NIRISS Bright Limits
The bright limits, above which saturation occurs, depends on subarray configurations for the various JWST NIRISS observing modes.
The NIRISS single object slitless spectroscopy (SOSS) and aperture masking interferometry (AMI) modes are optimized to observe bright objects, where the target is centered on a pixel. For imaging, and to some degree for slitless spectroscopy, the bright limit in some filters is significantly affected by whether a star is centered on a pixel or is located at the pixel corner. This effect is larger for the NIRISS short wavelength imaging filters where the PSF sampling is sparse. Values given here are for stars centered on a pixel, and hence represent the worst case.
Users should ultimately use the Exposure Time Calculator (ETC) for all saturation/sensitivity calculations.
NIRISS SOSS bright limits
The NIRISS single object slitless spectroscopy (SOSS) mode is optimized to obtain spectra from 0.6–2.8 μm of transiting exoplanets around bright stars. SOSS makes use of the GR700XD grism to disperse the light into 3 orders, 2 of which are useable, at a resolution of R ~ 700.
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Table 1. Estimated bright limits for NIRISS SOSS mode
|Subarray||Subarray size||Order||NGroups||J mag (Vega)†|
|SUBSTRIP256||256 × 2048||1||2|
|SUBSTRIP256||256 × 2048||2||2|
|SUBSTRIP96||96 × 2048||1||2|
† Reported magnitudes are simulated 2MASS J-band magnitudes. The bright limit varies as a function of wavelength and spectral type (see Figure 1).
The bright limit is a function of wavelength in each order for a given readout. Figure 1 shows the predicted bright limit for 2 groups and one integration for SUBSTRIP256 and the NISRAPID detector readout pattern, assuming a maximum signal level of 72,000 e–.
NIRISS AMI bright limits
See also: NIRISS Aperture Masking Interferometry
The NIRISS aperture masking interferometry (AMI) mode enables high spatial resolution imaging of bright objects and is optimized to identify close companions ~70–400 mas from their host stars. A non-redundant mask (NRM), consisting of 7 holes, produces an interferogram in the image plane, sampling 21 unique baselines. The AMI mode is used in conjunction with 3 medium-band filters (F380M, F430M, F480M) or one wideband filter (F277W) in the filter wheel.
Most observations with AMI will make use of the SUB80 subarray which covers 80 × 80 pixels on the detector. Table 2 lists the bright limits in A0V-based magnitudes, also called Vega magnitudes, for the various filters. Table 2 assumes a point source centered in a pixel. If the point source is placed at or near the corner of a pixel, the target could be about 1.5 magnitudes brighter because of the lower pixel response. For a full frame observation the bright limits will be about 5.4 magnitudes fainter than for a SUB80 observation. Effective saturation is assumed to occur at 30,000 e-/pixel, which is the limit at which charge from the central illuminated pixel begins accumulating in neighboring pixels.
Table 2. Estimated bright limits for NIRISS AMI mode in Vega magnitudes (i.e., the average A0V star has colors of 0.0 between filters), for an A0V type spectrum, for the SUB80 subarray
Magnitude in NIRISS filters assume an average A0V star has the same magnitude in all filters, and uses the Bohlin Sirius model (2020) as a template for this average star at magnitude -1.401. Note that quoted bright limits will vary for different spectral types.
†The magnitudes in NIRISS filters F277W and F380M roughly correspond to the WISE W1 magnitude.The magnitudes in NIRISS filters F430M and F480M roughly correspond to the WISE W2 magnitude. There is a ±0.05 magnitude uncertainty due to the conversion from NIRISS magnitude to WISE magnitudes, which is a function of the spectral shape of the source. The magnitudes of the WISE and NIRISS filters should match for an average A0V star and WISE magnitudes are predicted to be slightly smaller than the NIRISS magnitudes for later spectral types.
‡JWST ETC does not support Ngroups = 1, so the detected flux from the Ngroups = 2 calculation was scaled to estimate the bright limit for Ngroups = 1.
NIRISS WFSS bright limits
See also: NIRISS Wide Field Slitless Spectroscopy
The NIRISS wide field slitless spectroscopy (WFSS) mode enables low-resolution (R ≈ 150) spectroscopy over the wavelength range 0.8–2.2μm for all objects within the 2.2’ × 2.2’ field of view (FOV) of the NIRISS detector. WFSS observations are obtained using the GR150 grism with a blocking filter in the pupil wheel. Only full frame readout is supported.
The estimated bright limits for each filter are listed in Table 3. The magnitudes listed are Vega magnitudes in the NIRISS filters. For an average A0V star, the same magnitude applies in the 2MASS J, H, and K filters to within about 0.03 magnitudes. The wavelengths listed in Table 3 indicate the wavelength at which saturation is expected to first occur for an A0V star, for NISRAPID readout and 2 groups and one integration. Magnitudes and wavelengths at which saturation first occurs will be a bit different for a cool star or any other object of a distinctly different spectral shape.
Table 3. Estimated bright limits for NIRISS WFSS mode, for an accumulated signal of 72,000 e–
† Bright limit varies by wavelength. The table lists the wavelength at which saturation first occurs for an A0V star.
‡ Magnitude in NIRISS filters assuming an average A0V star has the same magnitude in all filters and using the Bohlin Sirius model (2020) as a template for this average star at magnitude -1.401. Note that quoted bright limits will vary for different spectral types.
NIRISS imaging bright limits
See also: NIRISS Imaging
NIRISS imaging is not supported as a prime observing mode, but can be used in parallel when another JWST instrument is primary. In the WFSS observing mode, direct images with NIRISS, using a filter in the pupil wheel, are required before and after a grism exposure sequence. Direct images can optionally be taken prior to an AMI observation with 3 medium-band filters (F380M, F430M, F480M) or one wideband filter (F277W) in the filter wheel.
Table 4 lists the estimated bright limits. The magnitude values listed are estimated Vega magnitudes in the NIRISS filters, so for an A0V star these magnitudes should match those of 2MASS or other filters in this wavelength range to within 0.03 magnitudes. These values are calculated for the case where a star is centered on the pixel, for NISRAPID readout and 2 groups and one integration; the bright limit will be higher for a star observed at the pixel corner where the peak signal is split about equally between 4 pixels.
Table 4. Estimated bright limits for NIRISS imaging mode, for an accumulated signal of 72,000 e–
|Pupil Wheel Filters|
|Filter Wheel Filters|
† Magnitude in NIRISS filters assuming an average A0V star has the same magnitude in all filters and using the Bohlin Sirius model (2020) as a template for this average star at magnitude -1.401.