NIRCam Time-Series APT Template
Instructions for designing JWST NIRCam Time Series imaging observations using the Astronomer's Proposal Tool (APT).
Time-series imaging is one of the five NIRCam observing modes and one of two NIRCam time-series observing modes. Each mode has a corresponding template in APT for users to design their observing programs.
No telescope moves (dithering nor mosaics) are allowed during NIRCam time series observations.
Lists of allowed values for each input parameter are documented and maintained in the NIRCam Time Series Imaging Template Parameters article.
Step-by-step APT instructions
Note: mosaics are not available for NIRCam time-series imaging.
Target acquisition parameters
Target acquisition may be performed either on the science target (SAME TARGET AS OBSERVATION) or any other target nearby (within 55"). Target acquisition occurs with a 32 × 32 pixel subarray on the long-wavelength channel of Module B located near the point source subarrays and uses the F335M filter.
Acq exposure time
ACQ READOUT PATTERN: The NIRCam detectors are read out continuously using readout patterns. Patterns with longer exposure times typically average more frames to reduce data volume (less of a concern for subarrays).
ACQ GROUPS/INT: The number of groups to include during an integration. Each group results in a saved image, perhaps averaged from multiple frames (reads).
Only one integration per exposure is permitted. Thus the exposure time and integration time are equal.
Time series parameters
Module B is used for this observing mode.
Users may opt to either read out two detectors completely or more quickly read out two detector subarrays, one in each wavelength channel. Smaller subarrays allow for brighter saturation limits in each integration. NIRCam's point source subarrays are available in this observing mode. The subarrays are read out through a single detector output; the full detector is read out through four outputs simultaneously.
Size in pixels
Nrows × Ncolumns
FOV (each side)
FOV (each side)
|FULL||2048 × 2048||132"|
(with 4"–5" gaps)
|SUB400P||400 × 400||12.7"||25.9"||1.65624||1|
|SUB160P||160 × 160||5.1"||10.4"||0.27864||1|
|SUB64P||64 × 64||2.0"||4.1"||0.05016||1|
Number of exposures
Multiple exposures may be performed in sequence to increase the total exposure time. Each exposure is executed as defined in the remaining sections below.
In APT, this section is named "Exposures/Dith" (Exposures per Dither) for consistency with other observing modes, even though no dithering is allowed in this mode.
In this APT template, users select both pupil and filter wheel elements. Light passes through both elements in series in each wavelength channel. Only certain combinations of these elements are allowed in APT.
In addition to broad, medium, and narrowband filters, the NIRCam weak lens WLP8 is available in this observing mode in the short wavelength channel. The weak lens defocuses incoming light, mitigating uncertainties (jitter and flat fields) and allowing for observations of brighter objects before saturation in a given integration time.
The pupil and filter wheel elements allowed in the long-wavelength channel are restricted based on those selected in the short-wavelength channel. For example, if the weak lens is selected in the short wavelength channel, then the long-wavelength observations must include a narrowband filter as well. These restrictions guide users to select elements with similar saturation limits in both wavelength channels, since exposures are obtained simultaneously in both.
Each exposure is defined as a readout pattern, number of groups per integration, and number of integrations per exposure. The resulting Total Exposure Time is reported. This readout configuration applies to both wavelength channels (short and long).
Users should consult the Exposure Time Calculator, ETC, to achieve sufficient signal-to-noise for their science without saturating during each integration. Approximate saturation limits may be found at NIRCam Time-Series Imaging.
Each group yields saved data. Each integration accumulates charge for its duration, preceded and followed by detector resets. Shorter integrations may prevent saturation. Saturated sources may be recovered (unsaturated) in earlier groups during the integration.
Each exposure is performed without moving the telescope nor any mechanisms, with one exception. Exposures of more than 10,000 s are permitted in this observing mode, but users are warned that the High Gain Antenna may need to move during a longer exposure. That movement may introduce jitter and affect data quality.