(click to enlarge)

• Back-to-back cube-corner reflectors on a common translator mechanism to provide the change in optical-path difference.

• Potassium bromide (KBr) for the beam splitter-recombiner and the compensator.

• A diode-pumped solid-state Nd:YAG laser for interferogram sampling control.

• Cassegrain telescopes for condensing and collimating wherever possible to minimize the number of transmissive elements in the system.

• A passive space-viewing radiator to maintain the interferometer and most of the associated optics at 180 K.

• A two-axis gimbaled pointing mirror operating at ambient temperature to permit observation over the full field of regard.

• Two independent focal-plane assemblies (1 and 2) maintained at 65 K with active pulse-tube coolers. The assemblies accept the dual outputs of the interferometer, which are further split by dichroics into A and B channels. Thus there are four independent focal planes, each an array of 1 x 16 elements and optically conjugated such that equivalent pixels in each focal plane see the same target. Each focal plane has an independent filter wheel in which the filters are typically 200-300 cm^-1 wide.