1st SPRING Workshop, November 26 – 28, 2013

Submitted titles and abstracts of the talks

Tuesday, November 26, 2013


Session I – Introduction


Markus Roth
Kiepenheuer-Institut für Sonnenphysik, Freiburg, Germany
The High-resolution Solar Physics Network (Solarnet)  is a new collaborative project of the European research groups active in solar physics funded under the European Union’s Framework Programme 7. Among others, one of the work packages of Solarnet is the Solar Physics Research Integrated Network Group (SPRING) which aims at designing a new network of ground-based full-disk telescopes for synoptic observations of the Sun.

In my talk I will summarize the activities of Solarnet and will report on the status of SPRING. Furthermore I will motivate the reasons for this meeting to provide a framework and schedule to collect the talks at the workshop and distill them into a scientific requirements document for SPRING.




Session II – Scientific drivers for a new synoptic network



Hector Socas-Navarro
Instituto de Astrofísica de Canarias, LaLaguna, Tenerife, Spain
Scientific requirements for a network of synoptic observatories in order to provide context data for the future high-resolution telescopes

In this presentation I will discuss some science requirements of the SPRING network of synoptic telescopes focusing on its use as context imagers for the future large-aperture telescopes (and, in particular, the EST). I will review some of the SPRING instrument concepts and briefly discuss possible advantages and disadvantages of each one.





Ales Kučera, Peter Gömöry
Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovakia
Solar local and global magnetism - new challenge for long-lasting synoptic observations
Open questions on local and global solar magnetism are summarized concerning a design of new generation of solar synoptic telescopes. Do we need long lasting polarimetric observations with synoptic facilities? If yes, what concept of synoptic telescopes we needs to keep sufficient spatial, spectral and temporal resolutions and measure full stokes parameters?




Rolf Schlichenmaier
Kiepenheuer-Institut für Sonnenphysik, Freiburg, Germany

Science with synoptic sunspot observations




Juan Manuel Borrero

Kiepenheuer-Institut für Sonnenphysik, Freiburg, Germany
Requirements for future synoptic measurements of the Sun's magnetic field




Michael Thompson
High-Altitude Observatory, Boulder, USA
Science requirements for chromospheric science




Frank Hill
National Solar Observatory, Tucson, USA
Science requirements for future helioseismology




Ilaria Ermolli
INAF Osservatorio Astronomico di Roma
Requirements from irradiance studies




Wednesday, November 27, 2013



Wolfgang Finsterle
World Radiation Center / PMOD, Davos
Space weather forecasting with radio observations
PMOD/WRC is developing a novel method for nowcasting and reconstructing the solar irradiance based on simultaneous measurements of radio flux at several wavelengths. These radio flux measurements can be used to decompose the solar activity into relative contributions from spots, faculae and the quiet sun. Such decomposition will, in turn, allow us to reconstruct the entire solar spectrum for the periods for which radio measurements are available using the theoretical knowledge of the entire solar spectrum for each component.




Dario Del Moro1, Stuart Jefferies2, and Francesco Berrilli1

1 Physics dept., University of Rome ToV, Italy
2IfA, University of Hawaii, USA

Multi-height observations with MOTH



Session III – Instrument Concepts



Dirk Soltau

Kiepenheuer-Institut für Sonnenphysik, Freiburg, Germany
General Considerations on Wide-Field Telescopes and Image Stabilisation




Miroslav Klvaňa, Michal Sobotka, and Michal Švanda
Astronomical Institute, Academy of Sciences of the Czech Republic, Ondřejov 
Optimised data archiving for a synoptic telescope
Modern telescopes easily produce so large volumes of data that not only their processing but even a manipulation with them becomes difficult. Therefore, the data are often discarded only for the reason that they do not contain the anticipated effect. The problems of storing large data volumes are currently solved mainly by data compression and an increase of storage capacities. On the other hand, large data volumes can be reduced by means of a selection of useful information.

In this work we describe required properties of a synoptic telescope, its basic functions, and present possibilities of their implementation. We discuss restrictions of the telescope's design imposed by characteristics of the currently available image detectors. The work is focused to the description of optimised data archiving that substantially reduces the archived volume of data down to 1 % of standard requirements. The method is suitable for an archiving of fast processes in the solar atmosphere. Thanks to the strongly reduced storage capacity it is possible to record the entire process without any time limitations. Algorithms needed for a full automation of observations and archiving of all data acquired by the synoptic telescope, including the fast processes, are currently elaborated.




Joachim Staiger
Kiepenheuer-Institut für Sonnenphysik, Freiburg, Germany

Spectrometer HELLRIDE as a Testing System for Fulldisk Velocity Mapping
We have recently installed the new etalon-based 2D-spectrometer HELLRIDE at the VTT which will be used for the analysis of waves in the solar atmosphere (HELLRIDE: Helioseismological Large Regions Interferometric Device). This instruments allows to measure velocities within up to 16 different atmospheric layers at a cadence of 1 Min in a quasi-simultaneous mode. The standard field-of-view is 100" by 100". By mosaic-type tiling a synthetic aperture of up to 300" by 300" has been successfully tested. The core element for  multiline operation is a matrix-type prefilter grid-mount allowing for fast wavelength band changes.

We plan to use this instrument at the VTT for full-disk spectrometer tests. We have created a full-disk setup receiving sunlight from the VTT guiding telescope by beam splitter. The test telescope aperture is 5 cm. The full-disk image has a diameter of 1.5 cm. We will place the HELLRIDE dual etalon configuration in front of the disk image using a collimated beam setup. We will carry out multiline tests in 2014 to find out the temporal and spectral resolution limits for full-disk line scanning.

We will describe the current status of HELLRIDE. We will describe hardware components and system properties. We will report about planned remote operation features and improvements.




Haosheng Lin
Institute for Astronomy, University of Hawaii

Demonstration of a 31-slit Full-Disk Spectroheligraph




Siraj Hasan
Indian Institute of Astrophysics, Bangalore
NLST and Solarnet
NLST is a two meter class solar telescope to be installed in Ladakh, India at a high altitude site at 4500 meters.
The high altitude and low humidity makes this an ideal site for near IR observations. The NLST location of longitude 78° 57' E makes it as one of the most important solar telescopes filling the longitude gap between Japan and Europe. This will ensure continuous observation of the Sun. The NLST instruments with fast narrow band imaging and spectropolarimetric capabilities will be able to provide data for local helioseismic studies. An important goal for NLST will be to observe the magnetic field and dynamic changes associated with active regions using high-resolution and good cadence vector magnetograms. The high spatial resolution data, in principle, will generate its own scientific interests and can also be used for support with other low resolution synoptic data (like in combination with full-disk H-alpha imager).
Simultaneous observations in G-Band, Ca II K - H, and would be facilitated along with NLST through use of full-disk mode auxiliary telescopes located close to the NLST site. Synoptic data would be routinely generated and made available to the solar community to understand the interconnections between small-scale and largescale structures especially in active regions. International collaborations will play an important role in the backend instrument development for NLST. The project is expected to be completed in 2019.




Toufik Abdelatif
CRAAG, Solar Physics Division, Algiers
A new Space Weather Observatory in Tamanrasset
The CRAAG  Solar Physics division  (Center of Astronomy, Astrophysics and Geophysics)  in Algiers plan to install a number of instruments at its unit in Tamanrasset  (southern part of Algeria). This unit has long been a magnetic station since 1930 and now is a INTERMAGNET station. The scientific objective of the project is to install instruments for studying the ionosphere because Tamanrasset is at 17 ° north of the magnetic equator and is therefore under the influence of the equatorial electrojet. The monitoring of solar activity will be done by flare patrol using H alpha observations and the spectro radiometric measurements. All data will be locally processed.  We will present the different instruments considered for this  new observatory.




Salvatore Scuderi
INAF - Osservatorio Astrofisico di Catania
Conceptual design study of a Broad Band Imager for the European Solar Telescope
We will describe the results of the conceptual study of a Broad Band Imager  (BBI) for the European Solar Telescope (EST), the project to realize a 4-m class solar telescope.
The EST Broad Band Imager is an imaging instrument whose function is to obtain diffraction limited images over the full field of view of EST at multiple wavelengths and high frame rate. Its scientific objective is the study of fundamental astrophysical processes at their intrinsic scales in the Sun’s atmosphere. The optical layout foresee two observational modes: a maximum field of view mode and a high resolution mode. The imager will have a 2'x2' corrected field of view in the first mode and an angular resolution better than 0.04" at 500nm in the latter mode. The imager will cover a wavelength range spanning from 390nm to 900nm through a number of filters with bandpasses between 0.05nm and 0.5nm. To optimize optical performances and throughput there will be two arms working simultaneously: a blue arm (covering the 380nm – 500nm range) and a red arm (600nm – 900nm). The blue arm will have two channels while the red arm only one. Each channel will be divided in three subchannels: one will host narrow band filters for chromospheric observations, another one, in focus wide band filters used as reference for speckle reconstruction and photospheric observations, and the last one, out of focus wide band filters for phase diversity reconstruction of photospheric observations.




Thursday, November 28, 2013


Session IV – Existing Infrastructures



Ganghua Lin
National Astronomical Observatories Chinese Academy of Sciences, Beijing
Solar Physics Observation and Research in China
In our presentation, four aspects are introduced: Chinese solar telescopes, observational and research achievements, data handling, and some thinks on future instrumental development.



Ales Kučera
Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovakia

Existing solar physics facilities and data bases at Astronomical institute of the Slovak Academy of Sciences
A brief summary of existing solar physics synoptic facilities and data bases at Astronomical Institute of the Slovak Academy of Sciences is given. Namely observations and data sets from the Double coronagraph at Lomnicky stit observatory are presented - "Homogeneous series of coronal green line intensities"(1939 - present) and "Catalogue of solar prominences (1967-present) and and white light observations from double solar telescope.




Salvatore Scuderi

INAF - Osservatorio Astrofisico di Catania
Infrastructure and facilities available at INAF – Catania Astrophysical Observatory
Observations of the Sun have been carried out at the INAF - Catania Astrophysical Observatory (OACt) since 1880. Current full-disc observations of the solar photosphere and chromosphere are performed by means of an equatorial spar equipped with two 150 mm refractors feeding two Halpha Lyot filters. These data are daily available for the scientific community and are distributed to several international Solar Data Centers.
We briefly describe the facilities available at the INAF – OACt with particular attention to the main characteristics of the observing mountain station M.G. Fracastoro, located on the southern slope of Mt. Etna volcano at Serra La Nave (1735 m a.s l) and to its related infrastructures.




Alexei Pevtsov
National Solar Observatory, Sunspot, USA
Status of the SOLIS instrument and recent research based on SOLIS data



P. Gömöry1, J. Ambróz1, J. Koza1, M. Kozák1, A. Kučera1, J. Rybák1, P. Schwartz1, S. Tomczyk2, S. Sewell2, P. Aumiller2, R. Summers2, L. Sutherland2, A. Watt2

1 Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovakia

2 High Altitude Observatory, The National Center for Atmospheric Research, Boulder, USA

Solar Chromospheric Detector for the Lomnicky peak Observatory – towards synoptic imaging spectroscopy and spectro-polarimetry.
We present technical parameters and observing capabilities of the Solar Chromospheric Detector (SCD) destined for the Lomnicky Peak Observatory (Slovakia). The core of SCD is a five-stage Lyot filter followed by polarization unit with operational spectral range from 500

nm to 1100 nm. The instrument will deliver full-disk imaging spectroscopy and spectro-polarimetry of the chromosphere and photosphere sequentially in several spectral lines. An ambition of the project is to advance current synoptic solar observations towards more comprehensive datasets involving Doppler shifts, spectral widths, and also information about magnetic fields. 




Session IV - Organization



Jesper Schou
Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau
Dos and don'ts when developing a helioseismology instrument




Alexei Pevtsov
National Solar Observatory, Sunspot, USA

Current status of the IAU Working Group on Coordination of Synoptic Observations of the Sun




Guy Davis
University of Birmingham, UK
Learning from over 30 years of BiSON operations
SPRING will lead to proposals of a ground-based network of telescopes and as such can benefit from the practical experience of BiSON or GONG.  Here we present the utopian concept of BiSON mini: a paradigm where many small and cheap Sun-as-a-star observatories form a large and widely distributed ground-based network; where contemporaneous data can be exploited to achieve a better calibration and produce higher signal-to-noise data sets. Yet, this is a network where logistics and day-to-day management can remain tractable. Through this blue sky thinking we show that lessons learnt by BiSON will benefit SPRING.