# Understanding Systematic Errors Through Modeling of ALMA Primary Beams

## TL;DR

This paper models ALMA primary beams to evaluate how beam inaccuracies impact imaging, showing that for certain observations simpler algorithms suffice, while for others more complex methods are necessary.

## Contribution

It provides a detailed analysis of ALMA primary beam effects on imaging quality, guiding the choice of algorithms based on source size and dynamic range.

## Key findings

- For dynamic range < 1000, primary beam accuracy beyond aperture size is negligible.
- Deconvolution errors dominate in large extended source imaging.
- Primary beam errors are indistinguishable in extended source observations.

## Abstract

Many aspects of the Atacama Large Millimeter Array (ALMA) instrument are still unknown due to its young age. One such aspect is the true nature of the primary beam of each baseline, and how changes to the individual primary beams affect astronomical observations when said changes are ignored during imaging. This paper aims to create a more thorough understanding of the strengths and weaknesses of ALMA through realistic modeling of the primary beams and simulated observations, which in turn can inform the user of the necessity of implementing more computationally costly algorithms, such as A-Projection, and when simpler, quicker algorithms will suffice. We quantify our results by examining the dynamic range of each observation, along with the ability to reconstruct the Stokes I amplitude of the test sources. These tests conclude that for dynamic ranges of less than 1000, for point sources and sources much smaller than the main lobe of the primary beam, the accuracy of the primary beam model beyond the physical size of the aperture simply doesn't matter. In observations of large extended sources, deconvolution errors dominate the reconstructed images and the individual primary beam errors were indistinguishable from each other.