Solar Physics

, 293:44 | Cite as

Image Quality in High-resolution and High-cadence Solar Imaging

  • C. Denker
  • E. Dineva
  • H. Balthasar
  • M. Verma
  • C. Kuckein
  • A. Diercke
  • S. J. González Manrique
Article

Abstract

Broad-band imaging and even imaging with a moderate bandpass (about 1 nm) provides a photon-rich environment, where frame selection (lucky imaging) becomes a helpful tool in image restoration, allowing us to perform a cost-benefit analysis on how to design observing sequences for imaging with high spatial resolution in combination with real-time correction provided by an adaptive optics (AO) system. This study presents high-cadence (160 Hz) G-band and blue continuum image sequences obtained with the High-resolution Fast Imager (HiFI) at the 1.5-meter GREGOR solar telescope, where the speckle-masking technique is used to restore images with nearly diffraction-limited resolution. The HiFI employs two synchronized large-format and high-cadence sCMOS detectors. The median filter gradient similarity (MFGS) image-quality metric is applied, among others, to AO-corrected image sequences of a pore and a small sunspot observed on 2017 June 4 and 5. A small region of interest, which was selected for fast-imaging performance, covered these contrast-rich features and their neighborhood, which were part of Active Region NOAA 12661. Modifications of the MFGS algorithm uncover the field- and structure-dependency of this image-quality metric. However, MFGS still remains a good choice for determining image quality without a priori knowledge, which is an important characteristic when classifying the huge number of high-resolution images contained in data archives. In addition, this investigation demonstrates that a fast cadence and millisecond exposure times are still insufficient to reach the coherence time of daytime seeing. Nonetheless, the analysis shows that data acquisition rates exceeding 50 Hz are required to capture a substantial fraction of the best seeing moments, significantly boosting the performance of post-facto image restoration.

Keywords

Granulation Sunspots Instrumental effects Instrumentation and data management 

Notes

Acknowledgements

The 1.5-meter GREGOR solar telescope was built by a German consortium under the leadership of the Kiepenheuer Institute for Solar Physics in Freiburg with the Leibniz Institute for Astrophysics Potsdam, the Institute for Astrophysics Göttingen, and the Max Planck Institute for Solar System Research in Göttingen as partners, and with contributions by the Instituto de Astrofísica de Canarias and the Astronomical Institute of the Academy of Sciences of the Czech Republic. We thank Drs. Peter Gömöry and Thomas Granzer for carefully reading the manuscript and providing valuable comments. CD, CK, HB, and MV were supported by grant DE 787/5-1 of the Deutsche Forschungsgemeinschaft (DFG). SJGM acknowledges support of project VEGA 2/0004/16 and is grateful for financial support from the Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics, a joint project of the Leibniz Institute for Astrophysics Potsdam and the Institute of Physics and Astronomy of the University of Potsdam. This study is supported by the European Commission’s FP7 Capacities Program under the Grant Agreement number 312495.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

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Authors and Affiliations

  1. 1.Leibniz-Institut für Astrophysik Potsdam (AIP)PotsdamGermany
  2. 2.Institut für Physik und AstronomieUniversität PotsdamPotsdamGermany
  3. 3.Astronomical Institute of the Slovak Academy of SciencesTatranská LomnicaSlovak Republic

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