1st SPRING Workshop, November 2013 Optimised data archiving for a synoptic telescope M. Klvaňa, M. Sobotka, and M.Švanda Astronomical Institute, Academy.

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1st SPRING Workshop, November 2013 Optimised data archiving for a synoptic telescope M. Klvaňa, M. Sobotka, and M.Švanda Astronomical Institute, Academy of Sciences of the Czech Republic, Ondřejov

Purposes of a solar synoptic telescope Monitoring of solar atmosphere in spectral channels according to scientific requirements Real-time visualisation of solar atmosphere and activity, including an internet access to fresh data (images, position measurement, Dopplergrams, magnetograms, etc.) Observation of fast active processes and their evolution (pre-onset situation, dynamic phase, slow changes, end of activity) – “flare catcher” Smart archiving of changes in fast active processes, including the scene before their onset (activity archives) Archiving of the history of long-term solar activity (long-term archive) Data archiving for helioseismology (helioseismology archive)

Requirements to a synoptic telescope A full-automatic operation (reliability !!) Open concept allowing modifications and improvements Simultaneous observations of all (active) processes in the solar atmosphere Records of transient active processes including periods before their onsets Large high-resolution solar telescopes have a small field of view, so that they cannot track simultaneously several active regions. The requirements are met by a full-disc telescope that shows the whole solar disc including near surroundings. However, the spatial resolution is limited by the resolution (number of pixels) of the used detector.

The full-disc telescope FOV, including an off-disc area, compared with a high-resolution telescope FOV.

Limiting factors of the full-disc telescope Limited resolution of a detector chip chips currently available on the market: 8000 x 6000 px (48 Mpx) Digital sampling of the image is limited by the chip resolution Diameter of the solar disc and its near surroundings: 3000 arcsec According to the Nyquist’s theorem: Digital image resolution = 1 arcsec The digital image resolution constraints the optical system The sufficient aperture of the full-disc telescope (concerning the resolution) is D = 150 mm for λ = 600 nm The control system of the telescope must keep the solar disc image always at the centre of the detector – otherwise we loose a part of FOV or we must make the image of the disc smaller, loosing the resolution

Example: Auxiliary full-disc telescope (AFDT) for the EST project Mechanical structure

Example: Auxiliary full-disc telescope (AFDT) for the EST project Optical scheme: D = 150 mm refractor

Parameters of the synoptic telescope The AFDT-type paralactic mount may be considered. Its advantage is a very high stability; a drawback is the flat mirror that introduces a time- dependent instrumental polarisation. The minimum aperture is 150 mm. Larger apertures should be considered, depending on photon flux required by post-focus instruments. Optical channels and post-focus instruments according to SRD. Equal size of the solar disc in all optical channels. Each optical channel shall have an autonomous automatic focusing and a correction for solar-disc deformation due to the refraction.

The problem of a large volume of data Data archiving in astronomy has the following problems: –The volumes of data continuously increase –The data manipulation becomes difficult –The data archiving requires huge storage capacities –The long-term maintenance of archives is laborious For these reasons, a reduction of archived data volume is needed. Possibilities of data volume reduction for synoptic observations: –Selection of an appropriate sampling frequency –“Smart” data archiving – selection and archiving of images containing a new useful information –Archiving of parts of images containing active phenomena instead of the whole FOV

Archiving of fast active processes Continuous check for dynamic phases of active processes in all selected channels. When a beginning of the dynamic phase is detected in any channel, start the 1 st phase of digitisation in all selected channels. Continuous check for the end of the active process in all selected channels. The end of the active process is defined when the time-sampling interval is longer than used for the long-term archiving. When the end of the active process is detected in all selected channels, finish the 1 st phase of digitisation. If a new active process is detected during the 1 st phase of digitisation, the 1 st phase of digitisation is re-launched from the beginning.

Frame acquisition with frequency ~ 10 fps; frame selection to obtain the sharpest image every 1 second. Selected frames are stored into the first-in first-out register (FIFO) with capacity of 600 frames (10 minutes of observation). Frames in FIFO are compared each to other. If a change in the solar scene (an activity) is detected, the frame is labelled. When a new active process is detected, all the frames in FIFO are labelled – to record the scene before the activity onset. All labelled frames are stored into the activity archive. Each active process has its own activity archive. 1 st phase of digitisation – full FOV

2 nd phase – final archiving of active processes Identification of the positions of active processes in the telescope’s FOV Division of the image according to the positions and areas of active processes By archiving of one active region of 200 x 300 arcsec instead of the full FOV we save 99.5 % of capacity.

Processed full-disc data with all measured physical parameters are stored into the long-term archive. The time-sampling is chosen to describe sufficiently in detail the long-term evolution of solar activity. For example, the best sample obtained in the interval of 15 minutes. In this archive, the fast active processes are sampled randomly, with an insufficient frequency. Therefore, the long-term archive will also include a chronologic list of observed active events with links to particular activity archives. Archiving of the history of long-term solar activity

Data archiving for helioseismology The helioseismology archive stores for instance: - full-disc intensities at different wavelengths in selected lines - full-disc Dopplergrams in the lines according to SRD - depths and equivalent widths of selected lines, etc. Sampling frequency: 30 – 60 sec, equidistant in time Spectral sampling: ~ 6 points per one line profile

Important hardware components Guider – the solar disc has to be centred at the detectors. The guiding can be realised by telescope drives or a tip-tilt mirror. Automatic focusing of all optical channels. Automatic evaluation of meteorological conditions and protection of the telescope against bad weather. Fast tip-tilt – depends on exposure times: for short ones, fast image motion and guiding errors can be compensated by software means. No adaptive optics – AO is not necessary due to the relatively small aperture and it is very hard to implement due to the extremely large FOV (> 2000 arcsec).

Test for clouds (false changes in images) Test for image quality (sharpness) Correction for image motion Test for changes in images (activity signs) Recognition of a new activity Test for activity evolution and end Important software components

The SPRING telescope should have the following functions: ● Data acquisition of solar disc and its vicinity ● Recognition and timely archiving of fast active processes ● Archiving of long-term history of solar activity ● Archiving of data for helioseismology These functions can be fully automated. The resolution of present detectors impose the following limitations: ● The solar disc must be centred on the detectors. ● The resolution of the full-disc telescope equipped with chips of 8000 x 6000 px will not be better that 1 arcsec. ● The useful aperture of the full-disc telescope is 150 mm at 600 nm. Larger apertures do not increase the resolution but collect more light. Summary

References: Klvaňa M., Sobotka M., Švanda M. 2011, Solar synoptic telescope: Characteristics, possibilities, and limits of design, Contrib. Astron. Obs. Skalnaté Pleso, 41, 92 Klvaňa M., Sobotka M., Švanda M. 2012, Optimisation of solar synoptic observations, in Observatory Operations: Strategies, Processes, and Systems IV, Proc. of SPIE Vol. 8448, 84480A Thanks for attention