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Bringas, V.; Lucero, D.; Corrales, A.; Uribe, J.; Rodríguez, A.; Montoya, J. M.; Estrada, R.; Alvarez, L.; Gómez,

E.; Sánchez, B.; Cuevas, S.; Espejo, C.; Flores, R.; Keiman, C.; Chapa, O.; Lara, G.; Eikenberry, S. S.

OPTO-MECHANICAL DESIGN OF FRIDA

Revista Mexicana de Astronomía y Astrofísica, vol. 42, 2013, p. 120

Instituto de Astronomía

Distrito Federal, México

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Revista Mexicana de Astronomía y Astrofísica,

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RevMexAA (Serie de Conferencias), 42, 120–120 (2013)

OPTO-MECHANICAL DESIGN OF FRIDA

V. Bringas,1 D. Lucero,1 A. Corrales,1 J. Uribe,1 A. Rodrıguez,1 J. M. Montoya,1 R. Estrada,1 L. Alvarez,1

E. Gomez,1 B. Sanchez,2 S. Cuevas,2 C. Espejo,2 R. Flores,2 C. Keiman,2 O.Chapa,2 G. Lara,2

and S. S. Eikenberry3

FRIDA (inFRrared Imager and Dissectorfor the Adaptive optics system of the GranTelescopio Canarias) is being designed ascryogenic and diffraction limited instrumentthat will offer with broad and narrow bandimaging and integral field spectroscopy capa-bilities with Low (R = 1400), intermediate(R = 4000) and high (R = 30000) to operatein the wavelength range 0.9–2.4 µm.

Both, the imaging mode and IFS observingmodes will use the same Teledyne 2K×2K detec-tor. This instrument will be installed at Nasmyth Bplatform, behind the GTC Adaptive Optics system.FRIDA cryogenic opto-mechanical design of the op-tics building blocks and mechanisms are described inthis contribution.

All FRIDA optical subsystems are based onCaF2/S-FTM16 infrared cryogenic achromatic dou-blets. That doublets are the FRIDA “buildingblock” of the optics. The ultimate optical perfor-mance is determined by the alignment of that dou-blet lenses and the integrity of the delicate CaF2glass lenses when the instrument is cooled down fromroom to cryogenical temperatures.

In Figure 1 we show a cut of the beam compressoropto-mechanics, which, working in concert with themedium camera optics, performs the coarse pixel size(0.04′′/pixel). It can be noted this is a two doubletsdesign, based on the FRIDA opto-mechanic “build-ing block”.

In Figure 2 it is shown the FRIDA “buildingblock” opto-mechanics prototype on the cold benchof one of the validation cryostats (FCTF). In thesame cold bench it is mounted a diffraction gratingfor its cryogenical validation. Furthermore, it shouldbe pointed out that two validation cryostats weredeveloped by the CIDESI-UNAM team (FCTF andColibrı) and are in operation.

1Centro de Ingenierıa y Desarrollo Industrial, P.de la Cuesta 702, Queretaro, Qro., 76310, Mexico(vbringas@cidesi.mx).

2Instituto de Astronomıa, Universidad Nacional Auto-noma de Mexico, Mexico.

3Department of Astronomy, University of Florida, USA.

Fig. 1. Cut of the FRIDA beam compressor. This sub-

system is formed by two achromatic doublets mounted

on the opto-mechanics “building block”.

Fig. 2. Collimator prototype mounted on the cold bench

of FCTF, one of the evaluation cryostats. A diffraction

grating is also mounted on the cold bench for a cryogeni-

cal validation.

We are grateful to Grupo Santander (Spain)through Encuentros Astrofısicos Blas Cabrera(UNAM-IAC) and our home institutions for theirsupport.

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