This page provides information on the reference files used by the JWST pipeline to process NIRISS data. The information is sorted by pipeline stages. Detailed information on the pipeline steps and files format is provided in the specified links.
The JWST NIRISS instrument offers 4 science observing modes that are automatically processed by the JWST pipeline: wide field slitless spectroscopy, single object slitless spectroscopy, aperture masking interferometry, and imaging. The following sections provide information on the NIRISS-specific reference files used by the pipeline, organised according to the different pipeline stages.
This pipeline stage process the LVL1 up-the-ramp raw files and returns the level 2a files in units of (counts/sec). All NIRISS data goes though the entire set of pipeline steps applied in CALDETECTOR1. To achieve that several the diverse steps in the correspondent NIR pipeline flow use the following reference files:
Table 1. NIRISS reference files used by the JWST pipeline module calwebb_detector1.
This pipeline branch is intended for use with dark exposures. It applies all of the same detector-level correction steps as CALWEBB_Slopes and uses the same reference files, but stops just before the application of the dark subtraction step.
CALWEBB_IMAGE2 reference files
In this pipeline stage individual exposures from the imaging modes are processed from counts/sec to absolute flux units. Details on the pipeline steps flow are given here.
Table 2. NIRISS reference files used by the JWST pipeline module calwebb_image2.
CALWEBB_SPEC2 reference files
This pipeline stage process Individual exposures from the spectroscopic modes from counts/sec to absolute flux and wavelength units. Nominally, this stage works on individual exposures obtained for the NIRISS wide field slitless grism observations, but the steps are not yet implemented.
Table 3. NIRISS reference files used by the JWST pipeline module calwebb_spec2.
CALWEBB_IMAGE3 reference files
Multiple exposures from the direct imaging modes (e.g., dither pattern or mosaic) are combined into a single rectified (distortion corrected) image. Details on the pipeline steps flow are given in this page.
Table 4. NIRISS reference files used by the JWST pipeline module calwebb_image3.
Multiple individual exposures for the spectroscopic modes (i.e. dither patters or mosaics) are combined into a single rectified cube and/or extracted spectrum.
Table 5. NIRISS reference files used by the JWST pipeline module calwebb_spec3.
The Level-3 Aperture Mask Interferometry pipeline is intended to be applied to associations of individual calibrated NIRISS AMI exposures and is used to compute fringe parameters and correct science target fringe parameters using observations of reference targets. Details on the individual pipeline steps can be found here.
Table 6. NIRISS reference files used by the JWST pipeline module calwebb_ami3.