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GREGOR Postfokus-Instruments

Wavelength Distribution at GREGOR

The image above shows the wavelength distribution and instruments at GREGOR foreseen for observations during the season 2022A. Two beamsplitters are located on a rotational stage. They transmit the IR and reflect the visible. The cutoff wavelength between transmission and reflection can be selected either as 900 nm or 650 nm. The IR beam goes towards GRIS. The visible beam goes towards the AO and the fast imaging cameras. When observing with the 900 nm beamsplitter, H-alpha is available for the fast cameras, but not in the slitjaw system and vice versa for the 650 nm beamsplitter. GRIS is available slit-scanner and in IFU mode in 2022A.

The wavelength range in the visible can be selected with interference filters. Regularly used filters are 430 nm (G-band), 450 nm (continuum), or 396 (Ca II K). The document vtt_filters_17.pdf contains a list of the available filters. See links on the right.



GRIS: spectropolarimetry in the near Infrared (slit or IFU)

GRIS (GREGOR Infrared Spectrograph) is the grating spectrograph installed at the GREGOR telescope. The spectrograph has a standard Czerny-Turner configuration with parabolic collimator and camera mirrors that belong to the same conic surface. Although nothing prevents its use at visible wavelengths, the spectrograph is mostly used in combination with the infrared detector of the Tenerife Infrared Polarimeter (TIP-II) in standard spectroscopic mode as well as for spectropolarimetric measurements. A slit scanner allows to scan some 60 arcsec, although scanning can also be performed with the AO. The slit length also corresponds to some 60 arcsec, with a sampling of 0.13 arcsec.


GRIS+TIP operates in the range 1.0–2.3 μm, however the polarimeter is optimized for 1–1.3 μm and 1.5–1.8 μm. The experience at the German Vacuum Tower Telescope (VTT), located at the same observatory, demonstrated that the most used spectral regions are those at 1.083μm (including the photospheric Si I and the chromospheric triplet He I) and at 1.565μm (with a number of iron lines including a line with g=3). As an example for the 1.565μm region: Five accumulations of 30ms exposure time each in the 4 polarimetric states yields a signal-to-noise ratio of 1000. In this case one scan step takes 3 sec. The instrument paper can be found here.


Starting in 2018B, GRIS is available in combination with the IFU built by the IAC. For a field of view (FOV) of 3" x 6" spatial and spectral information is then obtained simultaneously. The IFU is especially suitable for fast-cadence studies of a smaller FOV (e.g. evolution of granules), but it can also be used to scan across larger regions. The technical details can be found here. Changing the setup from slit-mode to IFU-mode requires maintenance time, and therefore the setup changes are minimized and usually only done between the two observing seasons.


Examples of GRIS scans from previous years can be viewed at the GRIS data archive.

GRIS is operated by the IAC. Manolo Collados is the Principal Investigator of GRIS.

BBI: broadband context imaging

The broadband imager consists of 2 sCMOS cameras, which are usually run at 30 Hz. Context imaging is useful to study the fast evolution of the Sun. BBI is usually run at the wavelength of G-band, TiO, or any two different filters can be selected for the 2 beams.The FOV is 59arcsec x 50arcsec, the resoultion 0.023arcsec/pix.

The observers are responsible for their own setup, including selecting filters. For further technical questions please contact Thomas Berkefeld (berke@~@leibniz-kis.de).

PI Institute: Leibniz Institute for Solar Physics

High-resolution Fast Imager (HiFI+)

The upgraded High-resolution Fast Imager (HiFI+) consists of three camera control computers with two synchronized sCMOS (16-bit digitization) or CMOS (12-bit digitization) cameras each. HiFI+ offers near-diffraction limited imaging at high cadence in six spectral windows:


–         HiFI+ No. 1: G-band at 430.7 nm and blue continuum at 450.6 nm, Imager sCMOS, FOV: 70.7″ × 59.6″ (2560 × 2160 pixel), 20-second cadence, image selection (best 100 out of 500 images), speckle masking image restoration or Multi-Object Multi-Frame Blind Deconvolution (MOMFBD)

–         HiFI+ No. 2: Narrow-band (FWHM = 60 pm) and broad-band (FWHM = 0.75 nm) Hα at 656.3 nm, Imager M-lite 2M, FOV: FOV: 76.5″ × 60.5″ (1536 × 1216 pixel), 6-second cadence, image selection (best 50 out of 500 images), MOMFBD

–         HiFI+ No. 3: Ca II H at 396.8 nm and TiO at 705.7 nm, Imager M-lite 2M, FOV: 48.2″ × 30.8″ (1536 × 1216 pixel) and 76.5″ × 60.5″ (1536 × 1216 pixel), 6-second cadence, image selection (best 100 out of 500 images), speckle masking image restoration

Please contact the instrument PI for an introduction of HiFI+, training with the data acquisition, and installation of the data reduction pipeline. A data reduction pipeline for Level 1 data is available on site, and the PIs of observing campaigns are expected to reduce their data for archiving (https://gregor.aip.de). The data pipeline also provides provisions for image restoration. However, only a very limited number of images can be restored on site.

Denker, C., Kuckein, C., Verma, M., González Manrique, S.J., Diercke, A., Enke, H., Klar, J., Balthasar, H., Louis, R.E., Dineva, E. 2018:High-cadence Imaging and Imaging Spectroscopy at the GREGOR Solar Telescope—A Collaborative Research Environment for High-resolution Solar Physics. The Astrophysical Journal Supplement Series 236, 5, DOI: 10.3847/1538-4365/aab773

Denker, C., Dineva, E., Balthasar, H., Verma, M., Kuckein, C., Diercke, A., González Manrique, S.J. 2018:Image Quality in High-resolution and High-cadence Solar Imaging. Solar Physics 293, 44, DOI: 10.1007/s11207-018-1261-1

Kuckein, C., Denker, C., Verma, M., Balthasar, H., González Manrique, S.J., Louis, R E., Diercke, A. 2017:sTools—A Data Reduction Pipeline for the GREGOR Fabry-Pérot Interferometer and the High-resolution Fast Imager at the GREGOR Solar Telescope. IAU Symposium 327, 20, DOI: 10.1017/S1743921317000114


PI Institute: Leibniz Institute for Astrophysics Potsdam (AIP)

Instrument PI: apl. Prof. Dr. Carsten Denker (cdenker@~@aip.de)

Instrument Webpage: gregor.aip.de/cms/instruments/