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Instrument Overview


The FRIDA Project

Instrument Overview

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IAC Contribution

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Sky coverage with AO with natural or laser guide star

Other NIR instruments

Sky characterization of the Canary Island's Observatory

IAC programs on high spatial resolution techniques and atmospheric optics

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FRIDA Concept:

FRIDA (inFRared Imager and Dissector for Adaptive optics) is the first instrument that will be built for the Adaptive Optics system of the 10.4 m Gran Telescopio de Canarias (GTCAO). 
There will be two observation modes:

× Near-IR imaging

with three different plate scales:

× Coarse (0.040 arcsec/pixel)
× Mediun (0.020 arcsec/pixel)
× Fine (0.010 arcsec/pixel)

FRIDA is optimized in the 1.1 - 2.4 µm range, in both imaging and integral field mode.

FRIDA Summary:

Operation modes Imaging and Integral field spectroscopy
Working Wavelength    0.9 - 2.5 µm   (optimized 1.1 - 2.4 µm)   
Detector Hawaii II 2048x2048 pix
Location Nasmyth platform at the output focus of GTCAO
Imaging mode
Scales 0.010 arcsec/pixel
0.020 arcsec/pixel
0.040 arcsec/pixel
FoV ~20x20 arcsec2
~40x40 arcsec2
 Integral field mode
Format 30 slices with 66 pixels/slice in the spatial direction and 2 pixels per 'resolution element' in the spectral direction.
Slice Scales
(spectral direction X spatial direction)
0.020 x 0.010 arcsec per slice X arcsec per pixel
0.040 x 0.020 
arcsec per slice X arcsec per pixel
0.080 x 0.040 
arcsec per slice X arcsec per pixel
FoV ~0.60 x 0.66 arcsec2
~1.20 x 1.32 arcsec2
~2.40 x 2.64 arcsec2
Spectral resolution R~ 1300 to cover H+K (goal: also  Z+H)
R~ 4000 in  Z, J, H or K

R~ 20,000 (goal 30,000) in selectable windows in 1.4 - 2.4 µm range

FRIDA Observation Modes:

Imaging Mode:
imag1

(Image from Marin-Franch, Lenorzer, Herrero & Najarro, 2007)


Integral Field Spectroscopy (IFS):
ifs1

(Image from Marin-Franch, Lenorzer, Herrero & Najarro, 2007)

Adaptive Optics:

FRIDA will be installed at the Nasmyth A platform behind the output focus of the GTC adaptive optic system (GTCAO).





GTCAO  will routinely deliver subarcsec resolutions down to the GTC diffraction limit, this being about 4 times that provided by HST at the same IR wavelengths.  FRIDA is designed to fully exploit these resolutions in its two observation modes: direct imaging and integral field spectroscopy, both working in the 0.9 -2.5 um range.

Two unique capabilities of FRIDA with respect to current or planned 2D spectrographs are: 1) its high spectral resolution mode, 20,000; 2) its separate imaging mode which will allow the observer very  fast switch to the integral-field-spectroscopy - mode. The combination will allow the user a fast selection of the field of interest for follow up spectroscopy, and facilitate a fast acquisition in the small FoV of the integral field unit.

GTCAO is a Shack-Hartmann-based wave-front sensor working with natural guide stars at optical wavelengths. For a median seeing, 0.65 arcsec,  at the GTC site, it  is expected to provide  an on-axis Strehl ratio of 0.60 in K-band, with guide stars of mR= 6-12,  down to ~ 0.30 for mR = 15. Measurements  of the isoplanatic angle  at La Palma Observatory indicate a degradation of the  Strehl in K-band  to ~10 % when the natural guide star is at 30 arcsec from the science target.

FRIDA Nyquist sample the diffraction limit of GTC in  J-, H- and K-bands in its imaging mode, in K-band  in its integral field mode, and partially in H- and J-bands in the integral field mode.
The integral field mode is provided with  three  spectral resolution sets: ~200 km/s, allowing two atmospheric bands to be observed at  once; ~ 75 km/s, to cover only one band at a time; and  ~15 km/s  to cover selectable regions in the 1.4 -2.5 µm range.

FRIDA design is being optimised in the 1.1 - 2.4 um range,  in both  imaging and integral field mode. Its ultimate performance is foreseen in the K-band where GTCAO is also expected to achieve   maximum atmosphere correction.  In this case,  FRIDA will deliver images and spectra with spatial resolutions close to GTC diffraction limit at 2 um, FWHM ~ 44 mas, with maximized image  contrast  and high throughput for point-like sources

A key advantage of FRIDA with respect to akin instruments is that it does not rotate - the rotated field will be provided  by the GTCAO system. This will  translate into  a highly stable instrument with minimum flexure, and an accurately-calibrated distortion pattern.





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