The Data Handling and Analysis Software for the Mid-Infrared Instrument (MIRI) on JWST

Morrison , Jane

The Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope (JWST) provides imaging and spectroscopic measurements over the wavelength range 5 - 28.3 µm. MIRI has three arsenic-doped silicon (Si:As) detector arrays. The camera module provides wide-field broadband imagery. The medium resolution spectrograph (MRS) obtains simultaneous spectral and spatial data on a relatively compact region of sky using four integral field units.

MIRI is jointly developed by the US and a nationally funded consortium of European institutes, working with ESA and NASA.

The MIRI Data Handling and Analysis System (DHAS) provides a software tool to support the MIRI Focal Plane Electronics (FPE) testing at JPL and to support the MIRI assembly, integration and, verification at Rutherford Appleton Lab in the UK.

The MIRI DHAS operates in non-real time on FITS-formatted science data captured earlier over one or more exposures. The MIRI DHAS is compromised of two components: a DHAS-Pipeline and a Viewing and Analysis Tool set. The DHAS–Pipeline consists of three C++ programs. The first routine, miri_sloper, converts the measured charge ramps into slope values for each pixel. The second routine, miri_caler, takes the output from miri_sloper and applies a dark or flat calibration image to the data. The third routine, miri_cube, is limited to MRS data and takes MRS data that has been run through miri_sloper/miri_caler and creates a spectral cube. The Viewing and Analysis tool set is a group of IDL software routines for displaying and analyzing the MIRI science frames, reduced images and spectral cubes. This tool set is comprised of two packages: the Quick-Look (ql) tool to display and analyze the science frames and reduced data and the Cube-View (cv) tool for displaying and analyzing spectral cubes.

With the MIRI DHAS software we have been able to analyze image quality, characterize the PSF, test various methods to process the data, characterize the detectors, and test the astrometric calibration of the spectrograph.

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