronomy
TRANSCRIPT
EST and the future of European solar astronomy
Manuel Collados and the EST team
EST: With a 4.2-metre primary mirror, it will be
the largest solar telescope in Europe
• Excellent polarimetric performance
• Superb spatial resolution
• Adequate set of instruments formultiwavelength imaging and spectropolarimetry
European Association for Solar Telescopes (EAST)
29 Institutions18 European countries
Schedule
PREPARATORY PHASECONSTRUCTION
EST Europeanstrategic
infrastructure(ESFRI) 2016
OPERATION
Project Office
Design consolidation
Telescope preliminary design
Site selection
Preparatory Phase Objectives
Specifications for detailed design and construction
Environmental impact study
Basic construction project
Final construction plan and cost book
Selected site at ORM
EST
Telescope light path
Telescope
Primary mirrorM1 (4.2 metros)
Adaptive Secondary MirrorM2
Heat rejecter
Telescope structureEST is a 4.2-metre solar telescopewith an on-axis Gregorian configuration
Primary Mirror
M1
ASSE
MBL
Y BLANK
ACTUATORS
THERMAL CONTROL
CELL
Heat rejecter
Heat rejecter
Hottest point of the while telescope.
Coolant inside the heat rejecter
Cooling system
Warm airCold air
Light cone feeding thesecondary morrir
Adaptive Secondary Mirror
First adaptive secondary mirror at a solar telescope
(800 mm diameter,~ 2000 actuators)
Focal plane Diameter (Aprox) Pitch (Aprox) Stroke (TBC)
DM 20KM 134,99mm 64 mm4,3 5 µm PtV
DM 12KM 92,23mm 75,7mm5 5 µm PtV
DM 9KM 78,33mm 85,7mm 5,75 µm PtV
DM 5km 260,14mm 119mm 85 µm PtV
• 4 ALTITUDE DMs• LAB OPTICAL BENCH• THERMAL CONTROL
DM MIRRORS PERFORMANCE
AO/MCAO system shall have enough range
and bandwidth to control de distortion
produced by seeing and wind.
TELESCOPE OPTICS TEMPERATURE
The temperature difference of the telescope
optics exposed to ambient air shall not exceed
+0.5ºC/-0.5ºC.
MCAO / TRANSFER OPTICS
CONTROL IS A CHALLENGE: NUMERICAL SIMULATIONS AND LABORATORY EXPERIMENTS NEEDED!!
Enclosure
OPTICS INSIDE PIER
Coudé InstrumentRoom
POP(vacuum tube)
Light distribution - Instruments
First generation
Courtesy ofJ. de la Cruz Rodriguez
Tunable Imaging Spectropolarimeter (TIS):Fabry-Perot Interferometers
CRISP@8542, the Swedish 1-m Solar Telescope
Tunable Imaging Spectropolarimeter (TIS):Fabry-Perot Interferometers
2D FoV and Spectrumsimultaneous:IAC Slicer IFU
Integral Field Spectrograph(IFS):based on image slicers
H! 656.3 nm - MIHI (SST, Courtesy of Michiel van Noort)
Integral Field Spectrograph(IFS):based on microlenses
Telescope
380-500 nm
680-2200 nm
680-1000 nm
1000-2200 nm
TIS/FBI V500-680 nm380-680 nm
500-680 nm
IFS V500-680 nm
IFS R680-1000 nm
IFS IR1083 nm1565 nm
TIS/FBI B380-500 nm
TIS/FBI R680-1000 nm
Exchangeable optical element
Dichroic BS
1. Dichoic BS2. Mirror3. Intensity BS
IFS Integral Field Spectro-polarimeter
TIS Tunable Imaging Spectro-polarimeter / Fixed Band Imager
I12200 nm
I3500-680 nm
I4380-500 nm
I2680-1000 nm
IFS B380-500 nm
D2B
D2R
R2R1
B1 B2
V2
V1
IR
D1
Second generation
Light distribution - Instruments
Technologies
Macro-optomechanics
Micro-optomechanics
All kind of optomechanical elements
Thermal control
Sensors for system control
Data handling. User interfaces
Civil works
Environmental studies
Services (coolant, air conditioning …)
