# MWA Tied-Array Processing I: Calibration and Beamformation

## TL;DR

This paper details the algorithms and pipeline developed for the Murchison Widefield Array to perform tied-array beam formation, enabling high-resolution pulsar observations and presenting initial polarimetric results.

## Contribution

It introduces new algorithms and a processing pipeline for tied-array beam formation in the MWA, enhancing its capabilities for high-time resolution radio astronomy.

## Key findings

- Successful formation of tied-array beams from calibrated antenna signals
- First polarimetric profiles of specific pulsars at 185 MHz using MWA
- Demonstration of high-time and frequency resolution observations

## Abstract

The Murchison Widefield Array is a low-frequency Square Kilometre Array precursor located at the Murchison Radio-astronomy Observatory in Western Australia. Primarily designed as an imaging telescope, but with a flexible signal path, the capabilities of this telescope have recently been extended to include off-line incoherent and tied-array beam formation using recorded antenna voltages. This has provided the capability for high-time and frequency resolution observations, including a pulsar science program. This paper describes the algorithms and pipeline that we have developed to form the tied array beam products from the summation of calibrated signals of the antenna elements, and presents example polarimetric profiles for PSRs J0437-4715 and J1900-2600 at 185 MHz.