NIRCam Grism Time Series
See also: NIRCam Grism Time-Series APT Template
The NIRCam grism time-series observing mode is designed to monitor bright, isolated, time-varying sources at 2.4–5.0 µm with spectroscopic resolving power R ~ 1,600 at 4µm. It is one of 2 modes available for NIRCam time-series observations (TSO), the other being time-series imaging. Both of these modes allow very long exposures (>50 hours with some interruptions and limitations) and disallow dithering and mosaics. A separate non-TSO grism mode is available for wide field grism observations.
In grism time-series mode, the module A "grism R" is used to disperse the target's spectrum along (parallel to) detector rows. The grism is used in conjunction with one of 4 wide filters in the long wavelength channel (2.4–5.0 µm): F277W, F322W2, F356W, and F444W.
Simultaneous short wavelength imaging is obtained with a weak lens to defocus the image. This choice offers saturation limits similar to the long wavelength grism for a given integration time (which must be identical for both wavelengths).
Integration times may be shortened for rapid cadence monitoring by using detector subarrays and/or multiple detector outputs. The shortest integration times enable observations without saturation of some stars visible to the naked eye (~5th magnitude).
Table 1. Available combinations of filters, weak lenses, and grism
Short wavelength channel (0.6–2.3 µm)
Long wavelength channel (2.4–5.0 µm)
Weak lens offering +8 or +4 waves defocus
Grism R plus a wide filter:
† The WLP4 weak lens is joined with a F212N2 narrowband filter with a 2.3% bandpass, to form a single optical element. (Note that this F212N2 filter is wider than the 1% bandpass F212N filter in the filter wheel that can be paired with WLP8.)
Grism throughput tables for both modules and for both 1st and 2nd orders can be downloaded here. Note that these are grism-only throughputs. Filter-only throughputs, can be dowloaded here. To obtain the full system throughputs, the grism-only throughputs need to be interpolated at the same wavelengths as the filter-only throughputs and multiplied by the filter-only throughputs.
Subarrays and readout times
Bright science targets require short integration times to avoid saturation. To shorten detector readout times, a subset of the detector rows may be read out (and the rest discarded). These subarrays will contain the entire spectrum for isolated compact science targets. Module A available subarrays for this mode contain 64, 128, or 256 pixel rows. Each of the subarrays include all 2048 pixel columns (2040 sensitive to light + 8 reference). The full 2048 × 2048 pixel array may be read out instead if desired.
The detector may be read out either through 4 outputs simultaneously (to speed readout and minimize saturation) or a single output (to reduce the data volume rate). This is the only NIRCam observing mode to offer this option; other modes always use 4 outputs to read the full detector (and a single output for subarrays). When 4 outputs are chosen, the detector output is split into 4 columns, or "stripes," each 512 pixels wide that are read simultaneously.
Table 2. Detector read out times for available subarrays and numbers of outputs
|Readout time (s)|
|Readout time (s)|
Each spectrum is dispersed by 1 nm/pix. The undeviated wavelength is 3.95 µm.
As shown in Figure 4, for wavelengths below 4 µm (F277W, F322W2, F356W), sources are positioned near the right of the detector (x = 1581), and the spectra disperse to the left (towards shorter wavelengths). Above 4 µm (F444W), a different reference position is used (x = 952) because the source disperses to the right (towards longer wavelengths).
Vertically, the sources are positioned at y = 35 on the long wavelength detectors when using the 64, 128, and 256 subarrays, and at y = 280 when using the full array. At short wavelengths, the defocused images land in the vertical center of the corresponding subarrays, which traverse two short wave detectors (with a 4″–5″ gap).
The reddest part of the F444W footprint (above 5.03 microns, where the throughput drops below 20% of the maximum) extends beyond the detector. The loss of data in this low-throughput region is balanced by two factors. First, the high-throughput portion of the spectrum has more overlap with the corresponding portions for the other 3 filters. This allows a better characterization of systematics at the sub-pixel level in the region in common. Second, this choice of the reference position would allow a larger fraction of the short-wavelength DHS spectra to land on the SW detector [see Schlawin et al. 2017]. SW DHS spectroscopy in parallel with LW grism time series not enabled for Cycle 1 but may be a future upscope of NIRCam capabilities. Maintaining the same reference positions for the LW grism time series with and without parallel DHS spectroscopy is advantageous as it would provide better overall LW F444W grism time series characterization.
See also: NIRCam Bright Source Limits
Based on preliminary estimates, A-type main sequence stars as bright as K ~ 4.5 (Vega mag) may be observed with the NIRCam grism without saturating the module A detectors at any wavelength when using the smallest subarray (2048 × 64 pixels), stripe mode (4 outputs), and a short integration time of 0.68 s (2 reads). Still brighter stars may be observed at the longest wavelengths, as shown in Figure 5.
Table 3. Subarray saturation limits
Approx. saturation limit
|Approx. saturation limit|
(K Vega mag)
Two NIRCam Channels are Better than One: How JWST Can Do More Science with NIRCam’s Short-wavelength Dispersed Hartmann Sensor