CALWEBB_CORON3

The algorithms for CALWEBB_CORON3, the 3rd stage of the JWST calibration pipeline for coronagraphic data, are described.  These algorithms process the data from calibrated slope images to combined, reference PSF subtracted coadded images.

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The CALWEBB_CORON3 module is the 3rd stage in the calibration pipeline for the NIRCam and MIRI Coronagraphic data.  The inputs to this stage are the calibrated slope images (CALWEBB_IMAGE2 output) and the output is a reference PSF subtracted image stack. The steps are listed in Figure 1 with the flow from the top to the bottom.

Unless otherwise stated, the algorithms described are the baseline version.

Figure 1. CALWEBB_CORON3

The steps in the CALWEBB_CORON3 module are shown.


NIR/MIR steps

Assemble reference PSFs

The available list of reference PSFs is generated.  These reference PSFs can include reference stars specifically observed for the target as well as observations of the target taken at different orientations.

Align reference PSFs

The reference PSFs are aligned with the target observation using the Fourier LSQ algorithm to measure the shifts and the Fourier Shift algorithm to apply the shifts to each reference PSF integration.

Reference PSF subtraction

The reference PSF that is subtracted from each target integration is created using the list of reference PSFs and the KLIP algorithm (Soummer et al. 2012).

Outlier detection

A 2nd pass at outlier detection is done using the image stack.  The majority of the outliers will be due to cosmic rays undetected during the 1st pass at outlier detection done in CALWEBB_DETECTOR1.  An iterative sigma clipping algorithm is used in pixel coordinates on the image stack.  The presence of an outlier results in a pixel flag being set.

Image combination

The target images (including those at different rotations) are combined into a single combined image.  This is done using the AstroDrizzle code with the output pixel size set to the input pixel size.

Create exposure level products

The exposure level products are re-created at this stage to provide the highest quality products that include the results of the ensemble processing (updated WCS, matching backgrounds, and 2nd pass outlier detection).  These products are for the archive and include the unrectified 2D images and rectified 2D images.



References

Soummer, R., Pueyo, R., Larkin, J., 2012, ApJ, 755, 28
Detection and Characterization of Exoplanets and Disks Using Projections on Karhunen-Loève Eigenimages




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