Echelle spectrograph

Ondřejov Echelle Spectrograph (OES) is a fibre-fed high-resolution spectrograph. The light reflected from the main mirror is from primary focus directed via optical fiber to the coudé room where it is reflected to a Zerodur echelle grating (by Richardson Grating Laboratories). The optical mirror reflects the light further to a equilateral prism (made by TOPTEC Turnov, CZ), which separates the orders that are then brought to a focus on the detector, which is a nitrogen-cooled CCD Camera Versarray 2048B (Roper Scientific, for more details see here) with working temperature of the detector -110°C.

The spectrograph can be fed independently through the same fiber by Thorium Argon calibration lamp and flat field calibration lamp. Also, the iodine cell is mounted on the telescope-spectrograph interface, providing a secondary (optional) spectral calibration source.

A more detailed technical description with mechanical setup and all optical elements can be found in the report from the installation phase of the OES by Koubský at al., Ondřejov Echelle Spectrograph – OES, Publ. Astron. Inst. ASCR, 92:37–43, 2004. For more details about OES see also Kabáth et al., 2020, PASP, 132, 5002.

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Left: OES spectrograph optical layout and light path from the slit to the detector. A – slit, B – collimator, C – echelle grating, D – first parabolic mirror, E – small flat mirror, F – second parabolic mirror (optical elements D, E and F are parts of so called white pupil, making the light beam more narrow), G- prism, H – objective lens and dewar vessel. Right: Upper image – the mechanical parts holding the optical elements of the Ondrejov Echelle Spectrograph. Lower image – the detector with the dewar vessel. Credit: Miroslav Šlechta.

Echelle Grating
  • Manufacturer: Richardson Grating Laboratories.
Dimensions Echelle Blaze angle Material
157 x 412 mm 54.5 g/mm 69° Zerodur
  • Manufacturer: Walter, Faculty of Mathematics and Physics, Charles University in Prague.
Dimensions Height Diffraction angle Material Density
144 x 118 mm 140 mm 54.5° Schott LF5 3.25 g/mm3
CCD Camera
  • Manufacturer: Versarray 2048B
ChipResolutionPixel sizeDynamical rangeTechnical
EEV 42-40-1-3682048 x 204813.5 x 13.5 μm16 bitDetails
Wavelength coverage and performance

The wavelength coverage of OES is from near UV (3753 Å) up to near IR (9195 Å). The resolving power is R=51600 at 5000 Å (R∼40000 in Hα) and spectral sampling is 2.4 Å/mm. The spectral range is covered by 56 usable orders. The number of spectral orders range from 92 to 36. The individual spectral order covers ∼70 Å in the near UV region and ∼145 Å in near IR regions. In blue, spectral orders overlap, thus, it is possible to merge them. The overlapping interval is ∼20 Å in near UV. However, the overlapping intervals gets shorter towards red and the last (short) overlapping intervals are between spectral orders covering 5782-5879 and 5879-5977 (the overlap is less than 1 Å). Between the orders covering 5879-5977 and 5978-6079, there is already a gap (∼1 Å). The gap is gradually increasing and around H the gap between consecutive orders is ∼13 Å and even ∼63 Å around 8800 Å.

Information about spectra calibration is available here.

Sample images
Th-Ar calibration lamp
α Lyr (Vega), exp. 30s
SNR vs. Exposure time

The appropriate exposure time can be roughly estimated using Fig. 3. It is seen that for the signal-to-noise ratio (SNR) of ~65, an 1-hour exposure time is needed for a 10-mag star. However, the particular SNR depends not only on the zenith distance but mainly on the observing conditions. The limiting precision regarding the radial velocities is in the order of hundreds m/s for faint stars. By using the iodine cell, precision is about a few tens of m/s.

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The exposure time needed to get desired SNR with OES. Credit: Miroslav Šlechta.