NIRISS Wide Field Slitless Spectroscopy APT Template
Wide field slitless spectroscopy (WFSS), one of 4 observing modes available in NIRISS, is used for low-resolution (R ≈ 150) multi-object spectroscopy of sources over the full 2.2' × 2.2' NIRISS field of view.
Main article: NIRISS Wide Field Slitless Spectroscopy
See also: JWST Wide Field Slitless Spectroscopy Roadmap, NIRISS WFSS Recommended Strategies, NIRISS WFSS with NIRCam Parallel Imaging of Galaxies in Lensing Clusters
This mode uses a pair of identical grisms (GR150R, GR150C) that are mounted orthogonally to each other in the filter wheel and cover the wavelength range from 0.8 to 2.2 μm. The relative dispersion directions are perpendicular to each other, allowing blended spectra to be disentangled in crowded fields. Individual WFSS grism exposures are performed with a filter in the pupil wheel (PW) to (1) select the wavelength range of interest, and (2) reduce blending spectra in different wavelength regions from objects throughout the field. Obtaining spectral coverage across the full 0.8–2.2 μm bandpass requires separate exposures in the adjacent filters.
Each WFSS observation will consist of one or more exposures in APT that include: 1) direct imaging and 2) dithered grism exposures using the same PW filter as the direct image. The direct imaging enables identification of objects in the grism image and calibration of the absolute wavelength zeropoint for grism spectra of each object in the field. One direct image will be taken at the first dither position and a final one at the last dither position. Since the NIRISS point spread function (PSF) is under-sampled over the WFSS wavelength range, dithering will be required for WFSS observations.
The observer will have control over 3 primary parameters for NIRISS WFSS: 1) filter for direct and grism images, 2) dithering pattern, and 3) detector readout mode and exposure time (via the number of groups and integrations). Allowed values are documented in the NIRISS WFSS 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 .
Choose the NIRISS WFSS dither pattern. The dither offsets are large enough to ensure that a compact source does not fall on the same pixel twice, but not so large as to be affected by distortion across the detector.
- Image Dithers: number of steps, where the first step corresponds to initial pointing; allowed values are 2, 3, 4, 6, 8, 12, 16
- Note: if the NIRISS WFSS mode is used as prime in coordinated parallel mode, additional customized dither patterns become available through the Image Dithers pull-down. (These customized dither patterns have been designed to work well for both the primary and the selected parallel instrument mode.) If such a customized dither pattern is selected, the next selector (Pattern Size) disappears.
- Pattern Size: amplitude of dither step; allowed values are SMALL (≈0.3"), MEDIUM (≈0.6"), and LARGE (≈1.2")
- Grism: GR150R, GR150C, BOTH
- Filter: F090W, F115W, F140M, F150W, F158M, F200W
- Readout Pattern
- NISRAPID: all frames are read and stored. Generally this can be used if the number of frames per integration is small and the data volume is not an issue. There is a limit of 30 on the number of groups per ramp in NISRAPID read out.
- NIS: four frames are averaged per group. Used for producing a lower data rate for longer integrations of faint targets.
- Groups/Int: the number of groups during an integration, equal to the number of frames read per integration (for NISRAPID), or the number of frames read out divided by 4 (for NIS).
- Integrations/Exp: the number of integrations during an exposure, where an integration is the time between detector resets.
- ETC Wkbk. Calc ID: the accompanying ETC workbook ID number for the calculation (optional).
The Exposure Time Calculator (ETC) should be used to determine the combination of Groups/Int and Integrations/Exp necessary to achieve the required signal to noise. Individual integrations longer than 1,000 s are discouraged because of the effect of cosmic ray hits on the detector. For long exposures, a suitable number of integrations and a number of groups less than or equal to 25 is suggested.
To take observations in different filters, Add additional observations and specify the appropriate filter. This option will by default add a corresponding direct image for the new grism observation in the Direct Image Exposure Parameters dialog box.
Direct image exposure parameters
A direct image will be taken before and after each set of dithered grism observations. In the case where both grisms are used with the same filter, two direct images are taken when switching between grisms, one at the dither position of the last exposure from the first set and another at the dither position of the first exposure from the second set.
Specify choice of the following parameters, whose meanings are identical to the descriptions above:
- Readout Pattern: NIS, NISRAPID
- ETC Wkbk. Calc ID
The Filter of the direct image will by default match the Filter specified for the corresponding grism image in Science Observation.
Note: the Exposure Time Calculator mode for WFSS does not include calculations for direct imaging. To run calculations for direct imaging to determine Groups/Int and Integrations/Exp, use the NIRISS imaging mode in ETC.
All exposures display
The All Exposures Display dialog box will show the sequence of observations for each science observation specified in the Science Observation dialog box. If BOTH grisms are selected in the Science Observation dialog box, the exposure sequence for that observation will be DIRECT → N × GRISM → 2 × DIRECT → N × GRISM → DIRECT, where all exposures in this sequence will have the same exposure number and N refers to the number of dithered grism exposures as specified in the Image Dithers parameter. Note: APT only shows one direct image in between the grism exposures, when in fact two direct images are actually taken. In the NIRISS WFSS observing mode, a direct image is required before and after a set of grism exposures. When switching between grims, the first direct image corresponds to the last direct image after the first set of dithered grism exposures, while the second direct image corresponds to the first direct image prior to the second set of dithered grism exposures.
Note: fields can not be edited in the All Exposures Display dialog box, but must be edited in the Science Observation and Direct Image Exposure Parameters dialog boxes. Changes to these parameters will be propagated to All Exposures Display.
The NIRISS WFSS mode can be used to obtain data for a region larger than the field-of-view by creating a mosaic pattern. Mosaics are required to ensure that complete spectra are obtained over the full 2.2' × 2.2' NIRISS FOV, as specified on the NIRISS Mosaics article. Visit the Mosaic Parameters article for information on setting up a mosaic.
A variety of observatory level special requirements may be chosen.