Cardiel López, NicolásEliche Moral, María del CarmenPascual, Sergio2023-06-202023-06-202012[1] Devaney, N., Bello, D., Femenias, B., et al., “Preliminary design and plans for the GTC Adaptive Optics System”, Proc. SPIE 5490, 913 (2004). [2] López, J.A., Bringas, V., Cuevas, S., et al., “FRIDA: Integral–field and spectrograph and imager for the adaptive optics system Gran Telescopio Canarias”, Proc. SPIE 6269, 119L (2007). [3] Cuevas S., Eikenberry, S.S., et al “FRIDA Integral Field Unit Opto-mechanical Design” Proc. SPIE 8450-67, (2012). [4] Cuevas S., Eikenberry, S.S., Sánchez, B., et al., “Optical design of FRIDA, the integral-field spectrograph and imager for the AO system of the Gran Telescopio Canarias”, Proc. SPIE 7014, 70146D (2008). [5] Cuevas S., Álvarez, L.C., et al., “Cryogenic Tests on FRIDA building blocks” Proc. SPIE 8450-67, (2012). [6] Flores Meza, R., Cuevas, S., et al., “Electronics and mechanisms control system for FRIDA (inFRared Imager and Dissector for Adaptive optics)”. Proc. SPIE 8451-138, (2012).0277-786X10.1117/12.926499https://hdl.handle.net/20.500.14352/44431© 2012 SPIE. Conference on Ground-Based and Airborne Telescopes (IV. 2012. Amsterdam, Netherlands). We are grateful to Grupo Santander (Spain) through Encuentros Astrofísicos Blas Cabrera (UNAM-IAC) and our home institutions for their support. We also gratefully acknowledge partial funding for this project through generous grants from PAPITT-UNAM (grant IT116311) and CONACYT grant INFR-2009-01-122664).FRIDA (inFRared Imager and Dissector for the Adaptive optics system of the Gran Telescopio Canarias) is designed as a diffraction limited instrument that will offer broad and narrow band imaging and integral field spectroscopy capabilities with low (R similar to 1,500), intermediate (R similar to 4,500) and high (R similar to 30,000) spectral resolutions to operate in the wavelength range 0.9 - 2.5 mu m. The integral field unit is based on a monolithic image slicer. The imaging and IFS observing modes will use the same Teledyne 2K x 2K detector. FRIDA will be based at the Nasmyth B platform of GTC, behind the AO system. The key scientific objectives of the instrument include studies of solar system bodies, low mass objects, circumstellar outflow phenomena in advanced stages of stellar evolution, active galactic nuclei, high redshift galaxies, resolved stellar populations, semi-detached binary systems, young stellar objects and star forming environments. FRIDA is a collaborative project between the main GTC partners, namely, Spain, Mexico and Florida. In this paper, we present the status of the instrument design as it is currently being prepared for its manufacture, after an intensive prototypes' phase and design optimization. The CDR was held in September 2011.engjournal articlehttp://dx.doi.org/10.1117/12.926499http://proceedings.spiedigitallibrary.org/open access52Infrared instrumentation - near infraredImagingIntegral field spectroscopyIFUGTCDiffraction limitedAstrofísicaAstronomía (Física)Física atmosférica2501 Ciencias de la Atmósfera