JWST Data Calibration Considerations
The requirements for the JWST absolute flux, wavelength, and position calibration are given in the tables below. At this point, we expect to meet all these requirements. The planned calibration programs are sufficient to meet or exceed these requirements.
The requirements for absolute flux calibration vary by instrument and observation mode. They are listed in Table 1. For the details of targets, etc. see the JWST Data Absolute Flux Calibration article. Note that the needed flux prediction accuracy on the targets exceeds those listed in the table as there are other terms involved beyond the prediction accuracy (aperture correction accuracy, stability, etc.).
Table 1. Absolute flux requirements
† For sources observed through slits, the value is for well centered observations.
‡ Not a formal requirement, by analogy with NIRSpec spectroscopy.
The requirements for absolute wavelength calibration vary by instrument. They are listed in Table 2. For the details of targets, etc. see the JWST Data Absolute Wavelength Calibration article. Note that the needed wavelength prediction accuracy on the targets exceeds those listed in the table as there are other terms involved beyond the prediction accuracy (aperture centering accuracy, stability, etc.).
Table 2. Absolute wavelength requirements
* Not a formal requirement, by analogy with NIRISS spectroscopy.
The requirement for absolute position (astrometric) calibration is 5 mas. Specifically, the 5 mas refers to the uncertainty in the observatory field distortion correction within any instrument and the guider. For details see the article titled JWST Data Absolute Astrometric Calibration.
Cycle 1 calibration programs
The instrument cycle 1 calibration programs will provide a set of deliverables needed to remove instrumental signatures and calibrate the JWST observations. The main deliverables from the calibration program are reference files for the science calibration pipeline. The cycle 1 calibration program will be used in combination with any similar observations taken during the JWST commissioning to produce the highest quality reference files.
- bad pixel maps
- read noise measurements
- flat fields (both pixel and illumination versions)
- linearity corrections
- persistence characterization
- PSF images and characterization
- astrometric solutions (including distortion characterization)
- wavelength calibration
- line spread function characterization (for the spectrographs)
- absolute (spectro)photometric calibration
- relative throughput of NIRSpec apertures
- NIRSpec MSA shutter contrast and failed shutter maps
- NIRISS WFSS spectral traces