8-EST_SOLARNET_Dublin_FZ_new_Zuccarellox

January 13, 2018 | Author: Anonymous | Category: Science, Astronomy, Telescopes
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The EST and SOLARNET projects FRANCESCA ZUCCARELLO and the EST & SOLARNET TEAMS

ESPM 14 Dublin 8-12 September 2014

Today: several national European solar facilities on Tenerife and La Palma

ESPM 14 Dublin 8-12 September 2014

ESPM 14 Dublin 8-12 September 2014

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 ESPM 14 Dublin 8-12 September 2014

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 ESPM 14 Dublin 8-12 September 2014

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) ?

ESPM 14 Dublin 8-12 September 2014

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,…)

ESPM 14 Dublin 8-12 September 2014

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

ESPM 14 Dublin 8-12 September 2014

ESPM 14 Dublin 8-12 September 2014

• 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 ESPM 14 Dublin 8-12 September 2014

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)

ESPM 14 Dublin 8-12 September 2014

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

ESPM 14 Dublin 8-12 September 2014

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 ESPM 14 Dublin 8-12 September 2014

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

ESPM 14 Dublin 8-12 September 2014

Synoptic Observations Solar Physics Research Network Group (SPRING)

4 working groups:  Synoptic magnetic fields  Solar seismology  Transient events  Solar awareness

ESPM 14 Dublin 8-12 September 2014

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) ESPM 14 Dublin 8-12 September 2014

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

ESPM 14 Dublin 8-12 September 2014

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: ESPM 14 Dublin 8-12 September 2014

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