MIRI Imaging APT Template
Instructions for filling out the Astronomer's Proposal Tool (APT) MIRI imaging template, including full field imaging, subarray imaging, and large imaging mosaic, are provided in this article.
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See also: MIRI Imaging, JWST Imaging Roadmap, MIRI Imaging Recommended Strategies, NIRCam Deep Field Imaging with MIRI Imaging Parallels, Proposal Planning Video Tutorials
Imaging is one of 4 observing modes available with the Mid-Infrared Instrument (MIRI). For standard imaging, the MIRI imager offers 9 broadband filters centered on wavelengths between 5.6 and 25.5 μm over an unobstructed field of view of up to 74" × 113" and a detector plate scale of 0.11"/pixel. The MIRI standard imaging mode supports the use of detector subarrays for bright targets as well as a variety of dither patterns, which may act to improve sampling at the shortest wavelengths, remove detector artifacts and cosmic ray hits, and facilitate self-calibration. The APT mosaicking tool can be used to design mosaic observations to image larger fields.
The observer will have control over 4 primary parameters for MIRI imaging:
- dithering pattern
- detector read out mode and exposure time (via the number of groups, integrations, and exposures).
Allowed values are documented and maintained in MIRI Imaging Template parameters (an article in the JWST Proposal Parameters documentation), but are also described below.
Step-by-step APT instructions are provided below.
Words in bold are GUI menus/
panels or data software packages;
bold italics are buttons in GUI
tools or package parameters.
Coordinated Parallel observations
See also: JWST Parallel Observations
MIRI imaging supports coordinated parallel observations with NIRCam or NIRISS. When the Coordinated Parallel box (visible when the Template parameter is set to MIRI Imaging) is checked, one of these 2 parameter values can be selected:
- MIRI-NIRCam Imaging
- MIRI Imaging-NIRISS WFSS
Note that the default option is None Selected.
MIRI Imaging tab
See also: MIRI Detector Subarrays
A pre-defined set of subarrays are available for selection in the Subarray parameter under the MIRI Imaging tab. They're used for observing targets bright enough to saturate the image in full frame readout. Each subarray is associated with a brightness limit, depending on the filter used, above which a point source will saturate in the shortest 2-group integration. A MIRI imaging observation can only support a single subarray. If the target must be imaged using another subarray, it is necessary to create a separate MIRI imaging observation.
Table 1. MIRI subarrays
Usable size (arcsec)
1024 × 1032
74" × 113"
512 × 512
56.3" × 56.3"
256 × 256
28.2" × 28.2"
128 × 136
14.1" × 14.1"
64 × 72
7" × 7"
See also: MIRI Imaging Dithering
Dither patterns, that must be created before defining your imaging sequence, are specified in the Dithers dialog box under the MIRI Imaging tab. Each dither is specified by setting several parameters: Dither Type, Starting Point, Number of Points, Starting Set, Number of Sets, Optimized for, Direction, and Pattern Size.
Note that the smallest subarrays are smaller than the largest dithers, so the choice of dither pattern may be constrained by the choice of subarray. The MIRI imaging template in APT will only display dither parameters that are valid for the selected subarray.
Table 2. MIRI dither patterns
|Dither type||Use case||Number of dithers|
|CYCLING||Shallow, flexible imaging, optimized for self-calibration||3–311|
|REULEAUX||Deep imaging, optimized for self-calibration||12|
|2-Point||Fast nod, for snapshots||2|
|4-Point-Sets||Flexible dithers for user-optimized imaging of point and extended sources||Multiple of 4|
|Patterns for Coordinated Parallels||Dithers optimized for both MIRI imaging and the parallel instrument (only available in coordinated parallel mode)||2–9|
Note that set number 6 of the 4-point-Sets dither type is centered on the FOV of the chosen subarray.
Small scale dithers are supported for imaging with F560W and F770W. To minimize overheads, small dithers are implemented using the telescope fine steering mirror (FSM). After slewing the telescope to each large dither, the small dither pattern will be executed in sequence, leading to a total of Ndithers = Nsmall × Nlarge separate exposures.
The option for no dithers (None) is currently available for the SUB64 subarray if the Times Series Observation Special Requirement is set. See the MIRI Imaging TSOs article for more information.
See also: MIRI Filters and Dispersers
The Filters dialog box, under the MIRI Imaging tab, is used to create the entire imaging sequence for a single observation for each filter. Each MIRI imaging observation can consist of multiple sets of images, each using a unique filter, dither pattern, and exposure configuration. Click on Add, below the dialog box, to add an image set for a filter. Note that image set definitions can be duplicated using the Duplicate button.
An imaging sequence must be completed by selecting an exposure configuration for each imaging filter. Each exposure configuration requires setting the readout pattern and characteristics parameters: Readout Pattern, Groups/Int, and Integrations/Exp. Finally, select a dither pattern from the Dither parameter pull-down list—select a number that corresponds to a dither that was pre-defined in the Dithers dialog box. Exposures will be repeated at each dither position following an offset of the telescope to the new position. The number of exposures at each dither position is set by Exposures/Dith.
Users should use the Exposure Time Calculator (ETC) to determine the best exposure configuration to optimize the signal to noise.
See also: MIRI Detector Readout Overview
MIRI offers 2 Readout Patterns for imaging:
The FASTR1 readout pattern is the default pattern, and is recommended for MIRI imaging observations.
Number of groups and integrations
See also: Understanding JWST Exposure Times
The MIRI exposure configuration is defined by only 2 parameters:
- Groups/Int: The number of groups during an integration, where a group is the time to cycle through and non-destructively read out all the pixels. Groups/Int = 2 requires permission from STScI, which can be obtained with a request through the Help Desk.
- Integrations/Exp: The number of integrations during an exposure, where integration is defined as the time between detector resets (destructive reads).
See also: JWST Mosaic Overview, MIRI Imaging Mosaics
See also: Specifying Mosaics in APT
The MIRI imager may be used to obtain data for a region larger than their size by creating a MIRI imaging mosaic pattern under the Mosaic Properties tab.
A variety of observatory level Special Requirements may be chosen under the Special Requirements tab.
The Comments field (under the Comments tab) should be used for observing notes.