Parent articles: NIRSpec Observing Modes → NIRSpec IFU Spectroscopy
JWST's NIRSpec supports integral field spectroscopy with an integral field unit (IFU). Light from the source of interest passes through a small (3" × 3") aperture in the MSA mounting frame and travels through the IFU image slicing mirror optics. Figure 1 shows the location of the IFU aperture on the MSA mounting frame between MSA quadrants 3 and 4. The to form an image of the source on the image slicer, which consists of 30 stacked mirror surfaces. he layout of the slices, numbered from 0 to 29, within the IFU aperture in the plane of the detector. Figure 1 additionally shows the layout of the slices as positioned on the detector, also numbered
hat can be seen in Figure 1 detector array boundaries in white. This gap affects NIRSpec high-resolution IFU observations, resulting in a gap in the wavelength coverage. The IFU observing mode article spectral wavelengths lost in the detector gap, but the precise values differ for the individual IFU data slices. This article provides additional information on the exact wavelengths lost in the detector wavelength gap per IFU slice for high-resolution IFU observations.
Figure 1. The IFU aperture in the NIRSpec aperture plane
The n on the mounting frame with respect to the NIRSpec fixed slits and MSA quadrants. It is marked by a small blue square halfway between the upper left quadrant (Q3) and the bottom left quadrant (Q4). The 30 pseudo-slits mapped to the detector are as a column of slits in blue to the left of quadrants #3 and #4.
Figure 2. IFU slices in the plane of the detectors
The NIRSpec IFU uses a slicer mirror to image the field of view into 30 slices. Each slice is 0.1" wide g on the sky. Here the slices are shown in the plane of the detectors.
Short wavelength cutoffs
. This effect is worst for the F070LP filter when used with the G140H disperser. Figure 3 illustrates that the spectral cutoffs with this filter/disperser combination occur from ~0.92 to ~0.96 microns, depending on the slice (top to bottom: slice #29 to slice #0, respectively). This blue-end cutoff also occurs using the G140M grating with the F070LP filter, but it occurs at shorter wavelengths in that case (from ~0.85 in slice #0 to ~0.90 microns for slice #29). The full range of the spectra can be examined for a given instrument setup JWST ETC.
Figure 3. IFU short-wavelength cutoffs with the F070LP filter
The missing wavelengths for each of the IFU slices due to the NRS1 detector edge using the G140H disperser.
he range of nominal wavelengths for the G140H/F070LP configuration is shown. Slit #29 (top) and slit #0 (bottom) show the extrema of these differences. In the worst case, wavelengths below 0.96 microns are cut off (slice #0, bottom). At the top (slice #29) wavelengths below 0.92 microns are cut off. Spectra of the fixed slits appear in the middle of the figure. The detector cutoffs are less severe for spectra of the fixed slits over the same wavelength range, as seen in the f.
The presence of a physical gap between detectors affects high-resolution IFU observations because the spectra are long enough to span both NIRSpec detectors. Figure 4 presents an example using disperser G140H and filter F100LP. The limits of the detectors are shown with thick white lines. For clarity, the spectra from the 30 IFU slices are shown in the region around the detector gaps. Note that the wavelength range that falls within the detector gap is different for each slice.
Figure 4. IFU missing wavelengths
The missing wavelengths for each of the IFU slices due to the detector gap.
: The complete range of nominal wavelengths for the G140H/F100LP configuration is shown. Spectra of the fixed slits also appear in the middle of the figure.
: A clipped portion of the nominal wavelength range near the gap is shown to more clearly show that the missing wavelengths differ for each slice, and to better differentiate the cutoff values using the color key. Slit #29 (top) and slit #0 (bottom) show the extrema of these differences. Spectra of the fixed slits over the same clipped wavelength range are shown, but in this case, the wavelengths land on the NRS2 detector and are recorded. Only a portion of the range from slit S200A2 falls off the right edge of NRS2.
that fall within the detector gaps as a function of slit number for G140H
, and G395H
respectively. Note that when using the grating-filter combination G140H/F070LP
the resulting spectra not have any gaps because the spectra do not extend beyond NRS1.
Figure 5. Disperser G140H
Wavelength gap in units of microns as a function of slit for IFU observations made using the high-resolution disperser G140H, and the F100LP filter.
Figure 6. Disperser G235H
Wavelength gap in units of μm as a function of slit for IFU observations made using the high-resolution disperser G235H.
Figure 7. Disperser G395H
Wavelength gap in units of microns as a function of slit for IFU observations made using the high-resolution disperser G395H.
Table 1 below lists the detector gap wavelength cutoff values for the numbered IFU virtual "slits" with the high-resolution gratings that are depicted in the figures above.
Table 1. Wavelength cutoffs of the detector gap for the IFU virtual slits
Table 1 Note: Values are in microns.