Algorithms for calwebb_ami3, which is stage 3 of the JWST Science Calibration Pipeline for NIRISS Aperture Masking Interferometry (AMI) are used to process data from calibrated slope images to fringe parameters. 

On this page

Words in bold are GUI menus/
panels or data software packages; 
bold italics are buttons in GUI
tools or package parameters.

The calwebb_ami3 module is stage 3 of the JWST Science Calibration Pipeline for NIRISS aperture masking interferometry (AMI) data. The inputs to this stage are the calibrated slope images (calwebb_image2 output) and the output is fringe parameters. 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_AMI3

Graphical representation of all the steps in the calwebb_ami3  module.

Steps for all AMI data

Assemble reference PSFs

The available list of reference PSFs is generated. These reference PSFs consist of reference stars specifically observed for the target.

Calculate fringe parameters

Software documentation outside JDox: AMI Analyze

The closure phases and visibilities for each reference PSF and target are calculated. As part of this calculation, the centers of the reference and target PSFs are determined (iteratively).

Average fringe parameters

Software documentation outside JDox: AMI Average 

Averaging the fringe parameters taken over multiple exposures improves the signal-to-noise of the measurements. The averaging is done for both the target and reference PSF observations.

Final fringe parameters

Software documentation outside JDox: AMI Normalize 

The reference PSF closure phases are subtracted from the target closure phases. The target visibilities are divided by the reference PSF visibilities. These 2 calculations are done matched by dither position.

Latest updates


Originally published