NIRCam Time-Series APT Template

Instructions for designing JWST NIRCam Time Series imaging observations using the Astronomer's Proposal Tool (APT).

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See also: NIRCam Time-Series ObservationsJWST Time-Series Observations RoadmapNIRCam Time-Series Observation Recommended StrategiesNIRCam Time-Series Imaging of HAT-P-18 b

Time-series imaging is one of the 5 NIRCam observing modes and one of 2 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

Mosaics are not available for NIRCam time-series imaging.


Words in bold italics are buttons 
or parameters in GUI tools. Bold 
style represents GUI menus/
panels & data software packages.

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 ACQ

See also: NIRCam Time-Series Imaging Target AcquisitionJWST ETC NIRCam Target Acquisition

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. The available filters for target acquisition are F335M and F405N. The F405N filter allows to perform target acquisition on bright science targets that would saturate if observed with the F335M filter.   

Figure 1. Target acquisition location
Target acquisition is performed with a 32 × 32 pixel subarray (yellow square) on the long wavelength detector B5. The target acquisition pointing is centered in the TA subarray, followed by a telescope slew to one of the yellow stars for the science exposures, collecting data within the subarrays shown or the FULL array. For simplicity, only the SW subarrays are shown here. Locations of the LW subarrays are shown below in Figure 2.

Acq exposure time

See also: Understanding JWST Exposure Times, NIRCam Readout Patterns

Please consult the Exposure Time Calculator (ETC). We recommend a signal-to-noise ratio of 30 or higher to obtain a centroid accuracy of 0.1 pixel for the TA source. We also recommend not saturating any pixels.

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


See also: NIRCam Modules

Module B is used for this observing mode.


See also: NIRCam Detector Subarrays

Users may opt to either read out 2 detectors completely or more quickly read out 2 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 4 outputs simultaneously.

Time series
Size in pixels
Nrows × Ncolumns 
Short wavelength
FOV (each side) 
Long wavelength
FOV (each side) 
time (s)
Number of
FULL2048 × 20482 x 64" + 4"–5" gaps129"10.736774
SUB400P400 × 40012.4"25.0"1.656241
SUB160P160 × 1605.0"10.0"0.278641
SUB64P64 × 642.0"4.0"0.050161

Figure 2. NIRCam point source subarrays

Subarrays available for NIRCam time series imaging, plotted in the NIRCam field of view, zooming in on the corners of detectors B1 and B5. Blue and red correspond to the short and long wavelength channels, respectively. By selecting a subarray size, the user is choosing 2 subarrays, one in each wavelength channel. The science target is always centered within the short wavelength subarray.

Number of exposures

See also: NIRCam FiltersUnderstanding JWST Exposure TimesNIRCam Pupil and Filter Wheels

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.

Short wavelength

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.

Long wavelength

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.

Exposure time

See also: Understanding JWST Exposure Times

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.


Latest updates
    Corrected frame times to values updated back in APT 25.4

  • Updated location of the TA subarray
Originally published