NEFER (Nuevo Espectrómetro Fabry-Perot de Extrema Resolución) is a high spectral resolution, scanning Fabry-Perot
Spectrometer. It will be installed in the OSIRIS instrument at the GTC 10 m telescope. This 3D instrument uses a high
order scanning Fabry-Perot to obtain highly accurate kinematical information of extended cosmic sources such as
galaxies or nebulae. Astronomical data obtained with this instrument lead to a 3D spectroscopic data cubes composed of
several images, each one at different gaps of the scanning Fabry-Perot Interferometer. In this work we present laboratory
testing of some characteristics of the ICOS Fabry-Perot acquired for this instrument such Finesse, free spectral range,
and peak transmission. We also present software design and development for the 3D data reduction standalone package
of this high resolution 3D instrument.
The scanning Fabry-Perot spectrograph could give highly accurate, kinematical information of star forming regions (HH
objects, protoplanetary disks and large scale flows) and the dynamics of isolated and interacting galaxies (resonances,
galaxy pairs, compact groups). In this project we are developing a high spectral resolution scanning Fabry-Perot
interferometer for the GTC 10 m telescope and the OSIRIS instrument. The system will provide the following
characteristics: high spectral resolution data (R up to 20000) over a whole field of view of approximate 8 × 8 arcmin,
0.125 arcsec pixel size in two spectral ranges; 6300 to 7000 Å (galactic projects) and 8000 to 9500 Å (OTELO objects
kinematics). ICOS ET100 Fabry-Perot will be used and installed within the OSIRIS collimated beam in the filter wheel
hosting the tunable filters. Several acquisition software features have been defined like: synchronizing Fabry-Perot
scanning with image acquisition, data cube assembly; single frame or data cube files would be provided according to the
observer data reduction process. Fabry-Perot plates parallelism is extremely important to improve Finesse. Our team has
developed an algorithm to accomplish this task.
We are developing an instrument to study the morphology and kinematics of the molecular gas and its interrelationship with the ionized gas in star forming regions, planetary nebulae and supernova remnants in our Galaxy and other galaxies, as well as the kinematics of the IR emitting gas in starburst and interacting galaxies. This instrument consists of a water-free fused silica scanning Fabry-Perot interferometer optimized in the spectral range from 1.5 to 2.4 micrometers with high spectral resolution. It will be installed in the collimated beam of a nearly 2:1 focal reducer, designed for the Cassegrain focus of the 2.1 m telescope of the San Pedro Martir National Astronomical Observatory. Mexico, in its f/7.5 configuration, yielding a field of view of 11.6 arc-min. It will provide direct images as well as interferograms to be focused on a 1024 X 1024 HAWAII array, covering a spectral range from 0.9 to 2.5 micrometers .
The kinematics of the interstellar medium may be studied by means of a scanning Fabry-Perot interferometer (SFPI). This allows the coverage of a wider field of view with higher spatial and spectral resolution than when a high-dispersion classical spectrograph is used. The system called PUMA consists of a focal reducer and a SFPI installed in the 2.1 m telescope of the San Pedro Martir National Astronomical Observatory (SPM), Mexico, in its f/7.5 configuration. It covers a field of view of 10 arcmin providing direct images as well as interferograms which are focused on a 1024 X 1024 Tektronix CCD, covering a wide spectral range. It is considered the integration of other optical elements for further developments. The optomechanical system and the developed software allow exact, remote positioning of all movable parts and control the FPI scanning and data acquisition. The parallelism of the interferometer plates is automatically achieved by a custom method. The PUMA provides spectral resolutions of 0.414 Angstrom and a free spectral range of 19.8 Angstrom. Results of high quality that compete with those obtained by similar systems in bigger telescopes, are presented.
The system called PUMA is an instrument consisting of a focal reducer coupled to a scanning Fabry-Perot interferometer (SFPI), which is being developed for the Observatorio Astronomicao Nacional at San Pedro Martir, B.C. It will be installed at the 2.0 m Ritchey-Chretien telescope with a focal ratio of F/7.9. It has interference filters, a calibration system, and field diaphragms. The SFPI can be moved out of the optical path in order to acquire direct images. The images produced by this instrument will be focused on an optoelectronic detector, a CCD, or a Mepsicron, depending on the spectral range used.