  The detectors in the Mid-Infrared Instrument (MIRI) of the James Webb Space
Telescope (JWST) are arsenic-21 doped silicon impurity band conduction (Si:As
IBC) devices and are direct descendants of the Spitzer IRAC22 long wavelength
arrays (channels 3 and 4). With appropriate data processing, they can provide
excellent per-23 formance. In this paper we discuss the various non-ideal
behaviors of these detectors that need to be addressed24 to realize their
potential. We have developed a set of algorithms toward this goal, building on
experience with25 previous similar detector arrays. The MIRI-specific stage 1
pipeline algorithms, of a three stage JWST cali-26 bration pipeline, were
developed using pre-flight tests on the flight detectors and flight spares and
have been27 refined using flight data. This paper describes these algorithms,
which are included in the first stage of the28 JWST Calibration Pipeline for
the MIRI instrument.
