MIRI LRS Slit Target Acquisition
Target Acquisition is highly recommended for MIRI Low Resolution Spectroscopy (LRS) observations with the slit for compact sources.
Calibration of MIRI LRS data requires accurate knowledge of the location of the target on the detector. To this end, users are advised to perform a target acquisition (TA) as part of their observation; this ensures that the target is placed with subpixel accuracy (< 10 mas) at the nominal slit center location (or at the first nod position).
LRS slit and slitless modes each have their own custom TA procedure. For slit spectroscopy, TA is particularly important to avoid slit losses and wavelength calibration issues that can arise from off-nominal source placement. Cases where TA may not be necessary are:
- when performing an off-source dedicated background observation
- when observing very extended sources.
TA is therefore not mandatory in the LRS APT template; however, for observations of point or compact sources it is highly recommended.
Pointing performance of the telescope is described in JWST Pointing Performance.
Typically the science target is used for TA. However, the procedure can also be carried out with a nearby bright star, which should be within 60" from the science target. Use of an offset TA target may be advisable in the following cases:
- the science target is spatially resolved, giving a higher uncertainty on the centroid location;
- the science target's spectral energy distribution is not well know in the TA filters; or
- the science target requires a long (~100s of seconds) integration to reach SNR of 20.
As integration length increases, cumulative cosmic ray hits increase the risk of inaccurate centroiding. In such cases using a bright nearby point source is likely to give a better result.
TA filters and exposure settings
Target Acquisition for LRS slit mode observations can use all filters, read mode, and observation settings described in the MIRI TA main article. The TA exposure is always carried out in a single integration. We recommend a SNR of > 20 for successful TA.
Users should always use the JWST Exposure Time Calculator (ETC) to help choose the best TA filter and exposure settings for their science.
Bold italics style indicates words that are also parameters or buttons in software tools (like the APT and ETC). Similarly, a bold style represents menu items and panels.
LRS Slit region of interest
See also: MIRI Optics and Focal Plane
The LRS slit target acquisition requires a region of interest (ROI) located as close to the LRS slit as possible. A 48 x 48 pixel (~5 × 5") ROI is located in the imager portion of the field of view, near the slit location (see Figure 1). Note that the ROI is not a detector subarray; TA exposures are performed with FULL array mode.
To provide a reference for the location of the target in the slit, users may request a verification image in the LRS Astronomers Proposal Tool (APT) template. This image is taken at the end of the TA sequence, after the telescope's small angle maneuver to place the target at the first pointing position for science, before the prism is selected in the filter wheel. While this image is not used in the calibration pipeline, it can inform the user on the exact placement of the target in the slit (which may affect the quality of the flux and wavelength calibrations).
The verification image is an exact repeat of the TA image itself, using the same number of groups and the same filter. Cases where users should not select this option if the target used for TA is not the same as the science target, and the science target's SED in the TA filter is unknown, or the science target is too faint in the TA filter band to produce a usable image in the TA exposure time.
If no TA was requested, for example in the case of an extended target, the verification image cannot be requested.
LRS TA Sequence
The sequence is as follows:
- The TA target is placed in the center of the LRS Slit ROI.
- An image is taken according to the APT specifications for filter, read mode, and number of groups.
- The on-board centroiding algorithm computes the centroid location of the target, and the offset to the first pointing location is computed (the slit center, or the first nod position). This computation includes the offset to the science target, if an offset target is used for TA.
- The telescope executes a small angle maneuver (SAM) to place the target at required location.
- A verification image is taken.
- The science observation is commenced, which starts with the acquisition of the double prism in the filter wheel.
Exposures taken during the TA sequence are downloaded to the archive and made available to the observer.