Coronagraphic imaging with JWST’s Mid-Infrared Instrument (MIRI) provides high-contrast imaging in wavelength bands from 10 to 23 μm, using one Lyot-type coronagraph and three 4-quadrant phase-mask (4QPM) coronagraphs.
The imaging channel on MIRI is equipped with four coronagraphs that provide high-contrast imaging (HCI), covering wavelength bands from 10 to 23 μm (Boccaletti et al. 2015).
In addition to the classical Lyot coronagraph (which provides an inner working angle (IWA) of ~3λ/D), MIRI also incorporates the 4-quadrant phase-mask coronagraph technology (4QPM; Rouan et al., 2000) to provide the smallest possible IWA of ~1 λ/D at 10 to 16 μm. These advantages might be used for studying exoplanets and other faint circumstellar sources.
Each coronagraph is at a fixed position in MIRI's focal plane so that no mechanisms are used. The observer will have control over two primary variables for MIRI coronagraphy: (1) fixed filter-coronagraph pairs and (2) exposure time (via the number of frames and integrations).
4QPMs have narrow spectral bandpasses. Coronagraphic filters are associated directly with each coronagraph and are fixed for each of the four coronagraphs. Selecting the filter also selects the coronagraph, and vice versa.
Table 1. Filter-coronagraph pair properties
|Filter||Coronagraph||Pupil mask transmission (%)1||Central wavelength (μm)||Bandwidth2 (μm)||IWA3 (arcsec)||Rejection4 (on-axis)|
|F2300C||Lyot spot 5||72||22.75||5.5||2.16||850|
JWST User Documentation Home
MIRI Coronagraph Masks
MIRI Detector Readout Overview
MIRI Coronagraphic Imaging Template APT Guide
MIRI Optics and Focal Plane
MIRI Filters and Bandpasses
JWST Astronomers Proposal Tool, APT
JWST APT website
JWST Exposure Time Calculator
JWST ETC website
Rouan, D. et al. 2000, PASP, 112, 1479
The Four-Quadrant Phase-Mask Coronagraph. I. Principle
Rouan et al. 2007, Proc. of SPIE, 6693, 16
A new concept of achromatic phase shifter for nulling interferometry
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