MIRI Dithering

The JWST Mid-Infrared Instrument (MIRI) provides dithering capabilities for the imaging, low-resolution spectroscopymedium-resolution spectroscopy, and coronagraphic imaging modes for optimal sampling, bad pixel mitigation, and background subtraction.

When using MIRI, dithering is required to achieve accurate photometry and to provide superior sampling (Arendt et al. 2000). Dither patterns for MIRI have been designed to account for the fact that telescope motions larger than ~20" typically result in new guide star acquisitions and larger observing overheads. The fine steering mirror (FSM) can be used for subpixel (≤50 mas) offsets, which will be used primarily for coronagraphy.  Larger dithers are accomplished by moving JWST.

Dithers and mosaics are distinct in terms of operational ordering. All dither positions must be executed before filter changes may be executed. All filter changes are executed before proceeding to the next tile in a mosaic. 

Words in bold italics are buttons 
or parameters in GUI tools. Bold 
style represents GUI menus/
panels & data software packages.

MIRI specific patterns can be implemented in the Astronomer's Proposal Tool (APT) for:



References

Arendt, R. G., et al., 2000, ApJ, 536, 500
Dithering Strategies for Efficient Self-Calibration of Imaging Arrays




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    Clarified coronagraphic dithering
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