NIRCam Grism Time-Series APT Template
Instructions for designing JWST NIRCam grism time-series observations using APT, the Astronomer's Proposal Tool.
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 Grism Time-Series Imaging Template Parameters article.
Step-by-step APT instructions
The following parameters are generic to all templates, and are not discussed in this article: observation Label, observations Comments, , ETC Wkbk. Calc ID (in the Filters dialog box),Mosaic Properties, and .
Note: mosaics are not available for NIRCam grism time-series.
Target acquisition parameters
Users can opt to do target acquisition on any nearby object, including the science target. Target acquisition occurs with a 32 × 32 pixel subarray on the long wavelength channel of Module A located near the grism field positions. Target acquisition objects other than the science target can be defined in Targets. Choose SAME TARGET AS OBSERVATION to use the science target. 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.
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, which may be averaged from multiple frames (reads), depending on the readout pattern.
Only one integration per exposure is permitted.
Thus the exposure time and integration time are equal.
Main article: NIRCam Modules
Note: Module A is used for this observing mode.
Main article: NIRCam Detector Subarrays
The grism time-series subarrays span all detector columns and either some or all rows. The same numbers of pixels are read out from all subarrays, so each short wavelength subarray covers a quarter the area on the sky as the long wavelength subarray. When a subset of rows are selected, subarrays are defined in 2 short wavelength detectors to overlap and be centered vertically within the long wavelength subarray's footprint on the sky.
Note the weak lenses WLP4 and WLP8 produce defocused images roughly 66 and 132 pixels across, respectively. Therefore, WLP8 images would be significantly truncated by the smallest subarray SUBGRISM64.
Size in pixels
Nrows × Ncolumns
No. of output channels
|FULL||2048 × 2048|
64" × (2 x 64" with 4"–5" gaps)
|129" × 129"||42.23000|
|SUBGRISM256||256 × 2048||8.1" × (2 x 64" with 4"–5" gaps)||16.6" × 129"|
|SUBGRISM128||128 × 2048||4.1" × (2 x 64" with 4"–5" gaps)||8.1" × 129"||2.67800|
|SUBGRISM64||64 × 2048||2.0" × (2 x 64" with 4"–5" gaps)||4.0" × 129"||1.35960|
Number of output channels
The detectors may be read out through a single output channel or more quickly through 4 output channels simultaneously. The latter produces roughly 4 times as much data for a given exposure time. (Put another way, for a given set of exposure parameters which produces a given data volume, the exposure time is roughly 4 times higher when using a single output channel instead of four.) Data rates and data volumes are limited somewhat by APT; tighter limitations may be required to facilitate scheduling (see Data Volume Limitations).
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.
Short pupil + filter
Two weak lenses are available in this mode for short wavelength observations, and one or the other must be used:
- WLP8 (8 waves of defocus at 2.12 µm)
- WLP4 + F212N2 (4 waves of defocus at 2.12 µm; coupled to a 2.12 µm narrowband filter with a 2.3% bandpass)
The weak lenses defocus incoming light, mitigating uncertainties (jitter and flat fields) and allowing for observations of brighter objects before saturation in a given integration time.
|Short wavelength pupil wheel||Short wavelength filter wheel|
|WLP8||F070W, F0140, F182M, F187N, F210M, or F212N|
WLP4 + F212N2
Long pupil + filter
The row dispersion grism GRISMR (in the pupil wheel) is used in combination with a wide long wavelength filter (in the filter wheel): F277W, F322W2, F356W, or F444W. See NIRCam Grism Time Series for more details.
See also: Understanding JWST Exposure Times
Each exposure is defined as a readout pattern, number of groups, and number of integrations. The resulting Total Exposure Time is reported. This readout configuration applies to both wavelength channels (short and long); the observations are obtained simultaneously using a dichroic.
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 Grism Time Series.
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.