Scanning Fabry-Perot interferometers (FPI)
Observations with the FPI consist of successive acquisition of a few dozen images of interference rings from the object (or from a calibration lamp) when changing the optical path between the parallel plates. The radius of the rings is a
function of wavelength and gap between the plates of the interferometer. The complete set of such images
which fills the free spectral range of the interferometer is called 'a scanning cycle'.
After data reduction images are collected in a data cube. Control of the scanning (change of the gap between flat reflecting plates) is managed by the controller CS100 IC Optical Systems Ltd., connected with a computer. The description of observations and data reduction is presented in the papers:
SCORPIO-2 has a set of bandpass filters which cut the desired narrow spectral range around the emission lines H-alpha, [OIII]5007, [NII]6548,6583, [SII]6717,6731. You can use this IDL-programm for chose an optimal filter for desired systemic velocities of target galaxies.
- Moiseev A.V. 2002, Bull. SAO, 54, 77 (English PDF, Ðóññêèé PS)
- Moiseev A.V., Egorov O.V., 2008, Astrophy. Bull., 63, 181 (English PDF, Russian PDF)
Moiseev A.V., 2015, Astrophy. Bull., 70, 494; ( Russian PDF ; arXiv:1511.03886);
The piezoelectric interferometers were mad by IC Optical Systems Ltd. (early name - Queensgate).
The main parameters if FPIs for observations with SCORPIO-2 in the Halpha spectral range.
|| IFP186 || IFP501|| IFP751|
|Interfringe || 35 A|
| 13 A |
| 8.7 A |
|Sp. resolution || 1.7 A|| 0.8A||0.4A|
|Finesse || 21|| 16||20|
|Number of spectral channels||40|| 36 ||40|
The photo shows IFP751 mounted into SCORPIO-2 during tuning procedures
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