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frida will be a second generation instrument for gtc , and the first proposed for the adaptative optics ( ao ) system of the telescope @xcite .
frida is being designed and constructed by an international consortium , lead by the instituto de astronoma of the unam .
it is an integral field spectrograph with imaging capabilities , optimized for the 1.1 - 2.4 @xmath0 m range , and it will provide broad and narrow band imaging and integral field spectroscopy ( ifs ) capabilities with low , intermediate and high spectral resolutions , and with different spatial resolutions in the nir ( see table [ tab : table ] ) .
its combination of high spectral and spatial resolutions will provide frida with unique capabilities among other existing integral field units ( ifus ) .
frida will be able to tackle a large number of astrophysical problems , from solar system bodies to cosmological surveys .
its characteristics and its operating wavelength range will expose dusty environments , rich in stellar absorption and emission lines from many different species and gas phases , and sample kinematics and stellar or gaseous content of high redshift galaxies .
frida will perform imaging at the diffraction limit of the telescope , thanks to the correction performed to the wavefront by the gtc ao module . in the ifs mode ,
a monolithic image slicer composed by a set of mirrors will break down a small portion of the ao - corrected field into 30 slices , that will play the role of 1d spectroscopy slits .
the light of each slice is dispersed by the spectrograph onto the detector . with these data ,
a 3d datacube can be built up containing a pseudo - monocromatic image of the ifu field - of - view ( fov ) in each plane ( see fig .  [
fig : fig1 ] for a explanatory sketch of the datacube obtention ) .
the frida ifu design is based on fisica ifu for flamingos - ii @xcite .    ]
figures [ fig : fig2 ] and [ fig : fig3 ] show the light path through the different frida optical components for the imaging and ifs modes , respectively @xcite . in both cases ,
the light path starts at the cryostat window ( on the left ) , coming directly from the gtc - ao module .
it crosses the mask and filter wheels .
the camera wheel selects the plate scale . in the ifs mode
, the ifu dissects a small portion of the fov into the 30 slices , and sends them to the grating carrousel for wavelength dispersion ( fig .
[ fig : fig3 ] ) . the dispersed light of each slice is finally focussed on the detector ( `` slitlet '' ) . in the imaging mode
, the beam avoids entering the ifu and a flat mirror replaces the grating in the spectrograph ( fig .  [
fig : fig2 ] ) .    ]    ]
guaix is developing the data reduction pipeline ( drp ) for frida .
it will consist on robust software tools following certain quality assessment rules , specially optimized for frida data .
the drp will perform two simultaneous and automatic data reduction processes in the telescope ( per observing block or after the user s request ) : a quick data reduction for quick - look analysis , and a scientific - level reduction for archiving purposes in the gtc database .
a stand - alone version is also under study . in order to avoid error correlation in those reduction steps that require interpolation or re - pixelation ,
error handling will be delayed during the reduction as far as possible .
this ensures a realistic errors computation during the major part of the reduction @xcite .
error flags will indicate the reliability of the computed errors to the user .
the drp main characteristics are the following :    * it is being coded following object - oriented structure . * it
will be composed of executable reduction recipes for generating completely - reduced data and final calibration products , for all the defined frida operational modes .
* error handling and propagation throughout the data reduction are usually absent in other data reduction packages .
frida drp will estimate them in parallel to the data reduction .
quality control checks will also be performed . *
the final products of the drp include : the processed calibrations , the reduced , re - constructed final datacubes , intermediate - reduced products , quality control flags
. the pipeline final product will be a datacube per nominal pointing and observing block .
ll + & nasmyth - a gtc platform , + & after the gtc - ao system + & 0.9 - 2.5 @xmath0 m , optimized for + & 1.1 - 2.4 @xmath0 m + & rockwell hawaii - ii 2k@xmath12k , + & hgcdte +   + imaging mode scales & 0.010 , 0.020 /pixel + fov ( arcsec@xmath2 ) & 20.48@xmath120.48 , 40.96@xmath140.96 + & broad band _ jhk _ , and + & narrow band in 0.9 - 2.5 @xmath0 m +   + & 0.010 /pixel @xmath1 0.020 /slice , + & 0.020 /pixel @xmath1 0.040 /slice + data format onto detector & 30 slices @xmath1 66 pixels / slice + fov ( arcsec@xmath2 ) & 0.66@xmath10.60 , 1.32@xmath11.20 + spectral resolutions & r@xmath31500 , 4000 , and 30,000 +   +    [ tab : table ]
we acknowledge support from the madrid regional government through the astrid project ( s0505/esp-0361 ) , for development and exploitation of astronomical instrumentation ( http://www.astrid-cm.org/ ) . partially funded by the spanish mec under the consolider - ingenio 2010 program grant csd2006 - 00070 : `` first science with the gtc '' ( http://www.iac.es/consolider-ingenio-gtc/ ) .
frida ( infrared imager and dissector for the adaptative optics system of the gtc ) will be a nir ( 1 - 2.5@xmath0 m ) imager and integral field unit spectrograph to operate with the adaptative optics system of the 10.4 m gtc telescope . 
 frida will offer broad and narrow band diffraction - limited imaging and integral field spectroscopy at low , intermediate and high spectral resolution . 
 the extragalactic astrophysics and astronomical instrumentation group of the universidad complutense de madrid ( guaix ) is developing the data reduction pipeline for frida . specific tools for converting output , reduced datacubes to the standard euro3d fits format will be developed , in order to allow users to exploit existing vo applications for analysis . 
 frida is to be commissioned on the telescope in 2011 .