MIRI is one of four instruments to be built for the James Webb Space Telescope. It provides imaging, coronography and
integral field spectroscopy over the 5-28.5um wavelength range. MIRI is the only instrument which is cooled to 7K by a
dedicated cooler, much lower than the passively cooled 40K of the rest of JWST, and consists of both an Optical System
and a Cooler System. This paper will describe the key features of the overall instrument design and then concentrate on
the status of the MIRI Optical System development. The flight model design and manufacture is complete, and final
assembly and test of the integrated instrument is now underway. Prior to integration, all of the major subassemblies have
undergone individual environmental qualification and performance tests and end-end testing of a flight representative
model has been carried out. The paper will provide an overview of results from this testing and describe the current
status of the flight model build and the plan for performance verification and ground calibration.
The Mid-Infrared Instrument (MIRI) is a 5 to 28 micron imager and spectrometer that is slated to fly aboard the JWST in
2013. Each of the flight arrays is a 1024×1024 pixel Si:As impurity band conductor detector array, developed by Raytheon
Vision Systems. JPL, in conjunction with the MIRI science team, has selected the three flight arrays along with their spares.
We briefly summarize the development of these devices, then describe the measured performance of the flight arrays along
with supplemental data from sister flight-like parts.
We present the development of a Focal Plane Module (FPM) for the Mid-Infrared Instrument on JWST. MIRI will
include three FPMs, two for the spectrometer channels and one for the imager channel. The FPMs are designed to
support the detectors at an operating temperature of 6.7 K with high temperature stability and precision alignment while
being capable of surviving the launch environment. The flight units will be built and will undergo a rigorous test
program in the first half of 2008. This paper includes a description of the full test program and will present the results.