Transcript 8-EST_SOLARNET_Dublin_FZ_new_Zuccarellox

The EST and SOLARNET projects
FRANCESCA ZUCCARELLO
and the EST & SOLARNET TEAMS
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Today: several national European solar facilities on Tenerife and La Palma
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EST
A large aperture 4-meter
telescope
to be built in the Canary Islands
EST is promoted by EAST
European Association for Solar
Telescopes:
a consortium formed by institutions
from 15 European countries with the
aim, among others, of undertaking
the development of the European
Solar Telescope, to keep Europe on
the front line of Solar Physics.
Countries represented
in EAST
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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
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EST goal is to provide an
answer to the following questions
• How does the magnetic field evolve and emerge 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) ?
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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 tunable filtergraphs from blue to
near-IR, simultaneously accessible
• Must have complementary imaging channels to observe
photospheric and chromospheric layers (G-Band, Hα,…)
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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
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• Diameter of the primary mirror: 4070 mm
• Diameter of the secondary mirror: 800 mm
• Spatial resolution on the solar disk: 30 km (goal 20 km)
Beam from telescope
NB1 (390-550 nm)
Upper floor
30-70
RED D3 10-90
NB3
(700-900 nm)
1090
BLUE
GREEN-RED
BB1 CaII core
NBNIR 1
(700-900 nm)
VIS
D2
D1
NIR
25/75
75-25
D4
NB2 (550-700 nm)
NBNIR2
900-1100 nm)
Lower floor
SPvis
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SPNIR
Integrated
Infrastructure Initiative
(I3)
INFRA-2012-1.1.26
Research Infrastructures for
High-Resolution Solar Physics
Grant Agreement no. 312495
Purpose:
I3 combine in this call
Coordinator institution :
IAC
1) Networking activities,
2) TransNational and Services
activities
3) Joint Research activities.
SOLARNET : AIMS
• Integrating the major European infrastructures in the field of highresolution 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
Data reduction and Archives
 Pipelines
• GREGOR: GFPI, GRIS,BLISS
• SST: CRISP, TRIPPEL, CHROMIS
• THEMIS: MTR, TUNIS
• VTT: TESOS, LARS
• DST: IBIS, ROSA
 Data Compression
 Image Restoration
 Solar Virtual Observatory (SVO)
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SOLARNET : AIMS
• Foster synergies between different
research communities by organising
meetings where each presents state-ofthe-art methodologies
• Train a new generation of solar
researchers through setting up schools
and a mobility programme
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SOLARNET : AIMS
• Develop prototypes
instruments
for
new-generation
post-focus
• Study local and non-local atmospheric turbulence, their
impact on image quality, and ways to negate their effects
• Improve designs of future large European ground-and spacebased solar telescopes
SOLARNET: Advanced Instrumentation
Development
Four instruments to be developed:
1. Large diameter Etalon Development
(100 – 300 mm)
Several layouts are explored
1. Image slicer for 2D spectroscopy
Design developed for EST has been adapted
for GRIS@GREGOR
1. Microlens-fed spectrograph
must be adapted and optimized for
polarimetric measurements
2. Fast Imaging Polarimeter
based on fast, low-noise pnCCD sensor
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Wavefront control
• Adaptive Optics (AO)
• Multiconjugate Adaptive Optics (MCAO)
Simulations and Tests
• Implementation of an AO prototype for THEMIS
• Development of an innovative heat rejecter
prototype for GREGOR
• Atmospheric Seeing Characterization
•Application of CFD techniques for local seeing
optimization
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Synoptic Observations
Solar Physics Research Network Group
(SPRING)
4 working groups:
 Synoptic magnetic fields
 Solar seismology
 Transient events
 Solar awareness
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Previous experience, limitations and advantages
Ground-based telescopes:
Wavelength range limited by Earth atmosphere absorption
Radio observations (useful for instance to investigate flares/CMEs
properties) not at the same resolution as optical observations (future:
ALMA)
Acquisition time interval severely limited by changes in seeing
conditions
Day/night constraints
Higher angular resolution
Possibility to repair, upgrade instruments
Change of the target in real time
Unique observations in the Hα line (patrol observations, but too low
spatial resolution)
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Previous experience, limitations
and advantages
Satellite Instruments:
Telemetry and data transfer limitation
Effects of energetic particles emitted during solar explosive
events
Instruments: it is not possible to upgrade or repair
Lost of satellite control (see, e.g. SOHO)
Limited time interval of satellite observations (10 - 15 y ?)
Public release data
Pipelines (for instance, Solar Software) almost immediately
available
Well organized data archives and repository
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Synergies, advantages of GB and Sat
observations
EST and ATST-DKIST have the advantage of much higher data
return, but are limited to their vantage points on the Sun-Earth line.
Depending on the orbital configuration, significant synergy can be
achieved by combining Solar Orbiter’s remote-sensing data with either
high-resolution and/or high-cadence co-spatial data from other
observatories that provide additional spatial coverage
 Authors who use high resolution GB data very often “like” to put
them in a wider context and therefore use also Sat data
 The opposite occurs less often (probably because an accessible
archive does not yet exists or because the pipelines are not always
available, but remember the SOLARNET goals and the work going
on !!)
Synergies, advantages of GB and Sat
observations
Coordinated Observational Campaigns: A Challenge
- Till now the target must be selected two days in
advance:
will it be possible to shorten this time interval ?
- How about having the same time cadence in data
acquisition ?
- Flares issue
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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