Calibration of MIRI LRS data requires accurate knowledge of the location of the target on the detector. To this end, the user is advised to perform target acquisition as part of their observation; this ensures that the target is placed with sub-pixel accuracy at the nominal slit or slitless 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-centre source placement; for slitless mode, TA ensures that different observations of the same target always fall onto the same detector pixels. Note that for LRS slitless observations, TA is mandatory. When using the slit it is highly recommended but optional; mapping observations of extended targets may not need TA. Pointing performance of the telescope is described in these articles.
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 target may be desirable if the science target is not a point source, or if the TA exposure would add an unacceptably long overhead to the observation (see below).
As for the other MIRI modes, LRS has 4 filters available for TA:
- FND (a neutral density filter)
The user should always use the JWST Exposure Time Calculator to help choose the best TA filter for their science.
TA exposure settings should be calculated using the ETC. The exposure should be carried out in a single integration, with a limit of approximately 1000 seconds to avoid too many cosmic ray hits. If sufficient SNR cannot be reached on the science target in this time (SNR > 20 is recommended), use of an offset target should be considered. The minimum number of groups in an integration for TA is 3.
LRS region of interest
The LRS slit target acquisition requires a region of interest (ROI) located as close to the LRS slit as possible. A 96 × 96 ROI is located in the imager portion of the field of view, near the slit location. Note that the ROI is not a detector subarray; TA exposures are performed with FULL array read mode.
LRS slit TA Sequence
The target acquisition procedure begins with placing the TA target, i.e. the science target itself or a suitable offset star, in the ROI in the imager field of view. An exposure is taken according to the setup specified by the user in APT. This exposure must be limited to a single integration. A dedicated algorithm will perform centroiding on the resulting image, to identify the location of the target centroid at sub-pixel accuracy. The images taken in TA will be available to the user.
After the centroiding algorithm has completed, the filter wheel will move from the TA filter position to the P750L location, which is the double prism. Following the filter wheel move, the telescope will perform a small angle maneuver (SAM) to place the target into the slit at the required position (at the slit centre, or the first nod position). The first science exposure can begin.