The Exo-Planets Imaging Camera and Spectrograph (EPICS), is the Planet Finder Instrument concept for the European
Extremely Large Telescope (ELT). The study made in the frame of the OWL 100-m telescope concept is being up-dated
in direct relation with the re-baselining activities of the European Extremely Large Telescope.
We discuss the quality of the spectro-imaging data (integral field spectroscopy) of the GraF instrument used with the ADONIS adaptive optics system at the ESO 3.6 m telescope in 1997-2001. The integral filed spectroscopy was obtained using a Fabry-Perot interferometer (FPI) in cross-dispersion with a grating spectrograph. A cube of spectro-imaging data at λ ≈ 2200 nm covers a 1.5" x 12.4" sky field sampled with 0.05" pixels; the field is recorded at 384 spectral points with the spectral resolution R ≈ 7000. The maximum field and spectral resolution are wavelength dependent, e.g. λ ≈ 1650 nm the field is 0.9" x 9" sampled with 0.035", recorded at 432 spectral points with R ≈ 10000. A spectrum of a B3III standard in the hydrogen Br-γ 2165.5 nm line and spectro-imaging of the complex central region of the eruptive star η Car in the spectral range 1668-1692 nm, including Br-11 1680.6 nm, [FeII] 1676.9 nm, FeII 1678.7 nm and FeII 1687.3 nm lines, are presented along with the discussion concentrated on the accurate calibration of the spatial point-spread function for the image deconvolution, the photometric monitoring of the FPI spectral scan channels, and on the final quality of the extracted spectra.
When combined with Adaptive Optics, integral field spectroscopy, i.e. observation of a sky field simultaneously in a number of spectral passbands, is the most efficient way to perform spectro-imaging at high angular resolution. GriF will provide the CFHT community with such a capability in the near infrared K-band. This extension will be completed by means of two simple optical devices to be installed in the KIR cryostat (the infrared camera of PUEO): a cooled grism in the filter-wheel and a cold aperture on an entrance focal plane wheel. They will be completed by a room-temperature Fabry- Perot (FP) interferometer in front of KIR. The FP selects narrow bandpass images while the grism spatially separates them, giving a 3-D spectroscopic capacity within a compact and light design. At each exposure, several (up to 9) monochromatic images of a rectangular field of about 36 arcseconds X 4 arc-seconds will be simultaneously acquired, allowing a precise subtraction of continuum and background. The cooled grism will guarantee a low background environment, thus a good sensitivity at K. The medium spectral resolution (about 2600) will fit to a number of programs and will represent a considerable improvement on imaging with narrow- band filters. Thus, combining high angular resolution with the spectroscopic diagnosis, GriF will allow the study of a large class of compact objects or structures, especially in the extragalactic domain where its sensitivity should be unique.
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