Instructions for filling out the Astronomer's Proposal Tool (APT) MIRI LRS templateincluding slit and slitless (time-series) spectroscopy.

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Main article: MIRI Low Resolution Spectroscopy
See also: JWST Slit Spectroscopy RoadmapTSO RoadmapMIRI LRS Recommended StrategiesMIRI TSO Recommended Strategies

Low resolution spectroscopy is one of 4 observing templates available with the the Mid-Infrared Instrument (MIRI)MIRI's low resolution spectrometer (LRS) offers both slit and slitless spectroscopy from 5 to 12 μm using a double prism mounted in the MIRI filter wheel, designed to provide a spectral resolving power of R = 40 at 5 μm, and R = 160 at 10 μm for compact sources (<2"). The slitless LRS mode is dedicated to time-series observations of time variable systems, such as eclipsing binaries or transiting exoplanets—APT parameters for slitless LRS are optimized for this type of observation. 

The APT template requires information on the following aspects of the observation:

  1. Target acquisition
  2. Subarray (which controls whether the observation will be slitless or with slit)
  3. Dither or mapping pattern
  4. Detector read mode and exposure settings
  5. Mosaic settings

 Allowed values are documented and maintained in the MIRI LRS Template parameters, but described below.


Step-by-step APT instructions


The following parameters are generic to all templates, and are not discussed in this article: observation Number, observation Labelobservations CommentsTarget name, ETC Wkbk. Calc ID (in the Filters dialog box), Mosaic Properties, and Special Requirements.

Target Acquisition Parameters 

Target acquisition (TA) is required for LRS slitless, but not for slit observations. These parameters, found under the MIRI Low Resolution Spectroscopy tab in the Target Acquisition Parameters panel, are Acq TargetAcq Filter, and Acq Exposure Time.  

Target ACQ  

Main article: LRS Slit Target Acq, LRS Slitless Target Acq

The target for the TA should be selected from the Acq Target parameter's pull-down list that contains targets defined in the proposal. The filter used for the TA are selected from the Acq Filter's drop-down list: F560WF1000WF1500W, and FND.   

Acq Exposure Time

A Target ACQ must be completed by selecting a MULTIACCUM exposure configuration. Each exposure is configured by setting the readout pattern and characteristics parameters: Acq Readout Pattern and Acq Groups/Int

Users should use the Exposure Time Calculator (ETC) to determine the best exposure configuration to optimize signal to noise.

Acq Readout Pattern

Main article: MIRI Detector Readout Overview

Choices for the Acq Readout Pattern parameter are

  1. FAST (the default)

Number of groups and integrations

Main article: Understanding JWST Exposure Times

Acq Groups/Int

The MIRI readout timing pattern for the TA exposure is defined by only one of the MULTIACCUM parameters: Acq Groups/Int, the number of groups per integration. 

Acq Integrations/ExpAcq Total Integrationsand Acq Total Exposure Time cannot be changed by the user. The MIRI TA is always carried out in a single integration and exposure.

The TA saturation limit for each filter depends on the array configuration used for TA, which also determines which subarray should be used for TA. The user should always refer to the ETC for signal-to-noise calculations.

LRS Verification Image

Obtain verification image?

Main article: MIRI LRS Slit Target AcquisitionMIRI LRS Slitless Target Acquisition

The MIRI LRS has the capability of taking an additional exposure between Target Acquisition and the Science Exposure, which will allow the user to verify the placement of the target. This option is enabled for LRS observations using the slit (subarray set to FULL). This exposure will use the same filter and number of groups as the TA exposure itself. Note that if the Acquisition Target chosen in in the TA Parameters section is different from the science target (e.g. in cases where the science target is too faint to achieve a good signal to noise ratio), the exposure setting are not likely to yield a useful image. In this case, the user can select “No” for this option for better time efficiency.

If the proposed science observation uses the SLITLESSPRISM subarray (for LRS slitless time series observations), this option will automatically be set to “Yes”. The verification image will always be part of the observation for the LRS in slitless mode.

If the user chooses not to perform a TA sequence, for example when observing extended targets, the Verification Image cannot be requested.

LRS Parameters


Main article: MIRI Detector SubarraysMIRI Low Resolution SpectroscopyMIRI Time-Series Observations

The MIRI LRS supports both slit and slitless configurations, each of which has its own scientific merit. In the LRS Parameters panel, the Subarray parameter choice controls whether the observation will use a slit or slitless setting. The slitless LRS configuration uses a dedicated detector subarray called SLITLESSPRISM—by default, slitless observations are time-series observations (TSO)Low resolution slit spectroscopy uses the FULL frame readout.


Main article: MIRI LRS Dithering

If you chose the SLITLESSPRISM subarray for slitless spectroscopy (a time-series observation), dithers are not permitted.

If you have chosen slit spectroscopy, you must choose one of two dither options for the observation from the drop-down menu for Dither Type:

ALONG SLIT NOD is recommended for point or point-like sources. This pattern moves a target between 2 positions along the slit. It allows for mitigation of bad pixels and provides a measurement of the background.

The MAPPING option can be used to define a small pointing grid, which is more suitable for extended targets. Additional parameters are required for this option: the number of steps for the spatial and spectral directions, and their respective step offsets (in units of arcseconds). The number of steps must be greater than 1 in one of the directions, so that the map will have a minimum of 2 positions. If an even number of mapping positions are chosen in either direction, then the targeted coordinates will be centered in one of the slit positions.  Users are strongly encouraged to check their observation by visualizing it with the Aladin Viewer.

Exposure Time 

Users should use the Exposure Time Calculator (ETC) to determine the best exposure configuration to optimize the signal-to-noise.

In the LRS Parameters panel, an LRS sequence must be completed by selecting a MULTIACCUM exposure configuration. Each exposure is configured by setting the readout pattern and characteristics parameters: Readout PatternGroups/Int, Integration/Exp, and Exposures/Dith. Three greyed-out boxes will show calculated parameters based on the exposure dither setting entered; these fields are not editable by the user.

Readout Pattern

Main article: MIRI Detector Readout Overview

For the LRS slitless configuration, only the FAST mode readout pattern is available.

For the LRS slit configuration, the following options can be selected:

  1. FAST (default)
  2. SLOW

Number of groups and integrations

Main article: Understanding JWST Exposure Times

The MIRI timing pattern per exposure is defined by 3 MULTIACCUM parameters: 

  1. Groups/Int: the number of groups during an integration;
  2. Integration/Expthe number of integrations during an exposure, where integration is defined as the time between resets;
  3. Exposures/Dith: the number of exposures per dither position.

Total Dithers (not user-editable) returns the total number of dither steps for the observations. For ALONG SLIT NOD dithering, the box will show a value of 2. For MAPPING observations, the total number of dithers will be the product of No. Spatial Steps and No. Spectral Steps

Total Integrations (not user-editable) shows the total number of integrations for the observation, taking into account the dither and exposure settings. The formula used is Total Integrations = Total Dithers × Integrations/Exp × Exposures/Dith.

Total Exposure Time (not user-editable) returns the total exposure time calculated from the dither and exposure settings. The formula used is Total Exposure Time = Groups/Int × Total Integrations × "group read time". The group read times for FULL and SLITLESSPRISM array configurations are documented in the MIRI Detector Subarrays article for each subarray. The time is given in seconds.

Other tabs

Mosaic Properties

The MIRI LRS may be used to obtain data for a region larger than the slit size by creating a MIRI LRS mosaic pattern under the Mosaic Properties tab. Use of the mosaic pattern is not supported when using the LRS in slitless mode.

Special Requirements

A variety of observatory level Special Requirements may be chosen under the Special Requirements tab. 

When using the LRS in the slitless configuration (SLITLESSPRISM subarray) the Time Series Observation and No Parallel special requirements are automatically selected. For most TSOs of transiting exoplanets (or similar), the user should specify timing constraints to specify the phase timing of the observation. The Time Series Observation special requirement cannot be selected for LRS slit observations.


The Comments field (under the Comments tab) should be used for observing notes.



Latest updates
    Updated text on dithers to align with the APT.

    Updated information about what subarrays require TA.

    Added paragraph about verification images.